FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Dwek, E
Arendt, RG
Bouchet, P
Burrows, DN
Challis, P
Danziger, IJ
De Buizer, JM
Gehrz, RD
Kirshner, RP
McCray, R
Park, S
Polomski, EF
Woodward, CE
AF Dwek, Eli
Arendt, Richard G.
Bouchet, Patrice
Burrows, David N.
Challis, Peter
Danziger, I. John
De Buizer, James M.
Gehrz, Robert D.
Kirshner, Robert P.
McCray, Richard
Park, Sangwook
Polomski, Elisha F.
Woodward, Charles E.
TI Infrared and X-ray evidence for circumstellar grain destruction by the
blast wave of supernova 1987A
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; infrared : general; ISM : individual (SNR 1987A);
supernova remnants; X-rays : general
ID SPITZER-SPACE-TELESCOPE; LARGE-MAGELLANIC-CLOUD; SN 1987A; CHANDRA
OBSERVATIONS; REMNANT 1987A; DUST; EMISSION; SN-1987A; SPECTROGRAPH;
ENVIRONMENT
AB Multiwavelength observations of supernova remnant 1987A show that its morphology and luminosity are rapidly changing at X-ray, optical, infrared (IR), and radio wavelengths as the blast wave from the explosion expands into the circumstellar equatorial ring, produced by mass loss from the progenitor star. The observed IR radiation arises from the interaction of dust grains that formed in mass outflow with the soft X-ray-emitting plasma component of the shocked gas. Spitzer Infrared Spectrograph spectra at 5-30 mu m taken on day 6190 since the explosion show that the emission arises from similar to 1.1 x 10(-6) M-circle dot of silicate grains radiating at a temperature of similar to 180(-15)(+20) K. Subsequent observations on day 7137 show that the IR flux had increased by a factor of 2 while maintaining an almost identical spectral shape. The observed IR-to-X-ray flux ratio (IRX) is consistent with that of a dusty plasma with standard Large Magellanic Cloud dust abundances. IRX has decreased by a factor of similar to 2 between days 6190 and 7137, providing the first direct observation of the ongoing destruction of dust in an expanding supernova blast wave on dynamic timescales. Detailed models consistent with the observed dust temperature, the ionization timescale of the soft X-ray emission component, and the evolution of IRX suggest that the radiating silicate grains are immersed in a 3.5 x 10(6) K plasma with a density of (0.3-1) x 10(4) cm(-3) and have a size distribution that is confined to a narrow range of radii between 0.023 and 0.22 mu m. Smaller grains may have been evaporated by the initial UV flash from the supernova.
C1 [Dwek, Eli] NASA, Goddard Space Flight Ctr, Observ Cosmol Lab, Greenbelt, MD 20771 USA.
[Arendt, Richard G.] NASA, Goddard Space Flight Ctr, SSAI, Greenbelt, MD 20771 USA.
[Bouchet, Patrice] CEA Saclay, Serv Astrophys, DSM, DAPNIA, F-91191 Gif Sur Yvette, France.
[Burrows, David N.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Challis, Peter; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Danziger, I. John] Osserv Astron Trieste, I-34131 Trieste, Italy.
[De Buizer, James M.] So Operat Ctr, Gemini Observ, La Serena, Chile.
[Gehrz, Robert D.; Polomski, Elisha F.; Woodward, Charles E.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA.
[McCray, Richard] Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA.
RP Dwek, E (reprint author), NASA, Goddard Space Flight Ctr, Observ Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
EM eli.dwek@nasa.gov; Patrice.Bouchet@cea.fr
RI Dwek, Eli/C-3995-2012;
OI Arendt, Richard/0000-0001-8403-8548
NR 30
TC 44
Z9 44
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2008
VL 676
IS 2
BP 1029
EP 1039
DI 10.1086/529038
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 281WW
UT WOS:000254530600020
ER
PT J
AU Thejappa, G
MacDowall, RJ
AF Thejappa, G.
MacDowall, R. J.
TI Effects of scattering on radio emission from the quiet Sun at low
frequencies
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE radio continuum : solar system; Sun : corona
ID INNER SOLAR-WIND; CORONAL SCATTERING; LARGE-SCALE; DECAMETER
WAVELENGTHS; DENSITY-FLUCTUATIONS; PLASMA FREQUENCY; TURBULENCE;
RADIATION; SPECTRUM; METER
AB The observations of the quiet Sun at meter and decameter wavelengths show that its brightness temperatures can be similar to 1 order of magnitude lower than the expected values of 10(6) K and the apparent diameters can be very large. We examine whether this unusual behavior is due to refraction in the smoothly varying coronal plasma and scattering by random density fluctuations using an improved Monte Carlo simulation technique. We use a three-dimensional model for the electron density, N-e, and a power-law spectrum for the density fluctuations with an exponential index of alpha. We consider two cases: (1) alpha = 11/3 (Kolmogorov spectrum), relative level of density fluctuations epsilon = Delta N-e/Ne = 0.1, and scale heights ranging from the inner scale l(i) = 684(N-e cm(-3))(-1/2) to outer scale l(o) = 10(6)l(i), and (2)alpha = 3 (flat spectrum), epsilon = 0.02, and scale heights ranging from 50 to 75 km. We consider the fluctuations to be anisotropic with axial ratios of similar to 10. The Kolmogorov type of fluctuations yield slightly lower brightness temperatures in comparison with those of a flat spectrum. The brightness temperature distributions, east-west diameters, and central brightness temperatures at various frequencies indicate that the refraction and scattering are probably the underlying reasons for the unusual behavior of the quiet-Sun radio emission. This study clearly demonstrates that Monte Carlo techniques can be very effective in extracting the coronal electron temperatures accurately from the radio data, provided the information about the density distributions and density fluctuations is known by some independent methods.
C1 [Thejappa, G.] Univ Maryland, Dept Astron, College Pk, MD 20716 USA.
[MacDowall, R. J.] NASA, Goddard Space Flight Ctr, College Pk, MD 20742 USA.
RP Thejappa, G (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20716 USA.
EM thejappa@astro.umd.edu; robert.macdowall@nasa.gov
RI MacDowall, Robert/D-2773-2012
NR 51
TC 25
Z9 25
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2008
VL 676
IS 2
BP 1338
EP 1345
DI 10.1086/528835
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 281WW
UT WOS:000254530600048
ER
PT J
AU Sabbi, E
Gallagher, JS
Smith, LJ
De Mello, DF
Mountain, M
AF Sabbi, E.
Gallagher, J. S.
Smith, L. J.
De Mello, D. F.
Mountain, M.
TI Holmberg IX: The nearest young galaxy
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies : evolution; galaxies : individual (Holmberg IX); galaxies :
interactions; galaxies : photometry
ID DWARF GALAXIES; STAR-FORMATION; NEUTRAL-HYDROGEN; M81 GROUP; SURFACE
PHOTOMETRY; IRREGULAR GALAXIES; HI SURVEY; BRIDGE
AB We present a study of the M81 companion dwarf irregular galaxy Holmberg IX using deep images taken with the Wide Field Channel of the Advanced Camera for Surveys on board the Hubble Space Telescope. Based on color-magnitude diagrams the resolved stellar population toward Holmberg IX contains numerous stars with ages of <= 200 Myr as well as older red giant stars. By charting the spatial distribution of the red giant stars and considering their inferred metallicities, we conclude that most of these older stars are associated with M81 or its tidal debris. At least 20% of the stellar mass in Holmberg IX was produced in the last similar to 200 Myr, giving it the youngest stellar population of any nearby galaxy. The location of Holmberg IX, its high gas content, and its youthful stellar population suggest that it is a tidal dwarf galaxy, perhaps formed during the last close passage of M82 around M81.
C1 [Sabbi, E.; Smith, L. J.; Mountain, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Sabbi, E.] Univ Heidelberg, Zentrum Astron, Astron Rechen Inst, Heidelberg, Germany.
[Sabbi, E.; Smith, L. J.] European Space Agcy, Res & Sci Support Dept, Baltimore, MD 21218 USA.
[Gallagher, J. S.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Smith, L. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[De Mello, D. F.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[De Mello, D. F.] Catholic Univ Amer, Washington, DC 20064 USA.
[De Mello, D. F.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
RP Sabbi, E (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
NR 30
TC 24
Z9 24
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 APR 1
PY 2008
VL 676
IS 2
BP L113
EP L117
DI 10.1086/587548
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 291ZK
UT WOS:000255235900006
ER
PT J
AU Dodson, R
Fomalont, EB
Wiik, K
Horiuchi, S
Hirabayashi, H
Edwards, PG
Murata, Y
Asaki, Y
Moellenbrock, GA
Scott, WK
Taylor, AR
Gurvits, LI
Paragi, Z
Frey, S
Shen, ZQ
Lovell, JEJ
Tingay, SJ
Rioja, MJ
Fodor, S
Lister, ML
Mosoni, L
Coldwell, G
Piner, BG
Yang, J
AF Dodson, R.
Fomalont, E. B.
Wiik, K.
Horiuchi, S.
Hirabayashi, H.
Edwards, P. G.
Murata, Y.
Asaki, Y.
Moellenbrock, G. A.
Scott, W. K.
Taylor, A. R.
Gurvits, L. I.
Paragi, Z.
Frey, S.
Shen, Z. -Q.
Lovell, J. E. J.
Tingay, S. J.
Rioja, M. J.
Fodor, S.
Lister, M. L.
Mosoni, L.
Coldwell, G.
Piner, B. G.
Yang, J.
TI The VSOP 5 GHz active galactic nucleus survey. V. Imaging results for
the remaining 140 sources
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE galaxies : active; radio continuum : galaxies; surveys
ID REFERENCE FRAME SOURCES; EXTRAGALACTIC RADIO-SOURCES; HEMISPHERE ICRF
SOURCES; VLBA OBSERVATIONS; SPACE VLBI; ASTROMETRIC SUITABILITY;
TEMPERATURE DISTRIBUTION; SCALE STRUCTURE; AGN SURVEY; QUASARS
AB In 1997 February, the Japanese radio astronomy satellite HALCA was launched to provide the space-bourne element for the VLBI Space Observatory Program (VSOP) mission. Approximately 25% of the mission time was dedicated to the VSOP survey of bright compact active galactic nuclei (AGNs) at 5 GHz. This paper, the fifth in the series, presents images and models for the remaining 140 sources not included in the third paper in the series, which contained 102 sources. For most sources, the plots of the (u, v) coverage, the visibility amplitude versus (u, v) distance, and the high-resolution image are presented. Model fit parameters to the major radio components are determined, and the brightness temperature of the core component for each source is calculated. The brightness temperature distributions for all of the sources in the VSOP AGN survey are discussed.
C1 [Dodson, R.; Wiik, K.; Hirabayashi, H.; Edwards, P. G.; Murata, Y.; Asaki, Y.; Moellenbrock, G. A.; Shen, Z. -Q.; Lovell, J. E. J.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Dodson, R.; Rioja, M. J.] Observ Astron Nacl, E-28803 Alcala De Henares, Spain.
[Fomalont, E. B.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Wiik, K.] Univ Turku, Tuorla Observ, FIN-21500 Piikkio, Finland.
[Horiuchi, S.] Natl Astron Observ, Mitaka, Tokyo 1818588, Japan.
[Horiuchi, S.; Tingay, S. J.; Fodor, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Horiuchi, S.; Tingay, S. J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Horiuchi, S.] Canberra Deep Space Commun Complex, Tuggeranong, ACT 2901, Australia.
[Hirabayashi, H.; Murata, Y.; Asaki, Y.] Grad Univ Adv Studies, Sch Phys Sci, Dept Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Edwards, P. G.; Lovell, J. E. J.] Commonwealth Sci & Ind Res Org, Australia Telescope Natl Facil, Epping, NSW 2122, Australia.
[Moellenbrock, G. A.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Scott, W. K.; Taylor, A. R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
[Gurvits, L. I.; Paragi, Z.; Yang, J.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands.
[Frey, S.; Mosoni, L.] FOMI Satellite Geodet Observ, H-1521 Budapest, Hungary.
[Shen, Z. -Q.; Yang, J.] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China.
[Paragi, Z.; Frey, S.] MTA Res Grp Phys Geodesy & Geodynam, H-1521 Budapest, Hungary.
[Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas, Australia.
[Tingay, S. J.] Curtin Univ Technol, Dept Imaging & Appl Phys, Perth, WA, Australia.
[Fodor, S.; Piner, B. G.] Whittier Coll, Dept Phys, Whittier, CA 90608 USA.
[Lister, M. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Mosoni, L.] MTA Konkoly Observ, H-1525 Budapest, Hungary.
[Coldwell, G.] Univ Nacl Cordoba, Astron Observ, RA-5000 Cordoba, Argentina.
RP Dodson, R (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan.
RI Tingay, Steven/B-5271-2013; Frey, Sandor/G-4465-2013
OI Frey, Sandor/0000-0003-3079-1889
NR 41
TC 25
Z9 25
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD APR
PY 2008
VL 175
IS 2
BP 314
EP 355
DI 10.1086/525025
PG 42
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 327WN
UT WOS:000257759300002
ER
PT J
AU Eisele, F
Davis, DD
Helmig, D
Oltmans, SJ
Neff, W
Huey, G
Tanner, D
Chen, G
Crawford, J
Arimoto, R
Buhr, M
Mauldin, L
Hutterli, M
Dibb, J
Blake, D
Brooks, SB
Johnson, B
Roberts, JM
Wang, YH
Tan, D
Flocke, F
AF Eisele, Fred
Davis, Douglas D.
Helmig, Detlev
Oltmans, Samuel J.
Neff, William
Huey, Greg
Tanner, David
Chen, Gao
Crawford, Jim
Arimoto, Richard
Buhr, Martin
Mauldin, Lee
Hutterli, Manuel
Dibb, Jack
Blake, D.
Brooks, Steven B.
Johnson, Bryan
Roberts, James M.
Wang, Yuhang
Tan, David
Flocke, Frank
TI Antarctic Tropospheric Chemistry Investigation (ANTCI) 2003 overview
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Editorial Material
DE antarctic photochemistry; south pole chemistry; nitric oxide; hydroxyl
radical; ozone
ID 8 GLACIAL CYCLES; ICE-CORE; SOUTH-POLE; METHANESULFONATE;
DIMETHYLSULFIDE; RECORD; FLUX
AB The Antarctic Tropospheric Chemistry Investigation (ANTCI) was carried out from late November to December 2003 with both extended ground-based and tethered balloon studies at Amundsen Scott Station, South Pole. ANTCI 2003 was the first of two Antarctic field studies with the primary goal of further exploring the active photochemistry of the South Pole region that was first identified in the previous Investigation of Sulfur Chemistry in the Antarctic Troposphere (ISCAT) program. Since ISCAT was fully ground-based, ANTCI 2003 goals included expanding chemical studies both vertically upward to investigate mixing and horizontally to better understand large-scale plateau NO, production and transport. Thus, in addition to ground-based experiments at South Pole, Twin Otter aircraft sampling took place out to hundreds of kilometers in several directions from the South Pole. These were designed to specifically address the issue of how representative past South Pole chemical measurements are of the surrounding high plateau region. The Twin Otterwas also used to make transects along the coast both north and south of McMurdo Station. The present paper summarizes the overall setting and results of this investigation and highlights the many new findings that were obtained. (C) 2007 Elsevier Ltd. All rights reserved.
C1 [Eisele, Fred; Flocke, Frank] Natl Ctr Atm Res, Atm Chem Div, Boulder, CO 80305 USA.
[Eisele, Fred; Davis, Douglas D.; Huey, Greg; Tanner, David; Wang, Yuhang; Tan, David] Georgia Inst Technol, Sch Earth & Atm Sci, Atlanta, GA 30332 USA.
[Helmig, Detlev] Univ Colorado, INSTAAR, Boulder, CO 80309 USA.
[Oltmans, Samuel J.; Neff, William; Roberts, James M.] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Chen, Gao; Crawford, Jim] NASA, Langley Res Ctr, Atm Sci Div, Hampton, VA 23681 USA.
[Arimoto, Richard] New Mexico State Univ, Carlsbad Envir Monitoring Res Ctr, Carlsbad, NM 88220 USA.
[Buhr, Martin] Air Qual Design Inc, Golden, CO 80403 USA.
[Hutterli, Manuel] British Antarctic Survey, Cambridge CB3 0ET, England.
[Hutterli, Manuel] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
[Dibb, Jack] Univ New Hampshire, Climate Change Res Ctr, Durham, NH 03824 USA.
[Blake, D.] Univ Calif Irvine, Dept Chem, Irvine, CA 92717 USA.
[Brooks, Steven B.] NOAA, Atmospher Turbulence & Diffus Div, Oak Ridge, TN USA.
[Johnson, Bryan] NOAA, Syst Res Lab, Global Monitoring Div, Boulder, CO 80305 USA.
RP Eisele, F (reprint author), Natl Ctr Atm Res, Atm Chem Div, Boulder, CO 80305 USA.
EM eisele@ucar.edu
RI Roberts, James/A-1082-2009; Crawford, James/L-6632-2013; Wang,
Yuhang/B-5578-2014; Neff, William/E-2725-2010; Manager, CSD
Publications/B-2789-2015
OI Roberts, James/0000-0002-8485-8172; Crawford, James/0000-0002-6982-0934;
Neff, William/0000-0003-4047-7076;
NR 28
TC 34
Z9 35
U1 0
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD APR
PY 2008
VL 42
IS 12
BP 2749
EP 2761
DI 10.1016/j.atmosenv.2007.04.013
PG 13
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 314YS
UT WOS:000256845700002
ER
PT J
AU Davis, DD
Seelig, J
Huey, G
Crawford, J
Chen, G
Wang, YH
Buhr, M
Helmig, D
Neff, W
Blake, D
Arimoto, R
Eisele, F
AF Davis, Douglas D.
Seelig, Jon
Huey, Greg
Crawford, Jim
Chen, Gao
Wang, Yuhang
Buhr, Marty
Helmig, Detlev
Neff, William
Blake, Don
Arimoto, Rich
Eisele, Fred
TI A reassessment of Antarctic plateau reactive nitrogen based on ANTO 2003
airborne and ground based measurements
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Antarctic plateau; reactive nitrogen; nitric oxide; airborne profiles;
nitrate; recycling; hydroxyl radicals; oxidizing canopy; ice core
chemical proxies
ID FROZEN NITRATE SOLUTIONS; NEAR-SURFACE SNOW; SOUTH-POLE; BOUNDARY-LAYER;
ICE CORES; PHOTOCHEMICAL PRODUCTION; ATMOSPHERIC CHEMISTRY; QUANTUM
YIELDS; ACID; NOX
AB The first airborne measurements of nitric oxide (NO) on the Antarctic plateau have demonstrated that the previously reported elevated levels of this species extend well beyond the immediate vicinity of South Pole. Although the current database is still relatively weak and critical laboratory experiments are still needed, the findings here suggest that the chemical uniqueness of the plateau may be substantially greater than first reported. For example, South Pole ground-based findings have provided new evidence showing that the dominant process driving the release of nitrogen from the snowpack during the spring/summer season (post-depositional loss) is photochemical in nature with evaporative processes playing a lesser role. There is also new evidence suggesting that nitrogen, in the form of nitrate, may undergo multiple recycling within a given photochemical season. Speculation here is that this may be a unique property of the plateau and much related to its having persistent cold temperatures even during summer. These conditions promote the efficient adsorption of molecules like HNO(3) (and very likely HO(2)NO(2)) onto snow-pack surface ice where we have hypothesized enhanced photochemical processing can occur, leading to the efficient release of NO(x) to the atmosphere. In addition, to these process-oriented tentative conclusions, the findings from the airborne studies, in conjunction with modeling exercises suggest a new paradigm for the plateau atmosphere. The near-surface atmosphere over this massive region can be viewed as serving as much more than a temporary reservoir or holding tank for imported chemical species. It defines an immense atmospheric chemical reactor which is capable of modifying the chemical characteristics of select atmospheric constituents. This reactor has most likely been in place over geological time, and may have led to the chemical modulation of some tracespecies now found in ice cores. Reactive nitrogen has played a critical role in both establishing and in maintaining this reactor. (C) 2007 Elsevier Ltd. All rights reserved.
C1 [Davis, Douglas D.; Seelig, Jon; Huey, Greg; Wang, Yuhang] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Crawford, Jim; Chen, Gao] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Buhr, Marty] Air Qual Design, Golden, CO 80403 USA.
[Helmig, Detlev] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
[Neff, William] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Blake, Don] Univ Calif Irvine, Dept Chem, Irvine, CA USA.
[Arimoto, Rich] New Mexico State Univ, Carsbad Environm Monitoring & Res Ctr, Carlsbad, NM 88220 USA.
[Eisele, Fred] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80303 USA.
RP Davis, DD (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
EM douglas.davis@eas.gatech.edu
RI Crawford, James/L-6632-2013; Wang, Yuhang/B-5578-2014; Neff,
William/E-2725-2010
OI Crawford, James/0000-0002-6982-0934; Neff, William/0000-0003-4047-7076
NR 71
TC 46
Z9 48
U1 0
U2 12
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 APR
PY 2008
VL 42
IS 12
BP 2831
EP 2848
DI 10.1016/j.atmosenv.2007.07.039
PG 18
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 314YS
UT WOS:000256845700008
ER
PT J
AU Chambers, LH
Alston, EJ
Phelps, CS
Moore, SW
Diones, DD
Oots, PC
Fischer, JD
Mims, FM
AF Chambers, L. H.
Alston, E. J.
Phelps, C. S.
Moore, S. W.
Diones, D. D.
Oots, P. C.
Fischer, J. D.
Mims, F. M., III
TI The MY NASA DATA project
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
C1 [Chambers, L. H.; Alston, E. J.] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
[Phelps, C. S.; Moore, S. W.; Diones, D. D.; Oots, P. C.; Fischer, J. D.] Sci Applicat Int Corp, Hampton, VA USA.
[Mims, F. M., III] Geronimo Creek Observ, Seguin, TX USA.
RP Chambers, LH (reprint author), NASA, Langley Res Ctr, Climate Sci Branch, MS 420, Hampton, VA 23681 USA.
EM l.h.chambers@larc.nasa.gov
NR 1
TC 0
Z9 0
U1 0
U2 1
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 APR
PY 2008
VL 89
IS 4
BP 437
EP 442
DI 10.1175/BAMS-89-4-437
PG 6
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 299YZ
UT WOS:000255792800008
ER
PT J
AU Teixeira, J
Stevens, B
Bretherton, CS
Cederwall, R
Doyle, JD
Golaz, JC
Holtslag, AAM
Klein, SA
Lundquist, JK
Randall, DA
Siebesma, AR
Soares, PMM
AF Teixeira, J.
Stevens, B.
Bretherton, C. S.
Cederwall, R.
Doyle, J. D.
Golaz, J. C.
Holtslag, A. A. M.
Klein, S. A.
Lundquist, J. K.
Randall, D. A.
Siebesma, A. R.
Soares, P. M. M.
TI Parameterization of the atmospheric boundary layer
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID LARGE-EDDY SIMULATIONS
C1 [Teixeira, J.] Naval Res Lab, Monterey, CA USA.
[Teixeira, J.] NATO Undersea Res Ctr, La Spezia, Italy.
[Stevens, B.] Univ Calif Los Angeles, Los Angeles, CA USA.
[Bretherton, C. S.] Univ Washington, Seattle, WA 98195 USA.
[Cederwall, R.; Klein, S. A.; Lundquist, J. K.] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Doyle, J. D.; Golaz, J. C.] USN, Res Lab, Monterey, CA USA.
[Golaz, J. C.] Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Holtslag, A. A. M.] Wageningen Univ, Wageningen, Netherlands.
[Randall, D. A.] Colorado State Univ, Ft Collins, CO 80523 USA.
[Siebesma, A. R.] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands.
[Soares, P. M. M.] Univ Lisbon, P-1699 Lisbon, Portugal.
[Soares, P. M. M.] Inst Super Engn Lisboa, Lisbon, Portugal.
RP Teixeira, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-237, Pasadena, CA 91109 USA.
EM Teixeira@ipl.nasa.gov
RI Randall, David/E-6113-2011; Soares, Pedro /K-6239-2012; Stevens,
Bjorn/A-1757-2013; Golaz, Jean-Christophe/D-5007-2014; Klein,
Stephen/H-4337-2016; Holtslag, Albert/B-7842-2010
OI Randall, David/0000-0001-6935-4112; Soares, Pedro /0000-0002-9155-5874;
Stevens, Bjorn/0000-0003-3795-0475; Golaz,
Jean-Christophe/0000-0003-1616-5435; Klein, Stephen/0000-0002-5476-858X;
Holtslag, Albert/0000-0003-0995-2481
NR 7
TC 31
Z9 31
U1 1
U2 12
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 APR
PY 2008
VL 89
IS 4
BP 453
EP 458
DI 10.1175/BAMS-89-4-453
PG 6
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 299YZ
UT WOS:000255792800011
ER
PT J
AU Creilson, JK
Pippin, MR
Henderson, BL
Ladd, IH
Fishman, J
Votapkova, D
Krpcova, I
AF Creilson, John K.
Pippin, Margaret R.
Henderson, Bryana L.
Ladd, Irene H.
Fishman, Jack
Votapkova, Dana
Krpcova, Ilona
TI Surface ozone measured at globe schools in the Czech Republic - A
demonstration of the importance of student contribution to the larger
science picture
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
AB Global Learning and Observations to Benefit the Environment (GLOBE) is a worldwide, hands-on, primary and secondary school-based education and science program, which is developed to give students a chance to perform real science by making measurements, analyzing data, and participating in research through collaboration with scientists. As part of the GLOBE Surface Ozone of the TEREZA Association in the Czech Republic, schools in the Czech Republic have been making and reporting daily measurements of surface ozone and surface meteorological data since 2001. Using a hand-held ozone monitor developed for GLOBE, students at several Czech schools have generated multiyear data records of surface ozone from 2001 to 2005. Analysis of the data shows that surface ozone levels were anomalously high during the summer of 2003 relative to other summers. These findings are consistent with the measurements of the European Environment Agency, which highlight the summer of 2003 as having exceptionally long-lasting and spatially extensive episodes of high surface ozone, especially during the first half of August. Further analysis of the summer's prevailing meteorology shows not only that it was one of the hottest on record, a finding also. seen in the student data, but the conditions for production of ozone were ideal. Findings such as these increase student, teacher, and scientist confidence in the utility of the GLOBE data for engaging budding scientists in the collection, analysis, and eventual interpretation of the data for inquiry-based education.
C1 [Creilson, John K.] John K Creilson Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Pippin, Margaret R.; Ladd, Irene H.; Fishman, Jack] NASA, Langley Res Ctr, Chem & Dynam Branch, Hampton, VA 23665 USA.
[Henderson, Bryana L.] NASA, Langley Res Ctr, Langley Aerosp Res Summer Scholars Program, Hampton, VA 23665 USA.
[Votapkova, Dana; Krpcova, Ilona] TEREZA Assoc, Prague, Czech Republic.
RP Creilson, JK (reprint author), John K Creilson Sci Syst & Applicat Inc, 1 Enterprise Pkway,Suite 200, Hampton, VA 23666 USA.
EM john.k.creilson@nasa.gov
NR 16
TC 1
Z9 1
U1 1
U2 4
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 APR
PY 2008
VL 89
IS 4
BP 505
EP +
DI 10.1175/BAMS-89-4-505
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 299YZ
UT WOS:000255792800016
ER
PT J
AU Ferrick, MG
Mulherin, ND
Haehnel, RB
Coutermarsh, BA
Durell, GD
Tantillo, TJ
Curtis, LA
Clair, TLS
Weiser, ES
Cano, RJ
Smith, TM
Martinez, EC
AF Ferrick, M. G.
Mulherin, N. D.
Haehnel, R. B.
Coutermarsh, B. A.
Durell, G. D.
Tantillo, T. J.
Curtis, L. A.
Clair, T. L. St.
Weiser, E. S.
Cano, R. J.
Smith, T. M.
Martinez, E. C.
TI Evaluation of ice release coatings at cryogenic temperature for the
space shuttle
SO COLD REGIONS SCIENCE AND TECHNOLOGY
LA English
DT Article
DE double lap shear testing; cryogenic temperatures; ice adhesion; ice
phobic coatings; space shuttle
AB The brackets that secure the liquid oxygen feed line to the external tank are known locations of frost and ice growth during the pre-launch period following fuel loading. This experimental program quantified the reduction in adhesion that resulted when ice phobic coatings were applied to test coupons that simulated the bracket surface. Double lap shear testing of coated and uncoated coupons provided robust test specimens and consistent load response patterns with exceptional resolution. Ice was grown as strong and consistently as possible for these tests and then subjected to temperature decreases comparable to those of the bracket. All tests were conducted at a constant temperature of -112 degrees C (-170 degrees F) and included uncoated controls with each group of samples. The program evolved in three phases. Phase I evaluated a wide range of coatings, and showed that Rain-X mixed with MP-55 powdered Teflon (RXM) was an outstanding coating to reduce ice adhesion to Koropon coated aluminum. Coating material retained on the ice surface following each test indicated failure in the coating and the potential for loss of effectiveness with repeated ice formation and release. Phase 2 evaluated modifications to RXM that might enhance durability while maintaining effectiveness. However, the modified mixtures did not improve coating durability or ice release. Phase 3 focused on the effects of mixing method, cure time, wiping off of excess coating, and coating resistance to weathering by water. A progressive coating loss again occurred through repeat test cycles, but performance generally improved. Results also indicated that cure times longer than 1.5 h prior to coating disturbance are needed for optimal performance. The MP-55 remaining on coupon surfaces after 3 cycles of testing and on one untested coupon from the same group was measured with XPS. The tested coupons retained slightly less MP-55 than the untested coupon, confirming the loss of coating. Contact angle analysis of these same coupons showed that the hydrophobic performance of the tested surfaces was largely preserved. Scanning electron microscopy with an energy dispersive spectroscopy elemental map indicated that the MP-55 was evenly dispersed throughout the coated surface, and abrasive wiping did not remove a significant portion of the Teflon. Test results suggest follow-up studies to refine the optimal coating formulation, mixing and application procedures, and understanding of reaction processes, cure time, and coating durability. Double lap shear testing and XPS analysis can quantify ice adhesion and coating profile thickness changes with cycling, and is capable of resolving these remaining issues. (c) 2007 Elsevier B.V. All rights reserved.
C1 [Ferrick, M. G.; Mulherin, N. D.; Haehnel, R. B.; Coutermarsh, B. A.; Durell, G. D.; Tantillo, T. J.] USA, Cold Reg Res & Engn Lab, Engineer Res & Dev Ctr, Hanover, NH 03755 USA.
[Clair, T. L. St.] Natl Inst Aerosp, Hampton, VA USA.
[Weiser, E. S.; Cano, R. J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Smith, T. M.] NASA, John F Kennedy Space Ctr, KSC, Kennedy Space Ctr, FL 32899 USA.
RP Ferrick, MG (reprint author), USA, Cold Reg Res & Engn Lab, Engineer Res & Dev Ctr, 72 Lyme Rd, Hanover, NH 03755 USA.
EM michael.g.ferrick@crdc.usace.army.mil
NR 5
TC 12
Z9 12
U1 3
U2 15
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0165-232X
J9 COLD REG SCI TECHNOL
JI Cold Reg. Sci. Tech.
PD APR
PY 2008
VL 52
IS 2
BP 224
EP 243
DI 10.1016/j.coldregions.2007.03.002
PG 20
WC Engineering, Environmental; Engineering, Civil; Geosciences,
Multidisciplinary
SC Engineering; Geology
GA 291YX
UT WOS:000255234600011
ER
PT J
AU Wahlgren, GM
AF Wahlgren, G. M.
TI Weak emission lines and peculiar stars
SO CONTRIBUTIONS OF THE ASTRONOMICAL OBSERVATORY SKALNATE PLESO
LA English
DT Article; Proceedings Paper
CT CP/AP Workshop 2007
CY SEP 10-14, 2007
CL Vienna, AUSTRIA
SP House Cafe Eat, Univ Wien, Power Horse Energy Drink, Kultur Niederosterreich, Wien Kultur, MKS, Ltrock Brot, EDV Serv Doppler, Rosch Frisch, OGA, Comp Delphin, Bank Austria Creditanstalt, J Syst Em Tech, UniCredit Grp
DE stars : B-type; stars : chemically peculiar; spectral lines : emission
ID MAIN-SEQUENCE STARS; X-RAY-EMISSION; B-TYPE STARS; MNII EMISSION;
SPECTRUM; CENTAURI; ANGSTROM; 3-CEN-A; ORIGIN
AB Weak emission lines (WELs) of metals are observed in sharp-lined spectra of mid- to late-B type stars. The WELs are detected over a range of element abundance and are found among both chemically-normal and chemically-peculiar stars. The characteristics of this ubiquitous phenomenon are reviewed and their potential for the study of inhomogeneous stellar atmospheres is presented.
C1 [Wahlgren, G. M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Wahlgren, G. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Wahlgren, GM (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
NR 18
TC 3
Z9 3
U1 0
U2 1
PU SLOVAK ACADEMY SCIENCES ASTRONOMICAL INST
PI TATRANSKA LOMINICA
PA SLOVAK ACADEMY SCIENCES ASTRONOMICAL INST, TATRANSKA LOMINICA, SK-059
60, SLOVAKIA
SN 1335-1842
J9 CONTRIB ASTRON OBS S
JI Contrib. Astron. Obs. S.
PD APR
PY 2008
VL 38
IS 2
BP 279
EP 284
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 310FJ
UT WOS:000256514000028
ER
PT J
AU Wahlgren, GM
Leckrone, DS
AF Wahlgren, G. M.
Leckrone, D. S.
TI Heavy elements in the hot-Am star HR 3383
SO CONTRIBUTIONS OF THE ASTRONOMICAL OBSERVATORY SKALNATE PLESO
LA English
DT Article; Proceedings Paper
CT CP/AP Workshop 2007
CY SEP 10-14, 2007
CL Vienna, AUSTRIA
SP House Cafe Eat, Univ Wien, Power Horse Energy Drink, Kultur Niederosterreich, Wien Kultur, MKS, Ltrock Brot, EDV Serv Doppler, Rosch Frisch, OGA, Comp Delphin, Bank Austria Creditanstalt, J Syst Em Tech, UniCredit Grp
DE stars : chemically peculiar; stars : abundances; techniques :
spectroscopic; ultraviolet : stars
AB The ultraviolet spectrum of the hot-Am star HR 3383 is analyzed through synthetic spectrum fitting for identification of lines from post iron-group elements. Spectral lines for a number of ions are detected for the first time in this star.
C1 [Wahlgren, G. M.] Catholic Univ Amer, Washington, DC 20064 USA.
[Wahlgren, G. M.; Leckrone, D. S.] NASA, Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA.
RP Wahlgren, GM (reprint author), Catholic Univ Amer, Washington, DC 20064 USA.
NR 4
TC 2
Z9 2
U1 0
U2 1
PU SLOVAK ACADEMY SCIENCES ASTRONOMICAL INST
PI TATRANSKA LOMINICA
PA SLOVAK ACADEMY SCIENCES ASTRONOMICAL INST, TATRANSKA LOMINICA, SK-059
60, SLOVAKIA
SN 1335-1842
J9 CONTRIB ASTRON OBS S
JI Contrib. Astron. Obs. S.
PD APR
PY 2008
VL 38
IS 2
BP 463
EP 464
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 310FJ
UT WOS:000256514000078
ER
PT J
AU Harvey, CC
Gangloff, M
King, T
Perry, CH
Roberts, DA
Thieman, JR
AF Harvey, Christopher C.
Gangloff, Michel
King, Todd
Perry, Christopher H.
Roberts, D. Aaron
Thieman, James R.
TI Virtual observatories for space and solar physics research
SO EARTH SCIENCE INFORMATICS
LA English
DT Review
DE Datamodel; Interoperability; Solar system plasma; SPASE; Virtual
observatory
AB As soon as the first data became available online over the Internet, it was obvious that different sites holding related datasets should appear to the end user as a single data system, even if the data itself is stored at multiple locations. To achieve this objective in the context of continuing parallel development of multiple data centres, in 2003 several actors in the realm of space plasmas created the international consortium Space Physics Archive Search and Extract (SPASE). Since 2005 US participation in SPASE has been supported by NASA, and early in 2006 NASA funded five new Virtual Observatories to cater for different aspects of solar system plasma science. This paper outlines the current status of the SPASE effort, the opportunities it offers, its specificities with respect to other parts of the astronomical virtual observatory, and the possibilities it offers for space weather.
C1 [Harvey, Christopher C.; Gangloff, Michel] CNRS CESR, Toulouse 04, France.
[King, Todd] Univ Calif Los Angeles, UCLA IGPP, Los Angeles, CA 90024 USA.
[Thieman, James R.] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, NASA GSFC, Greenbelt, MD 20771 USA.
[Perry, Christopher H.] Rutherford Appleton Lab, Didcot OX11 0WX, Oxon, England.
RP Harvey, CC (reprint author), CNRS CESR, 9 Ave Colonel Roche,BP 4346, Toulouse 04, France.
EM Harvey@cesr.fr; Gangloff@cesr.fr; tking@igpp.ucla.edu;
C.H.Perry@rl.ac.uk; aaron.roberts@nasa.gov; james.r.thieman@nasa.gov
NR 9
TC 3
Z9 3
U1 0
U2 1
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1865-0473
J9 EARTH SCI INFORM
JI Earth Sci. Inform.
PD APR
PY 2008
VL 1
IS 1
BP 5
EP 13
DI 10.1007/s12145-008-0008-1
PG 9
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA V15EM
UT WOS:000207785300003
ER
PT J
AU King, T
Merka, J
Walker, R
Joy, S
Narock, T
AF King, Todd
Merka, Jan
Walker, Raymond
Joy, Steven
Narock, Tom
TI The architecture of a multi-tiered virtual observatory
SO EARTH SCIENCE INFORMATICS
LA English
DT Article
DE Harvesting; Search registry; Topology; Virtual observatory
AB Virtual observatories are being established in a wide range a disciplines, supported by a variety of agencies. Groups such as the International Virtual Observatory Alliance (IVOA), Planetary Data System (PDS) and the Space Physics Archive Search and Extract (SPASE) consortium are defining metadata standards to aid in archiving and sharing of information resources. The role of the virtual observatories in this resource sharing environment is to locate available resources and help users find the resources they need and then gain access to those resources. There are many different existing resource providers from which virtual observatories must collect descriptions of their resources. These resource providers may have associations with other providers so the topology of information exchange can be complicated. We explore the variety of topologies that can exist and discuss methods of collecting (harvesting) information from providers such as scheduled and on-demand harvesting. We compare the benefits of each approach and look at the issues of management overhead, adaptability and timeliness. We also explore the benefits of combining searching and harvesting services as part of a comprehensive solution.
C1 [King, Todd; Walker, Raymond; Joy, Steven] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Merka, Jan; Narock, Tom] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Merka, Jan; Narock, Tom] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA.
RP King, T (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
EM tking@igpp.ucla.edu
OI Narock, Tom/0000-0002-9785-4496
FU National Aeronautics and Space Administration [NNX07AC95G, NNX07AC93G];
Virtual Observatories for Solar and Space Physics Data [S3CVO]
FX This work was supported by the National Aeronautics and Space
Administration under Grants No. NNX07AC95G and NNX07AC93G and issued
through the Virtual Observatories for Solar and Space Physics Data
(S3CVO). The UCLA/IGPP publication number is 6359.
NR 13
TC 4
Z9 4
U1 0
U2 2
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1865-0473
J9 EARTH SCI INFORM
JI Earth Sci. Inform.
PD APR
PY 2008
VL 1
IS 1
BP 21
EP 28
DI 10.1007/s12145-008-0006-3
PG 8
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA V15EM
UT WOS:000207785300005
ER
PT J
AU King, T
Narock, T
Walker, R
Merka, J
Joy, S
AF King, Todd
Narock, Tom
Walker, Raymond
Merka, Jan
Joy, Steven
TI A brave new (virtual) world: distributed searches, relevance scoring and
facets
SO EARTH SCIENCE INFORMATICS
LA English
DT Article
DE Relevance scoring facets virtual observatory search
AB Our ability to deal with complex systems has improved through information system research which includes improved modeling (both data and system), the use of semantics and advances in distributed computing. The past decade has seen an explosion in the amount and variety of geosciences data and the emergence of true open data repositories through which scientists can freely access this data. Those data are found in thousands of repositories located around the world. Virtual observatories have been created to address the challenge of helping scientists search those repositories to find and access the required data. This challenge is been addressed by using technologies such as the Internet (with ample connectivity and bandwidth), the Web, cheap computing power, cheap storage and standards for critical components. Many scientific disciplines are developing virtual observatories. Yet some of the most compelling science questions cross multiple domains. While semantics can provide cross domain reasoning, often the first step in answering a question is determining what resources are available which may be relevant to a topic. The topic can be expressed as simple phrases or word sequences. Using a common relevance scoring method at all locations can enable a federated search across loosely coupled providers. The results of which can be organized into facets to aid the user in selecting the most promising resources with which to pursue the scientific investigation. We describe an approach to developing and deploying relevance scoring methods and faceted results in this brave new (virtual) world. We have found that a scoring method which considers both the presence of terms and the proximity of these terms relative to the order of the terms in the query improves the assessment of relevance. We call this Term Presence-Proximity (TPP) scoring and describe a method for calculating a normalized score. TPP scoring compares favorably with other scoring approaches.
C1 [King, Todd; Walker, Raymond; Joy, Steven] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Narock, Tom; Merka, Jan] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Narock, Tom; Merka, Jan] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA.
RP King, T (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
EM tking@igpp.ucla.edu
FU National Aeronautics and Space Administration [NNX07AC95G, NNX07AC93G];
Virtual Observatories for Solar and Space Physics Data [S3CVO]
FX This work was supported by the National Aeronautics and Space
Administration under Grants No. NNX07AC95G and NNX07AC93G and issued
through the Virtual Observatories for Solar and Space Physics Data
(S3CVO). The UCLA/IGPP publication number is 6360.
NR 10
TC 5
Z9 5
U1 0
U2 1
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1865-0473
J9 EARTH SCI INFORM
JI Earth Sci. Inform.
PD APR
PY 2008
VL 1
IS 1
BP 29
EP 34
DI 10.1007/s12145-008-0002-7
PG 6
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA V15EM
UT WOS:000207785300006
ER
PT J
AU Merka, J
Narock, TW
Szabo, A
AF Merka, Jan
Narock, Thomas W.
Szabo, Adam
TI Navigating through SPASE to heliospheric and magnetospheric data
SO EARTH SCIENCE INFORMATICS
LA English
DT Article
DE Middleware; SPASE metadata; VHO; Virtual observatory search; VMO
AB Virtual observatories have been introduced by the astrophysics community as an environment connecting distributed data sources with a unified interface. The heliophysics community soon recognized that they faced a similar problem of many distributed data sets with varying amount of information about them and several discipline specific virtual observatories have been established. Two of them, the virtual heliospheric observatory (VHO) and the virtual magnetospheric observatory (VMO), share a common architecture design with development efforts oriented towards a structured data search. This paper describes the VHO/VMO middleware and its components from metadata preparation and processing to the user interface.
C1 [Merka, Jan; Narock, Thomas W.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA.
[Merka, Jan; Narock, Thomas W.; Szabo, Adam] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA.
RP Merka, J (reprint author), Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA.
EM jan.merka@nasa.gov
OI Narock, Tom/0000-0002-9785-4496
FU National Aeronautics and Space Administration [NNX07AC95G]; virtual
observatories for Solar and Space Physics Data [S3CVO]
FX This work was supported by the National Aeronautics and Space
Administration under Grant No. NNX07AC95G issued through the virtual
observatories for Solar and Space Physics Data (S3CVO).
NR 9
TC 5
Z9 5
U1 0
U2 2
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1865-0473
J9 EARTH SCI INFORM
JI Earth Sci. Inform.
PD APR
PY 2008
VL 1
IS 1
BP 35
EP 42
DI 10.1007/s12145-008-0004-5
PG 8
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA V15EM
UT WOS:000207785300007
ER
PT J
AU Narock, TW
King, T
AF Narock, T. W.
King, T.
TI Developing a SPASE Query Language
SO EARTH SCIENCE INFORMATICS
LA English
DT Article
DE Virtual observatory; Data search; Data retrieval; Virtual observatory
communication
AB The advent of the Virtual Observatory has begun an evolution in the space physics data environment. A number of nascent and discipline specific Virtual Observatories have started to emerge with an emphasis on data search and retrieval. As this new data environment takes shape an emphasis will be placed on interdisciplinary communication in attempts to address large scale and global problems. To this end we formulate the development of a query language to facilitate Virtual Observatory to Virtual Observatory communication. Furthermore, we outline the goals of such a language, how it would work and how existing community efforts can be leveraged to speed the development of this query language.
C1 [Narock, T. W.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Narock, T. W.] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA.
[King, T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
RP Narock, TW (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
EM Thomas.W.Narock@nasa.gov
OI Narock, Tom/0000-0002-9785-4496
FU NASA Research Opportunities in Space and Earth Sciences [NNX07AC95G]
FX This work was supported under NASA Research Opportunities in Space and
Earth Sciences grant NNX07AC95G. The authors would like to thank the
SPASE consortium and Virtual Observatory members for helpful discussions
during the development of this work.
NR 7
TC 4
Z9 4
U1 0
U2 0
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1865-0473
J9 EARTH SCI INFORM
JI Earth Sci. Inform.
PD APR
PY 2008
VL 1
IS 1
BP 43
EP 48
DI 10.1007/s12145-008-0007-2
PG 6
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA V15EM
UT WOS:000207785300008
ER
PT J
AU Whitacre, JF
Valdez, TI
Narayanan, SR
AF Whitacre, J. F.
Valdez, T. I.
Narayanan, S. R.
TI A high-throughput study of PtNiZr catalysts for application in PEM fuel
cells
SO ELECTROCHIMICA ACTA
LA English
DT Article
DE PEM fuel cell catalyst; PtNi; PtNiZr; combinatorial; thin film; sputter
deposition
ID OXYGEN REDUCTION REACTION; ALLOY ELECTRODES; ELECTROCATALYSTS;
ELECTROREDUCTION; SURFACES; FE; NI; CO
AB The effects of adding Zr to PtNi oxygen reduction reaction (ORR) electrocatalyst alloys were examined in a study aimed at probing the possibility of creating catalysts with enhanced resistance to corrosion in a PEM fuel cell environment. Samples consisting of pure Pt or PtNiZr alloys with a range of compositions (not exceeding 11 at.% Zr) were fabricated using co-sputter deposition. A high-throughput fabrication approach was used wherein 18 distinct thin film catalyst alloy samples with varying compositions were deposited onto a large-area substrate with individual Au current collector structures. A multi-channel pseudo-potentiostat allowed for the simultaneous quantitative study of catalytic activity for all 18 electrodes in a single test bath, a first for the study of ORR electrocatalysts. A properly stirred oxygenated I M H2SO4 electrolyte solution was used to provide each electrode with a steady-state flow of reactants during electrochemical evaluation. The onset potentials, absolute current density values, and Tafel analysis data obtained using this technique were compared with literature reports. The analyses showed that most PtNiZr alloys tested offered improvements over pure Pt, however those surfaces with a high mole fraction (>4 at.%) of Zr exhibited reduced activity that was roughly inversely correlated to the amount of Zr present. Film composition, morphology, and crystallographic properties were examined using X-ray energy dispersive spectroscopy (XEDS), X-ray photoelectron spectroscopy (XPS), SEM, and synchrotron X-ray diffraction. These data were then correlated with electrochemical data to elucidate the relationships between composition, structure, and relative performance for this ternary system. (c) 2007 Elsevier Ltd. All rights reserved.
C1 [Whitacre, J. F.] Carnegie Mellon Univ, Dept Mat Sci & Engn, Pittsburgh, PA 15213 USA.
[Whitacre, J. F.] Carnegie Mellon Univ, Dept Engn & Publ Policy, Pittsburgh, PA 15213 USA.
[Valdez, T. I.; Narayanan, S. R.] CALTECH, Jet Prop Lab, Electrochem Technol Grp, Pasadena, CA 91109 USA.
RP Whitacre, JF (reprint author), Carnegie Mellon Univ, Dept Mat Sci & Engn, 4323 Wean Hall, Pittsburgh, PA 15213 USA.
EM whitacre@andrew.cinu.edu
NR 20
TC 20
Z9 20
U1 3
U2 23
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0013-4686
J9 ELECTROCHIM ACTA
JI Electrochim. Acta
PD APR 1
PY 2008
VL 53
IS 10
BP 3680
EP 3689
DI 10.1016/j.electacta.2007.12.017
PG 10
WC Electrochemistry
SC Electrochemistry
GA 279KO
UT WOS:000254354300015
ER
PT J
AU Menon, S
Unger, N
Koch, D
Francis, J
Garrett, T
Sednev, I
Shindell, D
Streets, D
AF Menon, Surabi
Unger, Nadine
Koch, Dorothy
Francis, Jennifer
Garrett, Tim
Sednev, Igor
Shindell, Drew
Streets, David
TI Aerosol climate effects and air quality impacts from 1980 to 2030
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE aerosols; ozone; radiative forcing
ID BLACK CARBON; EMISSIONS; CLOUDS; SENSITIVITY; SIMULATIONS; OZONE; INDIA;
CHINA
AB We investigate aerosol effects on climate for 1980, 1995 ( meant to reflect present day) and 2030 using the NASA Goddard Institute for Space Studies climate model coupled to an on-line aerosol source and transport model with interactive oxidant and aerosol chemistry. Aerosols simulated include sulfates, organic matter ( OM), black carbon ( BC), sea-salt and dust and, additionally, the amount of tropospheric ozone is calculated, allowing us to estimate both changes to air quality and climate for different time periods and emission amounts. We include both the direct aerosol effect and indirect aerosol effects for liquid-phase clouds. Future changes for the 2030 A1B scenario are examined, focusing on the Arctic and Asia, since changes are pronounced in these regions. Our results for the different time periods include both emission changes and physical climate changes. We find that the aerosol indirect effect ( AIE) has a large impact on photochemical processing, decreasing ozone amount and ozone forcing, especially for the future ( 2030-1995). Ozone forcings increase from 0 to 0.12 W m(-2) and the total aerosol forcing decreases from -0.10 to -0.94W m(-2) ( AIE decreases from -0.13 to -0.68W m(-2)) for 1995-1980 versus 2030-1995. Over the Arctic we find that compared to ozone and the direct aerosol effect, the AIE contributes the most to net radiative flux changes. The AIE, calculated for 1995-1980, is positive (1.0 W m(-2)), but the magnitude decreases (-0.3Wm(-2)) considerably for the future scenario. Over Asia, we evaluate the role of biofuel- and transportation- based emissions ( for BC and OM) via a scenario ( 2030A) that includes a projected increase ( factor of 2) in biofuel- and transport-based emissions for 2030 A1B over Asia. Projected changes from present day due to the 2030A emissions versus 2030 A1B are a factor of 4 decrease in summertime precipitation in Asia. Our results are sensitive to emissions used. Uncertainty in present-day emissions suggests that future climate projections warrant particular scrutiny.
C1 [Menon, Surabi; Sednev, Igor] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
[Unger, Nadine; Koch, Dorothy; Shindell, Drew] Columbia Univ, New York, NY USA.
[Unger, Nadine; Koch, Dorothy; Shindell, Drew] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Francis, Jennifer] Rutgers State Univ, New Brunswick, NJ 08903 USA.
[Garrett, Tim] Univ Utah, Salt Lake City, UT USA.
[Streets, David] Argonne Natl Lab, Argonne, IL 60439 USA.
RP Menon, S (reprint author), Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
EM smenon@lbl.gov
RI Shindell, Drew/D-4636-2012; Unger, Nadine/M-9360-2015;
OI Streets, David/0000-0002-0223-1350
NR 38
TC 30
Z9 31
U1 1
U2 24
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD APR-JUN
PY 2008
VL 3
IS 2
AR 024004
DI 10.1088/1748-9326/3/2/024004
PG 12
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 319PX
UT WOS:000257177300005
ER
PT J
AU Hays, MD
Beck, L
Barfield, P
Lavrich, RJ
Dong, YJ
Vander Wal, RL
AF Hays, Michael D.
Beck, Lee
Barfield, Pamela
Lavrich, Richard J.
Dong, Yuanji
Vander Wal, Randy L.
TI Physical and chemical characterization of residential oil boiler
emissions
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID FINE-PARTICLE EMISSIONS; ULTRAFINE PARTICLES; FUEL-OIL; SIZE
DISTRIBUTIONS; AEROSOL EMISSIONS; COMBUSTION; SAMPLER; MATTER; MASS
AB The toxicity of emissions from the combustion of home heating oil coupled with the regional proximity and seasonal use of residential oil boilers (ROB) is an important public health concern. Yet scant physical and chemical information about the emissions from this source is available for climate and air quality modeling and for improving our understanding of aerosol-related human health effects. The gas- and particle-phase emissions from an active ROB firing distillate fuel oil (commonly known as diesel fuel) were evaluated to address this deficiency. Ion chromatography of impactor samples showed that the ultrafine ROB aerosol emissions were similar to 45% (w/w) sulfate. Gas chromatography-mass spectrometry detected various n-alkanes at trace levels, sometimes in accumulation mode particles, and out of phase with the size distributions of aerosol mass and sulfate. The carbonaceous matter in the ROB aerosol was primarily light-adsorbing elemental carbon. Gas chromatography-atomic emission spectroscopy measured a previously unrecognized organosulfur compound group in the ROB aerosol emissions. High-resolution transmission electron microscopy of ROB soot indicated the presence of a highly ordered primary particle nanostructure embedded in larger aggregates. Organic gas emissions were measured using EPA Methods TO-15 and TO-11A. The ROB emitted volatile oxygenates (8 mg/(kg of oil burned)) and olefins (5 mg/(kg of oil burned)) mostly unrelated to the base fuel composition. In the final analysis, the ROB tested was a source of numerous hazardous air pollutants as defined in the Clean Air Act Amendments. Approximations conducted using emissions data from the ROB tests show relatively low contributions to a regional-level anthropogenic emissions inventory for volitile organic compounds, PM2.5, and SO2 mass.
C1 [Hays, Michael D.; Beck, Lee; Barfield, Pamela; Lavrich, Richard J.] US EPA, Natl Risk Management Res Lab, Res Triangle Pk, NC 27711 USA.
[Dong, Yuanji] ARCADIS, Res Triangle Pk, NC 27711 USA.
[Vander Wal, Randy L.] NASA, Glenn Res Ctr, Univ Space Res Assoc, Cleveland, OH 44135 USA.
RP Hays, MD (reprint author), US EPA, Natl Risk Management Res Lab, Res Triangle Pk, NC 27711 USA.
EM hays.michael@epa.gov
RI Hays, Michael/E-6801-2013; Wang, Linden/M-6617-2014
OI Hays, Michael/0000-0002-4029-8660;
NR 38
TC 13
Z9 13
U1 3
U2 29
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
EI 1520-5851
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD APR 1
PY 2008
VL 42
IS 7
BP 2496
EP 2502
DI 10.1021/es071598e
PG 7
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA 281JN
UT WOS:000254492800047
PM 18504987
ER
PT J
AU Gustafsson, T
Osterlund, T
von Walden, F
Trappe, T
Linnehan, R
Tesch, P
AF Gustafsson, Thomas
Osterlund, Ted
von Walden, Ferdinand
Trappe, Todd
Linnehan, Rick
Tesch, Per
TI Three days of unloading induces pre-translational changes in human
skeletal muscle
SO FASEB JOURNAL
LA English
DT Meeting Abstract
C1 [Gustafsson, Thomas; Osterlund, Ted; von Walden, Ferdinand; Tesch, Per] Karolinska Inst, Stockholm, Sweden.
[Osterlund, Ted; Tesch, Per] Mid Univ, Ostersund, Sweden.
[Trappe, Todd] Ball State Univ, Muncie, IN 47306 USA.
[Linnehan, Rick] NASA, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2008
VL 22
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA V25GZ
UT WOS:000208467807289
ER
PT J
AU Hitchcox, K
Wolf, M
Zwart, SR
Smith, SM
AF Hitchcox, Kristen
Wolf, Megan
Zwart, Sara R.
Smith, Scott M.
TI Stability of biochemical analytes in blood specimens subjected to
delayed processing
SO FASEB JOURNAL
LA English
DT Meeting Abstract
C1 [Hitchcox, Kristen] Colby Coll, Waterville, ME 04901 USA.
[Zwart, Sara R.] Univ Space Res Assoc, Houston, TX USA.
[Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
NR 0
TC 0
Z9 0
U1 1
U2 1
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2008
VL 22
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA V25GZ
UT WOS:000208467806518
ER
PT J
AU Howarth, MS
Moore, FB
Hinghofer-Szalkay, H
Jezova, D
Diedrich, A
Ferris, M
Schlegel, TT
Patwardhan, AR
Knapp, CF
Evans, JM
AF Howarth, Mark S.
Moore, Fritz B.
Hinghofer-Szalkay, Helmut
Jezova, Daniela
Diedrich, Andre'
Ferris, Mead
Schlegel, Todd T.
Patwardhan, Abhijit R.
Knapp, Charles F.
Evans, Joyce M.
TI Thoracic impedance as a potential indicator of Gz-induced presyncope
SO FASEB JOURNAL
LA English
DT Meeting Abstract
C1 [Howarth, Mark S.; Ferris, Mead; Patwardhan, Abhijit R.; Knapp, Charles F.; Evans, Joyce M.] Univ Kentucky, Ctr Biomed Engn, Lexington, KY 40506 USA.
[Moore, Fritz B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Hinghofer-Szalkay, Helmut] Inst Adapt & Spaceflight Physiol, Graz, Austria.
[Jezova, Daniela] Inst Expt Endocrinol SAS, Bratislava, Slovakia.
[Diedrich, Andre'] Vanderbilt Univ, Auton Dysfunct Ctr, Nashville, TN USA.
[Schlegel, Todd T.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2008
VL 22
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA V25GZ
UT WOS:000208467807204
ER
PT J
AU Liang, MTC
Lewis, KM
Spalding, TW
Bassin, SL
Arnaud, SB
AF Liang, Michael T. C.
Lewis, Kevin M.
Spalding, Thomas W.
Bassin, Stan L.
Arnaud, Sara B.
TI Bone Bending Stiffness and BMD in trained Cyclists, Runners and
Untrained Men
SO FASEB JOURNAL
LA English
DT Meeting Abstract
C1 [Liang, Michael T. C.; Lewis, Kevin M.; Spalding, Thomas W.] Calif State Polytech Univ Pomona, Pomona, CA 91768 USA.
[Bassin, Stan L.] UCI Med Ctr, Inst Clin & Translat Sci, Irvine, CA USA.
[Arnaud, Sara B.] NASA AMES, Life Sci Div, Moffett Field, CA USA.
NR 0
TC 0
Z9 0
U1 0
U2 2
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2008
VL 22
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA V25GY
UT WOS:000208467700703
ER
PT J
AU Macias, BR
Schneider, S
Lee, SMC
Guinet, P
Hughson, R
Smith, S
Watenpaugh, D
Hargens, A
AF Macias, Brandon Richard
Schneider, Suzanne
Lee, Stuart M. C.
Guinet, Patrick
Hughson, Richard
Smith, Scott
Watenpaugh, Donald
Hargens, Alan
TI WISE-2005: Lower Body Negative Pressure Treadmill and Resistive Exercise
Countermeasures Maintain Physiologic Function in Women during 60-days of
Simulated Microgravity
SO FASEB JOURNAL
LA English
DT Meeting Abstract
C1 [Macias, Brandon Richard; Guinet, Patrick; Watenpaugh, Donald; Hargens, Alan] Univ Calif San Diego, San Diego, CA 92103 USA.
[Schneider, Suzanne] Univ New Mexico, Albuquerque, NM 87131 USA.
[Lee, Stuart M. C.] Wyle Labs, Houston, TX USA.
[Hughson, Richard] Univ Waterloo, Waterloo, ON N2L 3G1, Canada.
[Smith, Scott] NASA, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2008
VL 22
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA V25GZ
UT WOS:000208467809411
ER
PT J
AU Meng, M
Stenger, M
Platts, S
Feiveson, A
Natapoff, A
Knapp, C
Evans, J
Paloski, W
AF Meng, Martha
Stenger, Michael
Platts, Steven
Feiveson, Al
Natapoff, Alan
Knapp, Charles
Evans, Joyce
Paloski, William
TI Cardiovascular mechanisms are maintained by intermittent artificial
gravity exposure during bed rest deconditioning
SO FASEB JOURNAL
LA English
DT Meeting Abstract
C1 [Meng, Martha; Knapp, Charles; Evans, Joyce] Univ Kentucky, Ctr Biomed Engn, Lexington, KY 40506 USA.
[Stenger, Michael] Wyle Labs, Houston, TX USA.
[Platts, Steven; Feiveson, Al; Paloski, William] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Natapoff, Alan] MIT, Cambridge, MA 02139 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2008
VL 22
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA V25GZ
UT WOS:000208467806568
ER
PT J
AU Smith, SM
Gardner, K
Locke, J
Zwart, SR
AF Smith, Scott M.
Gardner, Keri
Locke, James
Zwart, Sara R.
TI Efficacy of vitamin D supplementation in an Antarctic ground analog of
space flight
SO FASEB JOURNAL
LA English
DT Meeting Abstract
C1 [Smith, Scott M.; Locke, James] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Gardner, Keri] Univ Calif Los Angeles, Los Angeles, CA USA.
[Zwart, Sara R.] Univ Space Res Assoc, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2008
VL 22
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA V25GZ
UT WOS:000208467808715
ER
PT J
AU Zwart, SR
Smith, SM
AF Zwart, Sara R.
Smith, Scott M.
TI Oxidative Damage during a 10-to 12-d Saturation Dive
SO FASEB JOURNAL
LA English
DT Meeting Abstract
C1 [Zwart, Sara R.] Univ Space Res Assoc, Houston, TX USA.
[Smith, Scott M.] NASA Johnson Space Ctr, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2008
VL 22
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA V25GZ
UT WOS:000208467808689
ER
PT J
AU Orr, JW
Hawkins, S
AF Orr, James W.
Hawkins, Sharon
TI Species of the rougheye rockfish complex: resurrection of Sebastes
melanostictus (Matsubara, 1934) and a redescription of Sebastes
aleutianus (Jordan and Evermann, 1898) (Teleostei : Scorpaeniformes)
SO FISHERY BULLETIN
LA English
DT Article
ID NORTH PACIFIC-OCEAN; SYSTEMATICS
AB The widespread and commercially important rougheye rockfish, Sebastes aleutianus (Jordan and Evermann, 1898), has been considered a single variable species, with light- and dark-colored forms, found on the outer continental shelf and upper slope of the North Pacific Ocean. Genetic analysis of 124 specimens verified the presence of two species in new specimens collected from Alaska to Oregon, and the two species were analyzed for distinguishing color patterns and morphological characters. Characters distinguishing the two were extended to an analysis of 215 additional formalin-fixed specimens representing their geographic ranges. Sebastes aleutianus is pale, often has dark mottling on the dorsum in diffuse bands, and does not have distinct dark spots on the spinous dorsal fin; it ranges from the eastern Aleutian Islands and southeastern Bering Sea to California. Sebastes melanostictus (Matsubara, 1934), the blackspotted rockfish, ranges from central Japan, through the Aleutian Islands and Bering Sea, to southern California. It is darker overall and spotting is nearly always present on the spinous dorsal fin. Sebastes swifti (Evermann and Goldsborough, 1907) is a synonym of S. aleutianus; S. kawaradae (Matsubara, 1934) is a synonym of S. melanostictus. The subgenus Zalopyr is restricted to S. aleutianus and S. melanostictus. Nomenclatural synonymies, diagnoses, descriptions, and distributions are provided for each species.
C1 [Orr, James W.] NOAA, Natl Marine Fisheries Serv, Resource Assessment & Conservat Engn Div, Alaska Fisheries Sci Ctr, Seattle, WA 98115 USA.
[Hawkins, Sharon] NOAA, Ted Stevens Marine Res Inst, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr,Auke Bay Labs, Juneau, AK 99801 USA.
RP Orr, JW (reprint author), NOAA, Natl Marine Fisheries Serv, Resource Assessment & Conservat Engn Div, Alaska Fisheries Sci Ctr, 7600 Sand Point Way NE, Seattle, WA 98115 USA.
EM James.Orr@noaa.gov
NR 60
TC 14
Z9 19
U1 0
U2 2
PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE
PI SEATTLE
PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA
SN 0090-0656
J9 FISH B-NOAA
JI Fish. Bull.
PD APR
PY 2008
VL 106
IS 2
BP 111
EP 134
PG 24
WC Fisheries
SC Fisheries
GA 299CQ
UT WOS:000255733800001
ER
PT J
AU Parnel, MM
Emmett, RL
Brodeur, RD
AF Parnel, Maria M.
Emmett, Robert L.
Brodeur, Richard D.
TI Ichthyoplankton community in the Columbia River plume off Oregon:
effects of fluctuating oceanographic conditions
SO FISHERY BULLETIN
LA English
DT Article
ID CALIFORNIA CURRENT; NORTHEAST PACIFIC; JUVENILE SALMONIDS; FISH
PRODUCTION; ABUNDANCE; CLIMATE; LARVAL; OCEAN; ZONE; RECRUITMENT
AB Ichthyoplankton samples were collected at approximately 2-week intervals, primarily during spring and summer 1999-2004, from two stations located 20 and 30 km from shore near the Columbia River, Oregon. Northern anchovy (Engraulis mordax) was the most abundant species collected, and was the primary species associated with summer upwelling conditions, but it showed significant interannual and seasonal fluctuations in abundance and occurrence. Other abundant taxa included sanddabs (Citharichthys spp.), English sole (Parophrys vetulus), and blaeksmelts (Bathylagidae). Two-way cluster analysis revealed strong species associations based primarily on season (before or after the spring transition date). Ichthyoplankton abundances were compared to biological and environmental data, and egg and larvae abundances were found to be most correlated with sea surface temperature. The Pacific Decadal Oscillation changed sign (from negative to positive) in late 2002 and indicated overall warmer conditions in the North Pacific Ocean. Climate change is expected to alter ocean upwelling, temperatures, and Columbia River flows, and consequently fish eggs and larvae distributions and survival. Long-term research is needed to identify how ichthyoplankton and fish recruitment are affected by regional and large-scale oceanographic processes.
C1 [Parnel, Maria M.; Emmett, Robert L.; Brodeur, Richard D.] Hatfield Marine Sci Ctr, Natl Marine Fisheries Serv, Natl Ocean & Atmospher Adm, Newport, OR USA.
RP Parnel, MM (reprint author), Hatfield Marine Sci Ctr, Natl Marine Fisheries Serv, Natl Ocean & Atmospher Adm, 2030 S Marine Sci Dr, Newport, OR USA.
EM Robert.Emmett@noaa.gov
NR 62
TC 20
Z9 20
U1 3
U2 9
PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE
PI SEATTLE
PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA
SN 0090-0656
J9 FISH B-NOAA
JI Fish. Bull.
PD APR
PY 2008
VL 106
IS 2
BP 161
EP 173
PG 13
WC Fisheries
SC Fisheries
GA 299CQ
UT WOS:000255733800005
ER
PT J
AU McKean, JA
Isaak, DJ
Wright, CW
AF McKean, Jim A.
Isaak, Dan J.
Wright, Charles W.
TI Geomorphic controls on salmon nesting patterns described by a new,
narrow-beam terrestrial-aquatic lidar
SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT
LA English
DT Article
ID LANDSCAPES
AB Riverine aquatic biodiversity is rapidly being lost worldwide, but preservation efforts are hampered, in part because studies of these dynamic environments are limited by cost and logistics to small local surveys. Full understanding of stream ecosystems requires precise, high-resolution mapping of entire stream networks and adjacent landforms. We use a narrow-beam, water-penetrating, green lidar system to continuously map 10 km of a mountain stream channel, including its floodplain topography, and wavelet analyses to investigate spatial patterns of channel morphology and salmon spawning. Results suggest the broadest fluvial domains are a legacy of approximately 15 000 years of post-glacial valley evolution and that local pool-riffle channel topography is controlled by contemporary hydraulics operating on this broad template. Salmon spawning patterns closely reflect these hierarchical physical domains, demonstrating how geomorphic history can influence modem distributions of aquatic habitat and organisms. The new terrestrial-aquatic lidar could catalyze rapid advances in understanding, managing, and monitoring of valuable aquatic ecosystems through unprecedented and attendant analyses.
C1 [McKean, Jim A.; Isaak, Dan J.] US Forest Serv, Rocky Mt Res Stn, Boise, ID 83702 USA.
[Wright, Charles W.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
RP McKean, JA (reprint author), US Forest Serv, Rocky Mt Res Stn, Boise, ID 83702 USA.
EM jmckean@fs-fed.us
RI McKean, Jim/C-3581-2011; Isaak, Dan/C-8818-2011
NR 16
TC 46
Z9 47
U1 3
U2 12
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA
SN 1540-9295
J9 FRONT ECOL ENVIRON
JI Front. Ecol. Environ.
PD APR
PY 2008
VL 6
IS 3
BP 125
EP 130
DI 10.1890/070109
PG 6
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 282WF
UT WOS:000254597200017
ER
PT J
AU Asgharzadeh, MF
von Frese, RRB
Kim, HR
AF Asgharzadeh, M. F.
von Frese, R. R. B.
Kim, H. R.
TI Spherical prism magnetic effects by Gauss-Legendre quadrature
integration
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE magnetic anomalies : modelling and interpretation; satellite magnetics;
planetary tectonics
ID EARTH GRAVITY; ANOMALY MAP; SATELLITE; INVERSION
AB Regional spherical coordinate observations of the Earth's crustal magnetic field components are becoming increasingly available from shipborne, airborne, and satellite surveys. In assessing the geological significance of these data, theoretical anomalous magnetic fields from geologic models in spherical coordinates need to be evaluated. This study explicitly develops the elegant Gauss-Legendre quadrature formulation for numerically modelling the complete magnetic effects (i.e. potential, vector and tensor gradient fields) of the spherical prism. We also use these results to demonstrate the magnetic effects for the crustal prism and to investigate the crustal magnetic effects at satellite altitudes for a large region of the Middle East centred on Iran.
C1 [Asgharzadeh, M. F.; von Frese, R. R. B.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA.
[Kim, H. R.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, GSFC NASA, Greenbelt, MD 20771 USA.
RP Asgharzadeh, MF (reprint author), Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA.
EM vonfrese@osu.edu
NR 33
TC 5
Z9 6
U1 1
U2 3
PU BLACKWELL PUBLISHING
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND
SN 0956-540X
J9 GEOPHYS J INT
JI Geophys. J. Int.
PD APR
PY 2008
VL 173
IS 1
BP 315
EP 333
DI 10.1111/j.1365-246X.2007.03692.x
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 276FJ
UT WOS:000254126400022
ER
PT J
AU Trout, TJ
Johnson, LF
Gartung, J
AF Trout, Thomas J.
Johnson, Lee F.
Gartung, Jim
TI Remote sensing of canopy cover in horticultural crops
SO HORTSCIENCE
LA English
DT Article; Proceedings Paper
CT Annual Conference of the American-Society-for-Horticultural-Science
CY JUL 25-30, 2006
CL New Orleans, LA
SP Amer Soc Horticultural Sci
DE evapotranspiration; shaded area; NDVI; vegetation index; fractional
cover; crop coefficients
ID SHADED AREA; COEFFICIENTS; VEGETATION; RADIATION; INDEX; CORN
AB Canopy cover (CC) is an important indicator of stage of growth and crop water use in horticultural crops. Remote sensing of CC has been studied in several major crops, but not in most horticultural crops. We measured CC of 11 different annual and perennial horticultural crops in various growth stages on 30 fields on the west side of California's San Joaquin Valley with a handheld multispectral digital camera. Canopy cover was compared with normalized difference vegetation index (NDVI) values calculated from Landsat 5 satellite imagery. The NDVI was highly correlated and linearly related with measured CC across the wide range of crops, canopy structures, and growth stages (R-2 = 0.95, P < 0.01) and predicted CC with mean absolute error of 0.047 up to effective full cover. These results indicate that remotely sensed NDVI may be an efficient way to monitor growth stage, and potentially irrigation water demand, of horticultural crops.
C1 [Trout, Thomas J.] USDA ARS, Ft Collins, CO 80526 USA.
[Johnson, Lee F.] NASA, Ames Res Ctr, CSUMB SEP, Div Earth Sci, Moffett Field, CA 94035 USA.
[Gartung, Jim] USDA ARS, Parlier, CA 93548 USA.
RP Trout, TJ (reprint author), USDA ARS, 2150 Ctr Dr,Bldg D, Ft Collins, CO 80526 USA.
EM Thomas.Trout@ars.usda.gov
OI Trout, Thomas/0000-0003-1896-9170
NR 22
TC 24
Z9 24
U1 0
U2 11
PU AMER SOC HORTICULTURAL SCIENCE
PI ALEXANDRIA
PA 113 S WEST ST, STE 200, ALEXANDRIA, VA 22314-2851 USA
SN 0018-5345
EI 2327-9834
J9 HORTSCIENCE
JI Hortscience
PD APR
PY 2008
VL 43
IS 2
BP 333
EP 337
PG 5
WC Horticulture
SC Agriculture
GA 274UC
UT WOS:000254026400012
ER
PT J
AU Mitchell, DL
Halekas, JS
Lin, RP
Frey, S
Hood, LL
Acuna, MH
Binder, A
AF Mitchell, D. L.
Halekas, J. S.
Lin, R. P.
Frey, S.
Hood, L. L.
Acuna, M. H.
Binder, A.
TI Global mapping of lunar crustal magnetic fields by Lunar Prospector
SO ICARUS
LA English
DT Article
DE Moon; surface; magnetic fields; cratering; impact processes
ID IMPACT BASINS; RIMA-SIRSALIS; ANOMALIES; SURFACE; MODEL; MARS
AB The Lunar Prospector Electron Reflectometer has obtained the first global map of lunar crustal magnetic fields, revealing that the effects of basin-forming impacts dominate the large-scale distribution of remanent magnetic fields on the Moon. The weakest surface magnetic fields (<0.2 nT) are found within two of the largest and most recent impact basins, Orientale and Imbrium. Conversely, the largest concentrations of strong surface fields (>40 nT) are diametrically opposite to these same basins. This pattern is present though less pronounced for several other post-Nectarian impact basins larger than 500 km in diameter. The reduced strength and clarity of the pattern for older basins may be attributed to: (1) demagnetization from many smaller impacts, which erases antipodal magnetic signatures over time, (2) superposition effects from other large impacts, and (3) variation in the strength of the ambient magnetizing field. The absence of fringing fields stronger than I nT around the perimeter of the Imbrium basin or associated with craters within the basin implies that any uniform magnetization of the impact melt must be weaker than similar to 10(-6) G cm(3) g(-1). This limits the strength of any steady ambient magnetic field to no more than similar to 0.1 Oe at the lunar surface while the basin cooled for tens of millions of years following the Imbrium impact 3.8 billion years ago. (C) 2008 Elsevier Inc. All rights reserved.
C1 [Mitchell, D. L.; Halekas, J. S.; Lin, R. P.; Frey, S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Lin, R. P.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Hood, L. L.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Acuna, M. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Binder, A.] Lunar Res Inst, Tucson, AZ 85747 USA.
RP Mitchell, DL (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM mitchell@ssl.berkeley.edu
OI Halekas, Jasper/0000-0001-5258-6128
NR 40
TC 79
Z9 83
U1 1
U2 7
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD APR
PY 2008
VL 194
IS 2
BP 401
EP 409
DI 10.1016/j.icarus.2007.10.027
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 284DM
UT WOS:000254685900002
ER
PT J
AU Malin, MC
Calvin, WM
Cantor, BA
Clancy, RT
Haberle, RM
James, PB
Thomas, PC
Wolff, MJ
Bell, JE
Lee, SW
AF Malin, Michael C.
Calvin, Wendy M.
Cantor, Bruce A.
Clancy, R. Todd
Haberle, Robert M.
James, Philip B.
Thomas, Peter C.
Wolff, Michael J.
Bell, James E., III
Lee, Steven W.
TI Climate, weather, and north polar observations from the Mars
Reconnaissance Orbiter Mars Color Imager
SO ICARUS
LA English
DT Article
DE Mars, atmosphere; Mars, polar caps
ID HUBBLE-SPACE-TELESCOPE; LASER ALTIMETER; WATER ICE; CLOUDS; APHELION;
VIKING; SIMULATION; ATMOSPHERE; BEHAVIOR; AEROSOL
AB The Mars Reconnaissance Orbiter observes Mars from a nearly circular, polar orbit. From this vantage point, the Mars Color Imager extends the similar to 5 Mars years record of Mars Global Surveyor global, visible-wavelength multi-color observations of meteorological events and adds measurements at three additional visible and two ultraviolet wavelengths. Observations of the global distribution of ozone (which anti-correlates with water vapor) and water ice and dust clouds allow tracking of atmospheric circulation. Regional and local observations emphasize smaller scale atmospheric dynamics, especially those related to dust lifting and subsequent motion. Polar observations detail variations related to the polar heat budget, including changes in polar frosts and ices, and storms generated at high thermal contrast boundaries. (C) 2007 Elsevier Inc. All rights reserved.
C1 [James, Philip B.; Thomas, Peter C.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Malin, Michael C.; Cantor, Bruce A.] Malin Space Syst, San Diego, CA 92191 USA.
[Bell, James E., III] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Calvin, Wendy M.] Univ Nevada, Dept Geol Sci, Reno, NV 89557 USA.
[Clancy, R. Todd; Wolff, Michael J.; Lee, Steven W.] Space Sci Inst, Boulder, CO 80301 USA.
[Haberle, Robert M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Lee, Steven W.] Denver Museum Nat & Sci, Denver, CO 80205 USA.
RP James, PB (reprint author), Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
EM pjames@cableone.net
NR 37
TC 21
Z9 21
U1 1
U2 9
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD APR
PY 2008
VL 194
IS 2
BP 501
EP 512
DI 10.1016/j.icarus.2007.10.016
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 284DM
UT WOS:000254685900009
ER
PT J
AU Barr, AC
Milkovich, SM
AF Barr, Amy C.
Milkovich, Sarah M.
TI Ice grain size and the rheology of the martian polar deposits
SO ICARUS
LA English
DT Article
DE Mars; ices
ID DYNAMIC RECRYSTALLIZATION; MARS; CAP; STRESS; FLOW; TEMPERATURE;
DEPENDENCE; GREENLAND; TEXTURES; FABRICS
AB The history and dynamics of the martian polar deposits (MPD), the largest known water reservoirs on Mars, are of great interest, but estimates of ice grain size are required before detailed modeling can be performed. We clarify the microphysical processes that may control grain size in the MPD. If the MPD are similar to 2% dust by mass, the maximum ice grain size is similar to 1 mm due to grain boundary pinning by silicate microparticles. Relatively dusty layers in the MPD will have smaller grain sizes. If MPD ice has a very low impurity content and has experienced a significant amount of strain, grains may reach a steady state size of similar to 1.5 to 3 mm due to dynamic recrystallization, wherein a steady state grain size is maintained due to the balance of grain growth and destruction during flow. If the near-bed ice in the MPD is warmed close to its melting point and has been extensively sheared, grain sizes at its base may be between 10 and 40 mm, by analogy with warm, dirty, near-bed ice in terrestrial ice sheets. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Barr, Amy C.] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA.
[Milkovich, Sarah M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Barr, AC (reprint author), SW Res Inst, Dept Space Studies, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA.
EM amy@boulder.swri.edu
NR 32
TC 10
Z9 10
U1 0
U2 2
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD APR
PY 2008
VL 194
IS 2
BP 513
EP 518
DI 10.1016/j.icarus.2007.11.018
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 284DM
UT WOS:000254685900010
ER
PT J
AU Lillis, RJ
Mitchell, DL
Lin, RP
Acuna, MH
AF Lillis, Robert J.
Mitchell, David L.
Lin, Robert P.
Acuna, Mario H.
TI Electron reflectometry in the martian atmosphere
SO ICARUS
LA English
DT Article
DE Mars; magnetic fields; Mars, atmosphere
ID SPHERICAL HARMONIC MODEL; CRUSTAL MAGNETIC-FIELD; SOLAR-CYCLE VARIATION;
MARS GLOBAL SURVEYOR; IMPACT IONIZATION; LUNAR PROSPECTOR;
CROSS-SECTIONS; ARGON; IONOSPHERE; EXCITATION
AB The technique of electron reflectometry, a method for remote estimation of planetary magnetic fields, is expanded from its original use of mapping crustal magnetic fields at the Moon to achieving the same purpose at Mars, where the presence of a substantial atmosphere complicates matters considerably. The motion of solar wind electrons, incident on the martian atmosphere, is considered in detail, taking account of the following effects: the electrons' helical paths around the magnetic field lines to which they are bound, the magnetic mirror force they experience due to converging field lines in the vicinity of crustal magnetic anomalies, their acceleration/deceleration by electrostatic potentials, their interactions with thermal plasma. their drifts due to magnetic field line curvature and perpendicular electric fields and their scattering off, and loss of energy through a number of different processes to, atmospheric neutrals. A theoretical framework is thus developed for modeling electron pitch angle distributions expected when a spacecraft is on a magnetic field line which is connected to both the martian crust and the interplanetary magnetic field. This framework, along with measured pitch angle distributions from the Mars Global Surveyor (MGS) Magnetometer/Electron Reflectometer (MAG/ER) experiment, can be used to remotely measure crustal magnetic field magnitudes and atmospheric neutral densities at similar to 180 km above the martian datum, as well as estimate average parallel electric fields between 200 and 400 km altitude. Detailed analysis and full results, concerning the crustal magnetic field and upper thermospheric density of Mars, are left to two companion papers. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Lillis, Robert J.; Mitchell, David L.; Lin, Robert P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Acuna, Mario H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Lillis, RJ (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM rlillis@ssl.berkeley.edu
RI Lillis, Robert/A-3281-2008
OI Lillis, Robert/0000-0003-0578-517X
NR 56
TC 22
Z9 22
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 0019-1035
J9 ICARUS
JI Icarus
PD APR
PY 2008
VL 194
IS 2
BP 544
EP 561
DI 10.1016/j.icarus.2007.09.030
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 284DM
UT WOS:000254685900012
ER
PT J
AU Lillis, RJ
Bougher, SW
Mitchell, DL
Brain, DA
Lin, RP
Acuna, MH
AF Lillis, Robert J.
Bougher, Stephen W.
Mitchell, David L.
Brain, David A.
Lin, Robert P.
Acuna, Mario H.
TI Continuous monitoring of nightside upper thermospheric mass densities in
the martian southern hemisphere over 4 martian years using electron
reflectometry
SO ICARUS
LA English
DT Article
DE Mars; magnetic fields; Mars, atmosphere
ID GENERAL-CIRCULATION MODEL; SPHERICAL HARMONIC MODEL; CRUSTAL
MAGNETIC-FIELD; SOLAR-CYCLE VARIATION; MARS GLOBAL SURVEYOR;
UPPER-ATMOSPHERE; MGS ACCELEROMETER; HIGH-ALTITUDE; SIMULATIONS;
IONOSPHERE
AB Details are presented of an improved technique to use atmospheric absorption of magnetically reflecting solar wind electrons to constrain neutral mass densities in the nightside martian upper thermosphere. The helical motion of electrons on converging magnetic field lines, through an extended neutral atmosphere, is modeled to enable prediction of loss cone pitch angle distributions measured by the Magnetometer/Electron Reflectometer (MAG/ER) experiment on Mars Global Surveyor at 400 km altitude. Over the small fraction of Mars' southern hemisphere (similar to 2.5%) where the permanent crustal magnetic fields are both open to the solar wind and sufficiently strong as to dominate the variable induced martian magnetotail field, spherical harmonic expansions of the crustal fields are used to prescribe the magnetic field along the electron's path, allowing least-squares fitting of measured loss cones, in order to solve for parameters describing the vertical neutral atmospheric mass density profile from 160 to 230 km. Results are presented of mass densities in the southern hemisphere at 2 a.m. LST at the mean altitude of greatest sensitivity, 180 km. continuously over four martian years. Seasonal variability in densities is largely explained by orbital and latitudinal changes in dayside insolation that impacts the nightside through the resulting thermospheric circulation. However, the physical processes behind repeatable rapid, late autumnal cooling at mid-latitudes and near-aphelion warming at equatorial latitudes is not fully clear. Southern winter polar warming is generally weak or nonexistent over several Mars years, in basic agreement with MGS and MRO accelerometer observations. The puzzling response of mid-latitude densities from 160 degrees to 200 degrees E to the 2001 global dust storm suggests unanticipated localized nightside upper thermospheric lateral and vertical circulation patterns may accompany such storms. The downturn of the 11-year cycle of solar EUV flux is likely responsible for lower aphelion densities in 2004 and 2006 (Mars years 27 and 28). (C) 2007 Elsevier Inc. All rights reserved.
C1 [Lillis, Robert J.; Mitchell, David L.; Brain, David A.; Lin, Robert P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Bougher, Stephen W.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Acuna, Mario H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Lillis, RJ (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM rlillis@ssl.berkeley.edu
RI Bougher, Stephen/C-1913-2013; Lillis, Robert/A-3281-2008
OI Bougher, Stephen/0000-0002-4178-2729; Lillis, Robert/0000-0003-0578-517X
NR 47
TC 16
Z9 16
U1 0
U2 2
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD APR
PY 2008
VL 194
IS 2
BP 562
EP 574
DI 10.1016/j.icarus.2007.09.031
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 284DM
UT WOS:000254685900013
ER
PT J
AU Lillis, RJ
Frey, HV
Manga, M
Mitchell, DL
Lin, RP
Acuna, MH
Bougher, SW
AF Lillis, Robert J.
Frey, Herbert V.
Manga, Michael
Mitchell, David L.
Lin, Robert P.
Acuna, Mario H.
Bougher, Stephen W.
TI An improved crustal magnetic field map of Mars from electron
reflectometry: Highland volcano magmatic history and the end of the
martian dynamo
SO ICARUS
LA English
DT Article
DE Mars; magnetic fields; cratering; Mars, interior; volcanism
ID IMPACT EXCITATION; CASCADE RANGE; SYRTIS MAJOR; CONSTRAINTS; EVOLUTION;
REGION; ARGON; RATES; ANOMALIES; CRATERS
AB We apply improved kinetic modeling of electron transport in the martian thermosphere to fit pitch angle distributions measured by the Mars Global Surveyor (MGS) Magnetometer/Electron Reflectometer (MAG/ER), together with appropriate filtering, binning, averaging and error correction techniques, to create the most reliable ER global map to date of crustal magnetic field magnitude at 185 km altitude, with twice the spatial resolution and considerably higher sensitivity to crustal fields than global maps of magnetic field components produced with MAG data alone. This map compares favorably to sparsely sampled dayside MAG data taken at similar altitudes, insofar as a direct comparison is meaningful. Using this map, we present two case studies. The first compares the magnetic signatures of two highland volcanoes, concluding that the comparatively greater thermal demagnetization at Syrtis Major compared with Tyrrhena Patera is likely due to a higher ratio of intruded to extruded magmas. The second uses the map along with topographic data to compare the magnetic signatures and crater retention ages of the demagnetized Hellas impact basin and magnetized Ladon impact basin. From this comparison, we determine that the martian global dynamo magnetic field went from substantial to very weak or nonexistent in the absolute model age time interval 4.15 +/- 0.05 to 4.07 +/- 0.05 Ga ago. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Lillis, Robert J.; Mitchell, David L.; Lin, Robert P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Frey, Herbert V.; Acuna, Mario H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Manga, Michael] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Bougher, Stephen W.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RP Lillis, RJ (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM rlillis@ssl.berkeley.edu
RI Bougher, Stephen/C-1913-2013; Manga, Michael/D-3847-2013; Lillis,
Robert/A-3281-2008;
OI Bougher, Stephen/0000-0002-4178-2729; Lillis,
Robert/0000-0003-0578-517X; Manga, Michael/0000-0003-3286-4682
NR 78
TC 66
Z9 68
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 APR
PY 2008
VL 194
IS 2
BP 575
EP 596
DI 10.1016/j.icarus.2007.09.032
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 284DM
UT WOS:000254685900014
ER
PT J
AU Chambers, LS
Cuzzi, JN
Asphaug, E
Colwell, J
Sugita, S
AF Chambers, Lindsey S.
Cuzzi, Jeffrey N.
Asphaug, Erik
Colwell, Joshua
Sugita, Seiji
TI Hydrodynamical and radiative transfer modeling of meteoroid impacts into
Saturn's rings
SO ICARUS
LA English
DT Article
DE planetary rings; Saturn; impact processes; radiative transfer
ID MOVING PLASMA CLOUDS; PLANETARY RINGS; HYPERVELOCITY IMPACTS; IMAGING
SCIENCE; SPOKE FORMATION; VAPOR CLOUDS; LIGHT FLASH; B-RING;
BOMBARDMENT; SYSTEM
AB In a small hypervelocity impact, superheated gas and particles glow brightly with thermal emission for a brief time interval at short wavelengths; this phenomenon is referred to as an impact flash. Over the past decade, impact flashes have been observed on the Moon and in the laboratory in both the IR and visible portions of the spectrum. These phenomena have been used to constrain impactor parameters, such as impact size, velocity and composition. With the arrival of the Cassini spacecraft at Saturn, we embarked on a study of impact flashes in Saturn's rings. We present results on the feasibility of observing impact flashes and therefore estimating the flux of meteoroids impacting Saturn's rings using Cassini's Ultraviolet Imaging Spectrograph (UVIS). Our modeling effort is two-fold. We start by simulating impacts using the CTH hydrodynamical code. Impacts involve an icy ring particle and a serpentine meteoroid, modeled with the ANEOS equation of state. The objects are centimeters to meters in diameter and collide at 30 to 50 km s(-1). We then use the resulting temperatures and densities of the impact plumes in a radiative transfer calculation. We calculate bound-free, free-free, electron scattering and negative ion opacities along a line-of-sight through the center of each impact plume. Our model has shown that impact flashes will not be seen with the UVIS because (1) the plumes are optically thick when their central temperatures are high, with photosphere temperatures too cool to emit observable UV flux and (2) when the plumes become optically thin, even the hottest region of the plume is too cool to observe in the UV. This corroborates the lack of UVIS impact flash detections to date. Impact flashes are not likely to be seen by other Cassini instruments because of the short lifetimes of the plumes. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Chambers, Lindsey S.; Asphaug, Erik] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
[Cuzzi, Jeffrey N.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Colwell, Joshua] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA.
[Sugita, Seiji] Univ Tokyo, Grad Sch Frontier Sci, Dept Complexity Sci & Engn, Chiba 2778561, Japan.
RP Chambers, LS (reprint author), Univ Calif Santa Cruz, Dept Earth & Planetary Sci, 1156 High St, Santa Cruz, CA 95064 USA.
EM lchambers@pmc.ucsc.edu
NR 77
TC 8
Z9 8
U1 0
U2 0
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD APR
PY 2008
VL 194
IS 2
BP 623
EP 635
DI 10.1016/j.icarus.2007.11.017
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 284DM
UT WOS:000254685900017
ER
PT J
AU Alvarellos, JL
Zahnle, KJ
Dobrovolskis, AR
Hamill, P
AF Alvarellos, Jose Luis
Zahnle, Kevin J.
Dobrovolskis, Anthony R.
Hamill, Patrick
TI Transfer of mass from Io to Europa and beyond due to cometary impacts
SO ICARUS
LA English
DT Article
DE Io; Europa; cratering; impact processes
ID CRATERING RATES; SATURN SYSTEM; EJECTA; SATELLITES; PLANETS; ORIGIN;
BODIES
AB We simulate the production and orbital evolution of escaping ejecta due to cometary impacts on Io. The model includes the-four Galilean satellites. Amalthea, Thebe, Jupiter's gravitational moments, Saturn and the Sun. Five scenarios are examined: an impact at the apex, the sub-jovian point. the anti-jovian point, the antapex, and at the south pole of Io. We estimate that on average a cometary impact injects thrice its mass (in the form of Io surface material) into jovicentric orbit. The majority of the escaping debris comes back to Io, but a sizeable fraction (between 5.0 and 8.7%) manages to reach Europa, and a smaller fraction Ganymede (between 1.5 and 4.6%). Smaller fractions reached Amalthea Thebe, Callisto, and Jupiter itself. For million year time scales, the mass transfer to Europa is estimated as 1.8-3.1 x 10(14) g/Myr. The median time for transfer of ejecta from Io to Europa is similar to 56 years. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Alvarellos, Jose Luis] Space Syst Loral, Palo Alto, CA 94303 USA.
[Zahnle, Kevin J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Dobrovolskis, Anthony R.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
[Hamill, Patrick] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA.
RP Alvarellos, JL (reprint author), Space Syst Loral, 3825 Fabian Way,MS G-76, Palo Alto, CA 94303 USA.
EM alvarellosjose@ssd.loral.com
NR 34
TC 10
Z9 10
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 0019-1035
J9 ICARUS
JI Icarus
PD APR
PY 2008
VL 194
IS 2
BP 636
EP 646
DI 10.1016/j.icarus.2007.09.025
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 284DM
UT WOS:000254685900018
ER
PT J
AU Zahnle, K
Alvarellos, JL
Dobrovolskis, A
Hamill, P
AF Zahnle, Kevin
Alvarellos, Jose L.
Dobrovolskis, Anthony
Hamill, Patrick
TI Secondary and sesquinary craters on Europa
SO ICARUS
LA English
DT Article
DE impact processes; cratering; Io; Europa; Jupiter, satellites
ID GALILEAN SATELLITES; EJECTA; FRAGMENTS; SURFACES; COMETS; SYSTEM; RATES
AB We address impact cratering on Io and Europa, with the emphasis on the origin of small craters on Europa as secondary to the primary impacts of comets on In, Europa, and Ganymede. In passing we also address the origin of secondary craters generated by Zunil, a well-studied impact crater on Mars that is a plausible analog to impact craters on Io. At nominal impact rates, and taking volcanic resurfacing into account, we find that there should be 1.3 impact craters on Io, equally likely to be of any diameter between 100 m and 20 km. The corresponding model age of Europa's surface is between 60 and 100 Ma. This range of ages does not include a factor three uncertainty stemming from the uncertain sizes and numbers of comets. The mass of basaltic impact ejecta from Io to reach Europa is found to meet or exceed the micrometeoroid flux as a source of rock-forming elements to Europa's ice crust. To describe impact ejecta in more detail we adapt models for impact-generated spalls and Grady-Kipp fragments originally developed by Melosh. Our model successfully reproduces the observed size-number distributions of small craters on both Mars and Europa. However, the model predicts that a significant fraction of the 200-500 m, diameter craters on Europa are not traditional secondary craters but are instead sesquinary craters caused by impact ejecta from Io that had gone into orbit about Jupiter. This prediction is not supported by observation, which implies that high speed spalls usually break up into smaller fragments that make smaller sesquinary craters. logenic basalts are also interesting because they provide stratigraphic horizons on Europa that in principle could be used to track historic motions of the ice. and they provide materials suitable to radiometric dating of Europa's surface. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Zahnle, Kevin] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Alvarellos, Jose L.] Space Syst Loral, Palo Alto, CA 94303 USA.
[Dobrovolskis, Anthony] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
[Hamill, Patrick] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA.
RP Zahnle, K (reprint author), NASA, Ames Res Ctr, Div Space Sci, MS 245-3, Moffett Field, CA 94035 USA.
EM kevin.j.zahnle@nasa.gov
NR 34
TC 30
Z9 30
U1 0
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 APR
PY 2008
VL 194
IS 2
BP 660
EP 674
DI 10.1016/j.icarus.2007.10.024
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 284DM
UT WOS:000254685900020
ER
PT J
AU Radebaugh, J
Loren, RD
Lunine, JI
Wall, SD
Boubin, G
Reffet, E
Kirk, RL
Lopes, RM
Stofan, ER
Soderblom, L
Allison, M
Janssen, M
Paillou, P
Callahan, P
Spencer, C
AF Radebaugh, J.
Loren, R. D.
Lunine, J. I.
Wall, S. D.
Boubin, G.
Reffet, E.
Kirk, R. L.
Lopes, R. M.
Stofan, E. R.
Soderblom, L.
Allison, M.
Janssen, M.
Paillou, P.
Callahan, P.
Spencer, C.
CA Cassini Radar Team
TI Dunes on Titan observed by Cassini Radar
SO ICARUS
LA English
DT Article
DE Titan; satellites, surfaces; Saturn, satellites
ID LONGITUDINAL DUNES; SEDIMENT TRANSPORT; GENERAL-CIRCULATION; HUYGENS
PROBE; SURFACE; WINDS; VENUS; PREDICTIONS; ATMOSPHERE; SIMULATION
AB Thousands of longitudinal dunes have recently been discovered by the Titan Radar Mapper on the surface of Titan. These are found mainly within +/-30 degrees of the equator in optically-, near-infrared-, and radar-dark regions, indicating a strong proportion of organics, and cover well over 5% of Titan's surface. Their longitudinal duneform, interactions with topography, and correlation with other aeolian forms indicate a single, dominant wind direction aligned with the dune axis plus lesser, off-axis or seasonally alternating winds. Global compilations of dune orientations reveal the mean wind direction is dominantly eastwards, with regional and local variations where winds are diverted around topographically high features, such as mountain blocks or broad landforms. Global winds may carry sediments from high latitude regions to equatorial regions, where relatively drier conditions prevail, and the particles are reworked into dunes, perhaps on timescales of thousands to tens of thousands of years. On Titan, adequate sediment supply, sufficient wind, and the absence of sediment carriage and trapping by fluids are the dominant factors in the presence of dunes. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Radebaugh, J.; Spencer, C.] Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA.
[Loren, R. D.] Johns Hopkins Univ, Dept Space, Planetary Explorat Grp, Laurel, MD 20723 USA.
[Lunine, J. I.; Boubin, G.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Wall, S. D.; Lopes, R. M.; Janssen, M.; Callahan, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Reffet, E.] Observ Paris, LESIA, F-92195 Meudon, France.
[Kirk, R. L.; Soderblom, L.] Lowell Observ, Astrogeol Div, Flagstaff, AZ 86001 USA.
[Stofan, E. R.] Proxemy Res, Bowie, MD 20715 USA.
[Allison, M.] Goddard Inst Space Studies, New York, NY 10025 USA.
[Paillou, P.] Observ Aquatain Sci Univers, UMR 5804, Floirac, France.
RP Radebaugh, J (reprint author), Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA.
EM jani.radebaugh@byu.edu
RI Lorenz, Ralph/B-8759-2016; Lopes, Rosaly/D-1608-2016;
OI Lorenz, Ralph/0000-0001-8528-4644; Lopes, Rosaly/0000-0002-7928-3167;
Spencer, Christopher/0000-0003-4264-3701
NR 62
TC 99
Z9 99
U1 1
U2 10
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD APR
PY 2008
VL 194
IS 2
BP 690
EP 703
DI 10.1016/j.icarus.2007.10.015
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 284DM
UT WOS:000254685900022
ER
PT J
AU Zebker, HA
Wye, LC
Janssen, MA
AF Zebker, Howard A.
Wye, Lauren C.
Janssen, Michael A.
CA Cassini Radar Team
TI Titan's surface from reconciled Cassini microwave reflectivity and
emissivity observations
SO ICARUS
LA English
DT Article
DE Titan; radar observations; satellites, surfaces
ID THERMAL EMISSION; RADAR; APPROXIMATION; POLARIZATION; ROUGHNESS
AB The surface of Titan, Saturn's largest moon, appears to consist of solid hydrocarbons or CO2 with considerable small-scale structure, according to a new electromagnetic scattering model that uses both Cassini radar reflectivity and emissivity measurements. Our model resolves a well-known ambiguity in active and passive observations of surfaces, namely that the dielectric constant retrieved from radiometric data is usually less than that obtained from radar backscatter analysis. We present here parameters of Titan derived from radar and radiometric responses using a single set of surface physical descriptors. The observed dielectric constant ranges from 1.75-2.5, consistent with the solids above, but also with unconsolidated water or water/ammonia ice. Inferred rms slopes of the surface range from 10 degrees-16 degrees at Cassini's 2.2 cm-lambda, with radar albedos of about 30%. Emissivities of the surface are quite high, on the order of 90%. We find that the majority of the backscattered radar energy results from volume, rather than surface, scattering processes. Thus large-scale variations in radar brightness are mainly diagnostic of composition and structure within Titan's near subsurface. The high level of volume scatter (about 15% of incident energy) and consequent high radar albedo suggest significant wavelength-scale structure and multiple scatter within the medium. This is most consistent with a surface composed either of ubiquitous mm-size bubbles within the "ice," analogous to a vesicular cryolava, or structures similar to ice pipes and lenses found in terrestrial ice sheets. The cryovolcanic hypothesis suggests planet-wide resurfacing by active volcanism to explain the large-scale uniformity of observed backscatter. If the lens/pipe mechanism pertains, it can imply percolation of precipitating liquid or surface melt through the Titan "firn." (C) 2007 Elsevier Inc. All rights reserved.
C1 [Zebker, Howard A.; Wye, Lauren C.] Stanford Univ, Dept Geophys, Stanford, CA 94305 USA.
[Zebker, Howard A.; Wye, Lauren C.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA.
[Janssen, Michael A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cassini Radar Team] CALTECH, Jet Prop Lab, Cassini Project, Pasadena, CA 91109 USA.
RP Zebker, HA (reprint author), Stanford Univ, Dept Geophys, Stanford, CA 94305 USA.
EM zebker@stanford.edu
NR 26
TC 17
Z9 17
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 0019-1035
J9 ICARUS
JI Icarus
PD APR
PY 2008
VL 194
IS 2
BP 704
EP 710
DI 10.1016/j.icarus.2007.10.019
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 284DM
UT WOS:000254685900023
ER
PT J
AU Rappaport, NJ
Iess, L
Wahr, J
Lunine, JI
Armstrong, JW
Asmar, SW
Tortora, P
Di Benedetto, M
Racioppa, P
AF Rappaport, Nicole J.
Iess, Luciano
Wahr, John
Lunine, Jonathan I.
Armstrong, J. W.
Asmar, Sami W.
Tortora, Paolo
Di Benedetto, Mauro
Racioppa, Paolo
TI Can Cassini detect a subsurface ocean in Titan from gravity
measurements?
SO ICARUS
LA English
DT Article
DE Titan; interiors
ID INTERNAL STRUCTURE; TIDAL RESPONSE; HIGH-PRESSURE; SURFACE; DYNAMICS;
ROTATION; ORIGIN; METHANE; EUROPA; EARTH
AB Recent models of Titan's interior predict that the satellite contains an ocean of water and ammonia under an icy layer. Direct evidence for the presence of an ocean can be provided on the Cassini mission only by radio science determination of Titan Love number k(2). Simulations that use the five flybys T11, T22 T33, T45, and T68 (the latter two belonging to the extended mission) lead to the result that in the elastic case, where the Love number is real, k(2) will be determined with a one-sigma accuracy of 0.1. In the viscoelastic case, where k(2) is complex, the real and imaginary parts of k(2) will be determined with one sigma accuracies of 0.138 and 0.115, respectively. Ocean and oceanless models that include a viscoelastic theology are built. In the viscoelastic case, there is a 93% probability to correctly predict the presence or absence of an ocean; this probability improves to 97% in the elastic case. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Rappaport, Nicole J.; Armstrong, J. W.; Asmar, Sami W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Iess, Luciano; Di Benedetto, Mauro; Racioppa, Paolo] Univ Roma La Sapienza, Dipartimento Ingn Aerospaziale Astronaut, I-00184 Rome, Italy.
[Wahr, John] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Lunine, Jonathan I.] INAF IFSI, I-00133 Rome, Italy.
[Lunine, Jonathan I.] Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Tortora, Paolo] Univ Bologna, DIEM, Fac Engn 2, I-47100 Forli, Italy.
RP Rappaport, NJ (reprint author), CALTECH, Jet Prop Lab, MS 301-150,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM nicole.j.rappaport@jpl.nasa.gov
RI IESS, Luciano/F-4902-2011; Tortora, Paolo/J-6191-2012
OI IESS, Luciano/0000-0002-6230-5825; Tortora, Paolo/0000-0001-9259-7673
NR 30
TC 21
Z9 21
U1 0
U2 2
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD APR
PY 2008
VL 194
IS 2
BP 711
EP 720
DI 10.1016/j.icarus.2007.11.024
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 284DM
UT WOS:000254685900024
ER
PT J
AU Anderson, CM
Young, EF
Chanover, NJ
Mckay, CP
AF Anderson, C. M.
Young, E. F.
Chanover, N. J.
McKay, C. P.
TI HST spectral imaging of Titan's haze and methane profile between 0.6 and
1 mu m during the 2000 opposition
SO ICARUS
LA English
DT Article
DE Titan; atmospheres, structure; radiative transfer
ID NORTH POLAR STRATOSPHERE; TROPOSPHERIC CLOUDS; LOWER ATMOSPHERE;
SURFACE; AEROSOLS; MODEL; ALBEDO; REANALYSIS; ABUNDANCES; WINDS
AB We report on the analysis of high spatial resolution visible to near-infrared spectral images of Titan at L-s = 240 degrees in November 2000, obtained with the Space Telescope Imaging Spectrograph instrument on board the Hubble Space Telescope as pan of program GO-8580. We employ a radiative transfer fractal particle aerosol model with a Bayesian parameter estimation routine that computes Titan's absolute reflectivity per pixel for 122 wavelengths by modeling the vertical distribution of the lower atmosphere haze and tropospheric methane. Analysis of these data suggests that Titan's haze concentration in the lower atmosphere varies in strength with latitude. We find Titan's tropospheric methane profile to be fairly consistent with latitude and longitude, and we find evidence for local areas of a CH4-N-2 binary saturation in Titan's troposphere. Our results suggest that a methane and haze profile at one location on Titan would not be representative of global conditions. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Anderson, C. M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Anderson, C. M.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Young, E. F.] SW Res Inst, Dept Space Sci, Boulder, CO 80302 USA.
NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Anderson, CM (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Code 661, Greenbelt, MD 20771 USA.
EM carrie.anderson@gsfc.nasa.gov
RI Anderson, Carrie/C-8097-2012
NR 54
TC 8
Z9 8
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 APR
PY 2008
VL 194
IS 2
BP 721
EP 745
DI 10.1016/j.icarus.2007.11.008
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 284DM
UT WOS:000254685900025
ER
PT J
AU Ipatov, SI
Kutyrev, AS
Madsen, GJ
Mather, JC
Moseley, SH
Reynolds, RJ
AF Ipatov, Sergei I.
Kutyrev, Alexander S.
Madsen, Greg J.
Mather, John C.
Moseley, S. Harvey
Reynolds, Ronald J.
TI Dynamical zodiacal cloud models constrained by high resolution
spectroscopy of the zodiacal light
SO ICARUS
LA English
DT Article
DE asteroids; comets, dust; trans-neptunian objects; spectroscopy; zodiacal
light
ID INTERPLANETARY DUST PARTICLES; FRAUNHOFER LINE-PROFILES; KUIPER-BELT
DUST; RADIAL-VELOCITY MEASUREMENTS; TRANS-NEPTUNIAN OBJECTS;
SOLAR-SYSTEM DUST; NEAR-EARTH SPACE; TERRESTRIAL PLANETS; ORBITAL
EVOLUTION; COSMIC DUST
AB The simulated Doppler shifts of the solar Mg I Fraunhofer line produced by scattering on the solar light by asteroidal, cometary, and trans-neptunian dust particles are compared with the shifts obtained by Wisconsin H-Alpha Mapper (WHAM) spectrometer. The simulated spectra are based on the results of integrations of the orbital evolution of particles under the gravitational influence of planets, the Poynting-Robertson drag, radiation pressure, and solar wind drag. Our results demonstrate that the differences in the line centroid position in the solar elongation and in the line width averaged over the elongations for different sizes of particles are usually less than those for different sources of dust. The deviation of the derived spectral parameters for various sources of dust used in the model reached maximum at the elongation (measured eastward from the Sun) between 90 degrees and 120 degrees. For the future zodiacal light Doppler shifts measurements, it is important to pay a particular attention to observing at this elongation range. At the elongations of the fields observed by WHAM, the model-predicted Doppler shifts were close to each other for several scattering functions considered. Therefore the main conclusions of our paper do not depend on a scattering function and mass distribution of particles if they are reasonable. A comparison of the dependencies of the Doppler shifts on solar elongation and the mean width of the Mg I line modeled for different sources of dust with those obtained from the WHAM observations shows that the fraction of cometary particles in zodiacal dust is significant and can be dominant. Cometary particles originating inside Jupiter's orbit and particles originating beyond Jupiter's orbit (including trans-neptunian dust particles) can contribute to zodiacal dust about 1/3 each, with a possible deviation from 1/3 up to 0.1-0.2. The fraction of asteroidal dust is estimated to be similar to 0.3-0.5. The mean eccentricities of zodiacal particles located at 1-2 AU from the Sun that better fit the WHAM observations are between 0.2 and 0.5, with a more probable value of about 0.3. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Ipatov, Sergei I.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Ipatov, Sergei I.] Moscow Space Res Inst, Moscow 117997, Russia.
[Kutyrev, Alexander S.; Mather, John C.; Moseley, S. Harvey] NASA, GSFC, Greenbelt, MD 20771 USA.
[Madsen, Greg J.] Anglo Australian Observ, Epping, NSW 1710, Australia.
[Reynolds, Ronald J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
RP Ipatov, SI (reprint author), Carnegie Inst Washington, Dept Terr Magnetism, 5241 Broad Branch Rd, Washington, DC 20015 USA.
EM siipatov@hotmail.com
RI Ipatov, Sergei/O-2302-2014
OI Ipatov, Sergei/0000-0002-1413-9180
NR 77
TC 11
Z9 11
U1 0
U2 2
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD APR
PY 2008
VL 194
IS 2
BP 763
EP 782
DI 10.1016/j.icarus.2007.11.009
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 284DM
UT WOS:000254685900028
ER
PT J
AU Nna-Mvondo, D
Khare, B
Ishihara, T
McKay, CP
AF Nna-Mvondo, Delphine
Khare, Bishun
Ishihara, Tomoko
McKay, Christopher P.
TI Experimental impact shock chemistry on planetary icy satellites
SO ICARUS
LA English
DT Review
DE ices; impact processes; prebiotic chemistry
ID PROTON IRRADIATED H2O+CO2; HUBBLE-SPACE-TELESCOPE; WATER-ICE;
HYPERVELOCITY IMPACT; ORGANIC-MOLECULES; HYDROGEN-PEROXIDE; GALILEAN
SATELLITES; COMETARY DELIVERY; AMINO-ACIDS; ULTRAVIOLET PHOTOLYSIS
AB We present new experimental results on impact shock chemistry into icy satellites of the outer planets. Icy mixtures of pure water ice with CO(2), Na(2)CO(3), CH(3)OH, and CH(3)OH/(NH(4))(2)SO(4) at 77 K were ablated with a powerful pulsed laser-a new technique used to simulate shock processes which can occur during impacts. New products were identified by GC-MS and FTIR analyses after laser ablation. Our results show that hydrogen peroxide is formed in irradiated H(2)O/CO(2) ices with a final concentration of 0.23%. CO and CH(3)OH were also detected as main products. The laser ablation of frozen H(2)O/Na(2)CO(3) generates only CO and CO(2) as destruction products from the salt. Pulsed irradiation of water ice containing methanol leads also to the formation of CO and CO(2), generates methane and more complex molecules containing carbonyl groups like acetaldehyde, acetone, methyl formate, and a diether, dimethyl formal. The last three compounds are also produced when adding ammonium sulfate to H(2)O/CH(3)OH ice, but acetone is more abundant. The formation of two hydrocarbons, CH(4) and C(2)H(6) is observed as well as the production of three nitrogen compounds, nitrous oxide, hydrogen cyanide, and acetonitrile. (C) 2007 Elsevier Inc. All fights reserved.
C1 [Nna-Mvondo, Delphine; Khare, Bishun; Ishihara, Tomoko; McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Khare, Bishun; Ishihara, Tomoko] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
RP Nna-Mvondo, D (reprint author), Inst Nacl Tecn Aeroespacial, Ctr Astrobiol, CSIC INTA, Planetary Geol Lab, Carretera Ajalvir,Km 4, Madrid 28850, Spain.
EM nnamvondod@inta.es
NR 113
TC 15
Z9 15
U1 1
U2 13
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD APR
PY 2008
VL 194
IS 2
BP 816
EP 829
DI 10.1016/j.icarus.2007.11.001
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 284DM
UT WOS:000254685900032
ER
PT J
AU Hodyss, R
Johnson, PV
Orzechowska, GE
Goguen, JD
Kanik, I
AF Hodyss, Robert
Johnson, Paul V.
Orzechowska, Grazyna E.
Goguen, Jay D.
Kanik, Isik
TI Carbon dioxide segregation in 1 : 4 and 1 : 9 CO2 : H2O ices
SO ICARUS
LA English
DT Article
DE ices; ices, IR spectroscopy; satellites, surfaces; photochemistry
ID SOLAR-SYSTEM BODIES; WATER-ICE; ASTROPHYSICAL IMPLICATIONS; INFRARED
SPECTRUM; BAND STRENGTHS; CO2; SPECTROMETER; SPECTROSCOPY; MIXTURES;
SURFACE
AB The mid-infrared spectra of mixed vapor deposited ices of CO2 and H2O were studied as a function of both deposition temperature and warming from 15 to 100 K. The spectra of ices deposited at 15 K show marked changes on warming beginning at 60 K. These changes are consistent with CO2 segregating within the ice matrix into pure CO2 domains. Ices deposited at 60 and 70 K show a greater degree of segregation, as high as 90% for 1:4 CO2:H2O ice mixtures deposited at 70 K. As the ice is warmed above 80 K, preferential sublimation of the segregated CO2 is observed. The kinetics of the segregation process is also examined. The segregation of the CO2 as the ice is warmed corresponds to temperatures at which the structure of the water ice matrix changes from the high density amorphous phase to the low density amorphous phase. We show how these microstructural changes in the ice have a profound effect on the photochemistry induced by ultraviolet irradiation. These experimental results provide a framework in which observations of CO2 on the icy bodies of the outer Solar System can be considered. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Hodyss, Robert; Johnson, Paul V.; Orzechowska, Grazyna E.; Goguen, Jay D.; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Hodyss, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM robert.p.hodyss@jpl.nasa.gov
RI Johnson, Paul/D-4001-2009
OI Johnson, Paul/0000-0002-0186-8456
NR 39
TC 10
Z9 10
U1 1
U2 11
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD APR
PY 2008
VL 194
IS 2
BP 830
EP 836
DI 10.1016/j.icarus.2007.10.005
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 284DM
UT WOS:000254685900033
ER
PT J
AU Noor, AK
Venneri, SL
AF Noor, Ahmed K.
Venneri, Samuel L.
TI ISE: Intelligent Synthesis Environment for future aerospace systems
SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE
LA English
DT Article
AB The Intelligent Synthesis Environment (ISE) being developed by NASA, UVA, and JPL for significantly enhancing the rapid creation of innovative affordable products and missions is described. ISE uses a synergistic combination of leading-edge technologies, including high-performance computing, high-capacity communications and networking, virtual product development, knowledge-based engineering, computational intelligence, human-computer interaction, and product information management. The environment will link scientists, design teams, manufacturers, suppliers, and consultants who participate in the mission synthesis, as well as in the creation and operation of the aerospace system. It will radically advance the process by which complex science missions are synthesized, and high-tech engineering systems are designed, manufactured, and operated. The evolution of engineering design is described along with the shortcomings of current product development techniques. The need for ISE to create high-science payoff missions and aerospace systems at affordable costs is discussed. The five major components critical to ISE and some of their sub-elements are described: namely, human-ISE interaction; infrastructure for distributed collaboration; rapid synthesis and simulation tools; intelligent life-cycle system integration; and cultural change in the creative process. Related government and industry programs are outlined and future impact of ISE on complex missions and aerospace systems is discussed.
C1 [Noor, Ahmed K.] Univ Virginia, Ctr Adv Computat Technol, Langley Res Ctr, NASA, Hampton, VA 23681 USA.
[Venneri, Samuel L.] NASA Headquarters, Washington, DC 20546 USA.
RP Noor, AK (reprint author), Univ Virginia, Ctr Adv Computat Technol, Langley Res Ctr, NASA, Hampton, VA 23681 USA.
NR 10
TC 1
Z9 1
U1 0
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 0885-8985
J9 IEEE AERO EL SYS MAG
JI IEEE Aerosp. Electron. Syst. Mag.
PD APR
PY 2008
VL 23
IS 4
BP 31
EP 44
DI 10.1109/MAES.2008.4493440
PG 14
WC Engineering, Aerospace; Engineering, Electrical & Electronic
SC Engineering
GA 332HX
UT WOS:000258075200006
ER
PT J
AU Gitelson, AA
Vina, A
Masek, JG
Verma, SB
Suyker, AE
AF Gitelson, Anatoly A.
Vina, Andres
Masek, Jeffrey G.
Verma, Shashi B.
Suyker, Andrew E.
TI Synoptic monitoring of gross primary productivity of maize using Landsat
data
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE optical imaging; remote sensing; vegetation mapping
ID NET PRIMARY PRODUCTION; LIGHT-USE EFFICIENCY; TERRESTRIAL GROSS;
VEGETATION INDEX; CO2 EXCHANGE; EOS-MODIS; REFLECTANCE; ECOSYSTEM;
CHLOROPHYLL; MODEL
AB There is a growing interest in monitoring the gross primary productivity (GPP) of crops due mostly to their carbon sequestration potential. Both within- and between-field variability are important components of crop GPP monitoring, particularly for the estimation of carbon budgets. In this letter, we present a new technique for daytime GPP estimation in maize based,on the close and consistent relationship between GPP and crop chlorophyll content, and entirely on remotely sensed data. A recently proposed chlorophyll index (CI), which involves green and near-infrared spectral bands, was used to retrieve daytime GPP from Landsat Enhanced Thematic Mapper Plus (ETM+) data. Because of its high spatial resolution (i.e., 30 x 30 m/pixel), this satellite system is particularly appropriate for detecting not only between- but also within-field GPP variability during the growing season. The CI obtained using atmospherically corrected Landsat ETM+ data was found to be linearly related with daytime maize GPP: root mean squared error of less than 1.58 gC.m(-2).d(-1) in a GPP range of 1.88 to 23.1 gC.m(-2).d(-1); therefore, it constitutes an accurate surrogate measure for GPP estimation. For comparison purposes, other vegetation indices were also tested. These results open new possibilities for analyzing the spatiotemporal variation of the GPP of crops using the extensive archive of Landsat imagery acquired since the early 1980s.
C1 [Gitelson, Anatoly A.; Verma, Shashi B.; Suyker, Andrew E.] Univ Nebraska, Sch Nat Resources, Lincoln, NE 68588 USA.
[Vina, Andres] Michigan State Univ, Dept Fisheries & Wildlife, Ctr Syst Integrat & Sustainabil, E Lansing, MI 48824 USA.
[Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
RP Gitelson, AA (reprint author), Univ Nebraska, Sch Nat Resources, Lincoln, NE 68588 USA.
RI Masek, Jeffrey/D-7673-2012; Gitelson, Anatoly/G-3452-2012
FU NASA Land Cover and Land Use Change Program [NNG06GG17G]; U.S.
Department of Energy (DoE) EPSCoR [DE-FG-02-00ER45827]; DoE Office of
Science (BER) [DE-FG02-03ER63639]
FX This work was supported by in part by the NASA Land Cover and Land Use
Change Program under Grant NNG06GG17G, in part by the U.S. Department of
Energy (DoE) EPSCoR program under Grant DE-FG-02-00ER45827 and the DoE
Office of Science (BER) under Grant DE-FG02-03ER63639, and in part by
the Hatch Act.
NR 35
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U1 1
U2 23
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1545-598X
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD APR
PY 2008
VL 5
IS 2
BP 133
EP 137
DI 10.1109/LGRS.2008.915598
PG 5
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 342EH
UT WOS:000258766900003
ER
PT J
AU Halthore, RN
Shettle, EP
Markham, BL
Mango, SA
AF Halthore, Rangasayi N.
Shettle, Eric P.
Markham, Brian L.
Mango, Stephen A.
TI Role of aerosol absorption in satellite sensor calibration
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE aerosol absorption; vicarious calibration; Visible/Infrared
Imager/Radiometer Suite (VIIRS)
ID PERFORMANCE
AB The importance of aerosol absorption in satellite sensor vicarious calibration and/or satellite measurement of physical parameters is reiterated in a sensitivity study performed using a radiative transfer model, with field-measured data as input. Broadband shortwave surface fluxes need to be measured according to new protocols, described herein, to infer atmospheric absorption to improve calibration accuracy to within the +/- 2% stated goal of next-generation sensors such as Visible/Infrared Imager/Radiometer Suite.
C1 [Halthore, Rangasayi N.; Shettle, Eric P.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA.
[Halthore, Rangasayi N.] NASA Headquarters, Washington, DC 20546 USA.
[Markham, Brian L.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Mango, Stephen A.] Natl Polar Orbiting Operat Environm Satellite Sys, Integrated Program Off, Silver Spring, MD 20910 USA.
RP Halthore, RN (reprint author), USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA.
RI Markham, Brian/M-4842-2013
OI Markham, Brian/0000-0002-9612-8169
FU Integrated Program Office, National Polar-orbiting Operational
Environmental Satellite System; NRL
FX This work was supported in part by the Integrated Program Office,
National Polar-orbiting Operational Environmental Satellite System and
in part by the NRL 6.1 under the in-house funding for aerosol research.
NR 16
TC 0
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U1 1
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1545-598X
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD APR
PY 2008
VL 5
IS 2
BP 157
EP 161
DI 10.1109/LGRS.2008.915735
PG 5
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 342EH
UT WOS:000258766900008
ER
PT J
AU Wenny, BN
Xiong, X
AF Wenny, Brian N.
Xiong, Xiaoxiong
TI Using a cold earth surface target to characterize long-term stability of
the MODIS thermal emissive bands
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE calibration stability; Moderate Resolution Imaging Spectroradiometer
(MODIS); remote sensing; thermal emissive bands (TEB)
ID DOME-C; ANTARCTICA
AB The Moderate Resolution Imaging Spectroradiometer (MODIS) has successfully provided Earth image products for instruments on the Terra and Aqua satellites since 2000 and 2002, respectively. Maintaining accurate radiometric calibration and calibration consistency between two sensors is an important issue for continued quality of long-term data records, especially as the instruments operate beyond their original projected mission lifetime. A strategy to use frequent MODIS measurements of the brightness temperature of the land surface in the area surrounding Dome Concordia, Antarctica (75.1 degrees S, 123.4 degrees E) to track the long-term stability of MODIS Band 31 is presented. Dome Concordia, located on the Antarctic plateau, is one of the most homogeneous land surfaces on Earth in terms of surface temperature and emissivity, with a seasonal temperature range of 190-250 K. The extremely dry, cold, and rarefied atmosphere of the site makes it ideal to track and detect any long-term changes in the MODIS thermal band response through trend analyses of near-nadir MODIS overpass data in conjunction with surface temperature measurements. Application of this approach shows an average relative bias between Terra and Aqua MODIS Band 31 (11 mu m) measurements of -0.08 K, which is well within the calibration uncertainty.
C1 [Wenny, Brian N.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
RP Wenny, BN (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
NR 18
TC 25
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U1 0
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1545-598X
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD APR
PY 2008
VL 5
IS 2
BP 162
EP 165
DI 10.1109/LGRS.2008.915603
PG 4
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 342EH
UT WOS:000258766900009
ER
PT J
AU Zhan, XW
Crow, WT
Jackson, TJ
O'Neill, PE
AF Zhan, Xiwu
Crow, Wade T.
Jackson, Thomas J.
O'Neill, Peggy E.
TI Improving spaceborne radiometer soil moisture retrievals with
alternative aggregation rules for ancillary parameters in highly
heterogeneous vegetated areas
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE microwave; remote sensing; soil moisture
ID MICROWAVE; BAND
AB Retrieving soil moisture from spaceborne microwave radiometer observations often requires ancillary parameters such as surface vegetation opacity or vegetation water content (VWC). The conventional approach for deriving representative footprint-scale values of these parameters is to simply average the corresponding parameters of high-resolution pixels over the entire radiometer footprint. However, previous work has shown that simple averaging of ancillary parameter values may result in biased soil moisture retrievals from spaceborne radiometers. This letter uses a synthetic observing-system simulation experiment framework to theoretically demonstrate that ancillary VWC or canopy-opacity parameter values obtained with an alternative aggregation rule may significantly reduce the magnitude of soil moisture retrieval errors for highly heterogeneous vegetated areas.
C1 [Zhan, Xiwu] NOAA, Natl Environm Satellite Data & Informat Serv, Camp Springs, MD 20746 USA.
[Crow, Wade T.; Jackson, Thomas J.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
[O'Neill, Peggy E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zhan, XW (reprint author), NOAA, Natl Environm Satellite Data & Informat Serv, Camp Springs, MD 20746 USA.
EM xiwu.zhan@noaa.gov
RI Zhan, Xiwu/F-5487-2010; O'Neill, Peggy/D-2904-2013
FU National Aeronautics and Space Administration [NAG8-1517, NAG5-6494];
National Oceanic and Atmospheric Administration [NA96GP0413]
FX This work was supported in part by the National Aeronautics and Space
Administration under Grants NAG8-1517 and NAG5-6494 and in part by the
National Oceanic and Atmospheric Administration under Grant NA96GP0413.
The views, opinions, and findings contained in this paper 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 13
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U1 0
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1545-598X
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD APR
PY 2008
VL 5
IS 2
BP 261
EP 265
DI 10.1109/LGRS.2008.915931
PG 5
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 342EH
UT WOS:000258766900030
ER
PT J
AU Durden, SL
Tanelli, S
AF Durden, S. L.
Tanelli, S.
TI Predicted effects of nonuniform beam filling on GPM radar data
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE attenuation; meteorological radar; rain
ID TRMM PRECIPITATION RADAR; RETRIEVAL; RAIN
AB The Global Precipitation Measurement mission (GPM) will carry the first dual-frequency spaceborne radar (DPR) for rainfall observation. We use dual-frequency airborne radar data to simulate observations at GPM DPR resolution and frequencies and to investigate errors due to nonuniform beam filling effects. Errors at Ku-band are similar to those found in previous studies. Errors in the Ka-band path-integrated attenuation and near-surface reflectivity are larger than at Ku-band. Errors in rain-top reflectivity, where attenuation is neglected, are smaller at Ka-band than at Ku-band because the Ka-band Z-R relation is closer to being linear.
C1 [Durden, S. L.; Tanelli, S.] 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 NASA
FX The research described here was performed at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration. Support from the NASA
Precipitation Measurement Missions program is gratefully acknowledged.
NR 9
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U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1545-598X
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD APR
PY 2008
VL 5
IS 2
BP 308
EP 310
DI 10.1109/LGRS.2008.916068
PG 3
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 342EH
UT WOS:000258766900040
ER
PT J
AU Shen, SH
Leptoukh, GG
Acker, JG
Yu, ZJ
Kempler, SJ
AF Shen, Suhung
Leptoukh, Gregory G.
Acker, James G.
Yu, Zuojun
Kempler, Steven J.
TI Seasonal variations of chlorophyll a concentration in the northern South
China Sea
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE data management; ocean color; remote sensing
ID LUZON
AB Monthly climatology of chlorophyll a concentration (chl a) based on nine years of SeaWiFS data is used to illustrate seasonal variations and spatial structures in the northern South China Sea (SCS). Chl a starts to increase in September at the northern coast of Luzon Island, continues to increase in the autumn, and reaches its maximum in December or January. Maximum chl a is centered in the northern SCS off the northwestern coast of Luzon Island. Chl a starts to decrease gradually in February, and its values become very low from June to August. The region of elevated chl a during the winter bloom season is funnel shaped, with the narrow end at the northern coast of Luzon Island, where the chl a value is highest and opening toward the northwest. The sea surface temperature (SST) in this funnel-shaped region is significantly colder than SST in surrounding regions of the same latitude. The present study indicates that the winter blooms indicated by higher chl a and colder SST in the northern SCS are linked strongly to the local winter monsoon. The initial data exploration and analysis presented in this study was carried out using Giovanni, a state-of-the-art Web-based data analysis and visualization tool.
C1 [Shen, Suhung] George Mason Univ, Fairfax, VA 22030 USA.
[Shen, Suhung; Leptoukh, Gregory G.; Acker, James G.; Kempler, Steven J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Acker, James G.] RS Informat Syst Inc, Greenbelt, MD 20771 USA.
[Yu, Zuojun] Univ Hawaii, Int Pacific Res Ctr, Honolulu, HI 96822 USA.
RP Shen, SH (reprint author), George Mason Univ, Fairfax, VA 22030 USA.
EM Suhung.Shen@gsfc.nasa.gov
FU Goddard Earth Sciences Data and Information Services Center; National
Aeronautics and Space Administration [CAN 02-OES-01]; Ocean Color
Time-Series Project (PI, Watson Gregg)
FX The authors gratefully acknowledge the high-quality technical support
from the Giovanni team at the Goddard Earth Sciences Data and
Information Services Center. This work was supported partly by the
National Aeronautics and Space Administration CAN 02-OES-01, Ocean Color
Time-Series Project (PI, Watson Gregg).
NR 16
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U1 0
U2 9
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1545-598X
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD APR
PY 2008
VL 5
IS 2
BP 315
EP 319
DI 10.1109/LGRS.2008.915932
PG 5
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 342EH
UT WOS:000258766900042
ER
PT J
AU Radisic, V
Sawdai, D
Scott, D
Deal, WR
Dang, L
Li, D
Cavus, A
Fung, A
Samoska, L
To, R
Gaier, T
Lai, R
AF Radisic, Vesna
Sawdai, Donald
Scott, Dennis
Deal, William R.
Dang, Linh
Li, Danny
Cavus, Abdullah
Fung, Andy
Samoska, Lorene
To, Richard
Gaier, Todd
Lai, Richard
TI Demonstration of 184 and 255-GHz amplifiers using InPHBT technology
SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS
LA English
DT Article
DE amplifier; heterojunction bipolar transistor (HBT); MM-wave; monolithic
microwave integrated circuit (MMIC); sub-millimeter wave
ID G-BAND; MMIC AMPLIFIER; GHZ; 35-NM
AB In this letter, 184 and 255 GHz single-stage heterojunction bipolar transistor (HBT) amplifiers are reported. Each amplifier uses a single-emitter 0.4 mu m x 15 mu m InP HBT device with maximum frequency of oscillation (f(max)) greater than 500 GHz and f(T) of similar to 200 GHz. The 183 GHz single-stage amplifier has demonstrated gain of 4.3 +/- 0.4 dB for all sites on the wafer. The 255 GHz amplifier has measured gain of 3.5 dB and demonstrates the highest frequency measured HBT amplifier gain reported to date. Both amplifiers show excellent agreement with original simulation.
C1 [Radisic, Vesna; Sawdai, Donald; Scott, Dennis; Deal, William R.; Dang, Linh; Li, Danny; Cavus, Abdullah; To, Richard; Lai, Richard] Northrop Grumman Corp, Redondo Beach, CA USA.
[Fung, Andy; Samoska, Lorene; Gaier, Todd] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Radisic, V (reprint author), Northrop Grumman Corp, Redondo Beach, CA USA.
EM vesna@ieee.org
NR 10
TC 16
Z9 16
U1 0
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1531-1309
J9 IEEE MICROW WIREL CO
JI IEEE Microw. Wirel. Compon. Lett.
PD APR
PY 2008
VL 18
IS 4
BP 281
EP 283
DI 10.1109/LMWC.2008.918952
PG 3
WC Engineering, Electrical & Electronic
SC Engineering
GA 288JC
UT WOS:000254981500021
ER
PT J
AU Wang, JR
Racette, PE
Pieprneier, JR
AF Wang, James R.
Racette, Paul E.
Pieprneier, Jeffrey R.
TI A comparison of near-concurrent measurements from the SSMIS and CoSMIR
for some selected channels over the frequency range of 50-183 GHz
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE calibration; microwave; radiometer; Special Sensor Microwave
Imager/Sounder (SSMIS)
ID ATMOSPHERIC WATER-VAPOR
AB Ten underflights of the Special Sensor Microwave Imager/Sounder (SSMIS) with Conical Scanning Millimeter-wave Imaging Radiometer (CoSMIR) onboard the NASA ER-2 aircraft were conducted over the coastal region of California between March 2004 and March 2005. The measured brightness temperature (T-b) values from both sensors are collocated and compared at frequencies of 50.3, 52.8, 53.6, 91.655, 150,183.3 +/- 1, 183.3 +/- 3, and 183.3 +/- 6.6 GHz. The more transparent channels at 50.3, 91.655, and 150 GHz are strongly affected by the changes in surface emission and low-level liquid clouds. Thus, the average differences in T-b, values (delta T-b), measured by the two sensors, and their changes from flight to flight are difficult to assess. For the remaining opaque channels, using the CoSMIR measurements as reference, the lowest SSMIS Tb values occur when the SSMIS is completely under the Earth's shadow. As the satellite moves out of the Earth's shadow in the ascending passes, the SSMIS Tb values are found to gradually increase with more exposure to the sun. The magnitudes of these T-b changes are about 4-5 K for the three 183.3-GHz channels and about 2 K for the 52.8- and 53.6-GHz channels.
C1 [Wang, James R.; Racette, Paul E.; Pieprneier, Jeffrey R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Wang, JR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM james.r.wang@nasa.gov
NR 8
TC 7
Z9 7
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD APR
PY 2008
VL 46
IS 4
BP 923
EP 933
DI 10.1109/TGRS.2007.904038
PN 1
PG 11
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 285YJ
UT WOS:000254811800006
ER
PT J
AU Swadley, SD
Poe, GA
Bell, W
Hong, Y
Kunkee, DB
McDermid, S
Leblanc, T
AF Swadley, Steven D.
Poe, Gene A.
Bell, William
Hong, Ye
Kunkee, David B.
McDermid, Stuart
Leblanc, Thierry
TI Analysis and characterization of the SSMIS upper atmosphere sounding
channel measurements
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE calibration; Doppler frequency shift; microwave; polarized radiative
transfer; radiometer; Special Sensor Microwave Imager/Sounder (SSMIS);
Zeeman effect
ID TEMPERATURE-MEASUREMENTS; OXYGEN; MESOSPHERE; FIELD; MODEL; PROPAGATION;
FREQUENCIES; VALIDATION; SPECTRUM; MIDDLE
AB Analyses and results of the radiometric calibration accuracy and measurement characteristics of the first Defense Meteorological Satellite Program (DMSP)'s Special Sensor Microwave Imager/Sounder (SSMIS) upper atmosphere sounding (IJAS) channels are presented herein. Launched on October 18, 2003, aboard the DMSP F-16 spacecraft in a sun-synchronous orbit, the SSMIS UAS channels provide the first operational measurements of microwave radiation emitted by the Earth's atmosphere at mesospheric altitudes. The analysis of the SSMIS radiometer absolute calibration and stability is based upon extensive comparisons with a fully polarimetric radiative transfer model (RTM) that solves for all four Stokes parameters using coincident atmospheric temperature profiles derived from collocated Rayleigh lidar observations merged with the European Centre for Medium-Range Weather Forecasting temperature analyses and climatological data sets. The resulting merged profiles provide a physically consistent temperature profile from the surface to 100 km, as needed by the RTMs. The results presented herein of the SSMIS instrument show that significant hardware and scientific technical challenges arise from microwave temperature sounding of the mesosphere. These include the following: 1) addressing the impact of large noise-equivalent temperature difference associated with narrow channel bandwidths; 2) achieving high channel center-frequency stability; 3) compensation of large spacecraft-induced Doppler shift; 4) better characterization of the Zeeman splitting of the oxygen absorption lines; 5) development of a fast polarimetric RTM; and 6) designing stable and accurate on-orbit radiometric calibration targets. Results to date show that the uncertainties of the calibration accuracy of the SSMIS UAS channels are consistent and in agreement with the limits derived for the SSMIS UAS channels and with the simulated radiances derived from the merged lidar profiles.
C1 [Swadley, Steven D.] METOC Consulting, Monterey, CA 93943 USA.
[Swadley, Steven D.; Poe, Gene A.] USN, Res Lab, Monterey, CA 93943 USA.
[Bell, William] Satellite Radiance Assimilat Grp, Met Off, Exeter EX1 3PB, Devon, England.
[Hong, Ye; Kunkee, David B.] Aerosp Corp, El Segundo, CA 90245 USA.
[McDermid, Stuart; Leblanc, Thierry] CALTECH, Jet Prop Lab, Table Mt Facil, Wrightwood, CA 92397 USA.
RP Swadley, SD (reprint author), METOC Consulting, Monterey, CA 93943 USA.
EM steve.swadley@nrlmry.navy.mil
NR 35
TC 14
Z9 14
U1 0
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD APR
PY 2008
VL 46
IS 4
BP 962
EP 983
DI 10.1109/TGRS.2008.916980
PN 1
PG 22
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 285YJ
UT WOS:000254811800009
ER
PT J
AU Freeman, A
AF Freeman, A.
TI Response to "Corrections to 'Calibration of linearly polarized
polarimetric SAR data subject to faraday rotation'"
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Letter
DE cafibration; Faraday rotation; polarimetry; syntethic aperture radar
(SAR)
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Freeman, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 2
TC 2
Z9 2
U1 0
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD APR
PY 2008
VL 46
IS 4
BP 1279
EP 1279
DI 10.1109/TGRS.2008.919875
PN 2
PG 1
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 285YL
UT WOS:000254812000022
ER
PT J
AU Schulze-Makuch, D
Fairen, AG
Davila, AF
AF Schulze-Makuch, Dirk
Fairen, Alberto G.
Davila, Alfonso F.
TI The case for life on Mars
SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY
LA English
DT Review
DE Life; Mars; water; habitability; Viking; ALH84001; Panspermia
ID MARTIAN METEORITE ALH84001; BACILLUS-SUBTILIS SPORES; GAS-EXCHANGE
EXPERIMENT; LONG-TERM SURVIVAL; MAGNETOTACTIC BACTERIA; MAGNETITE
CRYSTALS; NORTHERN PLAINS; MICROBIAL METHANOGENESIS; EXTREME
ENVIRONMENTS; ATMOSPHERIC METHANE
AB There have been several attempts to answer the question of whether there is. or has ever been. life oil Mars. The boldest attempt was the only ever life detection experiment conducted oil another planet : the Viking mission. The mission was a great Success, but it failed to provide I clear answer to the question of life Oil Mars. More than 30 years after the Viking mission our understanding of the history and evolution of Mars, has increased vastly to reveal,I wetter Martian past and the Occurrence of diverse environments that Could have Supported microbial life similar to that oil Earth for extended periods of time. The discovery of Terran extremophilic microorganisms. adapted to environments previously though to be Prohibitive for lifer has greatly expanded the limits of habitability in our Solar System, and has opened new avenues For the search of life oil Mars. Remnants of a possible early biosphere may be found in the Martian meteorite ALH84001. This claim is based oil I collection of facts and observations consistent with biogenic origins, but individual links in the collective chain of evidence remain controversial. Recent evidence for contemporary liquid water oil Mars and the detection of methane in the Martian atmosphere further enhance the case for life oil Mars. We argue that. given the cumulative evidence provided, life has and is likely to exist oil Mars, and we have already found evidence of it. However, to obtain a compelling certainty a new, mission is needed. one which is devoted to the detection of life oil mars.
C1 [Schulze-Makuch, Dirk] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99163 USA.
[Fairen, Alberto G.; Davila, Alfonso F.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Washington, DC 20546 USA.
RP Schulze-Makuch, D (reprint author), Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99163 USA.
EM dirksm@wsu.edu
RI Davila, Alfonso/A-2198-2013;
OI Davila, Alfonso/0000-0002-0977-9909; Schulze-Makuch,
Dirk/0000-0002-1923-9746
NR 219
TC 18
Z9 18
U1 15
U2 58
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 1473-5504
EI 1475-3006
J9 INT J ASTROBIOL
JI Int. J. Astrobiol.
PD APR
PY 2008
VL 7
IS 2
BP 117
EP 141
DI 10.1017/S1473550408004175
PG 25
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 541AL
UT WOS:000273382900003
ER
PT J
AU Coyne, JT
Baldwin, CL
Latorella, KA
AF Coyne, Joseph T.
Baldwin, Caffyl L.
Latorella, Kara A.
TI Pilot weather assessment: Implications for visual flight rules flight
into instrument meteorological conditions
SO INTERNATIONAL JOURNAL OF AVIATION PSYCHOLOGY
LA English
DT Article
ID ADVERSE WEATHER; DECISIONS
AB Visual flight rules flight into instrument meteorological conditions (IMC) account for over 10% of the fatalities in general aviation. Evidence suggests that pilots' assessments of weather conditions are related to their decision to continue. This study investigated pilots'ability to assess ceiling and visibility in a flight simulator. Assessment accuracy did not differ between instrument- and non-instrument-rated pilots for ceiling accuracy, but visibility accuracy was better for non-instrument-rated pilots. The data indicated pilots allowed their estimates of ceiling and visibility to influence each other. That is, pilots tended to judge a ceiling to be higher than it actually was when it was paired with a high visibility. This interaction may play a significant role in pilots' decisions to continue into IMC.
C1 [Coyne, Joseph T.] USN, Res Lab, Washington, DC 20375 USA.
[Baldwin, Caffyl L.] Old Dominion Univ, Norfolk, VA USA.
[Latorella, Kara A.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Coyne, JT (reprint author), USN, Res Lab, Code 5511,4555 Overlook Ave SW, Washington, DC 20375 USA.
EM coyne@itd.nrl.navy.mil
NR 12
TC 2
Z9 2
U1 1
U2 2
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA
SN 1050-8414
J9 INT J AVIAT PSYCHOL
JI Int. J. Aviat. Psychol.
PD APR-JUN
PY 2008
VL 18
IS 2
BP 153
EP 166
DI 10.1080/10508410801926756
PG 14
WC Psychology, Applied
SC Psychology
GA 294NO
UT WOS:000255413000002
ER
PT J
AU Huebner, LD
Hall, RM
Haynes, DA
Pamadi, BN
Taylor, TL
Seaford, CM
AF Huebner, Lawrence D.
Hall, Robert M.
Haynes, Davy A.
Pamadi, Bandu N.
Taylor, Terry L.
Seaford, C. Mark
TI Status, plans and initial results for Ares I Crew Launch Vehicle
aerodynamics
SO JBIS-JOURNAL OF THE BRITISH INTERPLANETARY SOCIETY
LA English
DT Article; Proceedings Paper
CT 57th International Astronautical Congress
CY OCT 02-06, 2006
CL Valencia, SPAIN
DE Ares I Crew Launch Vehicle; aerodynamics; wind tunnel testing;
computational fluid dynamics
AB Following the completion of NASA's Exploration Systems Architecture Study in August 2004 for the NASA Exploration Systems Mission Directorate (ESMD), the Ares Projects Office at the NASA Marshall Space Flight Center was assigned project management responsibilities for the design and development of the first vehicle in the architecture, the Ares I Crew Launch Vehicle (CLV), which will be used to launch astronauts to low earth orbit and rendezvous with either the International Space Station or the ESMD's earth departure stage for lunar or other future missions beyond low Earth orbit. The primary elements of the Ares I CLV project are the first stage, the upper stage, the upper stage engine, and vehicle integration. Within vehicle integration is an effort in integrated design and analysis which is comprised of a number of technical disciplines needed to support vehicle design and development. One of the important disciplines throughout the life of the project is aerodynamics. This paper will present the status, plans, and initial results of Ares I CLV aerodynamics as the project was preparing for the Ares I CLV Systems Requirements Review. Following a discussion of the specific interactions with other technical panels and a status of the current activities, the plans for aerodynamic support of the Ares I CLV until the initial crewed flights will be presented.
C1 [Huebner, Lawrence D.; Hall, Robert M.; Pamadi, Bandu N.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Haynes, Davy A.; Taylor, Terry L.; Seaford, C. Mark] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Huebner, LD (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM Lawrence.D.Huebner@nasa.gov; Robert.M.Hall@nasa.gov;
Davy.A.Haynes@nasa.gov; Bandu.N.Pamadi@nasa.gov;
Terry.L.Taylor@nasa.gov; Dr.C.Seaford@nasa.gov
NR 2
TC 2
Z9 2
U1 0
U2 0
PU BRITISH INTERPLANETARY SOC
PI LONDON
PA 27-29 S LAMBETH RD, LONDON SW8 1SZ, ENGLAND
SN 0007-084X
J9 JBIS-J BRIT INTERPLA
JI JBIS-J. Br. Interplanet. Soc.
PD APR
PY 2008
VL 61
IS 4
BP 128
EP 138
PG 11
WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences,
Multidisciplinary
SC Engineering; Astronomy & Astrophysics; Geology
GA 275AG
UT WOS:000254043700003
ER
PT J
AU Jiang, HY
Halverson, JB
Simpson, J
Zipser, EJ
AF Jiang, Haiyan
Halverson, Jeffrey B.
Simpson, Joanne
Zipser, Edward J.
TI Hurricane "Rainfall Potential" derived from satellite observations aids
overland rainfall prediction
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID MICROWAVE SOUNDING UNIT; ATLANTIC TROPICAL CYCLONES; PRECIPITATION
CHARACTERISTICS; GLOBAL PRECIPITATION; STORM RAINFALL; TRAP TECHNIQUE;
PART II; ALGORITHMS; INTENSITY; LANDFALL
AB The Tropical Rainfall Measuring Mission-based National Aeronautics and Space Administration Goddard Multisatellite Precipitation Analysis (MPA) product is used to quantify the rainfall distribution in tropical cyclones that made landfall in the United States during 1998-2004. A total of 37 tropical cyclones (TC) are examined, including 2680 three-hourly MPA precipitation observations. Rainfall distributions for overland and overocean observations are compared. It is found that the TC rainfall over ocean bears a strong relationship with the TC maximum wind, whereas the relationship for overland conditions is much weaker. The rainfall potential is defined by using the satellite-derived rain rate, the satellite-derived storm size, and the storm translation speed. This study examines the capability of the overocean rainfall potential to predict a storm's likelihood of producing heavy rain over land. High correlations between rain potentials before landfall and the maximum storm total rain over land are found using the dataset of the 37 landfalling TCs. Correlations are higher with the average rain potential on the day prior to landfall than with averages over any other time period. A TC overland rainfall index is introduced based on the rainfall potential study. This index can be used to predict the storm peak rainfall accumulation over land. Six landfalling storms during the 2005 Atlantic Ocean hurricane season are examined to verify the capability of using this index to forecast the maximum storm total rain over land in the United States. The range of the maximum storm overland rain forecast error for these six storms is between 2.5% and 24.8%.
C1 [Jiang, Haiyan; Halverson, Jeffrey B.] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21201 USA.
[Jiang, Haiyan] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Branch, Greenbelt, MD 20771 USA.
[Simpson, Joanne] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Zipser, Edward J.] Univ Utah, Dept Meteorol, Salt Lake City, UT 84112 USA.
RP Jiang, HY (reprint author), 135 S 1460 E,Rm 819 WBB, Salt Lake City, UT 84112 USA.
EM h.jiang@utah.edu
NR 35
TC 13
Z9 13
U1 0
U2 3
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD APR
PY 2008
VL 47
IS 4
BP 944
EP 959
DI 10.1175/2007JAMC1619.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 302RG
UT WOS:000255986400002
ER
PT J
AU Arguez, A
Yu, P
O'Brien, JJ
AF Arguez, Anthony
Yu, Peng
O'Brien, James J.
TI A new method for time series filtering near endpoints
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID TEMPERATURES; OSCILLATION
AB Time series filtering (e. g., smoothing) can be done in the spectral domain without loss of endpoints. However, filtering is commonly performed in the time domain using convolutions, resulting in lost points near the series endpoints. Multiple incarnations of a least squares minimization approach are developed that retain the endpoint intervals that are normally discarded due to filtering with convolutions in the time domain. The techniques minimize the errors between the predetermined frequency response function (FRF) - a fundamental property of all filters - of interior points with FRFs that are to be determined for each position in the endpoint zone. The least squares techniques are differentiated by their constraints: 1) unconstrained, 2) equal-mean constraint, and 3) an equal-variance constraint. The equal-mean constraint forces the new weights to sum up to the same value as the predetermined weights. The equal-variance constraint forces the new weights to be such that, after convolved with the input values, the expected time series variance is preserved. The three least squares methods are each tested under three separate filtering scenarios [involving Arctic Oscillation (AO), Madden-Julian oscillation (MJO), and El Nino-Southern Oscillation (ENSO) time series] and compared to each other as well as to the spectral filtering method - the standard of comparison. The results indicate that all four methods (including the spectral method) possess skill at determining suitable endpoints estimates. However, both the unconstrained and equal-mean schemes exhibit bias toward zero near the terminal ends due to problems with appropriating variance. The equal-variance method does not show evidence of this attribute and was never the worst performer. The equal-variance method showed great promise in the ENSO project involving a 5-month running mean filter, and performed at least on par with the other realistic methods for almost all time series positions in all three filtering scenarios.
C1 [Arguez, Anthony] NOAA, NCDC, Asheville, NC 28801 USA.
[Yu, Peng] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[O'Brien, James J.] Ctr Ocean Atmospher Predict Studies, Tallahassee, FL USA.
RP Arguez, A (reprint author), NOAA, NCDC, CAB 514,151 Patton Ave, Asheville, NC 28801 USA.
EM anthony.arguez@noaa.gov
NR 13
TC 8
Z9 8
U1 1
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
EI 1520-0426
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD APR
PY 2008
VL 25
IS 4
BP 534
EP 546
DI 10.1175/2007JTECHA924.1
PG 13
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 291CF
UT WOS:000255169200003
ER
PT J
AU Su, WY
Dutton, E
Charlock, TP
Wiscombe, W
AF Su, Wenying
Dutton, Ellsworth
Charlock, Thomas P.
Wiscombe, Warren
TI Performance of commercial radiometers in very low temperature and
pressure environments typical of polar regions and of the stratosphere:
A laboratory study
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID LONGWAVE IRRADIANCE UNCERTAINTY; THERMAL OFFSET; RADIATION;
PYRGEOMETERS; CALIBRATION
AB Characterizing the performance of ground-based commercial radiometers in cold and/or low-pressure environments is critical for developing accurate flux measurements in the polar regions and in the upper troposphere and stratosphere. Commercially available broadband radiometers have a stated operational temperature range of, typically, -20 degrees to +50 degrees C. Within this range, their temperature dependencies of sensitivities change less than 1%. But for deployments on high-altitude platforms or in polar regions, which can be much colder than -20 degrees C, information on temperature dependency of sensitivity is not always available. In this paper, the temperature dependencies of sensitivities of popular pyranometers and pyrgeometers manufactured by Kipp and Zonen were tested in a thermal-vacuum chamber. When their body temperature is lowered to -60 degrees C, pyranometer sensitivity drops by 4%-6% from the factory-default specification. Pyrgeometer sensitivity increases by 13% from the factory-default specification during a similar temperature change. When the chamber pressure is lowered from 830 to 6 hPa, the sensitivity decreases by about 2% for the pyranometer, and increases by about 2% for the pyrgeometer. Note that these temperature and pressure dependencies of sensitivities are specific for the instruments that were tested and should not be applied to others. These findings show that for measurements suitable for climate studies, it is crucial to characterize temperature and/or pressure effects on radiometer sensitivity for deployments on high-altitude platforms and in polar regions.
C1 [Su, Wenying; Charlock, Thomas P.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Su, Wenying] Sci Syst & Applicat Inc, Hampton, VA USA.
[Dutton, Ellsworth] NOAA, Global Monitoring Div, Boulder, CO USA.
[Wiscombe, Warren] NASA, Goddard Space Flight Ctr, Hampton, VA 23681 USA.
RP Su, WY (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
EM wenying.su-1@nasa.gov
RI Wiscombe, Warren/D-4665-2012
OI Wiscombe, Warren/0000-0001-6844-9849
NR 18
TC 3
Z9 3
U1 0
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD APR
PY 2008
VL 25
IS 4
BP 558
EP 569
DI 10.1175/2007JTECHA1005.1
PG 12
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 291CF
UT WOS:000255169200005
ER
PT J
AU Xu, KM
Wong, T
Wielicki, BA
Parker, L
AF Xu, Kuan-Man
Wong, Takmeng
Wielicki, Bruce A.
Parker, Lindsay
TI Statistical analyses of satellite cloud object data from CERES. Part IV:
Boundary layer cloud objects during 1998 El Nino
SO JOURNAL OF CLIMATE
LA English
DT Article
ID MARINE STRATOCUMULUS CLOUDS; ANGULAR-DISTRIBUTION MODELS; RADIATIVE FLUX
ESTIMATION; ENERGY SYSTEM INSTRUMENT; SURFACE OBSERVATIONS;
GENERAL-CIRCULATION; STRATIFORM CLOUDS; LIQUID WATER; ISCCP; PACIFIC
AB Three boundary layer cloud object types-overcast, stratocumulus, and cumulus-that occurred over the Pacific Ocean during January-August 1998 are identified from the Clouds and the Earth's Radiant Energy System (CERES) single scanner footprint data. Characteristics of each cloud object type matched with atmospheric states are examined for large regions in the tropics and subtropics and for different size categories. Stratocumulus cloud objects dominate the entire boundary layer cloud population in all regions and size categories. Overcast cloud objects, which have the largest average size, are more prevalent in the subtropics and near the coastal regions, while cumulus cloud objects are prevalent over the open oceans and the equatorial regions, particularly within the small-size categories. Cloud objects with equivalent diameters less than 75 km are excluded in the analysis.
The differences between the tropical and subtropical statistical distributions of cloud properties are small for liquid water path (LWP), cloud optical depth, and top-of-the-atmosphere (TOA) albedo, but large for cloud-top temperature and outgoing longwave radiation (OLR), for each of the three cloud object types. The larger cloud objects have higher LWPs, cloud optical depths, TOA albedos, and OLRs, but lower SSTs and cloud-top heights for the stratocumulus and overcast types. Lower-tropospheric stability seems to be the primary factor for the differences in the distributions of cloud physical properties between the regions or between the size categories. Atmospheric dynamics also play a role in determining the differences in the distributions of cloud physical properties between the size categories, but not a significant role for those between the types or between the regions. The latter may be due to uncertainties in the matched vertical velocity data. When the three cloud object types are combined in small regions, lower-tropospheric stability determines the transition of boundary layer cloud types along a Pacific transect. The proportion of each type is the most important factor for diagnosing the combined cloud properties along this transect, such as LWP, cloud optical depth, and TOA albedo. Atmospheric dynamics also play complicated roles in determining the combined cloud properties along this transect.
C1 [Xu, Kuan-Man; Wong, Takmeng; Wielicki, Bruce A.] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
[Parker, Lindsay] Sci Syst Applicat Inc, Hampton, VA USA.
RP Xu, KM (reprint author), NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
EM kuan-man.xu@nasa.gov
RI Xu, Kuan-Man/B-7557-2013
OI Xu, Kuan-Man/0000-0001-7851-2629
NR 49
TC 19
Z9 19
U1 0
U2 3
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
J9 J CLIMATE
JI J. Clim.
PD APR 1
PY 2008
VL 21
IS 7
BP 1500
EP 1521
DI 10.1175/2007JCLI1710.1
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 288RR
UT WOS:000255004000004
ER
PT J
AU Hartley, TT
Lorenzo, CF
AF Hartley, Tom T.
Lorenzo, Carl F.
TI Application of Incomplete Gamma Functions to the Initialization of
Fractional-Order Systems
SO JOURNAL OF COMPUTATIONAL AND NONLINEAR DYNAMICS
LA English
DT Article
CT ASME International Design Engineering Technical Conferences/Computers
and Information in Engineering Conference
CY SEP 04-07, 2007
CL Las Vegas, NV
SP ASME, Design Engn Div, ASME, Comp & Informat Engn Div
DE gamma function; fractional-order system initialization
AB This paper reviews some properties of the gamma function, particularly the incomplete gamma function and its complement, as a function of the Laplace variable s. The utility of these functions in the solution of initialization problems in fractional-order system theory is demonstrated. Several specific differential equations are presented, and their initialization responses are found for a variety of initializations. Both the time-domain and Laplace-domain solutions are obtained and compared. The complementary incomplete gamma function is shown to be essential in finding the Laplace-domain solution of a fractional-order differential equation.
C1 [Hartley, Tom T.] Univ Akron, Akron, OH 44325 USA.
[Lorenzo, Carl F.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Hartley, TT (reprint author), Univ Akron, Akron, OH 44325 USA.
EM thartley@uakron.edu; carl.f.lorenzo@nasa.gov
NR 4
TC 4
Z9 4
U1 1
U2 2
PU ASME-AMER SOC MECHANICAL ENG
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 1555-1423
J9 J COMPUT NONLIN DYN
JI J. Comput. Nonlinear Dyn.
PD APR
PY 2008
VL 3
IS 2
AR 021103
DI 10.1115/1.2833480
PG 6
WC Engineering, Mechanical; Mechanics
SC Engineering; Mechanics
GA 359QC
UT WOS:000260002200004
ER
PT J
AU Lorenzo, CF
Hartley, TT
AF Lorenzo, Carl F.
Hartley, Tom T.
TI Initialization of Fractional-Order Operators and Fractional Differential
Equations
SO JOURNAL OF COMPUTATIONAL AND NONLINEAR DYNAMICS
LA English
DT Article
CT ASME International Design Engineering Technical Conferences/Computers
and Information in Engineering Conference
CY SEP 04-07, 2007
CL Las Vegas, NV
SP ASME, Design Engn Div, ASME, Comp & Informat Engn Div
ID SYSTEMS
AB It has been known that the initialization of fractional operators requires time-varying functions, a complicating factor; This paper simplifies the process of initialization of fractional differential equations by deriving Laplace transforms for the initialized fractional integral and derivative that generalize those for the integer-order operators. The new transforms unify the initialization of systems of fractional and ordinary differential equations. The paper provides background on past work in the area and determines the Laplace transforms for the initialized fractional integral and fractional derivatives of any (real) order. An application provides insight and demonstrates the theory.
C1 [Lorenzo, Carl F.] NASA, Glenn Res Ctr, Div Instrumentat & Controls, Cleveland, OH 44135 USA.
[Hartley, Tom T.] Univ Akron, Dept Elect & Comp Engn, Akron, OH 44325 USA.
RP Lorenzo, CF (reprint author), NASA, Glenn Res Ctr, Div Instrumentat & Controls, Cleveland, OH 44135 USA.
NR 13
TC 18
Z9 18
U1 1
U2 6
PU ASME-AMER SOC MECHANICAL ENG
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 1555-1423
J9 J COMPUT NONLIN DYN
JI J. Comput. Nonlinear Dyn.
PD APR
PY 2008
VL 3
IS 2
AR 021101
DI 10.1115/1.2833585
PG 9
WC Engineering, Mechanical; Mechanics
SC Engineering; Mechanics
GA 359QC
UT WOS:000260002200002
ER
PT J
AU Nourgaliev, RR
Liou, MS
Theofanous, TG
AF Nourgaliev, R. R.
Liou, M. -S.
Theofanous, T. G.
TI Numerical prediction of interfacial instabilities: Sharp interface
method (SIM)
SO JOURNAL OF COMPUTATIONAL PHYSICS
LA English
DT Article
DE interfacial instability; interfacial flows; gas-liquid interfaces;
sharp-interface treatment; viscous Kelvin-Helmholtz instability; Yih
instability; Rayleigh-Taylor instability; instability-seeding in
numerical simulations
ID RAYLEIGH-TAYLOR INSTABILITY; INCOMPRESSIBLE 2-PHASE FLOWS; CHARACTERIZED
VISCOELASTIC FLUIDS; NAVIER-STOKES EQUATIONS; DRIVEN CHANNEL FLOW;
ADAPTIVE LEVEL SET; MULTIPHASE FLOW; SURFACE-TENSION; FRONT-TRACKING;
LINEAR-STABILITY
AB We introduce a sharp interface method (SIM) for the direct numerical simulation of unstable fluid-fluid interfaces. The method is based on the level set approach and the structured adaptive mesh refinement technology, endowed with a corridor of irregular, cut-cell grids that resolve the interfacial region to third-order spatial accuracy. Key in that regard are avoidance of numerical mixing, and a least-squares interpolation method that is supported by irregular datasets distinctly on each side of the interface. Results on test problems show our method to be free of the spurious current problem of the continuous surface force method and to converge, on grid refinement, at near-theoretical rates. Simulations of unstable Rayleigh-Taylor and viscous Kelvin-Helmholtz flows are found to converge at near-theoretical rates to the exact results over a wide range of conditions. Further, we show predictions of neutral-stability maps of the viscous Kelvin-Helmholtz flows (Yih instability), as well as self-selection of the most unstable wave-number in multimode simulations of Rayleigh-Taylor instability. All these results were obtained with a simple seeding of random infinitesimal disturbances of interface-shape, as opposed to seeding by a complete eigenmode. For other than elementary flows the latter would normally not be available, and extremely difficult to obtain if at all. Sample comparisons with our code adapted to mimic typical diffuse interface treatments were not satisfactory for shear-dominated flows. On the other hand the sharp dynamics of our method would appear to be compatible and possibly advantageous to any interfacial flow algorithm in which the interface is represented as a discrete Heaviside function. Published by Elsevier Inc.
C1 [Nourgaliev, R. R.; Theofanous, T. G.] Univ Calif Santa Barbara, Ctr Risk Studies & Safety, Santa Barbara, CA 93106 USA.
[Liou, M. -S.] NASA, Glenn Res Ctr, Aeroprop Div, Cleveland, OH USA.
RP Nourgaliev, RR (reprint author), Idaho Natl Lab, Idaho Falls, ID 83415 USA.
EM robert.nourgaliev@inl.gov; meng-sing.liou@grc.nasa.gov;
theo@engr.ucsb.edu
NR 74
TC 20
Z9 21
U1 0
U2 15
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0021-9991
J9 J COMPUT PHYS
JI J. Comput. Phys.
PD APR 1
PY 2008
VL 227
IS 8
BP 3940
EP 3970
DI 10.1016/j.jcp.2007.12.008
PG 31
WC Computer Science, Interdisciplinary Applications; Physics, Mathematical
SC Computer Science; Physics
GA 288BG
UT WOS:000254960600011
ER
PT J
AU Trunek, AJ
Neudeck, PG
Matocha, K
Dunne, G
AF Trunek, Andrew J.
Neudeck, Philip G.
Matocha, Kevin
Dunne, Greg
TI Increased nitrogen doping of thin lateral SiC cantilevers
SO JOURNAL OF CRYSTAL GROWTH
LA English
DT Article; Proceedings Paper
CT 15th International Conference on Crystal Growth
CY AUG 12-17, 2007
CL Salt Lake City, UT
SP ACCG
DE doping; cantilevers; chemical vapor deposition; mesas; silicon carbide;
MOS capacitors
ID EPITAXIAL-GROWTH; SURFACES; MESAS
AB We report on a recently-observed difference in nitrogen doping during the growth of homoepitaxial films grown on on-axis 4H-SiC (SiC-silicon carbide) substrates patterned with arrays of mesas. In particular, the doping of webbed cantilevered regions that grew laterally from the tops of mesas free of axial screw dislocations was observed to be significantly greater than solid mesas with screw dislocations that grew vertically along the [0001] c-axis. (c) 2007 Elsevier B.V. All rights reserved.
C1 [Trunek, Andrew J.] NASA Glenn, OAI, Cleveland, OH 44135 USA.
[Neudeck, Philip G.] NASA, Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA.
[Matocha, Kevin; Dunne, Greg] GE Global Res, Niskayuna, NY 12309 USA.
RP Trunek, AJ (reprint author), NASA Glenn, OAI, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA.
EM Andrew.J.Trunek@grc.nasa.gov
NR 12
TC 0
Z9 0
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0248
J9 J CRYST GROWTH
JI J. Cryst. Growth
PD APR
PY 2008
VL 310
IS 7-9
SI SI
BP 1794
EP 1798
DI 10.1016/j.jcrysgro.2007.11.029
PG 5
WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied
SC Crystallography; Materials Science; Physics
GA 300RP
UT WOS:000255843200090
ER
PT J
AU Gubinyi, Z
Batur, C
Sayir, A
Dynys, F
AF Gubinyi, Z.
Batur, C.
Sayir, A.
Dynys, F.
TI Electrical properties of PZT piezoelectric ceramic at high temperatures
SO JOURNAL OF ELECTROCERAMICS
LA English
DT Article
DE high temperature PZT piezoceramic; changes in electrical and mechanical
properties with respect to temperature
ID SINGLE-CRYSTALS; THERMODYNAMIC THEORY; PHASE-TRANSITIONS
AB Advanced aeronautic and space structures need active components that can function at high frequencies and temperatures. Piezoelectric materials can provide frequency response but their use at elevated temperatures is limited. The reason for the lack of insertion of piezoelectric for high temperature active component and sensors are two fold. First, the database of piezoelectric properties that describe the piezoelectric constants is lacking for high temperatures engineering applications. Most studies measure the dielectric constants to determine the Curie temperature but do not provide piezoelectric coefficients as a function of temperature. Second, piezoelectric materials with Curie temperature (T(C)) exceeding 500 degrees C are sought for aeronautics and aerospace applications. This investigation describes a measurement system that captures the impedance dependence upon temperature for piezoelectric materials. Commercially available lead zirconate titanate (PZT) was studied as to determine the piezoelectric activity to define the operating envelope with respect to temperature. The elastic properties (c(ijkl)(E)), piezoelectric coefficients (e(ik)(S)), dielectric properties (epsilon(S)(ik)), and electro-mechanical coupling factors were determined as a function of temperature. The coupling factor k(33) was found to be relatively constant to 200 degrees C and exhibit slight temperature dependence above 200 degrees C. The temperature sensitivity for both piezoelectric coefficient and electromechanical coupling factor were very small; the slopes Delta d(31)(T)/d(31)(T) and k(33)/k(33) were found to be 0.01 and (-0.07) respectively in the range of 120 to 200 degrees C. This measurement technique will populate databases that describe the piezoelectric properties of commercially available PZT piezoelectric materials. It can also facilitate the assessment of new piezoelectric materials that are currently being developed for higher temperature applications.
C1 [Gubinyi, Z.; Batur, C.] Univ Akron, Dept Mech Engn, Akron, OH 44325 USA.
[Sayir, A.; Dynys, F.] NASA Glenn Res Ctr, Cleveland, OH USA.
RP Batur, C (reprint author), Univ Akron, Dept Mech Engn, Akron, OH 44325 USA.
EM batur@uakron.edu
NR 27
TC 20
Z9 20
U1 1
U2 26
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1385-3449
J9 J ELECTROCERAM
JI J. Electroceram.
PD APR
PY 2008
VL 20
IS 2
BP 95
EP 105
DI 10.1007/s10832-007-9364-3
PG 11
WC Materials Science, Ceramics
SC Materials Science
GA 259DX
UT WOS:000252920400005
ER
PT J
AU De Witt, JK
Hagan, RD
Cromwell, RL
AF De Witt, John K.
Hagan, R. Donald
Cromwell, Ronita L.
TI The effect of increasing inertia upon vertical ground reaction forces
and temporal kinematics during locomotion
SO JOURNAL OF EXPERIMENTAL BIOLOGY
LA English
DT Article
DE biomechanics; locomotion; ground reaction force; inertia; gravity;
weight; mass; human
ID SIMULATED REDUCED-GRAVITY; BODY-WEIGHT SUPPORT; CENTER-OF-MASS; HUMAN
WALKING; METABOLIC COST; MECHANICS; PARAMETERS; ENERGETICS; INSIGHTS;
BONE
AB The addition of inertia to exercising astronauts could increase ground reaction forces and potentially provide a greater health benefit. However, conflicting results have been reported regarding the adaptations to additional mass (inertia) without additional net weight (gravitational force) during locomotion. We examined the effect of increasing inertia while maintaining net gravitational force on vertical ground reaction forces and temporal kinematics during walking and running. Vertical ground reaction force was measured for 10 healthy adults (five male/five female) during walking (1.34 m s(-1)) and running (3.13 m s(-1)) using a force-measuring treadmill. Subjects completed locomotion at normal weight and mass and at 10, 20, 30 and 40% of added inertial force. The added gravitational force was relieved with overhead suspension, so that the net force between the subject and treadmill at rest remained equal to 100% body weight. Ground reaction forces were affected by the added inertial force, but not to the magnitude predicted by the increase in mass, suggesting that adaptations in motion occurred. Vertical ground reaction force production and adaptations in gait temporal kinematics were different between walking and running. Peak vertical impact forces and loading rates increased with increased inertia during walking, and decreased during running. As inertia increased, peak vertical propulsive forces decreased during walking and did not change during running. Stride time increased during walking and running, and contact time increased during running. The increased inertial forces were utilized independently from gravitational forces by the motor control system when determining coordination strategies.
C1 [De Witt, John K.] Wyles Life Sci Grp, Houston, TX 77058 USA.
[Hagan, R. Donald] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Cromwell, Ronita L.] Univ Texas Galveston, Med Branch, Dept Phys Therapy, Galveston, TX USA.
RP De Witt, JK (reprint author), Wyles Life Sci Grp, Houston, TX 77058 USA.
EM john.k.dewitt@nasa.gov
NR 25
TC 17
Z9 17
U1 0
U2 3
PU COMPANY OF BIOLOGISTS LTD
PI CAMBRIDGE
PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL,
CAMBS, ENGLAND
SN 0022-0949
J9 J EXP BIOL
JI J. Exp. Biol.
PD APR
PY 2008
VL 211
IS 7
BP 1087
EP 1092
DI 10.1242/jeb.012443
PG 6
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 280YS
UT WOS:000254463300015
PM 18344482
ER
PT J
AU Baldwin, RE
Miller, TW
Brodeur, RD
Jacobson, KC
AF Baldwin, R. E.
Miller, T. W.
Brodeur, R. D.
Jacobson, K. C.
TI Expanding the foraging history of juvenile Pacific salmon: combining
stomach-content and macroparasite-community analyses for studying marine
diets
SO JOURNAL OF FISH BIOLOGY
LA English
DT Article
DE food transmitted parasites; ocean ecology; salmon
ID NORTHERN CALIFORNIA CURRENT; ONCORHYNCHUS-KISUTCH; COHO SALMON;
LECITHASTER-GIBBOSUS; FEEDING CHRONOLOGY; LIFE-HISTORY; FOOD-HABITS;
PARASITES; FISH; CHINOOK
AB Stomach contents and macroparasites were examined from the same fishes collected off Oregon and California in June and August of 2000 and 2002 to provide a more comprehensive description of the diet of juvenile Chinook salmon Oncorhynchus tshawytscha and coho salmon Oncorhynchus kisutch during their first few months at sea. Temporal and spatial similarities of the two data sets were assessed using multivariate analyses. Both stomach contents and macroparasite communities indicated that fishes, euphausiids and hyperiid amphipods were consumed by both salmonid species, although their relative contribution to each species diet was highly variable. In June, the greater abundances of parasite species in Chinook salmon compared to coho salmon suggested that Chinook salmon consumed more infected intermediate hosts (crustaceans or larval fishes) shortly after ocean entry (April and May). Although the macroparasite analysis lacked the specificity of stomach analysis in identifying prey, macroparasites can provide a longer term history of feeding and diet information for fishes with empty stomachs. (c) 2008 The Authors Journal compilation (c) 2008 The Fisheries Society of the British Isles.
C1 [Baldwin, R. E.; Miller, T. W.] Oregon State Univ, Hatfield Marine Sci Ctr, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA.
[Brodeur, R. D.; Jacobson, K. C.] NOAA, Natl Marine Fisheries Serv, Northwest Fisheries Sci Ctr, Newport, OR 97365 USA.
RP Baldwin, RE (reprint author), Oregon State Univ, Hatfield Marine Sci Ctr, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA.
EM rebecca.baldwin@oregonstate.edu
NR 50
TC 13
Z9 14
U1 0
U2 17
PU BLACKWELL PUBLISHING
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND
SN 0022-1112
J9 J FISH BIOL
JI J. Fish Biol.
PD APR
PY 2008
VL 72
IS 6
BP 1268
EP 1294
DI 10.1111/j.1095-8649.2007.01792.x
PG 27
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 285XJ
UT WOS:000254809200003
ER
PT J
AU Choi, YH
Vay, SA
Vadrevu, KP
Soja, AJ
Woo, JH
Nolf, SR
Sachse, GW
Diskin, GS
Blake, DR
Blake, NJ
Singh, HB
Avery, MA
Fried, A
Pfister, L
Fuelberg, HE
AF Choi, Yonghoon
Vay, Stephanie A.
Vadrevu, Krishna P.
Soja, Amber J.
Woo, Jung-Hun
Nolf, Scott R.
Sachse, Glen W.
Diskin, Glenn S.
Blake, Donald R.
Blake, Nicola J.
Singh, Hanwant B.
Avery, Melody A.
Fried, Alan
Pfister, Leonhard
Fuelberg, Henry E.
TI Characteristics of the atmospheric CO2 signal as observed over the
conterminous United States during INTEX-NA
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Review
ID TRACE GAS-TRANSPORT; CARBON-DIOXIDE; NORTH-AMERICA; NITROGEN DEPOSITION;
ASIAN EMISSIONS; SULFUR-DIOXIDE; ATLANTIC-OCEAN; AIR-POLLUTANTS; BOREAL
FORESTS; PACIFIC
AB High resolution in situ measurements of atmospheric CO2 were made from the NASA DC-8 aircraft during the Intercontinental Chemical Transport Experiment-North America (INTEX-NA) campaign, part of the wider International Consortium for Atmospheric Research on Transport and Transformation (ICARTT). During the summer of 2004, eighteen flights comprising 160 h of measurements were conducted within a region bounded by 27 to 53 degrees N and 36 to 139 degrees W over an altitude range of 0.15 to 12 km. These large-scale surveys provided the opportunity to examine the characteristics of the atmospheric CO2 signal over sparsely sampled areas of North America and adjacent ocean basins. The observations showed a high degree of variability (<= 18%) due to the myriad source and sink processes influencing the air masses intercepted over the INTEX-NA sampling domain. Surface fluxes had strong effects on continental scale concentration gradients. Clear signatures of CO2 uptake were seen east of the Mississippi River, notably a persistent CO2 deficit in the lowest 2-3 km. When combining the airborne CO2 measurements with LANDSAT and MODIS data products, the lowest CO2 mixing ratios observed during the campaign (337 ppm) were tied to mid-continental agricultural fields planted in corn and soybeans. We used simultaneous measurements of CO, O-3, C2Cl4, C2H6, C2H2 and other unique chemical tracers to differentiate air mass types. Coupling these distinct air mass chemical signatures with transport history permitted identification of convection, stratosphere-troposphere exchange, long-range transport from Eastern Asia, boreal wildfires, and continental outflow as competing processes at multiple scales influencing the observed concentrations. Our results suggest these are important factors contributing to the large-scale distribution in CO2 mixing ratios thus these observations offer new constraints in the computation of the North American carbon budget.
C1 [Choi, Yonghoon; Soja, Amber J.] NIA, NASA, Langley Res Ctr, Hampton, VA 23666 USA.
[Woo, Jung-Hun] Konkuk Univ, Dept Adv Technol Fus, Seoul, South Korea.
[Vadrevu, Krishna P.] Ohio State Univ, Ohio Agr Res & Dev Ctr, Agroecosyst Management Program, Wooster, OH 44691 USA.
[Nolf, Scott R.] Comp Sci Corp, Hampton, VA USA.
[Blake, Donald R.; Blake, Nicola J.] Univ Calif Irvine, Dept Chem, Irvine, CA 92717 USA.
[Singh, Hanwant B.; Pfister, Leonhard] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Fuelberg, Henry E.] Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA.
RP Choi, YH (reprint author), NIA, NASA, Langley Res Ctr, 100 Explorat Way, Hampton, VA 23666 USA.
EM ychoi@nianet.org
OI Vadrevu, Krishna/0000-0003-4407-5605
NR 106
TC 19
Z9 19
U1 2
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 1
PY 2008
VL 113
IS D7
AR D07301
DI 10.1029/2007JD008899
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 284OY
UT WOS:000254716900001
ER
PT J
AU Gasso, S
AF Gasso, Santiago
TI Satellite observations of the impact of weak volcanic activity on marine
clouds
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SOUTH SANDWICH ISLANDS; SHIP TRACKS; SIZE DISTRIBUTIONS; OCEAN
PRODUCTIVITY; STRATIFORM CLOUDS; SULFUR EMISSIONS; WATER-VAPOR; LEE
WAVES; CLIMATE; AEROSOL
AB Because emissions from weak volcanic eruptions tend to remain in the low troposphere, they may have a significant radiative impact through the indirect effect on clouds. However, this type of volcanic activity is underreported and its global impact has been assessed only by model simulations constrained with very limited observations. First observations of the impact of high- latitude active volcanoes on marine boundary layer clouds are reported here. These observations were made using a combination of standard derived products and visible images from the MODIS, AMSR- E and GOES detectors. Two distinctive effects are identified. When there is an existing boundary layer cloud deck, an increase in cloud brightness and a decrease in both cloud effective radius and liquid water content were observed immediately downwind of the volcanoes. The visible appearance of these "volcano tracks'' resembles the effect of man-made ship tracks. When synoptic conditions favor low cloudiness, the volcano plume ( or volcano cloud) increases significantly the cloud cover downwind. The volcano cloud can extend for hundreds of kilometers until mixing with background clouds. Unlike violent eruptions, the volcano clouds reported here ( the Aleutian Islands in the North Pacific and the South Sandwich Islands in the South Atlantic) have retrieved microphysical properties similar to those observed in ship tracks. However, when comparing the volcano clouds from these two regions, liquid water content can decrease, increase or remain unchanged with respect to nearby unperturbed clouds. These differences suggest that composition at the source, type of eruption and meteorological conditions influence the evolution of the cloud.
C1 [Gasso, Santiago] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA.
RP Gasso, S (reprint author), NASA, Goddard Space Flight Ctr, Code 613-2, Greenbelt, MD 20771 USA.
EM santiago@climate.gsfc.nasa.gov
RI Gasso, Santiago/H-9571-2014
OI Gasso, Santiago/0000-0002-6872-0018
NR 83
TC 34
Z9 34
U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 1
PY 2008
VL 113
IS D14
AR D14S19
DI 10.1029/2007JD009106
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 284PB
UT WOS:000254717200001
ER
PT J
AU Leuschen, CJ
Swift, RN
Comiso, JC
Raney, RK
Chapman, RD
Krabill, WB
Sonntag, JG
AF Leuschen, Carlton J.
Swift, Robert N.
Comiso, Josefino C.
Raney, R. Keith
Chapman, Rickey D.
Krabill, William B.
Sonntag, John G.
TI Combination of laser and radar altimeter height measurements to estimate
snow depth during the 2004 Antarctic AMSR-E Sea Ice field campaign
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID ARCTIC-OCEAN; VARIABILITY; ROUGHNESS; SHEETS; COVER
AB Among the most important parameters needed to evaluate the present and future state of Antarctic sea ice cover is the ice thickness. The retrieval of ice thickness using remote sensing techniques has been hampered by the absence of a capability to remotely measure snow thickness covering the sea ice. Data sets collected with Johns Hopkins Applied Physics Laboratory's Delay-Doppler Phase Monopulse (D2P) radar and NASA's Airborne Topographic Mapper (ATM) scanning lidar during NASA's Antarctic AMSR-E Sea Ice field campaign over the Bellingshausen Sea are used to demonstrate the potential of a remote-sensing technique for retrieval of snow cover thickness from an airborne platform. The technique takes advantage of the fact that the radar is most sensitive to the snow-ice interface while the lidar responds to the highly optically reflective snow surface. The difference between the radar- and laser-determined surfaces yields an estimate of snow thickness that appears to be reasonably consistent with expected values. The technique requires careful registration of the instrument footprints. Because there was no absolute range calibration of the lidar due to predeployment scheduling difficulties, the vertical offset between the instruments was resolved by determining the difference between measurements over leads. Elsewhere over sea ice the radar-defined surface is generally below the laser-defined surface consistent with the radar defining the snow-ice interface. Over a relatively small portion of the data, we observed opposite relationship between the sensor-defined surfaces for which we discuss a plausible physical explanation.
C1 [Leuschen, Carlton J.] Univ Kansas, Ctr Remote Sensing Ice Sheets, Lawrence, KS 66045 USA.
[Swift, Robert N.; Sonntag, John G.] NASA, Goddard Space Flight Ctr, Observat Sci Branch, Wallops Isl, VA 23337 USA.
[Comiso, Josefino C.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA.
[Raney, R. Keith; Chapman, Rickey D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
RP Leuschen, CJ (reprint author), Univ Kansas, Ctr Remote Sensing Ice Sheets, 2335 Irving Hill Rd, Lawrence, KS 66045 USA.
EM leuschen@eecs.ku.edu
NR 31
TC 15
Z9 15
U1 0
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD APR 1
PY 2008
VL 113
IS C4
AR C04S90
DI 10.1029/2007JC004285
PG 10
WC Oceanography
SC Oceanography
GA 284PH
UT WOS:000254717800001
ER
PT J
AU Whitten, RC
Borucki, WJ
O'Brien, K
Tripathi, SN
AF Whitten, R. C.
Borucki, W. J.
O'Brien, K.
Tripathi, S. N.
TI Predictions of the electrical conductivity and charging of the cloud
particles in Jupiter's atmosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID TRANSFER CROSS-SECTIONS; COSMIC-RAY IONIZATION; LOW ENERGIES; DENSITY;
IONS; RECOMBINATION; STRATOSPHERE; MOBILITIES; AEROSOLS; DESCENT
AB The electrical conductivity and electrical charge on cloud particles ( composed of ammonia, ammonium hydrosulfide, and water) in the atmosphere of Jupiter are computed for pressures between 5.5 and 0.1 bars. The source of ionization is galactic cosmic rays ( GCR). The distribution of charge among the various reservoirs is a function of altitude and the total area of the aerosol particles. For pressures below 4 bars, the electrons are scavenged efficiently by the cloud particles, decreasing the electron- ion recombination rate and resulting in increased positive ion abundance over that in the absence of the particles. For the upper regions of each cloud layer, the area of the aerosols and the large diffusion rate of the electrons cause most aerosol particles to be negatively charged. Near the bases of the cloud layers, the larger total area of the aerosols causes most of the charge, positive and negative, to reside on particles. Where clouds are present, the reduction of the electron conductivity ranges from a factor of 30 at 0.1 bar to 10 4 at 4 bars. At pressures near 1 bar and 4 bars, the positive ion conductivity increases by a factor of 10 over that expected for the clear atmosphere. A parametric study of negative ions shows that they are likely to be insignificant. For altitudes below the 0.3- bar level the predicted positive and negative conductivities are well below the detection limit of the relaxation and mutual impedance instruments such as those employed on the Huygens entry probe.
C1 [Whitten, R. C.] SETI Inst, Mountain View, CA 94043 USA.
[Borucki, W. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[O'Brien, K.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA.
[Tripathi, S. N.] Indian Inst Technol, Kanpur 208016, Uttar Pradesh, India.
RP Whitten, RC (reprint author), SETI Inst, 515 N Whisman Rd, Mountain View, CA 94043 USA.
EM rwhitten@pacbell.net
RI Tripathi, Sachchida/J-4840-2016
NR 39
TC 10
Z9 10
U1 0
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD APR 1
PY 2008
VL 113
IS E4
AR E04001
DI 10.1029/2007JE002975
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 284PK
UT WOS:000254718100001
ER
PT J
AU Kenyon, M
Day, PK
Bradford, CM
Bock, JJ
Leduc, HG
AF Kenyon, M.
Day, P. K.
Bradford, C. M.
Bock, J. J.
Leduc, H. G.
TI Electrical properties of background-limited membrane-isolation
transition-edge sensing bolometers for Far-IR/Submillimeter
direct-detection spectroscopy
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE transition-edge sensor; far-IR spectrometer; submillimeter spectrometer;
Si(3)N4
AB We built and measured the electrical properties of membrane-isolation transition-edge sensing bolometers (TESs) suitable for background-limited far-IR/submillimeter direct-detection spectroscopy. Each TES consists of a Mo/Au bilayer patterned onto a suspended, thermally isolated absorber that is connected to the substrate through four Si (x) N (y) beams deposited by low pressure chemical vapor deposition (LPCVD). We fabricated TESs with straight and meander support beams. The dimensions of the meander (straight) support beams are 700 mu m (700 mu m) long by 0.25 mu m (0.5 mu m) thick by 0.35 mu m (0.5 mu m) wide. We measured I-V characteristics for these TESs and determined that the thermal conductance G equals 72 fW/K (straight) and 19 fW/K (meander) for our best devices. The thermal conductance exhibits a T-1/2 dependence with temperature which is evidence of effective elastic scattering of the acoustic phonon modes. The transition temperatures T-c for the same TESs are T-c =137 mK (straight) and T-c =71 mK (meander). If we assume the TESs are temperature-fluctuation noise limited, then the derived noise equivalent power (NEP) equals 1.9x10(-19) W/Hz(1/2) (straight) and 6.1x10(-20) W/Hz(1/2) (meander), using our measured values for G and T (c) . The meander-beam TES has a derived NEP that is close to two orders of magnitude lower than the state-of-the-art. Finally, we measured an effective time constant tau of about 300 ms (straight) and 400 ms (meander) using electrical and optical pulses. These values for the NEP and tau for the meander-beam TES meet the requirements for the Background-Limited far-IR/Submillimeter Spectrograph (BLISS), a proposed NASA instrument.
C1 [Kenyon, M.; Day, P. K.; Bradford, C. M.; Bock, J. J.; Leduc, H. G.] Jet Propuls Lab, Pasadena, CA 91109 USA.
RP Kenyon, M (reprint author), Jet Propuls Lab, Pasadena, CA 91109 USA.
EM matthew.e.kenyon@jpl.nasa.gov
NR 14
TC 15
Z9 15
U1 0
U2 4
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 112
EP 118
DI 10.1007/s10909-007-9630-4
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900016
ER
PT J
AU Bonetti, JA
Day, P
Kenyon, M
Turner, A
Leduc, HG
Kuo, CL
Bock, JJ
AF Bonetti, J. A.
Day, P.
Kenyon, M.
Turner, A.
LeDuc, H. G.
Kuo, C. L.
Bock, J. J.
TI Electrical and thermal characterization of membrane-isolated,
antenna-coupled, TES bolometers for the SPIDER experiment
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE TES bolometers; cosmology; CMB; cosmic microwave background;
polarization
ID ELECTROTHERMAL FEEDBACK
AB We have fabricated and measured the thermal and DC electrical properties of transition-edge sensing (TES) bolometers to be employed on the SPIDER experiment, a balloon-based observatory for studying the polarization of the cosmic microwave background (CMB). The bolometers consist of Al and Ti thermistors in series and a termination resistor which couples to an on-chip, polarization sensitive, 150 GHz slot-array antenna through a superconducting microstrip transmission line. Several important parameters were measured. Transition temperature measurements were performed by measuring the Johnson noise in the Ti thermistor. Current-voltage characteristic measurements were performed at various temperatures allowing for the deduction of the thermal conductance and the temperature coefficient of resistance. Electrical noise equivalent power was measured to sub-Hertz frequencies. Finally, the time constant of the bolometers was measured within the Al and Ti transitions where electrothermal feedback speeds up the bolometer response compared with the natural time constant measured just above the Ti transition temperature. The results of these measurements are within the design specifications for SPIDER.
C1 [Bonetti, J. A.; Day, P.; Kenyon, M.; Turner, A.; LeDuc, H. G.; Kuo, C. L.; Bock, J. J.] CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA.
RP Bonetti, JA (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA.
EM joseph.bonetti@jpl.nasa.gov
NR 2
TC 9
Z9 9
U1 1
U2 2
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 138
EP 143
DI 10.1007/s10909-007-9623-3
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900020
ER
PT J
AU Barrentine, EM
Timbie, PT
Stevenson, TR
Ali, S
Chervenak, JA
Wollack, E
Moseley, SH
Allen, CA
Hseih, WT
Miller, TM
Benford, DJ
Brown, AD
AF Barrentine, E. M.
Timbie, P. T.
Stevenson, T. R.
Ali, S.
Chervenak, J. A.
Wollack, E.
Moseley, S. H.
Allen, C. A.
Hseih, W. T.
Miller, T. M.
Benford, D. J.
Brown, A. D.
TI Sensitivity measurements of a transition-edge hot-electron
microbolometer for millimeter-wave astrophysical observations
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE microbolometers; transition-edge sensors; cosmic microwave background;
millimeter waves; hot-electron effect; transition-edge hot-electron
microbolometer
AB Future experiments to probe the Cosmic Microwave Background (CMB) polarization will need arrays of 1000s of sensitive bolometers. We are developing a Transition-edge Hot-electron Microbolometer (THM) to fill this need. This small-volume bolometer consists of a superconducting bilayer Transition-Edge Sensor (TES) with a thin-film absorber. Unlike traditional monolithic bolometers which make use of micromachined structures, the THM employs the decoupling between electrons and phonons at milliKelvin temperatures to provide thermal isolation. The devices are fabricated photolithographically and are easily integrated with antennas via microstrip transmission lines, and with SQUID readouts. We present the results of noise, responsivity, and thermal conductance measurements in which electrical power is dissipated in the absorber, and confirm a thermal model for a test THM with a Mo/Au TES and Bi/Au absorber.
C1 [Barrentine, E. M.; Timbie, P. T.] Univ Wisconsin, Madison, WI 53706 USA.
[Stevenson, T. R.; Chervenak, J. A.; Wollack, E.; Moseley, S. H.; Allen, C. A.; Hseih, W. T.; Miller, T. M.; Benford, D. J.; Brown, A. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ali, S.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
RP Barrentine, EM (reprint author), Univ Wisconsin, Madison, WI 53706 USA.
EM barrentine@wisc.edu
RI Brown, Ari/B-1693-2008; Benford, Dominic/D-4760-2012; Moseley,
Harvey/D-5069-2012; Wollack, Edward/D-4467-2012
OI Benford, Dominic/0000-0002-9884-4206; Wollack,
Edward/0000-0002-7567-4451
NR 13
TC 7
Z9 7
U1 0
U2 3
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 173
EP 179
DI 10.1007/s10909-007-9615-3
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900026
ER
PT J
AU Smith, SJ
Bandler, SR
Brown, AD
Chervenak, JA
Figueroa-Feliciano, E
Finkbeiner, F
Iyomoto, N
Kelley, RL
Kilbourne, CA
Porter, FS
Sadleir, JE
AF Smith, S. J.
Bandler, S. R.
Brown, A. -D.
Chervenak, J. A.
Figueroa-Feliciano, E.
Finkbeiner, F.
Iyomoto, N.
Kelley, R. L.
Kilbourne, C. A.
Porter, F. S.
Sadleir, J. E.
TI Characterizing the superconducting-to-normal transition in Mo/Au
transition-edge sensor bilayers
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE excess noise; critical current; Ginzburg-Landau
ID NOISE
AB We are developing arrays of Mo/Au bilayer transition-edge sensors (TES's) for future X-ray astronomy missions such as NASA's Constellation-X. The physical properties of the superconducting-to-normal transition in our TES bilayers, while often reproducible and characterized, are not well understood. The addition of normal metal features on top of the bilayer are found to change the shape and temperature of the transition, and they typically reduce the unexplained 'excess' noise. In order to understand and potentially optimize the properties of the transition, we have been studying the temperature, widths and current dependence of these transitions. We report on the characterization of devices both deposited on silicon substrates and suspended on thin silicon nitride membranes. This includes key device parameters such as the logarithmic resistance sensitivity with temperature alpha, and the logarithmic resistance sensitivity with current beta, and their correlation with excess noise.
C1 [Smith, S. J.; Bandler, S. R.; Brown, A. -D.; Chervenak, J. A.; Finkbeiner, F.; Iyomoto, N.; Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.; Sadleir, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Figueroa-Feliciano, E.] MIT, Kavli Inst Space Res, Cambridge, MA 02139 USA.
RP Smith, SJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM sjs@milkyway.gsfc.nasa.gov
RI Brown, Ari/B-1693-2008; Bandler, Simon/A-6258-2010; Smith,
Stephen/B-1256-2008; Porter, Frederick/D-3501-2012; Kelley,
Richard/K-4474-2012
OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675;
Porter, Frederick/0000-0002-6374-1119;
NR 6
TC 12
Z9 12
U1 0
U2 8
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 195
EP 200
DI 10.1007/s10909-007-9619-z
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900030
ER
PT J
AU Kilbourne, CA
Bandler, SR
Brown, AD
Chervenak, A
Figueroa-Feliciano, E
Finkbeiner, F
Iyomoto, N
Kelley, RL
Porter, FS
Smith, SJ
AF Kilbourne, C. A.
Bandler, S. R.
Brown, A. -D.
Chervenak, A.
Figueroa-Feliciano, E.
Finkbeiner, F.
Iyomoto, N.
Kelley, R. L.
Porter, F. S.
Smith, S. J.
TI Various optimizations of TES arrays for X-ray astrophysics
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE X-ray spectroscopy; X-ray calorimeter; transition-edge sensor
ID RESOLUTION; LINES; SPECTROMETER; SPECTROSCOPY
AB We are developing arrays of superconducting transition-edge sensors (TES) for imaging X-ray spectroscopy telescopes such as the XMS on Constellation-X. While our primary focus has been on arrays that meet the XMS requirements (of which, foremost, are an energy resolution of 2.5 eV at 6 keV and a band pass from similar to 0.3 keV to 12 keV), we are also beginning to investigate other optimizations that might be used to extend the XMS capabilities. In one of these optimizations, improved resolution below 1 keV is achieved by reducing the heat capacity. These low-energy pixels can be added to an array with broadband response either as a separate array or interspersed, depending on other factors that include telescope design and science requirements. To explore optimizations for higher count rates, we are also optimizing the design and operating temperature of pixels that are coupled to a solid substrate. We present analysis of the preliminary performance of such variations.
C1 [Kilbourne, C. A.; Bandler, S. R.; Brown, A. -D.; Chervenak, A.; Finkbeiner, F.; Iyomoto, N.; Kelley, R. L.; Porter, F. S.; Smith, S. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bandler, S. R.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Figueroa-Feliciano, E.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Finkbeiner, F.] RS Informat Syst Inc, Mclean, VA 22102 USA.
[Iyomoto, N.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Kilbourne, CA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Caroline.A.Kilbourne@nasa.gov
RI Brown, Ari/B-1693-2008; Bandler, Simon/A-6258-2010; Smith,
Stephen/B-1256-2008; Porter, Frederick/D-3501-2012; Kelley,
Richard/K-4474-2012
OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675;
Porter, Frederick/0000-0002-6374-1119;
NR 12
TC 10
Z9 10
U1 0
U2 6
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 223
EP 228
DI 10.1007/s10909-007-9643-z
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900035
ER
PT J
AU Chervenak, JA
Finkbeiner, FM
Bandler, SR
Brekosky, R
Brown, AD
Iyomoto, N
Kelley, RL
Kilbourne, CA
Porter, FS
Sadleir, J
Smith, S
AF Chervenak, J. A.
Finkbeiner, F. M.
Bandler, S. R.
Brekosky, R.
Brown, A. D.
Iyomoto, N.
Kelley, R. L.
Kilbourne, C. A.
Porter, F. S.
Sadleir, J.
Smith, S.
TI Materials development for auxiliary components for large compact Mo/Au
TES arrays
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE X-ray microcalorimeter; superconducting detector; heatsinking; crosstalk
AB Pursuing the feasibility of scaling conventionally-micromachined transition-edge-sensor (TES) arrays, we have undertaken a study of materials suitable for array integration. A potential limitation of increased pixel count is adequate heatsinking of each detector element to its base temperature. We describe technical approaches for heat sinking large compact TES microcalorimeter arrays and calculate the achievable heatsinking based on measured material parameters. Techniques include backside-deposited thick film copper on arrays with deep-etched wells in the substrates and electroplated gold and copper-filled micro-trenches on the substrate surface. Another limitation is the sensitivity of the thin film circuit elements to applied stress, which can arise in fabrication and mounting of arrays of increasing size. We have explored stress and deposition temperature sensitivity in our molybdenum-based bilayers. Such process parameters can impact options for array heat sinking and electrical interconnects.
C1 [Chervenak, J. A.; Finkbeiner, F. M.; Bandler, S. R.; Brekosky, R.; Brown, A. D.; Iyomoto, N.; Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.; Sadleir, J.; Smith, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Chervenak, JA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM James.A.Chervenak@nasa.gov
RI Brown, Ari/B-1693-2008; Bandler, Simon/A-6258-2010; Smith,
Stephen/B-1256-2008; Porter, Frederick/D-3501-2012; Kelley,
Richard/K-4474-2012
OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675;
Porter, Frederick/0000-0002-6374-1119;
NR 6
TC 6
Z9 6
U1 0
U2 4
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 255
EP 260
DI 10.1007/s10909-007-9636-y
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900041
ER
PT J
AU Allen, CA
Benford, DJ
Miller, TM
Moseley, SH
Staguhn, JG
Wollack, EJ
AF Allen, C. A.
Benford, D. J.
Miller, T. M.
Moseley, S. H.
Staguhn, J. G.
Wollack, E. J.
TI Design and fabrication highlights enabling a 2 mm, 128 element bolometer
array for GISMO
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE bolometer array; transition edge sensor
ID TES BOLOMETERS
AB The Backshort-Under-Grid (BUG) superconducting bolometer array architecture is intended to be highly versatile, operating over a large range of wavelengths and background conditions. To validate the basic array design and to demonstrate its applicability for future kilopixel arrays, we will demonstrate a 128-element bolometer array optimized for 2 mm wavelength using a new Goddard Space Flight Center instrument, GISMO (Goddard IRAM Superconducting 2-Millimeter Observer). The design considerations unique to GISMO and laboratory experimental results will be discussed.
C1 [Allen, C. A.; Benford, D. J.; Miller, T. M.; Moseley, S. H.; Staguhn, J. G.; Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Allen, CA (reprint author), NASA, Goddard Space Flight Ctr, Code 553, Greenbelt, MD 20771 USA.
EM christine.a.allen@nasa.gov
RI Benford, Dominic/D-4760-2012; Moseley, Harvey/D-5069-2012; Wollack,
Edward/D-4467-2012
OI Benford, Dominic/0000-0002-9884-4206; Wollack,
Edward/0000-0002-7567-4451
NR 8
TC 1
Z9 1
U1 1
U2 1
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 266
EP 270
DI 10.1007/s10909-007-9646-9
PG 5
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900043
ER
PT J
AU Burck, A
Kempf, S
Schafer, S
Rotzinger, H
Rodrigues, M
Wolf, T
Gastaldo, L
Fleischmann, A
Enss, C
AF Burck, A.
Kempf, S.
Schafer, S.
Rotzinger, H.
Rodrigues, M.
Wolf, T.
Gastaldo, L.
Fleischmann, A.
Enss, C.
TI Microstructured magnetic calorimeter with meander-shaped pickup coil
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE MMC; metallic magnetic calorimeter; low temperature detectors; rare
earth alloys; gold-erbium alloy; x-ray spectroscopy
AB In the last years metallic magnetic calorimeters (MMC) showed an energy resolution of a few eV for x-rays up to 10 keV. This makes MMCs a promising and powerful tool for many applications where photons or energetic massive particles have to be detected-like absolute activity measurements of radioactive isotopes, high resolution x-ray spectroscopy and x-ray fluorescence material analysis. However, in order to fulfill all requirements of these applications and to allow to reach the maximum resolving power a consequent micro-fabrication of the MMC detectors is needed. The micro-fabrication of metallic magnetic calorimeters requires reliable deposition and patterning processes for niobium structures with high critical currents and for paramagnetic sensors.
As one result of our advances in microstructuring a fully microfabricated MMC which consists of a meander shaped niobium thin film pickup coil and a 3 mu m thick sputter deposited paramagnetic Au:Er temperature sensor will be presented. Deposition of energy in the paramagnetic sensor causes a rise in temperature and results in a change of magnetization, which is measured by a low noise high bandwidth dc-SQUID. The sputter deposited Au:Er films we report on are working well and show thermodynamic properties close to the ones known from bulk material down to temperatures of 45 mK.
C1 [Burck, A.; Kempf, S.; Schafer, S.; Wolf, T.; Gastaldo, L.; Fleischmann, A.; Enss, C.] Univ Heidelberg, Kirchhoff Inst Phys, D-69120 Heidelberg, Germany.
[Rotzinger, H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rotzinger, H.] Brown Univ, Greenbelt, MD 20771 USA.
[Rodrigues, M.] CEA Saclay, DETECS, DRT, Lab Natl Henri Becquerel, F-91191 Gif Sur Yvette, France.
RP Burck, A (reprint author), Univ Heidelberg, Kirchhoff Inst Phys, INF 227, D-69120 Heidelberg, Germany.
EM Andreas.Burck@kip.uni-heidelberg.de
RI Kempf, Sebastian/P-7612-2016
OI Kempf, Sebastian/0000-0002-3303-128X
NR 6
TC 19
Z9 19
U1 0
U2 1
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 337
EP 344
DI 10.1007/s10909-007-9659-4
PG 8
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900055
ER
PT J
AU Rotzinger, H
Adams, J
Bandler, SR
Beyer, J
Eguchi, H
Figueroa-Feliciano, E
Hsieh, W
Seidel, GM
Stevenson, T
AF Rotzinger, H.
Adams, J.
Bandler, S. R.
Beyer, J.
Eguchi, H.
Figueroa-Feliciano, E.
Hsieh, W.
Seidel, G. M.
Stevenson, T.
TI Performance of micro-fabricated magnetic calorimeters arrays for X-ray
spectroscopy
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE magnetic calorimeter; X-ray spectroscopy; low temperature detector
AB We have been developing array technology for fabricating magnetic calorimeters for X-ray astronomy. The magnetization change in each pixel of the paramagnetic sensor material due to the heat input of an absorbed X-ray is sensed by a meander shaped coil. With this geometry it is possible to obtain excellent energy sensitivity, low magnetic cross-talk and large format arrays fabricated on wafers that are separate from the SQUID read-out. A magnetic bias field for each pixel is generated by the use of a persistent current that is stored. We report on the results from our prototype arrays, which are coupled to low noise DC-SQUIDs. The first test results are presented and the sensitivity is compared with calculations.
C1 [Rotzinger, H.; Adams, J.; Bandler, S. R.; Hsieh, W.; Stevenson, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Beyer, J.] Phys Tech Bundesanstalt, Berlin, Germany.
[Figueroa-Feliciano, E.] MIT, Boston, MA USA.
[Rotzinger, H.; Eguchi, H.; Seidel, G. M.] Brown Univ, Providence, RI 02912 USA.
RP Rotzinger, H (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM hannes.rotzinger@milkyway.gsfc.nasa.gov
RI Bandler, Simon/A-6258-2010
OI Bandler, Simon/0000-0002-5112-8106
NR 3
TC 12
Z9 12
U1 0
U2 2
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 351
EP 356
DI 10.1007/s10909-007-9658-5
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900057
ER
PT J
AU Hsieh, WT
Adams, JA
Bandler, SR
Beyer, J
Denis, KL
Eguchi, H
Figueroa-Feliciano, E
Rotzinger, H
Schneider, GH
Seidel, GM
Stevenson, TR
Travers, DE
AF Hsieh, W. -T.
Adams, J. A.
Bandler, S. R.
Beyer, J.
Denis, K. L.
Eguchi, H.
Figueroa-Feliciano, E.
Rotzinger, H.
Schneider, G. H.
Seidel, G. M.
Stevenson, T. R.
Travers, D. E.
TI Fabrication of metallic magnetic calorimeter X-ray detector arrays
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE magnetic calorimeter; X-ray detector; AuEr film
AB Microcalorimeters with metallic magnetic sensors show great promise for use in astronomical X-ray spectroscopy. We describe the design and fabrication of a lithographically patterned magnetic microcalorimeter. A paramagnetic AuEr film is sputter-deposited as the sensor, which is coupled to a low noise SQUID via a meander superconducting pickup loop used as an inductor. This inductor also provides the magnetic field bias to the sensor. The AuEr film is deposited over this meander such that the field created by a large current flowing in the loop magnetizes the sensor material. The use of thin film techniques in the fabrication of these magnetic sensors not only allows strong magnetic coupling between the sensor and the inductor, it also is scalable for array fabrication.
C1 [Hsieh, W. -T.; Adams, J. A.; Bandler, S. R.; Denis, K. L.; Rotzinger, H.; Schneider, G. H.; Stevenson, T. R.; Travers, D. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Beyer, J.] Phys Tech Bundesanstalt, Inst Berlin, D-10587 Berlin, Germany.
[Eguchi, H.; Seidel, G. M.] Brown Univ, Dept Phys, Providence, RI 02912 USA.
[Figueroa-Feliciano, E.] MIT, Dept Phys, Cambridge, MA 02139 USA.
RP Hsieh, WT (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM wen-ting.hsieh-1@nasa.gov
RI Bandler, Simon/A-6258-2010
OI Bandler, Simon/0000-0002-5112-8106
NR 4
TC 10
Z9 10
U1 2
U2 2
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 357
EP 362
DI 10.1007/s10909-007-9661-x
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900058
ER
PT J
AU Kelley, RL
Allen, CA
Galeazzi, M
Kilbourne, CA
McCammon, D
Porter, FS
Szymkowiak, AE
AF Kelley, R. L.
Allen, C. A.
Galeazzi, M.
Kilbourne, C. A.
McCammon, D.
Porter, F. S.
Szymkowiak, A. E.
TI Ion-implanted silicon X-ray calorimeters: Present and future
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
ID THERMAL DETECTORS; MICROCALORIMETER; SUZAKU
AB We now have about 25 years of experience with X-ray calorimeters based on doped semiconductor thermometers. Ion-implanted Si arrays have been used in astrophysics and laboratory atomic physics. The device properties and characteristics are sufficiently well understood to allow optimized designs for a wide variety of applications over the 0.1-100 keV range. With new absorber materials, approaches for absorber attachment and compact, low thermal conductance JFET arrays, it should be possible to advance this technology from the 36 pixel arrays of today to arrays that are about an order of magnitude larger, and with significantly improved energy resolution. These would enable new capabilities on instruments being considered now for missions that may fly in about five years.
C1 [Kelley, R. L.; Allen, C. A.; Kilbourne, C. A.; Porter, F. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Galeazzi, M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA.
[McCammon, D.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Szymkowiak, A. E.] Yale Univ, Dept Phys, New Haven, CT 06511 USA.
RP Kelley, RL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Richard.L.Kelley@nasa.gov
RI Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012; XRAY,
SUZAKU/A-1808-2009
OI Porter, Frederick/0000-0002-6374-1119;
NR 18
TC 7
Z9 7
U1 0
U2 2
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 375
EP 380
DI 10.1007/s10909-007-9663-8
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900061
ER
PT J
AU Bandler, SR
Brekosky, RP
Brown, AD
Chervenak, JA
Figueroa-Feliciano, E
Finkbeiner, FM
Iyomoto, N
Kelley, RL
Kilbourne, CA
Porter, FS
Sadleir, J
Smith, SJ
AF Bandler, S. R.
Brekosky, R. P.
Brown, A. -D.
Chervenak, J. A.
Figueroa-Feliciano, E.
Finkbeiner, F. M.
Iyomoto, N.
Kelley, R. L.
Kilbourne, C. A.
Porter, F. S.
Sadleir, J.
Smith, S. J.
TI Performance of TES X-ray microcalorimeters with a novel absorber design
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE microcalorimeters; transition edge sensors
AB Superconducting transition-edge sensor (TES) microcalorimeters have demonstrated the Constellation-X requirements for spectral resolution, speed, and pixel size in a close-packed geometry. We will present our recent breakthrough energy resolution with sensors that have all gold and bismuth-gold absorbers. This has been enabled by cantilevered absorbers that make contact to the TES only in regions that are not part of the active thermometer. With this approach, rapid thermalization of the x-ray energy is achieved and interaction between the absorber and TES sensor films is avoided. This design allows us to obtain uniform high performance and is compatible with large-format, high fill-factor arrays. We will discuss this design, the results we have achieved in 8x8 arrays of these pixels, and the dependence of the performance on the geometry of the absorber contact area and on stress within the sensor.
C1 [Bandler, S. R.; Brekosky, R. P.; Brown, A. -D.; Chervenak, J. A.; Finkbeiner, F. M.; Iyomoto, N.; Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.; Sadleir, J.; Smith, S. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Figueroa-Feliciano, E.] MIT, Kavli Inst, Cambridge, MA 02139 USA.
RP Bandler, SR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Simon.R.Bandler@nasa.gov
RI Brown, Ari/B-1693-2008; Bandler, Simon/A-6258-2010; Smith,
Stephen/B-1256-2008; Porter, Frederick/D-3501-2012; Kelley,
Richard/K-4474-2012
OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675;
Porter, Frederick/0000-0002-6374-1119;
NR 6
TC 56
Z9 56
U1 1
U2 12
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 400
EP 405
DI 10.1007/s10909-007-9673-6
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900065
ER
PT J
AU Iyomoto, N
Bandler, SR
Brekosky, RP
Brown, AD
Chervenak, JA
Figueroa-Feliciano, E
Finkbeiner, FM
Kelley, RL
Kilbourne, CA
Lindeman, MA
Porter, FS
Saab, T
Sadleir, JE
Smith, SJ
AF Iyomoto, N.
Bandler, S. R.
Brekosky, R. P.
Brown, A. -D.
Chervenak, J. A.
Figueroa-Feliciano, E.
Finkbeiner, F. M.
Kelley, R. L.
Kilbourne, C. A.
Lindeman, M. A.
Porter, F. S.
Saab, T.
Sadleir, J. E.
Smith, S. J.
TI Modeling of TES X-ray microcalorimeters with a novel absorber design
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE microcalorimeters; transition edge sensors; X-ray spectroscopy
ID IMPEDANCE MEASUREMENTS; CALORIMETER
AB We have successfully modeled our new TES (transition-edge sensor) X-ray microcalorimeters with a novel X-ray absorber design that is suitable for close-packed array with high quantum efficiency. We have determined device parameters that reproduce complex impedance curves and noise spectra throughout the transition. Observed pulse height, decay time and baseline energy resolution were in good agreement with simulated results using the same parameters.
C1 [Iyomoto, N.; Bandler, S. R.; Brekosky, R. P.; Brown, A. -D.; Chervenak, J. A.; Figueroa-Feliciano, E.; Finkbeiner, F. M.; Kelley, R. L.; Kilbourne, C. A.; Lindeman, M. A.; Porter, F. S.; Saab, T.; Sadleir, J. E.; Smith, S. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Iyomoto, N (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
EM Naoko.Iyomoto@nasa.gov
RI Brown, Ari/B-1693-2008; Bandler, Simon/A-6258-2010; Smith,
Stephen/B-1256-2008; Porter, Frederick/D-3501-2012; Kelley,
Richard/K-4474-2012
OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675;
Porter, Frederick/0000-0002-6374-1119;
NR 7
TC 18
Z9 18
U1 0
U2 6
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 406
EP 412
DI 10.1007/s10909-007-9668-3
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900066
ER
PT J
AU Brown, AD
Bandler, SR
Brekosky, R
Chervenak, JA
Figueroa-Feliciano, E
Finkbeiner, F
Iyomoto, N
Kelley, RL
Kilbourne, CA
Porter, FS
Smith, S
Saab, T
Sadleir, J
AF Brown, A. -D.
Bandler, S. R.
Brekosky, R.
Chervenak, J. A.
Figueroa-Feliciano, E.
Finkbeiner, F.
Iyomoto, N.
Kelley, R. L.
Kilbourne, C. A.
Porter, F. S.
Smith, S.
Saab, T.
Sadleir, J.
TI Absorber materials for transition-edge sensor X-ray microcalorimeters
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE transition-edge sensors; calorimeters; electroplating
ID BISMUTH
AB Arrays of superconducting transition-edge sensors (TES) can provide high spatial and energy resolution necessary for X-ray astronomy. High quantum efficiency and uniformity of response can be achieved with a suitable absorber material, in which absorber X-ray stopping power, heat capacity, and thermal conductivity are relevant parameters. Here we compare these parameters for bismuth and gold. We have fabricated electroplated gold, electroplated gold/electroplated bismuth, and evaporated gold/evaporated bismuth 8 x 8 absorber arrays and find that a correlation exists between the residual resistance ratio (RRR) and thin film microstructure. This finding indicates that we can tailor absorber material conductivity via microstructure alteration, so as to permit absorber thermalization on timescales suitable for high energy resolution X-ray microcalorimetry. We show that by incorporating absorbers possessing large grain size, including electroplated gold and electroplated gold/electroplated bismuth, into our current Mo/Au TES, devices with tunable heat capacity and energy resolution of 2.4 eV (gold) and 2.1 eV (gold/bismuth) FWHM at 5.9 keV have been fabricated.
C1 [Brown, A. -D.; Bandler, S. R.; Brekosky, R.; Chervenak, J. A.; Finkbeiner, F.; Iyomoto, N.; Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.; Smith, S.; Sadleir, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Figueroa-Feliciano, E.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Iyomoto, N.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Saab, T.] Univ Florida, Dept Phys, Gainesville, FL 32611 USA.
[Sadleir, J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
RP Brown, AD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM abrown@pop500.gsfc.nasa.gov
RI Brown, Ari/B-1693-2008; Bandler, Simon/A-6258-2010; Smith,
Stephen/B-1256-2008; Porter, Frederick/D-3501-2012; Kelley,
Richard/K-4474-2012
OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675;
Porter, Frederick/0000-0002-6374-1119;
NR 7
TC 11
Z9 11
U1 2
U2 11
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 413
EP 417
DI 10.1007/s10909-007-9669-2
PG 5
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900067
ER
PT J
AU Moseley, SJ
Allen, CA
Costin, N
Kelley, R
Kilbourne, C
Miller, T
AF Moseley, Samuel J.
Allen, Christine A.
Costin, Nicholas
Kelley, Richard
Kilbourne, Caroline
Miller, Timothy
TI Automated hybridization of X-ray absorber elements a path to large
format microcalorimeter arrays
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE X-ray absorbers; mercury telluride; SU-8; automated tile application;
adhesive attachment; XeF2 etching
AB We have developed an automated die-scale process for the attachment of X-ray absorbers onto microcalorimeters. Here, we describe the process for the production of absorber tiles on a handle wafer, their attachment to the microcalorimeter, and the removal of the supporting handle wafer. The process is shown to be a robust path to large format arrays of microcalorimeters.
C1 [Moseley, Samuel J.; Allen, Christine A.; Costin, Nicholas; Kelley, Richard; Kilbourne, Caroline; Miller, Timothy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20772 USA.
[Moseley, Samuel J.; Costin, Nicholas; Miller, Timothy] MEI Technol Inc, Seabrook, MD 20706 USA.
RP Moseley, SJ (reprint author), NASA, Goddard Space Flight Ctr, Code 553,8800 Greenbelt Rd, Greenbelt, MD 20772 USA.
EM sjmosele@pop500.gsfc.nasa.gov
RI Kelley, Richard/K-4474-2012
NR 2
TC 1
Z9 1
U1 0
U2 0
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 418
EP 423
DI 10.1007/s10909-007-9670-9
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900068
ER
PT J
AU Figueroa-Feliciano, E
Saab, T
Rivera-Ortiz, PM
Bandler, SR
Iyomoto, N
Kelley, RL
Kilbourne, CA
Porter, FS
Smith, SJ
AF Figueroa-Feliciano, E.
Saab, T.
Rivera-Ortiz, P. M.
Bandler, S. R.
Iyomoto, N.
Kelley, R. L.
Kilbourne, C. A.
Porter, F. S.
Smith, S. J.
TI Studies of thermal diffusion in planar absorber designs for the Micro-X
rocket
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE TES; microcalorimeter; Micro-X; diffusion; position dependence
AB We have studied a potential design for a transition-edge sensor (TES) microcalorimeter array for the Micro-X High Resolution Microcalorimeter X-ray Imaging Rocket. Diffusion simulations of a design that places a small TES in the center of the pixel with a large in-plane absorber around the TES demonstrate that with high-quality gold films (RRR > 6) 2 eV resolution is attainable in a 700 mu m pixel, meeting the Micro-X requirement. X-ray hits directly on the TES, however, create a non-gaussian high energy tail to the device response. This high energy tail contains 5% of incident photons and cannot be removed by lowering the optimal filter bandwidth.
C1 [Figueroa-Feliciano, E.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Saab, T.] Univ Florida, Dept Phys, Gainesville, FL 32611 USA.
[Rivera-Ortiz, P. M.] Univ Puerto Rico, Dept Mech Engn, Mayaguez, PR 00680 USA.
[Bandler, S. R.; Iyomoto, N.; Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.; Smith, S. J.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
RP Figueroa-Feliciano, E (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA.
EM enectali@mit.edu
RI Bandler, Simon/A-6258-2010; Smith, Stephen/B-1256-2008; Porter,
Frederick/D-3501-2012; Kelley, Richard/K-4474-2012
OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675;
Porter, Frederick/0000-0002-6374-1119;
NR 2
TC 2
Z9 2
U1 0
U2 2
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 424
EP 429
DI 10.1007/s10909-007-9667-4
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900069
ER
PT J
AU Stevenson, T
Benford, D
Bennett, C
Cao, N
Chuss, D
Denis, K
Hsieh, W
Kogut, A
Moseley, S
Panek, J
Schneider, G
Travers, D
U-Yen, K
Voellmer, G
Wollack, E
AF Stevenson, T.
Benford, D.
Bennett, C.
Cao, N.
Chuss, D.
Denis, K.
Hsieh, W.
Kogut, A.
Moseley, S.
Panek, J.
Schneider, G.
Travers, D.
U-Yen, K.
Voellmer, G.
Wollack, E.
TI Cosmic microwave background polarization detector with high efficiency,
broad bandwidth, and highly symmetric coupling to transition edge sensor
bolometers
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE polarimeter; microstrip; aluminum oxide; loss tangent; thin film;
microwave modeling
ID QUANTUM INTERFERENCE DEVICE; ARRAYS; TIME
AB We describe a prototype detector system designed for precise measurements of Cosmic Microwave Background polarization. The design combines a quasi-optical polarization modulator, a metal feedhorn, a superconducting planar microwave circuit, and a pair of transition-edge sensor (TES) bolometers operating at < 100 mK. The circular feedhorn produces highly symmetric beams with very low cross-polarization. The planar circuit preserves symmetry in coupling to bolometers measuring orthogonal polarizations. We implement the circuit with superconducting niobium transmission lines. Three-dimensional interfaces between the planar circuit and waveguides leading to feedhorn and backshort have been carefully designed with electromagnetic simulations. Power is thermalized in resistors and conducted to bolometers via normal electrons. Our system is designed for a 29-43 GHz signal band. We have tested individual circuit elements in this frequency range. Fabrication of a full single-pixel system is underway.
C1 [Stevenson, T.; Benford, D.; Cao, N.; Chuss, D.; Denis, K.; Hsieh, W.; Kogut, A.; Moseley, S.; Panek, J.; Schneider, G.; Travers, D.; U-Yen, K.; Voellmer, G.; Wollack, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bennett, C.] Johns Hopkins Univ, Dept Phys, Baltimore, MD 21218 USA.
RP Stevenson, T (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM thomas.r.stevenson@nasa.gov
RI Benford, Dominic/D-4760-2012; Moseley, Harvey/D-5069-2012; Kogut,
Alan/D-6293-2012; Wollack, Edward/D-4467-2012
OI Benford, Dominic/0000-0002-9884-4206; Wollack,
Edward/0000-0002-7567-4451
NR 22
TC 7
Z9 7
U1 0
U2 2
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 471
EP 476
DI 10.1007/s10909-007-9679-0
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900076
ER
PT J
AU Day, P
Leduc, HG
Dowell, CD
Lee, RA
Turner, A
Zmuidzinas, J
AF Day, P.
Leduc, H. G.
Dowell, C. D.
Lee, R. A.
Turner, A.
Zmuidzinas, J.
TI Distributed antenna-coupled TES for FIR detector arrays
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE TES; antenna; FIR
ID METALS
AB We report progress toward large arrays of sensitive TES bolometers for submillimeter and far-infrared wavelengths with noise equivalent power (NEP) suitable for either imaging from a cooled space telescope or ground based spectroscopy. The arrays are based on a pixel design that makes use of a distributed transition edge sensor (TES) coupled to a slot antenna array. We have electrically characterized prototype detectors consisting of 256 TiN hot-electron TES microbolometers biased in parallel with T (c) =50 mK. The measured electron-phonon thermal conductance of prototype devices is as low as 1.1 pW/K at 50 mK corresponding to an electrical NEP of 4x10(-19) W/Hz(1/2). The time constant of two detectors with different geometries and transition widths was measured under a range of bias conditions. We have measured time constants greater than or similar to 10(-3) seconds, which is long enough for straightforward multiplexing with existing multiplexer technology.
C1 [Day, P.; Leduc, H. G.; Dowell, C. D.; Lee, R. A.; Turner, A.; Zmuidzinas, J.] Jet Propuls Lab, Pasadena, CA 91109 USA.
RP Day, P (reprint author), Jet Propuls Lab, Pasadena, CA 91109 USA.
EM Peter.K.Day@jpl.nasa.gov
NR 8
TC 6
Z9 6
U1 2
U2 4
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 477
EP 482
DI 10.1007/s10909-007-9676-3
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900077
ER
PT J
AU Miller, TM
Costen, N
Allen, C
AF Miller, Timothy M.
Costen, Nick
Allen, Christine
TI Indium hybridization of large format TES bolometer arrays to readout
multiplexers for far-infrared astronomy
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE indium; hybridization; TES; bolometer; infrared; astronomy
ID FABRICATION; SCUBA-2
AB In our effort to develop large format kilo-pixel arrays of transition edge sensors, we are working toward demonstrating electrical connectivity of a hybridized 32x40 element detector to a NIST multiplexer. The geometry of large-scale arrays that attempt to maintain a high filling factor does not allow for typical fan-out wiring, thus the detector array is hybridized directly to the readout multiplexer. The two parts are bonded together with 10 micron tall indium bumps, which complete the electrical path and also provide mechanical strength. The indium hybridization was developed and performed at the Goddard Space Flight Center and has been shown to withstand tensile loading up to 0.26 gram-force per indium bump. A cavity is deep etched behind each pixel prior to bonding, leaving only 30 micron support walls, which maintains a high filling fraction. Electrical continuity has been shown through the indium path in room temperature measurements. We report on the fabrication process used to hybridize the parts and the subsequent electrical performance.
C1 [Miller, Timothy M.; Costen, Nick; Allen, Christine] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Miller, TM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM timothy.m.miller@nasa.gov
NR 9
TC 6
Z9 6
U1 0
U2 1
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 483
EP 488
DI 10.1007/s10909-007-9677-2
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900078
ER
PT J
AU Silverberg, RF
Benford, DJ
Chen, T
Chervenak, J
Finkbeiner, FM
Miller, NA
Schmidt, D
Ullom, JN
AF Silverberg, R. F.
Benford, D. J.
Chen, T.
Chervenak, J.
Finkbeiner, F. M.
Miller, N. A.
Schmidt, D.
Ullom, J. N.
TI Superconducting transition-edge sensor bolometers with integrated
electron-tunneling refrigerators
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE tunneling; NIS refrigerator; TES bolometer
ID NOISE
AB We discuss the development of an array of superconducting Transition-Edge Sensor (TES) bolometers intended for use at millimeter wavelengths. Each bolometer in the array uses a proximity-effect TES sensing element and each has integrated Normal-Insulator-Superconductor (NIS) refrigerators to cool the bolometer below the reference bath temperature. The NIS refrigerators and bolometers are fabricated on a single Silicon substrate. Four short, thin and narrow legs suspend the millimeter wavelength radiation-absorbing element. The leg geometry is used to control and optimize the thermal conductance of the bolometer. Using the technology developed at NIST, we fabricated NIS refrigerators at the base of each of the suspension legs. These NIS refrigerators remove hot electrons by quantum-mechanical tunneling and should be capable of reducing the temperature of the biased (similar to 10 pW) bolometers by more than 100 mK when operating from a local thermal reservoir provided by a He-3 system at similar to 300 mK. This lower temperature at the bolometer will allow the detectors to approach background-limited performance despite the simple cryogenic system. In this paper we describe the progress toward the development of these detectors designed for use in observations at the 100 m Green Bank Telescope at 3 mm wavelength and the results of laboratory tests of a prototype detector.
C1 [Silverberg, R. F.; Benford, D. J.; Chen, T.; Chervenak, J.; Finkbeiner, F. M.; Miller, N. A.; Schmidt, D.; Ullom, J. N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Silverberg, RF (reprint author), NASA, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA.
EM robert.silverberg@nasa.gov
RI Tomlin, Nathan/A-4927-2009; Benford, Dominic/D-4760-2012
OI Tomlin, Nathan/0000-0002-8313-9045; Benford, Dominic/0000-0002-9884-4206
NR 6
TC 1
Z9 1
U1 0
U2 5
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 489
EP 494
DI 10.1007/s10909-007-9674-5
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900079
ER
PT J
AU Iyomoto, N
Bandler, SR
Brekosky, RP
Brown, AD
Chervenak, JA
Figueroa-Feliciano, E
Finkbeiner, FM
Kelley, RL
Kilbourne, CA
Porter, FS
Sadleir, JE
Smith, SJ
AF Iyomoto, N.
Bandler, S. R.
Brekosky, R. P.
Brown, A. -D.
Chervenak, J. A.
Figueroa-Feliciano, E.
Finkbeiner, F. M.
Kelley, R. L.
Kilbourne, C. A.
Porter, F. S.
Sadleir, J. E.
Smith, S. J.
TI Heat sinking and crosstalk for large, close-packed arrays of
microcalorimeters
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE microcalorimeters; transition edge sensors; X-ray spectroscopy
AB We have studied crosstalk on our 8x8 transition-edge sensor (TES) x-ray microcalorimeter arrays. The shapes of thermal crosstalk pulses are well reproduced as a convolution of heat input from the source pixel and decay in the receiver pixel. We have measured the amount of thermal crosstalk as a function of distance between the source and receiver pixels. Using the results, we have estimated the degradation of energy resolution due to the thermal crosstalk as a function of count rate to determine the level of thermal crosstalk that is needed to satisfy the requirements of NASA's Constellation-X mission.
C1 [Iyomoto, N.; Bandler, S. R.; Brekosky, R. P.; Brown, A. -D.; Chervenak, J. A.; Figueroa-Feliciano, E.; Finkbeiner, F. M.; Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.; Sadleir, J. E.; Smith, S. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Iyomoto, N (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
EM Naoko.Iyomoto@nasa.gov
RI Brown, Ari/B-1693-2008; Bandler, Simon/A-6258-2010; Smith,
Stephen/B-1256-2008; Porter, Frederick/D-3501-2012; Kelley,
Richard/K-4474-2012
OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675;
Porter, Frederick/0000-0002-6374-1119;
NR 4
TC 4
Z9 4
U1 0
U2 0
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 506
EP 512
DI 10.1007/s10909-007-9682-5
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900082
ER
PT J
AU Mazin, BA
Eckart, ME
Bumble, B
Golwala, S
Day, PK
Gao, J
Zmuidzinas, J
AF Mazin, B. A.
Eckart, M. E.
Bumble, B.
Golwala, S.
Day, P. K.
Gao, J.
Zmuidzinas, J.
TI Optical/UV and x-ray microwave kinetic inductance strip detectors
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE microwave; kinetic; inductance; detector; MKID; LTD
ID SPECTROPHOTOMETER; ENERGY
AB Microwave Kinetic Inductance Detectors (MKIDs) are superconducting detectors that sense the change in the surface impedance of a thin superconducting film when Cooper Pairs are broken by using a high quality factor resonant circuit. We are developing strip detectors that have aluminum MKID sensors on both ends of a rectangular tantalum strip. These devices can provide one dimensional spatial imaging with high quantum efficiency, energy resolution, and microsecond time resolution for single photons from the IR to the X-ray. We have demonstrated X-ray strip detectors with an energy resolution of 62 eV at 6 keV, and hope to improve this substantially. We will also report on our progress towards optical arrays for a planned camera for the Palomar 200 '' telescope.
C1 [Mazin, B. A.; Eckart, M. E.; Bumble, B.; Golwala, S.; Day, P. K.; Gao, J.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mazin, BA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ben.mazin@jpl.nasa.gov
RI Mazin, Ben/B-8704-2011
OI Mazin, Ben/0000-0003-0526-1114
NR 10
TC 17
Z9 17
U1 0
U2 1
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 537
EP 543
DI 10.1007/s10909-007-9686-1
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900087
ER
PT J
AU Golwala, S
Gao, J
Moore, D
Mazin, B
Eckart, M
Bumble, B
Day, P
LeDuc, HG
Zmuidzinas, J
AF Golwala, S.
Gao, J.
Moore, D.
Mazin, B.
Eckart, M.
Bumble, B.
Day, P.
LeDuc, H. G.
Zmuidzinas, J.
TI A WIMP dark matter detector using MKIDs
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE WIMP detectors; dark matter detectors; microwave kinetic inductance
detectors; phonon-mediated detectors; strip detectors;
position-sensitive detectors; nuclear-recoil discrimination
ID DYNAMICS; ARRAYS
AB We are pursuing the development of a phonon- and ionization-mediated WIMP dark matter detector employing microwave kinetic inductance detectors (MKIDs) in the phonon-sensing channel. Prospective advantages over existing detectors include: improved reconstruction of the phonon signal and event position; simplified readout wiring and cold electronics; and simplified and more reliable fabrication. We have modeled a simple design using available MKID sensitivity data and anticipate energy resolution as good as existing phonon-mediated detectors and improved position reconstruction. We are doing preparatory experimental work by fabricating strip absorber architectures. Measurements of diffusion length, trapping efficiency, and MKID sensitivity with these devices will enable us to design a 1 cm(2) x 2 mm prototype device to demonstrate phonon energy resolution and position reconstruction.
C1 [Golwala, S.; Gao, J.; Moore, D.; Eckart, M.; Zmuidzinas, J.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Mazin, B.; Bumble, B.; Day, P.; LeDuc, H. G.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Golwala, S (reprint author), CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
EM golwala@caltech.edu
RI Mazin, Ben/B-8704-2011
OI Mazin, Ben/0000-0003-0526-1114
NR 15
TC 11
Z9 11
U1 0
U2 0
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 550
EP 556
DI 10.1007/s10909-007-9687-0
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900089
ER
PT J
AU Gao, J
Zmuidzinas, J
Vayonakis, A
Day, P
Mazin, B
Leduc, H
AF Gao, J.
Zmuidzinas, J.
Vayonakis, A.
Day, P.
Mazin, B.
Leduc, H.
TI Equivalence of the effects on the complex conductivity of superconductor
due to temperature change and external pair breaking
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article; Proceedings Paper
CT 12th International Workshop on Low Temperature Detectors
CY JUL 22-27, 2007
CL Paris, FRANCE
DE complex conductivity; kinetic inductance detector
AB The responsivity of microwave kinetic inductance detector (MKID) is related to the derivative of the complex conductivity sigma with respect to the quasiparticle density n(qp). For thermal quasiparticles, this derivative d sigma/dn(qp) can be evaluated from s( T) and nqp( T) given by the Marttis-Bardeen theory (Phys. Rev. 14: 412, 1958). For excess quasiparticles due to external pair breaking, d sigma/dn(qp) can be evaluated by introducing an effective chemical potential mu* into the Marttis-Bardeens theory, as did by Owen and Scalapino ( Phys. Rev. Lett. 28: 1559, 1972). In this paper, we derive the expressions of d sigma/dn(qp) for both thermal and excess quasiparticles and show that they are approximately equal within the temperature and frequency range MKIDs operate. This equivalence validates the method of using bath temperature sweep to calibrate the responsivity of MKIDs. Response curves of an antenna-coupled submm MKID to bath temperature sweep and blackbody source temperature sweep are compared which demonstrates this equivalence.
C1 [Gao, J.; Zmuidzinas, J.; Vayonakis, A.] CALTECH, Dept Phys, Pasadena, CA 91125 USA.
[Day, P.; Mazin, B.; Leduc, H.] Jet Propuls Lab, Pasadena, CA 91109 USA.
RP Gao, J (reprint author), CALTECH, Dept Phys, Pasadena, CA 91125 USA.
EM jiansong@caltech.edu
RI Mazin, Ben/B-8704-2011
OI Mazin, Ben/0000-0003-0526-1114
NR 8
TC 27
Z9 27
U1 1
U2 7
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD APR
PY 2008
VL 151
IS 1-2
BP 557
EP 563
DI 10.1007/s10909-007-9688-z
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 270CP
UT WOS:000253697900090
ER
PT J
AU Zak, M
AF Zak, Michail
TI Quantum-inspired maximizer
SO JOURNAL OF MATHEMATICAL PHYSICS
LA English
DT Article
ID DYNAMICS
AB The objective of this paper is to create a new kind of dynamical systems-a quantum-classical hybrid-that would preserve superposition and entanglement of random solutions while allowing one to measure their state variables by using classical methods. Such an optimal combination of characteristics is a perfect match for quantum-inspired computing. The model is represented by a modified Madelung equation in which the quantum potential is replaced by a different, specially chosen "computational" potential. As a result, the dynamics attains both quantum and classical properties. Similarities and differences of the proposed model with quantum systems are outlined. As an application, an algorithm for the global maximum of an arbitrary integrable function is proposed. The idea of the proposed algorithms is very simple: based on the quantum-inspired maximizer, introduce a positive function to be maximized as the probability density to which the solution is attracted. Then, the larger value of this function will have the higher probability to appear. Special attention is paid to the simulation of integer programming, NP-complete problems and information retrieval. (c) 2008 American Institute of Physics.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Zak, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM michail.zak@gmail.com
NR 17
TC 7
Z9 7
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0022-2488
J9 J MATH PHYS
JI J. Math. Phys.
PD APR
PY 2008
VL 49
IS 4
AR 042702
DI 10.1063/1.2908281
PG 15
WC Physics, Mathematical
SC Physics
GA 295DY
UT WOS:000255456400017
ER
PT J
AU Rothman, LS
Martin-Torres, FJ
Flaud, JM
AF Rothman, Laurence S.
Martin-Torres, F. Javier
Flaud, Jean-Marie
TI Special issue on planetary atmospheres - Preface
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Editorial Material
C1 [Rothman, Laurence S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
[Martin-Torres, F. Javier] AS&M Inc, NASA, Langley Res Ctr, Hampton, VA USA.
[Flaud, Jean-Marie] Univ Paris 12, F-94010 Creteil, France.
[Flaud, Jean-Marie] Univ Paris 07, LISA, F-75221 Paris, France.
[Flaud, Jean-Marie] CNRS, F-75700 Paris, France.
RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, MS50,60 Garden St, Cambridge, MA 02138 USA.
EM lrothman@cfa.harvard.edu
RI Martin-Torres, Francisco Javier/G-6329-2015;
OI Martin-Torres, Francisco Javier/0000-0001-6479-2236; Rothman,
Laurence/0000-0002-3837-4847
NR 0
TC 4
Z9 4
U1 0
U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD APR
PY 2008
VL 109
IS 6
BP 881
EP 881
DI 10.1016/j.jqsrt.2008.02.002
PG 1
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 292WZ
UT WOS:000255298100001
ER
PT J
AU Villanueva, GL
Mumma, MJ
Novak, RE
Hewagama, T
AF Villanueva, Gerommo L.
Mumma, Michael J.
Novak, Robert E.
Hewagama, Tilak
TI Discovery of multiple bands of isotopic CO2 in the prime spectral
regions used when searching for CH4 and HDO on Mars
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE carbon dioxide; isotopes; intensities; near infrared; Mars; biomarkers
ID ATMOSPHERE
AB We present new measurements of vibrational band systems of isotopic carbon dioxide (CO2) with multiple strong lines in the wavelength region 3.3-3.7 mu m. In our ground-based searches for methane (CH4) and other biomarker gases on Mars, we discovered two new vibrational band systems that we identify as the previously unknown v(2) + v(3) band of (OCO)-O-16-C-12-O-18 and the 2v(1) band of the rare isotope (OCO)-O-16-C-13-O-18. We also extended and provide refined spectroscopic constants for the 2v(1) band of (OCO)-O-16-C-12-O-17, detecting 38 new lines. The newly discovered 2v(1) band of (OCO)-O-16-C-13-O-18 at 3.7 mu m and the 2v(1) band of (OCO)-O-16-C-12-O-17 at 3.6 mu m extend over the prime spectral region used when searching for deuterated water (HDO) and formaldehyde (H2CO) on Mars. The v(2) + v(3) band of (OCO)-O-16-C-12-O-18 at 3.3 mu m interferes with the v(3) band of CH4 at 3.3 mu m. If unrecognized, even weak bands of CO2 can obscure searches for trace gases on Mars, so it is important to quantify them. Here, we report molecular parameters from the measured line positions that agree well with values calculated from the known energy levels of these isotopologues, and we provide absolute band strengths for each system. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Villanueva, Gerommo L.; Hewagama, Tilak] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Novak, Robert E.] Iona Coll, Dept Phys, New Rochelle, NY 10801 USA.
[Hewagama, Tilak] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Villanueva, GL (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Mailstop 693, Greenbelt, MD 20771 USA.
EM geronimo.villanueva@nasa.gov
RI Hewagama, T/C-8488-2012; mumma, michael/I-2764-2013
NR 16
TC 18
Z9 18
U1 0
U2 2
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD APR
PY 2008
VL 109
IS 6
BP 883
EP 894
DI 10.1016/j.jqsrt.2007.12.016
PG 12
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 292WZ
UT WOS:000255298100002
ER
PT J
AU Toth, RA
Brown, LR
Miller, CE
Devi, VM
Benner, DC
AF Toth, R. A.
Brown, L. R.
Miller, C. E.
Devi, V. Malathy
Benner, D. Chris
TI Spectroscopic database of CO2 line parameters: 4300-7000 cm(-1)
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE near infrared; carbon dioxide; CO2; positions; intensities;
self-broadening; air-broadening; Lorentz widths; pressure shifts;
database
ID CONSTRAINED MULTISPECTRUM ANALYSIS; NEAR-INFRARED SPECTROSCOPY;
CARBON-DIOXIDE; SPEED DEPENDENCE; ATMOSPHERIC CO2; ENERGY-LEVELS;
INTENSITIES; POSITIONS; BANDS; (CO2)-C-12-O-16
AB A new spectroscopic database for carbon dioxide in the near infrared is presented to support remote sensing of the terrestrial planets (Mars, Venus and the Earth). The compilation contains over 28,500 transitions of 210 bands from 4300 to 7000 cm(-1) and involves nine isotopologues: (OCO)-O-16-C-12-O-16 (626), (OCO)-O-16-C-13-O-16 (636), (OCO)-O-16-C-12-O-18 (628), (OCO)-O-16-C-12-O-17 (627), (OCO)-O-16-C-13-O-18 (638), (OCO)-O-16-C-13-O-17 (637), (OCO)-O-18-C-12-O-18 (828), (OCO)-O-17-C-12-O-18 (728) and (OCO)-O-18-C-13-O-18 (838). Calculated line positions, line intensities, Lorentz half-width and pressure-induced shift coefficients for self- and air-broadening are taken from our recent measurements and are presented for the Voigt molecular line shape. The database includes line intensities for 108 bands measured using the McMath-Pierce Fourier transform spectrometer located on Kitt Peak, Arizona. The available broadening parameters (half-widths and pressure-induced shifts) of (OCO)-O-16-C-12-O-16 are applied to all isotopologues. Broadening coefficients are computed using empirical expressions that have been fitted to the experimental data. There are limited data for the temperature dependence of widths and so no improvement has been made for those parameters. The line intensities included in the catalog vary from 4 x 10(-30) to 1.29 x 10(-21) cm(-1)/(molecule cm(-2)) at 296 K. The total integrated intensity for this spectral interval is 5.9559 x 10(-20) cm(-1)/(molecule cm(-2)) at 296 K. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Toth, R. A.; Brown, L. R.; Miller, C. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Devi, V. Malathy; Benner, D. Chris] Coll William & Mary, Williamsburg, VA 23187 USA.
RP Toth, RA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ratoth@jpl.nasa.gov
NR 55
TC 79
Z9 79
U1 1
U2 18
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD APR
PY 2008
VL 109
IS 6
BP 906
EP 921
DI 10.1016/j.jqsrt.2007.12.004
PG 16
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 292WZ
UT WOS:000255298100004
ER
PT J
AU Smith, MAH
Rinsland, CP
Blake, TA
Sams, RL
Benner, DC
Devi, VM
AF Smith, M. A. H.
Rinsland, C. P.
Blake, T. A.
Sams, R. L.
Benner, D. Chris
Devi, V. Malathy
TI Low-temperature measurements of HCN broadened by N-2 in the 14-mu m
spectral region
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE HCN; Lorentz N-2-broadening; N-2 pressure-induced shifts; relaxation
matrix elements; speed dependence; temperature dependence; line mixing
ID DIODE-LASER MEASUREMENTS; MOLECULAR SPECTROSCOPIC DATABASE;
MULTISPECTRUM ANALYSIS; SHIFT COEFFICIENTS; TITANS ATMOSPHERE; NU(2)
BAND; V(1) BAND; NU-2 BAND; V(2) BAND; PART II
AB Half-width and pressure-induced shift coefficients; the temperature-dependence exponents of the half-widths and the temperature-dependence coefficients of pressure-induced shifts have been measured for N-2-broadened transitions in the v(2) band of HCN. Line positions and intensities were also determined. A total of 34 laboratory absorption spectra, recorded at 0.002-0.005 cm(-1) resolution with two different Fourier transform spectrometers, were used in the determination of the spectral line parameters. The total pressures of the HCN-N-2 samples ranged from less than 1 torr up to nearly 1 atm, and temperatures were between 211 and 300 K. A multispectrum nonlinear least-squares fitting technique employing a modified Voigt line profile, including speed dependence and line mixing via the off-diagonal relaxation matrix formulation, was used in the analysis. Speed-dependence parameters were determined in the P and R branches of the v(2) band of (HCN)-C-12-N-14, and in the v(2) Q branches of (HCN)-C-12-N-14 and (HCN)-C-13-N-14 the off-diagonal relaxation matrix elements that characterize line mixing were included in the analysis to fit the data. Present results are compared with previous measurements reported in the literature. (C) 2007 Published by Elsevier Ltd.
C1 [Smith, M. A. H.; Rinsland, C. P.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
[Blake, T. A.; Sams, R. L.] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Benner, D. Chris; Devi, V. Malathy] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
RP Smith, MAH (reprint author), NASA, Langley Res Ctr, Sci Directorate, MS 401A, Hampton, VA 23681 USA.
EM Mary.Ann.H.Smith@nasa.gov
NR 45
TC 2
Z9 2
U1 2
U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD APR
PY 2008
VL 109
IS 6
BP 922
EP 951
DI 10.1016/j.jqsrt.2007.12.017
PG 30
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 292WZ
UT WOS:000255298100005
ER
PT J
AU Rinsland, CP
Devi, VM
Benner, DC
Blake, TA
Sams, RL
Brown, LR
Kleiner, I
Dehayem-Kamadjeu, A
Muller, HSP
Gamache, RR
Niles, DL
Masiello, T
AF Rinsland, C. P.
Devi, V. Malathy
Benner, D. Chris
Blake, T. A.
Sams, R. L.
Brown, L. R.
Kleiner, I.
Dehayem-Kamadjeu, A.
Mueller, H. S. P.
Gamache, R. R.
Niles, D. L.
Masiello, T.
TI Multispectrum analysis of the v(4) band of CH3CN: Positions,
intensities, self- and N-2-broadening, and pressure-induced shifts
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE CH3CN; atmosphere of Titan; remote sounding; Fourier transform infrared
(FTIR) spectroscopy; pressure broadening; pressure-induced shifts;
spectral line shape; partition function; transmission and scattering of
radiation
ID METHYL CYANIDE; SPECTROSCOPIC DATABASE; MOLECULAR-SPECTROSCOPY;
ROTATIONAL SPECTRUM; COLOGNE DATABASE; LIMB SOUNDER; LINE;
METHYLCYANIDE; FREQUENCIES; STATES
AB A multispectrum nonlinear least-squares fitting technique was applied to measure accurate zero-pressure line center positions, Lorentz self- and nitrogen (N-2)-broadened half-width coefficients, and self- and N-2-pressure-induced shift coefficients for over 700 transitions in the parallel v(4) band of CH3CN near 920 cm(-1). Fifteen high-resolution (0.0016 cm(-1)) laboratory absorption spectra of pure and N-2-broadened CH3CN recorded at room temperature using the Bruker IFS 125HR Fourier transform spectrometer located at the Pacific Northwest National Laboratory (PNNL) in Richland, Washington, USA, were analyzed simultaneously assuming standard Voigt line shapes. Short spectral intervals containing manifolds of transitions from the same value of J were fitted together. In all, high-precision line parameters were obtained for P(44)-P(3)(-) and R(0)-R(46) manifolds. As part of the analysis, quantum assignments were extended, and the total internal partition function sum was calculated for four isotopologs: (CH3CN)-C-12-C-12, (CH3CN)-C-13-C-12, (CH3CN)-C-12-C-13, and (CH3CN)-C-13-C-13. Measurements of N-2 broadening, self-broadening, N-2-shift, and self-shift coefficients for transitions with J up to 48 and K up to 12 were measured for the first time in the mid-infrared. Self-broadened half-width coefficients were found to be very large (up to similar to 2cm(-1) atm(-1) at 296K). Ratios of self-broadened half-width coefficients to N-2-broadened half-width coefficients show a compact distribution with rotational quantum number in both the P and R branches that range from similar to 4.5 to 14 with maxima near vertical bar m vertical bar = 24, where m = -J '', J '', and J '' + 1 for P, Q and R lines, respectively. Pressure-induced shifts for N-2 are small (few exceed + 0.006 cm(-1) atm(-1) at 294 K) and are both positive and negative. In contrast, self-shift coefficients are large (maxima of about +/- 0.08 cm(-1) atm(-1) at 294 K) and are both positive and negative as a function of rotational quantum numbers. The present measured half-widths and pressure shifts in v(4) were compared with corresponding measurements of rotational transitions. (C) 2007 Elsevier Ltd. All rights reserved.
C1 [Rinsland, C. P.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Devi, V. Malathy; Benner, D. Chris] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
[Blake, T. A.; Sams, R. L.; Masiello, T.] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Brown, L. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kleiner, I.; Dehayem-Kamadjeu, A.] Univ Paris 07, Lab Interuniv Syst Atmospher, F-94010 Creteil, France.
[Kleiner, I.; Dehayem-Kamadjeu, A.] Univ Paris 12, F-94010 Creteil, France.
[Kleiner, I.; Dehayem-Kamadjeu, A.] CNRS, F-94010 Creteil, France.
[Mueller, H. S. P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
[Gamache, R. R.; Niles, D. L.] Univ Massachusetts, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA.
RP Rinsland, CP (reprint author), NASA, Langley Res Ctr, Mail Stop 401A, Hampton, VA 23681 USA.
EM curtis.p.rinsland@nasa.gov; Malathy.D.Venkataraman@nasa.gov;
dcbenn@wm.edu; ta.blake@pnl.gov; robert.sams@pnl.gov;
Linda.R.Brown@jpl.nasa.gov; kleiner@lisa.univ-paris12.fr;
dehayem@lisa.univ-paris12.fr; hspm@ph1.uni-koeln.de;
Robert_Gamache@uml.edu; dlniles@gmail.com; tony.masiello@nist.gov
NR 49
TC 17
Z9 17
U1 0
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD APR
PY 2008
VL 109
IS 6
BP 974
EP 994
DI 10.1016/j.jqsrt.2007.11.013
PG 21
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 292WZ
UT WOS:000255298100008
ER
PT J
AU Jacquinet-Husson, N
Scott, NA
Chedina, A
Crepeau, L
Armante, R
Capelle, V
Orphal, J
Coustenis, A
Boonne, C
Poulet-Crovisier, N
Barbee, A
Birk, M
Brown, LR
Camy-Peyret, C
Claveau, C
Chance, K
Christidis, N
Clerbaux, C
Coheur, PF
Dana, V
Daumont, L
De Backer-Barilly, MR
Di Lonardo, G
Flaud, JM
Goldman, A
Hamdouni, A
Hess, M
Hurley, MD
Jacquemart, D
Kleiner, I
Kopke, P
Mandin, JY
Massie, S
Mikhailenko, S
Nemtchinov, V
Nikitin, A
Newnham, D
Perrin, A
Perevalov, VI
Pinnock, S
Regalia-Jarlot, L
Rinsland, CP
Rublev, A
Schreier, F
Schult, L
Smith, KM
Tashkun, SA
Teffo, JL
Toth, RA
Tyuterev, VG
Auwera, JV
Varanasi, P
Wagner, G
AF Jacquinet-Husson, N.
Scott, N. A.
Chedina, A.
Crepeau, L.
Armante, R.
Capelle, V.
Orphal, J.
Coustenis, A.
Boonne, C.
Poulet-Crovisier, N.
Barbee, A.
Birk, M.
Brown, L. R.
Camy-Peyret, C.
Claveau, C.
Chance, K.
Christidis, N.
Clerbaux, C.
Coheur, P. F.
Dana, V.
Daumont, L.
De Backer-Barilly, M. R.
Di Lonardo, G.
Flaud, J. M.
Goldman, A.
Hamdouni, A.
Hess, M.
Hurley, M. D.
Jacquemart, D.
Kleiner, I.
Koepke, P.
Mandin, J. Y.
Massie, S.
Mikhailenko, S.
Nemtchinov, V.
Nikitin, A.
Newnham, D.
Perrin, A.
Perevalov, V. I.
Pinnock, S.
Regalia-Jarlot, L.
Rinsland, C. P.
Rublev, A.
Schreier, F.
Schult, L.
Smith, K. M.
Tashkun, S. A.
Teffo, J. L.
Toth, R. A.
Tyuterev, Vl. G.
Auwera, J. Vander
Varanasi, P.
Wagner, G.
TI The GEISA spectroscopic database: Current and future archive for Earth
and planetary atmosphere studies
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Review
DE GEISA; spectroscopic database; line parameters; cross-sections;
atmospheric absorption; atmospheric aerosols; Earth's and planetary
atmospheres
ID ABSORPTION CROSS-SECTIONS; FOURIER-TRANSFORM SPECTROSCOPY; O-2 HERZBERG
BANDS; ROTATIONAL LINE POSITIONS; SENSING REFERENCE DATA; M SPECTRAL
REGION; 231-794 NM RANGE; MU-M; WATER-VAPOR; CARBON-DIOXIDE
AB The development of Gestion et Etude des Informations Spectroscopiques Atmospheriques (GEISA: Management and Study of Spectroscopic Information) was started over three decades at Laboratoire de Meteorologie Dynamique (LMD) in France. GEISA is a computer accessible spectroscopic database, designed to facilitate accurate forward radiative transfer calculations using a line-by-line and layer-by-layer approach. More than 350 users have been registered for on-line use of the GEISA facilities. The current 2003 edition of GEISA (GEISA-03) is a system comprising three independent sub-databases devoted respectively to: line transition parameters, infrared and ultraviolet/visible absorption cross-sections, microphysical and optical properties of atmospheric aerosols.
Currently., GEISA is involved in activities related to the assessment of the capabilities of IASI (Infrared Atmospheric Sounding Interferometer on board of the METOP European satellite) through the GEISA/IASI database derived from GEISA.
The GEISA-03 content is presented, placing emphasis on molecular species of interest for Earth and planetary atmosphere studies, with details on the updated 2008 archive underway. A critical assessment on the needs, in terms of molecular parameters archive, related with recent satellite astrophysical missions is made. Detailed information on free online GEISA and GEISA/IASI access is given at http://ara.lmd.polytechnique.fr and http://ether.ipsl.jussieu.fr. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Jacquinet-Husson, N.; Scott, N. A.; Chedina, A.; Crepeau, L.; Armante, R.; Capelle, V.] Ecole Polytech, Inst Pierre Simon Laplace, Meteorol Dynam Lab, F-91128 Palaiseau, France.
[Orphal, J.; Flaud, J. M.; Kleiner, I.; Perrin, A.] Fac Sci & Technol, Lab Interuniv Syst Atmospher, F-94010 Creteil, France.
[Coustenis, A.] Observ Paris, Lab Etud Spatiales & Instrumentat Astrophys, F-92195 Meudon, France.
[Barbee, A.; Daumont, L.; De Backer-Barilly, M. R.; Hamdouni, A.; Regalia-Jarlot, L.; Tyuterev, Vl. G.] Univ Reims, Grp Spectrometrie Mol & Atmospher, F-51062 Reims, France.
[Birk, M.; Schreier, F.; Wagner, G.] DLR, Remote Sensing Technol Inst, D-82234 Oberpfaffenhofen, Wessling, Germany.
[Brown, L. R.; Toth, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Camy-Peyret, C.; Claveau, C.; Dana, V.; Mandin, J. Y.; Teffo, J. L.] Univ Paris 06, Lab Phys Mol Atmosphere & Astrophys, F-94200 Ivry, France.
[Chance, K.; Clerbaux, C.; Coheur, P. F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Christidis, N.; Pinnock, S.] Univ Reading, Dept Meteorol, Reading RG6 2AU, Berks, England.
[Clerbaux, C.] Univ Paris 06, Inst Pierre Simon Laplace, Serv Aeron, F-75252 Paris, France.
[Coheur, P. F.; Auwera, J. Vander] Univ Libre Bruxelles, Serv Chim Quant & Photophys, B-1050 Brussels, Belgium.
[Di Lonardo, G.] Univ Bologna, Dipartimento Chim Fis & Inorgan, I-40136 Bologna, Italy.
[Goldman, A.] Univ Denver, Dept Phys, Denver, CO 80208 USA.
[Hurley, M. D.] Ford Res Lab, Dearborn, MI 48124 USA.
[Jacquemart, D.] Univ Paris 06, Lab Dynam Interact & React, F-75252 Paris, France.
[Koepke, P.] Univ Munich, Inst Meteorol, D-80333 Munich, Germany.
[Massie, S.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Mikhailenko, S.; Nikitin, A.; Perevalov, V. I.; Tashkun, S. A.] Russian Acad Sci, Inst Atmospher Opt, Lab Theoret Spect, Tomsk 634055, Russia.
[Nemtchinov, V.; Varanasi, P.] SUNY Stony Brook, Stony Brook, NY 11794 USA.
[Newnham, D.; Smith, K. M.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[Rinsland, C. P.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
[Rublev, A.] Russian Res Ctr, Inst Mol Phys, Kurchatov Inst, Moscow 123183, Russia.
[Schult, L.] Max Planck Inst Meteorol, D-20146 Hamburg, Germany.
RP Jacquinet-Husson, N (reprint author), Ecole Polytech, Inst Pierre Simon Laplace, Meteorol Dynam Lab, Route Dept 36, F-91128 Palaiseau, France.
EM jacquinet@lmd.polytechnique.fr
RI Orphal, Johannes/A-8667-2012; Nikitin, Andrei/K-2624-2013; Tashkun,
Sergey/E-8682-2014; clerbaux, cathy/I-5478-2013;
OI Orphal, Johannes/0000-0002-1943-4496; Nikitin,
Andrei/0000-0002-4280-4096; Chance, Kelly/0000-0002-7339-7577
NR 104
TC 126
Z9 127
U1 1
U2 21
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 APR
PY 2008
VL 109
IS 6
BP 1043
EP 1059
DI 10.1016/j.jqsrt.2007.12.015
PG 17
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 292WZ
UT WOS:000255298100013
ER
PT J
AU Kratz, DP
AF Kratz, David P.
TI The sensitivity of radiative transfer calculations to the changes in the
HITRAN database from 1982 to 2004
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE HITRAN database; line parameters; line-by-line calculation; correlated
k-distribution; infrared; radiances; fluxes; radiative forcings
ID MOLECULAR SPECTROSCOPIC DATABASE; K-DISTRIBUTION METHOD; WATER-VAPOR;
CERES WINDOW; Q-BRANCHES; ABSORPTION; EDITION; CLOUDS; COMPILATION;
ATMOSPHERES
AB Over the last quarter century, improvements in the determination of the spectroscopic characteristics of the infrared-active trace species have enhanced our ability to retrieve quantitative distributions of temperatures, clouds, and abundances for various trace species within the Earth's atmosphere. These improvements have also allowed for refinements in the estimates of climatic effects attributed to changes in the Earth's atmospheric composition. Modeling efforts, however, have frequently experienced significant delays in assimilating improved spectroscopic information. Such is the case for highly parameterized models, where considerable effort is typically required to incorporate any revisions. Thus, a line-by-line radiative transfer model has been used to investigate the magnitude of the effects resulting from modifications to the spectroscopic information. Calculations from this line-by-line model have demonstrated that recent modifications to the HITRAN (High Resolution Transmission) line parameters, the continuum formulation, and the CO2 line-mixing formulation can significantly affect the interpretation of the high spectral resolution radiance and brightness temperature retrievals. For certain moderate-resolution satellite remote sensing channels, modifications to these spectroscopic parameters and formulations have shown the capacity to induce changes in the calculated radiances equivalent to brightness temperature differences of 1-2K. Model calculations have further shown that modifications of the spectroscopic characteristics tend to have a modest effect on the determination of spectrally integrated radiances, fluxes, and radiative forcing estimates, with the largest differences being of order 1 W m(-2) for the total thermal infrared fluxes, and of order 2-3% of the calculated radiative forcing at the tropopause attributed to the combined doubling of CO2, N2O, and CH4. The results from this investigation are intended to function as a guide to differentiate between cases where older parameterizations provide acceptable results, within specified accuracy bounds, and cases where upgrades to the latest spectroscopic database are necessary. Published by Elsevier Ltd.
C1 NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
RP Kratz, DP (reprint author), NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
EM david.p.kratz@nasa.gov
NR 40
TC 15
Z9 17
U1 1
U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD APR
PY 2008
VL 109
IS 6
BP 1060
EP 1080
DI 10.1016/j.jqsrt.2007.10.010
PG 21
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 292WZ
UT WOS:000255298100014
ER
PT J
AU Hewagama, T
Goldstein, J
Livengood, TA
Buhl, D
Espenak, F
Fast, K
Kostiuk, T
Schmulling, F
AF Hewagama, T.
Goldstein, J.
Livengood, T. A.
Buhl, D.
Espenak, F.
Fast, K.
Kostiuk, Th.
Schmuelling, F.
TI Beam integrated high-resolution infrared spectra: Accurate modeling of
thermal emission from extended clear atmospheres
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE radiative transfer; beam integration; spectroscopy; infrared;
atmospheres
ID SPECTROSCOPIC DATABASE; TEMPERATURE; TRANSMITTANCE; ABUNDANCE; ETHANE
AB We describe a technique for analysis of high resolution thermal IR spectra measured with a finite beam (field of view) on the target planetary atmosphere. The model developed allows a beam integrated radiative transfer calculation over the varying line-of-sight velocity, temperature, and species abundance distributed over the field of view, thus recovering information on atmospheric composition, dynamics, and thermal structure. The modeling procedure is comprises four primary aspects: segmentation of the projected observational beam to a grid of beam elements; determining the geometrical properties of the planetary atmospheric region associated with each beam element; calculating the spectrum emergent from the top of the atmosphere of each element; and weighting the ensemble of spectra with the characteristic observational beam response profile and accumulating the contributions. This prescription results in a beam integrated spectrum-a more accurate representation of fully resolved IR rotation-vibration molecular spectra of planetary atmospheres observed with finite aperture telescopes. The method is implemented as a numerical code appropriate for modeling the spectroscopic observations. This paper describes the basic formalism for beam integrated radiation transfer of planetary atmospheres, discusses the salient points of the modeling process, and quantifies limitations. Application of this technique will be illustrated using high resolution atmospheric molecular spectral line measurements of Titan obtained by infrared heterodyne spectroscopy to extract zonal wind field, temperature and C2H6 abundance. (C) 2007 Elsevier Ltd. All rights reserved.
C1 [Hewagama, T.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Goldstein, J.; Livengood, T. A.] Natl Ctr Earth & Space Sci Educ, Columbia, MD 21044 USA.
[Hewagama, T.; Livengood, T. A.; Buhl, D.; Espenak, F.; Fast, K.; Kostiuk, Th.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Schmuelling, F.] Univ Cologne, D-5000 Cologne 41, Germany.
RP Hewagama, T (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM tilak@cuzco.gsfc.nasa.gov
RI Livengood, Timothy/C-8512-2012; Hewagama, T/C-8488-2012; Kostiuk,
Theodor/A-3077-2014
NR 36
TC 6
Z9 6
U1 0
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD APR
PY 2008
VL 109
IS 6
BP 1081
EP 1097
DI 10.1016/j.jqsrt.2007.12.022
PG 17
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 292WZ
UT WOS:000255298100015
ER
PT J
AU Ustinov, EA
AF Ustinov, Eugene A.
TI Linearization of radiative heating and cooling rates for the case of
non-scattering planetary atmospheres
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE radiative transfer; sensitivity analysis; heating and cooling rates
ID WEIGHTING FUNCTIONS; ADJOINT
AB Rates of radiative heating and cooling of the non-scattering planetary atmosphere and scattering underlying surface are analytically linearized with respect to the atmospheric and surface parameters. Resulting expressions for sensitivities of radiative heating and cooling rates are used to formulate the linearized ID radiative model of atmospheric dynamics which directly incorporates the relevant linearized atmospheric and surface parameters. Applications to more sophisticated models of atmospheric dynamics, as well as extension to the case of presence of atmospheric scattering, are briefly discussed. (C) 2007 Elsevier Ltd. All rights reserved.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ustinov, EA (reprint author), CALTECH, Jet Prop Lab, Mail Stop 169-237,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Eugene.A.Ustinov@jpl.nasa.gov
RI Ustinov, Eugene/D-1350-2015
OI Ustinov, Eugene/0000-0003-0227-4286
NR 9
TC 0
Z9 0
U1 0
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD APR
PY 2008
VL 109
IS 6
BP 1098
EP 1117
DI 10.1016/j.jqsrt.2007.12.012
PG 20
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 292WZ
UT WOS:000255298100016
ER
PT J
AU Irwin, PGJ
Teanby, NA
de Kok, R
Fletcher, LN
Howett, CJA
Tsang, CCC
Wilson, CF
Calcutt, SB
Nixon, CA
Parrish, PD
AF Irwin, P. G. J.
Teanby, N. A.
de Kok, R.
Fletcher, L. N.
Howett, C. J. A.
Tsang, C. C. C.
Wilson, C. F.
Calcutt, S. B.
Nixon, C. A.
Parrish, P. D.
TI The NEMESIS planetary atmosphere radiative transfer and retrieval tool
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE retrievals; radiative transfer; correlated-k
ID MULTIPLE-SCATTERING; SPECTROSCOPIC DATABASE; LATITUDINAL VARIATIONS;
TITANS STRATOSPHERE; ABSORPTION-SPECTRA; CASSINI CIRS; PARAMETERS;
PHOSPHINE; AMMONIA; CM(-1)
AB With the exception of in situ atmospheric probes, the most useful way to study the atmospheres of other planets is to observe their electromagnetic spectra through remote observations, either from ground-based telescopes or from spacecraft. Atmospheric properties most consistent with these observed spectra are then derived with retrieval models. All retrieval models attempt to extract the maximum amount of atmospheric information from finite sets of data, but while the problem to be solved is fundamentally the same for any planetary atmosphere, until now all such models have been assembled ad hoc to address data from individual missions.
In this paper, we describe a new general-purpose retrieval model, Non-linear Optimal Estimator for MultivariatE Spectral analySIS (NEMESIS), which was originally developed to interpret observations of Saturn and Titan from the composite infrared spectrometer on board the NASA Cassini spacecraft. NEMESIS has been constructed to be generally applicable to any planetary atmosphere and can be applied from the visible/near-infrared right out to microwave wavelengths, modelling both reflected sunlight and thermal emission in either scattering or non-scattering conditions. NEMESIS has now been successfully applied to the analysis of data from many planetary missions and also ground-based observations. (C) 2007 Elsevier Ltd. All rights reserved.
C1 [Irwin, P. G. J.; Teanby, N. A.; de Kok, R.; Fletcher, L. N.; Howett, C. J. A.; Tsang, C. C. C.; Wilson, C. F.; Calcutt, S. B.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England.
[Nixon, C. A.] Univ Maryland, NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Parrish, P. D.] Univ Edinburgh, Sch Geosci, Inst Atmospher & Environm Sci, Edinburgh EH9 3JN, Midlothian, Scotland.
RP Irwin, PGJ (reprint author), Univ Oxford, Clarendon Lab, Parks Rd, Oxford OX1 3PU, England.
EM irwin@atm.ox.ac.uk
RI Fletcher, Leigh/D-6093-2011; Nixon, Conor/A-8531-2009;
OI Fletcher, Leigh/0000-0001-5834-9588; Nixon, Conor/0000-0001-9540-9121;
Calcutt, Simon/0000-0002-0102-3170; Teanby,
Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X
NR 27
TC 139
Z9 139
U1 1
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD APR
PY 2008
VL 109
IS 6
BP 1136
EP 1150
DI 10.1016/j.jqsrt.2007.11.006
PG 15
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 292WZ
UT WOS:000255298100018
ER
PT J
AU Nystuen, JA
Amitai, E
Anagnostou, EN
Anagnostou, MN
AF Nystuen, Jeffrey A.
Amitai, Eyal
Anagnostou, Emmanuel N.
Anagnostou, Marios N.
TI Spatial averaging of oceanic rainfall variability using underwater
sound: Ionian sea rainfall experiment 2004
SO JOURNAL OF THE ACOUSTICAL SOCIETY OF AMERICA
LA English
DT Article
ID NOISE
AB An experiment to evaluate the inherent spatial averaging of the underwater acoustic signal from rainfall was conducted in the winter of 2004 in the Ionian Sea southwest of Greece. A mooring with four passive aquatic listeners (PALs) at 60, 200, 1000, and 2000 in was deployed at 36.85 degrees N, 21.52 degrees E. 17 kin west of a dual-polarization X-band coastal radar at Methoni, Greece. The acoustic signal is classified into wind, rain, shipping, and whale categories. It is similar at all depths and rainfall is detected at all depths. A signal that is consistent with the clicking of deep-diving beaked whales is present 2% of the time, although there was no visual confirmation of whale presence. Co-detection of rainfall with the radar verifies that the acoustic detection of rainfall is excellent. Once detection is made, the correlation between acoustic and radar rainfall rates is high. Spatial averaging of the radar rainfall rates in concentric circles over the mooring verifies the larger inherent spatial averaging of the rainfall signal with recording depth. For the PAL at 2000 in, the maximum correlation was at 3-4 kin, suggesting a listening area for the acoustic rainfall measurement of roughly 30-50 km(2). (C) 2008 Acoustical Society of America.
C1 [Nystuen, Jeffrey A.] Univ Washington, Appl Phys Lab, Seattle, WA 98105 USA.
[Amitai, Eyal] George Mason Univ, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Amitai, Eyal] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Anagnostou, Emmanuel N.; Anagnostou, Marios N.] Univ Connecticut, Dept Civil & Environm Engn, Storrs, CT 06269 USA.
RP Nystuen, JA (reprint author), Univ Washington, Appl Phys Lab, 1013 NE 40th St, Seattle, WA 98105 USA.
EM nystuen@apl.washington.edu
NR 12
TC 9
Z9 11
U1 0
U2 5
PU ACOUSTICAL SOC AMER AMER INST PHYSICS
PI MELVILLE
PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA
SN 0001-4966
J9 J ACOUST SOC AM
JI J. Acoust. Soc. Am.
PD APR
PY 2008
VL 123
IS 4
BP 1952
EP 1962
DI 10.1121/1.2871485
PG 11
WC Acoustics; Audiology & Speech-Language Pathology
SC Acoustics; Audiology & Speech-Language Pathology
GA 289HD
UT WOS:000255044700017
PM 18397003
ER
PT J
AU Wilson, PS
Reed, AH
Wood, WT
Roy, RA
AF Wilson, Preston S.
Reed, Allen H.
Wood, Warren T.
Roy, Ronald A.
TI The low-frequency sound speed of fluid-like gas-bearing sediments
SO JOURNAL OF THE ACOUSTICAL SOCIETY OF AMERICA
LA English
DT Letter
ID ACOUSTIC PROPAGATION; WAVE-PROPAGATION; POROUS-MEDIA; IN-SITU; BUBBLES;
LIQUID; PREDICTIONS; SCATTERING; MIXTURE; MODEL
AB The low-frequency sound speed in a fluid-like kaolinite sediment containing air bubbles was measured using an acoustic resonator technique and found to be 114 m/s with negligible dispersion between 100 and 400 Hz. The sediment's void fraction and bubble size distribution was determined from volumetric images obtained from x-ray computed tomography scans. A simplified version of Wood's effective medium model, which is dependent only upon the ambient pressure, the void fraction, the sediment's bulk mass density, and the assumption that all the bubbles are smaller than resonance size at the highest frequency of interest, described the measured sound speed. (C) 2008 Acoustical Society of America.
C1 [Wilson, Preston S.] Univ Texas Austin, Appl Res Labs, Austin, TX 78713 USA.
[Wilson, Preston S.] Univ Texas Austin, Dept Mech Engn, Austin, TX 78712 USA.
[Reed, Allen H.; Wood, Warren T.] USN, Res Lab, Stennis Space Ctr, Marine GeoSci Div, Stennis Space Ctr, MS 39529 USA.
[Roy, Ronald A.] Boston Univ, Dept Aerosp & Mech Engn, Boston, MA 02215 USA.
RP Wilson, PS (reprint author), Univ Texas Austin, Appl Res Labs, POB 8029, Austin, TX 78713 USA.
EM pswilson@mail.utexas.edu; allen.reed@nrlssc.navy.mil;
warren.wood@nrlssc.navy.mil; ronroy@bu.edu
OI Roy, Ronald/0000-0001-6394-5667
NR 18
TC 4
Z9 4
U1 1
U2 5
PU ACOUSTICAL SOC AMER AMER INST PHYSICS
PI MELVILLE
PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA
SN 0001-4966
J9 J ACOUST SOC AM
JI J. Acoust. Soc. Am.
PD APR
PY 2008
VL 123
IS 4
BP EL99
EP EL104
DI 10.1121/1.2884081
PG 6
WC Acoustics; Audiology & Speech-Language Pathology
SC Acoustics; Audiology & Speech-Language Pathology
GA 289HD
UT WOS:000255044700071
PM 18396928
ER
PT J
AU Burnett, J
Smith, SM
Pickens, S
Aung, K
Dyer, CB
AF Burnett, J.
Smith, S. M.
Pickens, S.
Aung, K.
Dyer, C. B.
TI Vitamin D Deficiency and physical performance in vulnerable elders who
self-neglect
SO JOURNAL OF THE AMERICAN GERIATRICS SOCIETY
LA English
DT Meeting Abstract
CT Annual Meeting of the American-Geriatrics-Society
CY APR 30-MAY 04, 2008
CL Washington, DC
SP Amer Geriatr Soc
C1 [Burnett, J.; Pickens, S.; Aung, K.; Dyer, C. B.] Univ Texas Houston, Hlth Sci Ctr, Houston, TX USA.
[Smith, S. M.] NASA, Lyndon B Johnson Space Ctr, Human Adapt & Countermeasures Div, Houston, TX 77058 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU BLACKWELL PUBLISHING
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND
SN 0002-8614
J9 J AM GERIATR SOC
JI J. Am. Geriatr. Soc.
PD APR
PY 2008
VL 56
IS 4
SU S
MA D84
BP S188
EP S188
PG 1
WC Geriatrics & Gerontology; Gerontology
SC Geriatrics & Gerontology
GA 286IT
UT WOS:000254840300544
ER
PT J
AU Yeo, HS
AF Yeo, Hyeonsoo
TI Assessment of active controls for rotor performance enhancement
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article; Proceedings Paper
CT 62nd Annual Forum of the American-Helicopter-Society
CY MAY 09-11, 2006
CL Phoenix, AZ
ID TRAILING-EDGE FLAPS; HELICOPTER
AB A study was conducted to assess the capability of active controls to produce rotor performance improvements. The calculations were conducted using the comprehensive analysis CAMRAD II. The baseline rotor considered was a four-bladed articulated rotor with a VR-12 airfoil. Seven active control concepts were investigated: leading edge slat, variable droop leading edge, oscillatory jet, Gurney flap, individual blade control, active twist, and trailing edge flap. Comparative performance calculations have been conducted for two cases: (1) an airspeed sweep at C-T/sigma = 0.075 to examine rotor lift-to-drag ratio and (2) thrust sweeps at fixed airspeeds to estimate maximum blade loading capability. The individual blade control, active twist, and trailing edge flap concepts improved the rotor lift-to-drag ratio with a 2/rev harmonic control. The remaining four concepts-leading edge slat, variable droop leading edge, oscillatory jet, and Gurney flap-increased the blade maximum loading capability when these devices were used over the retreating side of the rotor disk.
C1 US Army Res Dev & Engn Command, Ames Res Ctr, Aeroflightdynam Directorate, Moffett Field, CA USA.
RP Yeo, HS (reprint author), US Army Res Dev & Engn Command, Ames Res Ctr, Aeroflightdynam Directorate, Moffett Field, CA USA.
EM hsyeo@mail.arc.nasa.gov
NR 31
TC 22
Z9 25
U1 0
U2 3
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD APR
PY 2008
VL 53
IS 2
BP 152
EP 163
PG 12
WC Engineering, Aerospace
SC Engineering
GA 288SS
UT WOS:000255006700004
ER
PT J
AU Masarati, P
Piatak, DJ
Quaranta, G
Singleton, JD
Shen, JW
AF Masarati, Pierangelo
Piatak, David J.
Quaranta, Giuseppe
Singleton, Jeffrey D.
Shen, Jinwei
TI Soft-inplane tiltrotor aeromechanics investigation using two
comprehensive multibody solvers
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
ID SYSTEMS; ROTORCRAFT; STABILITY; MODEL
AB This paper focuses on the development of multibody numerical models to predict the dynamic response, aeroelastic stability, and blade loading of a soft-inplane tiltrotor wind-tunnel model. Comprehensive rotorcraft-based multibody analyses enable modeling of the rotor system to a high level of detail such that complex mechanics and nonlinear effects associated with control system geometry, and joint deadband may be considered. The influence of these and other nonlinear effects on the aeromechanical behavior of the tiltrotor model is examined. To assess the reliability of the multibody approach to rotorcraft analysis, the results obtained using two different rotorcraft-based multibody solvers are analyzed and compared. A parametric study of some design parameters that may influence the aeromechanics of the soft-inplane rotor system is also included in this investigation.
C1 [Masarati, Pierangelo; Quaranta, Giuseppe] Politecn Milan, Dipartimento Ingn Aerospaziale, I-20133 Milan, Italy.
[Piatak, David J.] NASA, Langley Res Ctr, Aeroelast Branch, Hampton, VA 23665 USA.
[Singleton, Jeffrey D.] Army Res Labs, Vehicle Technol Directorate, Hampton, VA USA.
[Shen, Jinwei] Natl Inst Aerosp, Hampton, VA USA.
RP Quaranta, G (reprint author), Politecn Milan, Dipartimento Ingn Aerospaziale, I-20133 Milan, Italy.
EM quaranta@aero.polimi.it
RI Masarati, Pierangelo/I-3898-2012; Quaranta, Giuseppe/F-7955-2012
OI Masarati, Pierangelo/0000-0002-9347-7654; Quaranta,
Giuseppe/0000-0002-8873-7351
NR 33
TC 7
Z9 7
U1 0
U2 0
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD APR
PY 2008
VL 53
IS 2
BP 179
EP 192
DI 10.4050/JAHS.53.179
PG 14
WC Engineering, Aerospace
SC Engineering
GA 288SS
UT WOS:000255006700006
ER
PT J
AU Yeo, HS
Johnson, W
AF Yeo, Hyeonsoo
Johnson, Wayne
TI Prediction of rotor structural loads with comprehensive analysis
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article; Proceedings Paper
CT 31st European Rotorcraft Forum
CY SEP 13-15, 2005
CL Florence, ITALY
ID HELICOPTER
AB Blade flap and chord bending and torsion moments are investigated for five rotors operating at transition and high speed: H-34 in flight and wind tunnel, SA 330 (research Puma), SA 349/2, UH-60A full-scale, and BO-105 model (HART-I). The measured data from flight and wind tunnel tests are compared with calculations obtained using the comprehensive analysis CAMRAD II. The calculations were made using two free wake models: rolled-up and multiple-trailer with consolidation models. At transition speed, there is fair to good agreement for the flap and chord bending moments between the test data and analysis for the H-34, research Puma, and SA 349/2. Torsion moment correlation, in general, is fair to good for all the rotors investigated. Better flap bending and torsion moment correlation is obtained for the UH-60A and BO-105 rotors by using the multiple-trailer with consolidation wake model. In the high-speed condition, the analysis shows generally better correlation in magnitude than in phase for the flap bending and torsion moments. However, a significant underprediction of chord bending moment is observed for the research Puma and UH-60A. The poor correlation of the chord bending moment for the UH-60A appears to be caused by both the airloads model (at all radial locations) and the lag damper model (mostly at inboard locations).
C1 [Yeo, Hyeonsoo] USA, Aeroflightdynam Directorate, Res Dev & Engn Command, Ames Res Ctr, Moffett Field, CA USA.
[Johnson, Wayne] NASA, Ames Res Ctr, Aeromech Branch, Moffett Field, CA 94035 USA.
RP Yeo, HS (reprint author), USA, Aeroflightdynam Directorate, Res Dev & Engn Command, Ames Res Ctr, Moffett Field, CA USA.
EM hsyeo@mail.arc.nasa.gov
NR 13
TC 21
Z9 22
U1 0
U2 3
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD APR
PY 2008
VL 53
IS 2
BP 193
EP 209
PG 17
WC Engineering, Aerospace
SC Engineering
GA 288SS
UT WOS:000255006700007
ER
PT J
AU Luo, YL
Xu, KM
Morrison, H
McFarquhar, G
AF Luo, Yali
Xu, Kuan-Man
Morrison, Hugh
McFarquhar, Greg
TI Arctic mixed-phase clouds simulated by a cloud-resolving model:
Comparison with ARM observations and sensitivity to microphysics
parameterizations
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID RADIATIVE PROPERTIES; CLIMATE MODELS; ATMOSPHERIC RADIATION; STRATIFORM
CLOUDS; CIRRUS CLOUDS; ACCURATE PARAMETERIZATION; AEROSOL ACTIVATION;
ICE PARTICLES; WATER-VAPOR; CONVECTION
AB Single-layer mixed-phase stratiform (MPS) Arctic clouds, which formed under conditions of large surface heat flux combined with general subsidence during a subperiod of the Atmospheric Radiation Measurement (ARM) Program's Mixed-Phase Arctic Cloud Experiment (MPACE), are simulated with a cloud-resolving model (CRM). The CRM is implemented with either an advanced two-moment [ Morrison et al. (MCK)] or a commonly used one-moment [Lin et al. (LFO)] bulk microphysics scheme and a state-of-the-art radiative transfer scheme.
The MCK simulation, which uses the two-moment scheme and observed aerosol size distribution and ice nulei (IN) number concentration, reproduces the magnitudes and vertical structures of cloud liquid water content (LWC), total ice water content (IWC), and number concentration and effective radius of cloud droplets as suggested by the MPACE observations. The simulation underestimates ice crystal number concentrations by an order of magnitude and overestimates effective radius of ice crystals by a factor of 2-3. The LFO experiment, which uses the one-moment scheme, produces values of liquid water path (LWP) and ice plus snow water path (ISWP) that were about 30% and 4 times, respectively, those produced by MCK. The vertical profile of IWC exhibits a bimodal distribution in contrast to the constant distribution of IWC produced in MCK and observations.
A sensitivity test that uses the same ice-water saturation adjustment scheme as in LFO produces cloud properties that are more similar to the LFO simulation than MCK. The mean value of the intercept parameter of snow size spectra (N-0s) from MCK is one order of magnitude smaller than that assumed in LFO. A sensitivity test that prescribes the larger LFO N-0s results in 20% less LWP and 5 times larger snow water path than that in MCK. When an exponential ice size distribution replaces the gamma size distribution in MCK, the ISWP decreases by 70% but the LWP increases by 7% versus that in the MCK. Increasing the IN number concentration from the observed value of 0.16 to 3.2 L-1 forces the MPS clouds to become glaciated and dissipate, but the simulated ice number concentration agrees initially with the observations better. Physical explanations for these quantitative differences are provided. It is further shown that the differences between the LFO and MCK results are larger than those due to the estimated uncertainties in the prescribed surface fluxes. Additional observations and simulations of a variety of cases are required to further narrow down uncertainties in the microphysics schemes.
C1 [Luo, Yali] Natl Inst Aerosp, Hampton, VA USA.
[Luo, Yali; Xu, Kuan-Man] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Morrison, Hugh] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[McFarquhar, Greg] Univ Illinois, Urbana, IL 61801 USA.
RP Luo, YL (reprint author), Chinese Acad Meteorol Sci, State Key Lab Severe Weather, Beijing 100081, Peoples R China.
EM yali@cams.cma.gov.cn
RI Xu, Kuan-Man/B-7557-2013;
OI Xu, Kuan-Man/0000-0001-7851-2629; McFarquhar, Greg/0000-0003-0950-0135
NR 63
TC 22
Z9 24
U1 0
U2 8
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 APR
PY 2008
VL 65
IS 4
BP 1285
EP 1303
DI 10.1175/2007JAS2467.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 293VB
UT WOS:000255362400009
ER
PT J
AU Sabato, JS
AF Sabato, Jude S.
TI CO2 condensation in baroclinic eddies on early Mars
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID CARBON-DIOXIDE CLOUDS; MARTIAN ATMOSPHERE; PLANETARY-ATMOSPHERES;
RELATIVE-HUMIDITY; SIMPLIFIED MODEL; MASS SINK; CLIMATE; INSTABILITY;
WAVE; MIDLATITUDE
AB The efficacy of a cloud-radiative feedback on early Mars is reexamined in the context of the theory of baroclinic waves in midlatitudes. The feedback has been proposed to explain fluvial features on the surface of Mars. The radiative-convective models used to calculate the magnitude of the feedback require knowledge of the cloud depth, thickness, and areal coverage. Using a quasigeostrophic model and primitive equation simulations, it seems that less than 50% areal cloud cover is likely for early Mars, at least in midlatitudes. In accordance with previous studies for Earth, when condensational heating is included, the updraft region is narrower than in dry eddies. This results in reduced cloud cover and the feedback being weaker than previously thought. The simulations also show that condensation in eddies may have been important on a thick but cold early Mars but that its effects are much weaker for warmer climates.
C1 [Sabato, Jude S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Sabato, JS (reprint author), SW Res Inst, Dept Space Studies, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA.
EM jssabato@boulder.swri.edu
NR 47
TC 3
Z9 3
U1 0
U2 0
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 APR
PY 2008
VL 65
IS 4
BP 1378
EP 1395
DI 10.1175/2007JAS2504.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 293VB
UT WOS:000255362400014
ER
PT J
AU Grudinin, IS
Maleki, L
AF Grudinin, Ivan S.
Maleki, Lute
TI Efficient Raman laser based on a CaF2 resonator
SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA B-OPTICAL PHYSICS
LA English
DT Article
ID WHISPERING-GALLERY MODES; OPTICAL MICROCAVITIES; SCATTERING; CAVITY
AB We report on an ultralow-threshold Raman laser based on a CaF2 whispering-gallery-mode resonator. The laser is demonstrated to have a conversion efficiency above 60%. The observed low lasing threshold is made possible by the ultrahigh optical quality factor of the cavity, which is on the order of Q = 10(10). The laser is fiber-compatible and is fabricated with a very simple technique. We also demonstrate a single-mode operation of the laser in a multimode cavity as well as a multimode operation of the laser in a single-mode cavity. (C) 2008 Optical Society of America.
C1 [Grudinin, Ivan S.; Maleki, Lute] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Maleki, Lute] OEwaves, Pasadena, CA 91106 USA.
RP Grudinin, IS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM grudinin@caltech.edu
NR 18
TC 20
Z9 20
U1 1
U2 7
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0740-3224
J9 J OPT SOC AM B
JI J. Opt. Soc. Am. B-Opt. Phys.
PD APR
PY 2008
VL 25
IS 4
BP 594
EP 598
DI 10.1364/JOSAB.25.000594
PG 5
WC Optics
SC Optics
GA 294MS
UT WOS:000255410700014
ER
PT J
AU Bynum, MD
Hollis, BR
Hassan, HA
Xiao, X
AF Bynum, Michael D.
Hollis, Brian R.
Hassan, H. A.
Xiao, X.
TI Turbulent aeroheating on the mars science laboratory entry vehicle
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article; Proceedings Paper
CT AIAA 39th Thermophysics Conference
CY JUN 25-28, 2007
CL Miami, FL
SP AIAA
C1 [Bynum, Michael D.; Hassan, H. A.; Xiao, X.] N Carolina State Univ, Raleigh, NC 27695 USA.
[Hollis, Brian R.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
RP Bynum, MD (reprint author), N Carolina State Univ, Raleigh, NC 27695 USA.
NR 7
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0887-8722
J9 J THERMOPHYS HEAT TR
JI J. Thermophys. Heat Transf.
PD APR-JUN
PY 2008
VL 22
IS 2
BP 306
EP 309
DI 10.2514/1.33281
PG 4
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA 288DV
UT WOS:000254967300022
ER
PT J
AU Hamilton, D
Smart, K
Melton, S
Polk, JD
Johnson-Throop, K
AF Hamilton, Douglas
Smart, Kieran
Melton, Shannon
Polk, James D.
Johnson-Throop, Kathy
TI Autonomous medical care for exploration class space missions
SO JOURNAL OF TRAUMA-INJURY INFECTION AND CRITICAL CARE
LA English
DT Article
ID BREAST-CANCER; PNEUMOTHORAX; STRATEGIES; TRAUMA; DEATH
AB The US-based health care system of the International Space Station contains several subsystems, the Health Maintenance System, Environmental Health System and the Countermeasure System. These systems are designed to provide primary, secondary and tertiary medical prevention strategies. The medical system deployed in low Earth orbit for the International Space Station is designed to support a "stabilize and transport" concept of operations. In this paradigm, an ill or injured crewmember would be rapidly evacuated to a definitive medical care facility (DMCF) on Earth, rather than being treated for a protracted period on orbit.
The medical requirements of the short (7 day) and long duration (up to 6 months) exploration class missions to the moon are similar to low Earth orbit class missions but also include an additional 4 to 5 days needed to transport an ill or injured crewmember to a DMCF on Earth. Mars exploration class missions are quite different in that they will significantly delay or prevent the return of an ill or injured crewmember to a DMCF. In addition the limited mass, power and volume afforded to medical care will prevent the mission designers from manifesting the entire capability of terrestrial care. National Aeronautics and Space Administration has identified five levels of care as part of its approach to medical support of future missions including the Constellation program. To implement an effective medical risk mitigation strategy for exploration class missions, modifications to the current suite of space medical systems may be needed, including new crew medical officer training methods, treatment guidelines, diagnostic and therapeutic resources, and improved medical informatics.
C1 [Hamilton, Douglas; Smart, Kieran; Melton, Shannon] Wyle Life Sci, Houston, TX 77058 USA.
[Polk, James D.; Johnson-Throop, Kathy] NASA, Med Operat & Healthcare Syst, Washington, DC 20546 USA.
RP Hamilton, D (reprint author), Wyle Life Sci, 1290 Hercules Dr,Suite 120, Houston, TX 77058 USA.
EM dhamilton@wylehou.com
NR 19
TC 4
Z9 5
U1 1
U2 3
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA
SN 0022-5282
J9 J TRAUMA
JI J. Trauma-Injury Infect. Crit. Care
PD APR
PY 2008
VL 64
IS 4
SU S
BP S354
EP S363
DI 10.1097/TA.0b013e31816c005d
PG 10
WC Critical Care Medicine; Surgery
SC General & Internal Medicine; Surgery
GA 288WT
UT WOS:000255017400008
PM 18385587
ER
PT J
AU Kerrebrock, JL
Epstein, AH
Merchant, AA
Guenette, GR
Parker, D
Onnee, JF
Neumayer, F
Adamczyk, JJ
Shabbir, A
AF Kerrebrock, Jack L.
Epstein, Alan H.
Merchant, Ali A.
Guenette, Gerald R.
Parker, David
Onnee, Jean-Francois
Neumayer, Fritz
Adamczyk, John J.
Shabbir, Aamir
TI Design and test of an aspirated counter-rotating fan
SO JOURNAL OF TURBOMACHINERY-TRANSACTIONS OF THE ASME
LA English
DT Article
ID COMPRESSOR
AB The design and test of a two-stage, vaneless, aspirated counter-rotating fan is presented in this paper. The fan nominal design objectives were a pressure ratio of 3:1 and adiabatic efficiency of 87%. A pressure ratio of 2.9 at 89% efficiency was measured at the design speed. The configuration consists of a counter-swirl-producing inlet guide vane, followed by a high tip speed (1450 ft/s) nonaspirated rotor and a counter-rotating low speed (1150 ft/s) aspirated rotor. The lower tip speed and lower solidity of the second rotor result in a blade loading above conventional limits, but enable a balance between the shock loss and viscous boundary layer loss; the latter of which can be controlled by aspiration. The aspiration slot on the second rotor suction surface extends from the hub up to 80% span. The bleed flow is discharged inward through the blade hub. This fan was tested in a short duration blowdown facility. Particular attention was given to the design of the instrumentation to measure efficiency to 0.5% accuracy. High response static pressure measurements were taken between the rotors and downstream of the fan to determine the stall behavior. Pressure ratio, mass flow, and efficiency on speed lines from 90% to 102% of the design speed are presented and discussed along with comparison to computational fluid dynamics predictions and design intent. The results presented here complement those presented earlier for two aspirated fan stages with tip shrouds, extending the validated design space for aspirated compressors to include designs with conventional unshrouded rotors and with inward removal of the aspirated flow.
C1 [Kerrebrock, Jack L.; Epstein, Alan H.; Merchant, Ali A.; Guenette, Gerald R.; Parker, David; Onnee, Jean-Francois; Neumayer, Fritz] MIT, Gas Turbine Lab, Cambridge, MA 02139 USA.
[Adamczyk, John J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Shabbir, Aamir] Univ Toledo, Toledo, OH 43606 USA.
RP Kerrebrock, JL (reprint author), MIT, Gas Turbine Lab, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
NR 20
TC 6
Z9 11
U1 1
U2 11
PU ASME-AMER SOC MECHANICAL ENG
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0889-504X
J9 J TURBOMACH
JI J. Turbomach.-Trans. ASME
PD APR
PY 2008
VL 130
IS 2
AR 021004
DI 10.1115/1.2776951
PG 8
WC Engineering, Mechanical
SC Engineering
GA 279UP
UT WOS:000254380800004
ER
PT J
AU Templeton, TC
AF Templeton, Thomas Clay
TI Placing the library: An argument for the phenomenological and
constructivist approach to the human geography of the library
SO LIBRARY QUARTERLY
LA English
DT Article
ID INFORMATION
AB Place reminds us to tailor our professional work to the shifting concerns, and indeed the shifting criteria, of our shifting constituencies, rather than to a placeless professional vision of what librarianship, society, and literacy should be. Every place maker must make do, make sense, and make place in an environment that is technologically heterogeneous and in which the potential for novelty as well as recurrence is a persistent feature. The siege flag of place has been raised, not only in librarianship but in many sectors, in defense of the human and the parochial, of tradition and local turf. Taking a phenomenological cue, here we attempt to prune and redirect this problematic term. We arrive at what we consider reasonable criteria of success for ourselves: to what extent is our "library," in whatever professional sense we assign that word, vitally connected to the discursive practices of the places from which it draws its mandate? We contend that vitalizing a library in this respect requires us to step outside the sphere of our habitual familiarity and to explore other places. How we go about doing this is a matter of methodology. If a prior conception of place interferes with the absorption of ethnomethods, it should be held in suspension, bracketed at least until the practitioner can grasp the place that already exists.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Templeton, TC (reprint author), NASA, Goddard Space Flight Ctr, Code 305-0,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
NR 53
TC 6
Z9 6
U1 1
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0024-2519
J9 LIBR QUART
JI Libr. Q.
PD APR
PY 2008
VL 78
IS 2
BP 195
EP 209
DI 10.1086/528889
PG 15
WC Information Science & Library Science
SC Information Science & Library Science
GA 271FM
UT WOS:000253774300003
ER
PT J
AU Cintala, MJ
Horz, F
AF Cintala, Mark J.
Hoerz, Friedrich
TI Experimental impacts into chondritic targets, part I: Disruption of an
L6 chondrite by multiple impacts
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID HIGH-VELOCITY IMPACT; COLLISIONAL DISRUPTION; ASTEROIDS; METEORITES;
DENSITY; POROSITY; FRAGMENTATION; DESTRUCTION; SIMULATION; REGOLITHS
AB A fragment of an L6 chondrite (Allan Hills [ALH] 85017,13) with an initial mass (M-0) of 464.1 g was the target in a series of experimental impacts in which the largest remaining fragment (M-R) after each shot was impacted by a 3.18 mm ceramic sphere at a nominal speed of 2 km s(-1). This continued until the mass of the largest remaining piece was less than half the mass of the target presented to that shot (M-S). Two chunks of Bushveldt gabbro with similar initial masses were also impacted under the same conditions until M-R was less than half M-0. The two gabbro targets required a total of 1.51 x 10(7) and 1.75 x 10(7) erg g(-1) to attain 0.27 and 0.33 M-R/M-0, respectively; the chondrite, however, was considerably tougher, reaching 0.40 and 0.21 M-R/M-0 only after receiving 2.37 x 10(7) and 3.10 x 10(7) erg g(-1), respectively. The combined ejecta and spallation products from the gabbro impacts were coarser than those from the chondrite and in sufficient quantities that the new surface areas exceeded those from the meteorite until the fifth shot in the chondrite series, which was the number of impacts required to disrupt each gabbro target (i.e., M-R/M-0 <= 0.5). Unlike the behavior shown in previous regolith-evolution series, neither gabbro target produced an enhancement in the size fraction reflecting the mean size of the crystals composing the rock (about 3 mm), an effect possibly related to the width of the shock pulse. The original chondrite was so fine-grained and fractured, and the variance in its grain-size distribution so large, that effects related to grain size were relegated to the <63 mu m fraction. Impacts into ALH 85017 produced abundant, fine-grained debris, but otherwise the slopes of its size distributions were comparable to those from other experiments involving natural and fabricated terrestrial targets. The characteristic slopes of the chondrite's size distributions, however, were notably more constant over the entire nine-impact series than those from any of-the terrestrial targets, a testament to the control over comminution apparently exerted by pre-existing fractures and other, microscopic damage in the meteorite. The enhancement in the finer fraction of debris from ALH 85017 indicates that ordinary chondrites in solar orbit would be very efficient contributors to the cosmic-dust complex. At the same time, the greater resistance to disruption displayed by ordinary chondrites relative to that exhibited by igneous rocks indicates that a selection effect could be operative between the annealed, ordinary-chondritic breccias and relatively weaker, differentiated meteorites. Preferential survival from their time in the regoliths of their parent bodies through their transit to Earth and passage through the atmosphere suggests that meteorite collections could be biased in favor of the ordinary chondrites.
C1 [Cintala, Mark J.; Hoerz, Friedrich] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Cintala, MJ (reprint author), NASA, Lyndon B Johnson Space Ctr, Code KR, Houston, TX 77058 USA.
EM mark.j.cintala@nasa.gov
NR 56
TC 8
Z9 8
U1 2
U2 7
PU METEORITICAL SOC
PI FAYETTEVILLE
PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD APR
PY 2008
VL 43
IS 4
BP 771
EP 803
PG 33
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 346BX
UT WOS:000259044500010
ER
PT J
AU Mackenzie, AI
Baginski, ME
Rao, SM
AF Mackenzie, Anne I.
Baginski, Michael E.
Rao, Sadasiva M.
TI New basis functions for the electromagnetic solution of
arbitrarily-shaped, three dimensional conducting bodies using method of
moments
SO MICROWAVE AND OPTICAL TECHNOLOGY LETTERS
LA English
DT Article
DE method of moments; electromagnetics; scattering
ID SCATTERING; FIELD
AB In this work, we present a new set of basis functions, defined over a pair of planar triangular patches, for the solution of electromagnetic scattering and radiation problems associated with arbitrarily-shaped surfaces using the method of moments solution procedure. The basis functions are constant over the function subdomain and resemble pulse functions for one and two dimensional problems. Further, another set of basis functions, point-wise orthogonal to the first set, is also defined over the same function space. The primary objective of developing these basis functions is to utilize them for the electromagnetic solution involving conducting, dielectric, and composite bodies. However, in the present work, only the conducting body solution is presented and compared with other data. (C) 2008 Wiley Periodicals, Inc.
C1 [Baginski, Michael E.; Rao, Sadasiva M.] Auburn Univ, Dept E & CE, Auburn, AL 36849 USA.
[Mackenzie, Anne I.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Rao, SM (reprint author), Auburn Univ, Dept E & CE, Auburn, AL 36849 USA.
EM rao@eng.auburn.edu
NR 6
TC 2
Z9 2
U1 0
U2 1
PU JOHN WILEY & SONS INC
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 0895-2477
J9 MICROW OPT TECHN LET
JI Microw. Opt. Technol. Lett.
PD APR
PY 2008
VL 50
IS 4
BP 1121
EP 1124
DI 10.1002/mop.23295
PG 4
WC Engineering, Electrical & Electronic; Optics
SC Engineering; Optics
GA 275EW
UT WOS:000254055700080
ER
PT J
AU Yang, SC
Kalnay, E
Cai, M
Rienecker, MM
AF Yang, Shu-Chih
Kalnay, Eugenia
Cai, Ming
Rienecker, Michele M.
TI Bred vectors and tropical Pacific forecast errors in the NASA coupled
general circulation model
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID ENSEMBLE KALMAN FILTER; OCEAN-ATMOSPHERE MODEL; 4-DIMENSIONAL
VARIATIONAL ASSIMILATION; NINO SOUTHERN-OSCILLATION; MADDEN-JULIAN
OSCILLATION; 1997-98 EL-NINO; SINGULAR VECTORS; INITIAL CONDITIONS;
EQUATORIAL WAVES; ENSO
AB The breeding method has been implemented in the NASA Global Modeling and Assimilation Office coupled general circulation model (CGCM) in its operational configuration in which ocean data assimilation is used to initialize the coupled forecasts. Bred vectors (BVs), designed to capture the dominant growing errors in the atmosphere-ocean coupled system, are applied as initial ensemble perturbations. The potential improvement for ensemble prediction is investigated by comparing BVs with the oceanic growing errors, estimated by the one-month forecast error from the nonperturbed forecast. Results show that one-month forecast errors and BVs from the NASA CGCM share very similar features: BVs are clearly related to forecast errors in both SST and equatorial subsurface temperature-in particular, when the BV growth rate is large. Both the forecast errors and the BVs in the subsurface are dominated by large-scale structures near the thermocline. Results suggest that the forecast errors are dominated by dynamically evolving structures related to the variations of the background anomalous state, and that their shapes can be captured by BVs, especially during the strong 1997/98 El Nino. Hindcast experiments starting from January 1997 with one pair of BVs achieve a significant improvement relative to the control (unperturbed) hindcast by capturing many important features of this event, including the westerly wind burst in early 1997.
C1 [Yang, Shu-Chih; Kalnay, Eugenia] Univ Maryland, Dept Atmospher & Ocean Sci, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Yang, Shu-Chih; Rienecker, Michele M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Cai, Ming] Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA.
RP Yang, SC (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
EM scyang@atmos.umd.edu
RI Kalnay, Eugenia/F-4393-2010;
OI Kalnay, Eugenia/0000-0002-9984-9906
NR 66
TC 13
Z9 13
U1 0
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD APR
PY 2008
VL 136
IS 4
BP 1305
EP 1326
DI 10.1175/2007MWR2118.1
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 293RK
UT WOS:000255352200004
ER
PT J
AU Carrier, MJ
Zou, X
Lapenta, WM
AF Carrier, Matthew J.
Zou, Xiaolei
Lapenta, William M.
TI Comparing the vertical structures of weighting functions and adjoint
sensitivity of radiance and verifying mesoscale forecasts using AIRS
radiance observations
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID MODEL; ASSIMILATION; SYSTEM
AB An adjoint sensitivity analysis is conducted using the adjoint of the hyperspectral radiative transfer model (RTM) that simulates the radiance spectrum from the Advanced Infrared Sounder (AIRS). It is shown, both theoretically and numerically, that the height of the maximum sensitivity of radiance in a channel could be higher or lower than the height of the maximum weighting function of that channel. It is shown that the discrepancy between the two heights is determined by the vertical structures of the atmospheric thermodynamic state. The sensitivity finds the level at which changes in temperature and/or moisture will have the largest influence on the simulated brightness temperature (BT), and the maximum weighting function (WF) height indicates the level where the model atmosphere contributes most significantly to the emission at the top of the atmosphere. Based on the above findings, an adjoint method for forecast verification using AIRS radiances is presented. In this method, model forecasts are first mapped into radiance space by an RTM so that they can be compared directly with the observed radiance values. The adjoint sensitivity analysis results are then used to connect the deviations of the model forecasts from observed radiances to the changes of temperature and moisture variables in model space. This adjoint sensitivity based model verification provides useful information on forecast model performances based on indirect observations from satellites.
C1 [Carrier, Matthew J.; Zou, Xiaolei] Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA.
[Lapenta, William M.] NASA, George C Marshall Space Flight Ctr, Global Hydrol & Climate Ctr, Huntsville, AL 35812 USA.
RP Carrier, MJ (reprint author), Florida State Univ, Dept Meteorol, 404 Love Bldg, Tallahassee, FL 32306 USA.
EM mcarrier@met.fsu.edu
NR 17
TC 1
Z9 1
U1 0
U2 3
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD APR
PY 2008
VL 136
IS 4
BP 1327
EP 1348
DI 10.1175/2007MWR2057.1
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 293RK
UT WOS:000255352200005
ER
PT J
AU LaCasse, KM
Splitt, ME
Lazarus, SM
Lapenta, WM
AF LaCasse, Katherine M.
Splitt, Michael E.
Lazarus, Steven M.
Lapenta, William M.
TI The impact of high-resolution sea surface temperatures on the simulated
nocturnal Florida marine boundary layer
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID EASTERN EQUATORIAL PACIFIC; TROPICAL INSTABILITY WAVES; WIND STRESS;
REAL-TIME; PART I; NUMERICAL-SIMULATION; MESOSCALE ANALYSIS; AGULHAS
CURRENT; RETURN CURRENT; SST VARIATIONS
AB High- and low-resolution sea surface temperature (SST) analysis products are used to initialize the Weather Research and Forecasting (WRF) Model for May 2004 for short-term forecasts over Florida and surrounding waters. Initial and boundary conditions for the simulations were provided by a combination of observations, large-scale model output, and analysis products. The impact of using a l-km Moderate Resolution Imaging Spectroradiometer (MODIS) SST composite on subsequent evolution of the marine atmospheric boundary layer (MABL) is assessed through simulation comparisons and limited validation. Model results are presented for individual simulations, as well as for aggregates of easterly- and westerly-dominated low-level flows. The simulation comparisons show that the use of MODIS SST composites results in enhanced convergence zones, earlier and more intense horizontal convective rolls, and an increase in precipitation as well as a change in precipitation location. Validation of 10-m winds with buoys shows a slight improvement in wind speed. The most significant results of this study are that 1) vertical wind stress divergence and pressure gradient accelerations across the Florida Current region vary in importance as a function of flow direction and stability and 2) the warmer Florida Current in the MODIS product transports heat vertically and downwind of this heat source, modifying the thermal structure and the MABL wind field primarily through pressure gradient adjustments.
C1 [LaCasse, Katherine M.] Univ Alabama, Huntsville, AL 35805 USA.
[Splitt, Michael E.; Lazarus, Steven M.] Florida Inst Technol, Melbourne, FL 32901 USA.
[Lapenta, William M.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP LaCasse, KM (reprint author), Univ Alabama, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM kate.lacasse@nasa.gov
OI Splitt, Michael/0000-0002-7690-5100; Lazarus, Steven/0000-0002-5918-1059
NR 48
TC 17
Z9 17
U1 0
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD APR
PY 2008
VL 136
IS 4
BP 1349
EP 1372
DI 10.1175/2007MWR2167.1
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 293RK
UT WOS:000255352200006
ER
PT J
AU Schmidt, G
AF Schmidt, Gavin
TI To blog or not to blog?
SO NATURE GEOSCIENCE
LA English
DT Editorial Material
C1 Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Schmidt, G (reprint author), Columbia Univ, NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM Gavin.A.schmidt@nasa.gov
RI Schmidt, Gavin/D-4427-2012
OI Schmidt, Gavin/0000-0002-2258-0486
NR 0
TC 9
Z9 9
U1 0
U2 4
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK STREET, 9TH FLOOR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
J9 NAT GEOSCI
JI Nat. Geosci.
PD APR
PY 2008
VL 1
IS 4
BP 208
EP 208
DI 10.1038/ngeo170
PG 1
WC Geosciences, Multidisciplinary
SC Geology
GA 309BA
UT WOS:000256433500005
ER
PT J
AU Connolly, PJ
Jezorek, IG
Martens, KD
Prentice, EF
AF Connolly, Patrick J.
Jezorek, Ian G.
Martens, Kyle D.
Prentice, Earl F.
TI Measuring the performance of two stationary interrogation systems for
detecting downstream and upstream movement of PIT-tagged salmonids
SO NORTH AMERICAN JOURNAL OF FISHERIES MANAGEMENT
LA English
DT Article
ID JUVENILE ATLANTIC SALMON; INTEGRATED TRANSPONDER TAGS; CHINOOK SALMON;
HABITAT USE; COLUMBIA RIVERS; SMALL STREAMS; FISH; SURVIVAL; BEHAVIOR;
SNAKE
AB We tested the performance of two stationary interrogation systems designed for detecting the movement of fish with passive integrated transponder (PIT) tags. These systems allowed us to determine the direction of fish movement with high detection efficiency and high precision in a dynamic stream environment. We describe an indirect method for deriving an estimate for detection efficiency and the associated variance that does not rely on a known number of fish passing the system. By using six antennas arranged in a longitudinal series of three arrays, we attained detection efficiencies for downstream- and upstream-moving fish exceeding 96% during high-flow periods and approached 100% during low-flow periods for the two interrogation systems we tested. Because these systems did not rely on structural components, such as bridges or culverts, they were readily adaptable to remote, natural stream sites. Because of built-in redundancy, these systems were able to perform even with a loss of one or more antennas owing to dislodgement or electrical failure. However, the reduction in redundancy resulted in decreased efficiency and precision and the potential loss of ability to determine the direction of fish movement. What we learned about these systems should be applicable to a wide variety of other antenna configurations and to other types of PIT tags and transceivers.
C1 [Connolly, Patrick J.; Jezorek, Ian G.; Martens, Kyle D.] Western Fisheries Res Ctr, Columbia River Res Lab, US Geol Survey, Cook, WA 98605 USA.
[Prentice, Earl F.] Manchester Res Field Stn, Natl Marine Fisheries Serv, Manchester, WA 98353 USA.
RP Connolly, PJ (reprint author), Western Fisheries Res Ctr, Columbia River Res Lab, US Geol Survey, 5501A Cook-Underwood Rd, Cook, WA 98605 USA.
EM pconnolly@usgs.gov
NR 34
TC 30
Z9 30
U1 4
U2 18
PU AMER FISHERIES SOC
PI BETHESDA
PA 5410 GROSVENOR LANE SUITE 110, BETHESDA, MD 20814-2199 USA
SN 0275-5947
J9 N AM J FISH MANAGE
JI North Am. J. Fish Manage.
PD APR
PY 2008
VL 28
IS 2
BP 402
EP 417
DI 10.1577/M07-008.1
PG 16
WC Fisheries
SC Fisheries
GA 293BR
UT WOS:000255310300007
ER
PT J
AU Moiseev, AA
AF Moiseev, A. A.
TI Gamnia-ray large area space telescope: Mission overview
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article; Proceedings Paper
CT 1st Roma International Conference on Astroparticle Physics
CY JUN 20-22, 2007
CL Rome, ITALY
DE gamma-ray telescope; gamma rays; gamma-ray burst; AGN; pulsar; SNR
ID GLAST; TESTS
AB The new Gamma-ray Large Area Space Telescope (GLAST) is scheduled for launch in the middle of 2008. It contains the high energy gamma-ray telescope Large Area Telescope (LAT) which covers the energy range from 20 MeV to > 300 GeV and the GLAST Burst Monitor (GMB), covering 8 keV-30 MeV energy range. The GLAST science objectives include understanding the mechanism of charged particle acceleration in active galactic nuclei, pulsars and supernova remnants, determining the nature of the still-unidentified EGRET sources, detailed study of gamma-ray diffuse emission, high-energy emission from gamma-ray bursts and transient sources, and probing dark matter. A brief overview of the mission is given. (c) 2008 Elsevier B.V. All rights reserved.
C1 [Moiseev, A. A.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Moiseev, A. A.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
RP Moiseev, AA (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
EM alexander.a.moiseev@nasa.gov
NR 10
TC 8
Z9 8
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-9002
J9 NUCL INSTRUM METH A
JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc.
Equip.
PD APR 1
PY 2008
VL 588
IS 1-2
BP 41
EP 47
DI 10.1016/j.nima.2008.01.005
PG 7
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 295RF
UT WOS:000255490900010
ER
PT J
AU Emfietzoglou, D
Abril, I
Garcia-Molina, R
Petsalakis, ID
Nikjoo, H
Kyriakou, I
Pathak, A
AF Emfietzoglou, D.
Abril, I.
Garcia-Molina, R.
Petsalakis, I. D.
Nikjoo, H.
Kyriakou, I.
Pathak, A.
TI Semi-empirical dielectric descriptions of the Bethe surface of the
valence bands of condensed water
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM
INTERACTIONS WITH MATERIALS AND ATOMS
LA English
DT Article; Proceedings Paper
CT 18th International Conference on Ion Beam Analysis
CY SEP 23-28, 2007
CL Univ Hyderabad, Sch Phys, Hyderabad, INDIA
SP Inter Univ Accelerator Ctr, Inst Phys
HO Univ Hyderabad, Sch Phys
DE inelastic scattering; Bethe surface; Bethe ridge; dielectric function;
energy loss function; water; ice
ID MONTE-CARLO-SIMULATION; LOW-ENERGY ELECTRONS; X-RAY-SCATTERING;
INELASTIC CROSS-SECTIONS; MEAN FREE PATHS; LIQUID WATER; STOPPING
POWERS; OPTICAL-DATA; SECONDARY-ELECTRON; CHARGED-PARTICLES
AB The Bethe surface of a material is an essential element in the study of inelastic scattering at low impact energies where the optical approximation fails. In this work we examine various semi-empirical models for the dielectric response function of condensed water towards an improved description of the energy-loss function over the whole energy-momentum plane (i.e. Bethe surface). The experimental "optical" data (i.e. at zero momentum transfer) for the valence bands of liquid and solid water are analytically represented by a sum-rule constrained linear combination of Drude-type functions. The dependence on momentum transfer is introduced through various widespread "extension" schemes which are compared against the available Compton scattering data. It is shown that the widely used Lindhard function along with its "single-pole" (or "delta-oscillator") approximation used in the Penn and Ashley models, as well as the Ritchie and Howie extended-Drude scheme with a simple quadratic dispersion, predict a sharp Bethe ridge which compares poorly with the experimental profile. In contrast, the Mermin dielectric function provides a more realistic account of the observed broadening with momentum transfer. An improved fully-extended-Drude model is presented which incorporates the momentum broadening and line-shift of the Bethe ridge and distinguishes between the different dispersion of the discrete and continuum spectra of water. (c) 2007 Elsevier B.V. All rights reserved.
C1 [Pathak, A.] Univ Hyderabad, Sch Phys, Hyderabad 500046, Andhra Pradesh, India.
[Emfietzoglou, D.; Kyriakou, I.] Univ Ioannina, Sch Med, Med Phys Lab, GR-45110 Ioannina, Greece.
[Abril, I.] Univ Alicante, Dept Fis Aplicada, E-03080 Alicante, Spain.
[Garcia-Molina, R.] Univ Murcia, Dept Fis CIOyN, E-30080 Murcia, Spain.
[Petsalakis, I. D.] Natl Hellen Res Fdn, Inst Theoret & Phys Chem, GR-11635 Athens, Greece.
[Nikjoo, H.] USRA, NASA Johnson Space Ctr, Ctr Adv Space Studies, Houston, TX 77058 USA.
RP Pathak, A (reprint author), Univ Hyderabad, Sch Phys, Hyderabad 500046, Andhra Pradesh, India.
EM appsp@uohyd.ernet.in
RI Emfietzoglou, Dimitris/G-7168-2012; nhrf, tpci/M-8699-2013; Abril,
Isabel/L-6938-2014; Garcia-Molina, Rafael/L-5679-2014
OI Abril, Isabel/0000-0001-9366-3484; Garcia-Molina,
Rafael/0000-0001-8755-8709
NR 52
TC 21
Z9 21
U1 1
U2 20
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-583X
J9 NUCL INSTRUM METH B
JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms
PD APR
PY 2008
VL 266
IS 8
BP 1154
EP 1161
DI 10.1016/j.nimb.2007.11.057
PG 8
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Atomic, Molecular & Chemical; Physics, Nuclear
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 312NH
UT WOS:000256677600003
ER
PT J
AU Bousis, C
Emfietzoglou, D
Hadjidoukas, P
Nikjoo, H
Pathak, A
AF Bousis, C.
Emfietzoglou, D.
Hadjidoukas, P.
Nikjoo, H.
Pathak, A.
TI Electron ionization cross-section calculations for liquid water at high
impact energies
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM
INTERACTIONS WITH MATERIALS AND ATOMS
LA English
DT Article; Proceedings Paper
CT 18th International Conference on Ion Beam Analysis
CY SEP 23-28, 2007
CL Univ Hyderabad, Sch Phys, Hyderabad, INDIA
SP Inter Univ Accelerator Ctr, Inst Phys
HO Univ Hyderabad, Sch Phys
DE electrons; ionization; cross-sections; water
ID INELASTIC-SCATTERING; SECONDARY ELECTRONS; CHARGED PARTICLES; CONDENSED
MATTER; TRACK-STRUCTURE; MOLECULES; MODEL; COLLISIONS; ATOMS; H2O
AB Cross-sections for the ionization of liquid water is perhaps the most essential set of data needed for modeling electron transport in biological matter. The complexity of ab initio calculations for any multi-electron target has led to largely heuristic semi-empirical models which take advantage elements of the Bethe, dielectric and binary collision theories. In this work we present various theoretical models for calculating total ionization cross-sections (TICSs) for liquid water over the 10 keV-1 MeV electron energy range. In particular, we extend our recent dielectric model calculations for liquid water to relativistic energies using both the appropriate kinematic corrections and the transverse part. Comparisons are made with widely used atomic and molecular TICS models such as those of Khare and co-workers, Kim-Rudd, Deutsch-Mark, Vriens and Gryzinski. The required dipole oscillator strength was provided by our recent optical-data model which is based on the latest experimental data for liquid water. The TICSs computed by the above models differ by up to 40% from the dielectric results. The best agreement (to within similar to 10%) was obtained by Khare's original model and an approximate form of Gryzinski's model. In contrast, the binary-encounter-dipole (BED) models of both Kim-Rudd and Khare and co-workers resulted in similar to 10-20% higher TICS values, while discrepancies increased to similar to 30-40% when their simpler binary-encounter-Bethe (BEB) versions were used. Finally, we discuss to what extent the accuracy of the TICS is indicative of the reliability of the underlying differential cross-sections. (c) 2007 Elsevier B.V. All rights reserved.
C1 [Pathak, A.] Univ Hyderabad, Sch Phys, Hyderabad 500046, Andhra Pradesh, India.
[Bousis, C.; Emfietzoglou, D.] Univ Ioannina, Dept Med Phys, GR-45110 Ioannina, Greece.
[Hadjidoukas, P.] Univ Ioannina, Dept Comp Sci, GR-45110 Ioannina, Greece.
[Nikjoo, H.] USRA, NASA Johnson Space Ctr, Ctr Adv Space Studies, Houston, TX 77058 USA.
[Nikjoo, H.] Univ Nottingham, Sch Pharm, Nottingham NG7 2RD, England.
[Nikjoo, H.] Univ Nottingham, Ctr Biomol Sci, Nottingham NG7 2RD, England.
RP Pathak, A (reprint author), Univ Hyderabad, Sch Phys, Hyderabad 500046, Andhra Pradesh, India.
EM appsp@uohyd.ernet.in
RI Emfietzoglou, Dimitris/G-7168-2012;
OI Hadjidoukas, Panagiotis/0000-0002-2528-7568
NR 32
TC 17
Z9 17
U1 0
U2 3
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-583X
J9 NUCL INSTRUM METH B
JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms
PD APR
PY 2008
VL 266
IS 8
BP 1185
EP 1192
DI 10.1016/j.nimb.2007.11.015
PG 8
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Atomic, Molecular & Chemical; Physics, Nuclear
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 312NH
UT WOS:000256677600010
ER
PT J
AU Stysley, PR
Poulios, D
Coyle, DB
Kay, RB
AF Stysley, Paul R.
Poulios, Demetrios
Coyle, Donald B.
Kay, Richard B.
TI Highly efficient dual head 100 mJ TEM00 Nd : YAG oscillator
SO OPTICS AND LASER TECHNOLOGY
LA English
DT Article
DE Q-switched; Nd : YAG; LIDAR
ID LASER
AB A diode-pumped, Q-switched Nd:YAG laser employing a dual-pump zig-zag slab head scheme in an unstable resonator configuration for use in space-based planetary altimetry or atmospheric LIDAR is described. The pump heads are aligned orthogonally to each other, producing a symmetric overall thermal lens that eliminates the need for an intracavity cylindrical lens and aperture. This laser has demonstrated over 100 mJ in Q-switched operation with high optical efficiency (24%), good beam quality, high pointing stability, and large operational margins for multi-billion shot lifetimes. (C) 2007 Elsevier Ltd. All rights reserved.
C1 [Stysley, Paul R.; Poulios, Demetrios; Kay, Richard B.] American Univ, Dept Phys, Washington, DC 20016 USA.
[Coyle, Donald B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Stysley, PR (reprint author), American Univ, Dept Phys, Washington, DC 20016 USA.
EM Paul.R.Stysley@nasa.gov
NR 7
TC 5
Z9 5
U1 1
U2 2
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0030-3992
J9 OPT LASER TECHNOL
JI Opt. Laser Technol.
PD APR
PY 2008
VL 40
IS 3
BP 435
EP 440
DI 10.1016/j.optlastec.2007.07.009
PG 6
WC Optics; Physics, Applied
SC Optics; Physics
GA 242TA
UT WOS:000251747700002
ER
PT J
AU Arthur, KE
Balazs, GH
AF Arthur, Karen E.
Balazs, George H.
TI A comparison of immature green turtles (Chelonia mydas) diets among
seven sites in the main Hawaiian islands'
SO PACIFIC SCIENCE
LA English
DT Article
ID SEA-TURTLES; VARIABILITY; NUMBERS; GROWTH
AB Understanding resource acquisition and feeding ecology of threatened species is integral to their conservation because diet is intimately linked with growth rate and reproductive output. We examined diets of immature green sea turtles, Chelonia mnydas (L.), from seven sites on the islands of Hawai'i, O'ahu, Moloka'i, and Lana'i in January and August 2003. Diet analysis was based on 191 samples collected from 181 live green turtles by stomach lavage. These samples were identified and quantified using dissection microscopy and the principles of microstereology. Diet of green turtles in the Main Hawaiian Islands was dominated by red algae, and diet items most commonly encountered were Acanthophora spicifera (an introduced species), Hypnea sp., Pterocladiella sp., and Cladophora sp. Sea grasses (Halophila hawaiiana and H. decipiens) were an important component of diet in turtles from Kane'ohe Bay. Content of green turtle diets differed among foraging grounds, and these differences may provide an insight into previously documented differences in turtle growth rates among sites.
C1 [Arthur, Karen E.] Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia.
[Balazs, George H.] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA.
RP Arthur, KE (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA.
EM arthur@si.edu
RI Arthur, Karen/A-3089-2012
NR 41
TC 33
Z9 36
U1 1
U2 16
PU UNIV HAWAII PRESS
PI HONOLULU
PA 2840 KOLOWALU ST, HONOLULU, HI 96822 USA
SN 0030-8870
EI 1534-6188
J9 PAC SCI
JI Pac. Sci.
PD APR
PY 2008
VL 62
IS 2
BP 205
EP 217
DI 10.2984/1534-6188(2008)62[205:ACOIGT]2.0.CO;2
PG 13
WC Marine & Freshwater Biology; Zoology
SC Marine & Freshwater Biology; Zoology
GA 287VL
UT WOS:000254944500004
ER
PT J
AU Matsko, AB
Strekalov, DV
Yu, N
AF Matsko, A. B.
Strekalov, D. V.
Yu, N.
TI Sensitivity of terahertz photonic receivers
SO PHYSICAL REVIEW A
LA English
DT Article
ID FREQUENCY UP-CONVERSION; MICROWAVE RECEIVER; UPCONVERSION
AB We theoretically discuss sensitivity limitations of a THz receiver which is based on up-conversion of the THz radiation into optical domain using high quality factor crystalline whispering gallery mode resonators. We show that the sensitivity of the receiver operating in the nonlinear regime approaches the sensitivity of an ideal THz photon counter. Thermal noise of the counter can be substantially reduced because of transparency of the nonlinear material in the THz frequency range. We also show that the density of power fluctuations of the receiver operating in the linear regime is given by the THz shot noise.
C1 [Matsko, A. B.; Strekalov, D. V.; Yu, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Matsko, AB (reprint author), OEwaves Inc, 1010 E Union St, Pasadena, CA 91106 USA.
NR 13
TC 12
Z9 12
U1 0
U2 2
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD APR
PY 2008
VL 77
IS 4
AR 043812
DI 10.1103/PhysRevA.77.043812
PG 5
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 295EF
UT WOS:000255457100168
ER
PT J
AU Boykin, TB
Luisier, M
Klimeck, G
AF Boykin, Timothy B.
Luisier, Mathieu
Klimeck, Gerhard
TI Multiband transmission calculations for nanowires using an optimized
renormalization method
SO PHYSICAL REVIEW B
LA English
DT Article
ID SYSTEMS; SEMICONDUCTORS; TRANSPORT; DEVICES; MODEL
AB The discovery of an interesting nanostructure behavior or the design of useful nanodevices requires state-of-the-art physical models. Realistic, multiband nanowire calculations especially tend to be computationally intensive and slow. Here, we develop optimizations to the renormalization method of Grosso [Phys. Rev. B 40, 12328 (1989)] specifically for nanowires with [100]- or [111]-oriented axes. For no-spin-orbit models, our optimizations give far superior performance to other available methods, while for spin-orbit models on a single processor, our results are at least as good as the best alternative. More importantly, the parallel scalability of our optimizations is superior to that of other available methods, making optimized renormalization very attractive for multiple-processor computers. We demonstrate the method with calculations for Si nanowires.
C1 [Boykin, Timothy B.] Univ Alabama, Dept Elect & Comp Engn, Huntsville, AL 35899 USA.
[Luisier, Mathieu] ETH, Integrated Syst Lab, CH-8092 Zurich, Switzerland.
[Klimeck, Gerhard] Purdue Univ, Sch Elect & Comp Engn, Network Computat Nanotechnol, W Lafayette, IN 47907 USA.
[Klimeck, Gerhard] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Boykin, TB (reprint author), Univ Alabama, Dept Elect & Comp Engn, Huntsville, AL 35899 USA.
RI Klimeck, Gerhard/A-1414-2012
OI Klimeck, Gerhard/0000-0001-7128-773X
NR 19
TC 13
Z9 13
U1 0
U2 5
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 APR
PY 2008
VL 77
IS 16
AR 165318
DI 10.1103/PhysRevB.77.165318
PG 9
WC Physics, Condensed Matter
SC Physics
GA 295EJ
UT WOS:000255457500075
ER
PT J
AU Cantrell, JH
Cantrell, SA
AF Cantrell, John H.
Cantrell, Sean A.
TI Analytical model of the nonlinear dynamics of cantilever tip-sample
surface interactions for various acoustic atomic force microscopies
SO PHYSICAL REVIEW B
LA English
DT Article
ID TAPPING-MODE; VIBRATIONS; BEAM
AB An analytical model is developed of the interaction of the cantilever tip of an atomic force microscope with the sample surface that treats the cantilever and sample as independent systems coupled by a nonlinear force acting between the cantilever tip and a volume element of the sample surface. To maintain equilibrium, the volume element is subjected to a restoring force from the remainder of the sample. The model accounts for the positions on the cantilever of the cantilever tip, laser probe, and excitation force (if any). The model leads to a pair of coupled nonlinear differential equations that are solved analytically using a matrix iteration procedure. Solutions are obtained for the phase and amplitude signals generated by various acoustic atomic force microscope (A-AFM) techniques including force modulation microscopy, atomic force acoustic microscopy, ultrasonic force microscopy, heterodyne force microscopy, resonant difference-frequency atomic force ultrasonic microscopy (RDF-AFUM), and amplitude modulation-atomic force microscopy (AM-AFM) (intermittent contact mode). The solutions are used to obtain a quantitative measure of A-AFM image contrast resulting from variations in the Young modulus of the sample. Applications of the model to measurements of LaRC (TM)-CP2 polyimide film using RDF-AFUM and AM-AFM images predict maximum variations in the Young modulus of 24% and 18%, respectively, over a common scan area. Both predictions are in good agreement with the value of 21% obtained from independent mechanical stretching measurements of the polyimide sheet material.
C1 [Cantrell, John H.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Cantrell, Sean A.] Univ Virginia, Dept Phys, Charlottesville, VA 22901 USA.
RP Cantrell, JH (reprint author), NASA, Langley Res Ctr, Mail Stop 231, Hampton, VA 23681 USA.
EM john.h.cantrell@nasa.gov; sac3k@virginia.edu
NR 41
TC 19
Z9 19
U1 1
U2 20
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9950
EI 2469-9969
J9 PHYS REV B
JI Phys. Rev. B
PD APR
PY 2008
VL 77
IS 16
AR 165409
DI 10.1103/PhysRevB.77.165409
PG 16
WC Physics, Condensed Matter
SC Physics
GA 295EJ
UT WOS:000255457500107
ER
PT J
AU Lawson, JW
Srivastava, D
AF Lawson, John W.
Srivastava, Deepak
TI Formation and structure of amorphous carbon char from polymer materials
SO PHYSICAL REVIEW B
LA English
DT Article
ID FLAMMABILITY PROPERTIES; NANOCOMPOSITES; COMPOSITES
AB Amorphous carbonaceous char produced from burning polymer solids has insulating properties that make it valuable in thermal protection and fire-retardant systems. A pyrolytic molecular dynamics simulation method is devised to study the transformation of the local microstructure from virgin polymer to a dense, disordered char. Release of polymer hydrogen is found to be critical to allow the system to collapse into a highly coordinated char structure. Mechanisms of the char formation process and the morphology of the resulting structures are elucidated.
C1 [Lawson, John W.; Srivastava, Deepak] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Lawson, JW (reprint author), NASA, Ames Res Ctr, Mail Stop 269-2, Moffett Field, CA 94035 USA.
EM john.w.lawson@nasa.gov; dsrivastava@mail.arc.nasa.gov
NR 16
TC 16
Z9 16
U1 0
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 APR
PY 2008
VL 77
IS 14
AR 144209
DI 10.1103/PhysRevB.77.144209
PG 6
WC Physics, Condensed Matter
SC Physics
GA 295EH
UT WOS:000255457300033
ER
PT J
AU Berti, E
Cardoso, V
AF Berti, Emanuele
Cardoso, Vitor
TI Quasinormal modes and thermodynamic phase transitions
SO PHYSICAL REVIEW D
LA English
DT Article
ID BLACK-HOLES
AB It has recently been suggested that scalar, Dirac, and Rarita-Schwinger perturbations are related to thermodynamic phase transitions of charged (Reissner-Nordstrom) black holes. In this Brief Report we show that this result is probably a numerical coincidence, and that the conjectured correspondence does not straightforwardly generalize to other metrics, such as Kerr or Schwarzschild (anti-)de Sitter. Our calculations do not rule out a relation between dynamical and thermodynamical properties of black holes, but they suggest that such a relation is nontrivial.
C1 [Berti, Emanuele] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cardoso, Vitor] Inst Super Tecn, Dept Fis, Ctr Multidisciplinar Astrofis CENTRA, P-1049001 Lisbon, Portugal.
[Cardoso, Vitor] Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA.
RP Berti, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM berti@wugrav.wustl.edu; vcardoso@fisica.ist.utl.pt
RI Berti, Emilio/F-5256-2012; Berti, Emanuele/C-9331-2016; Cardoso,
Vitor/K-1877-2015
OI Berti, Emanuele/0000-0003-0751-5130; Cardoso, Vitor/0000-0003-0553-0433
NR 25
TC 13
Z9 13
U1 0
U2 2
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD APR
PY 2008
VL 77
IS 8
AR 087501
DI 10.1103/PhysRevD.77.087501
PG 4
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 295EN
UT WOS:000255457900091
ER
PT J
AU Umstatter, R
Tinto, M
AF Umstaetter, Richard
Tinto, Massimo
TI Bayesian comparison of post-Newtonian approximations of gravitational
wave chirp signals
SO PHYSICAL REVIEW D
LA English
DT Article
ID MODEL
AB We estimate the probability of detecting a gravitational wave signal from coalescing compact binaries in simulated data from a ground-based interferometer detector of gravitational radiation using Bayesian model selection. The simulated wave form of the chirp signal is assumed to be a spinless post-Newtonian (PN) wave form of a given expansion order, while the searching template is assumed to be either of the same post-Newtonian family as the simulated signal or one level below its post-Newtonian expansion order. Within the Bayesian framework, and by applying a reversible jump Markov Chain Monte Carlo simulation algorithm, we compare PN1.5 vs PN2.0 and PN3.0 vs PN3.5 wave forms by deriving the detection probabilities, the statistical uncertainties due to noise as a function of the signal-to-noise ratio, and the posterior distributions of the parameters. Our analysis indicates that the detection probabilities are not compromised when simplified models are used for the comparison, while the accuracies in the determination of the parameters characterizing these signals can be significantly worsened, no matter what the considered post-Newtonian order expansion comparison is.
C1 [Umstaetter, Richard; Tinto, Massimo] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Umstaetter, Richard; Tinto, Massimo] CALTECH, LIGO Labs, Pasadena, CA 91125 USA.
RP Umstatter, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM richard.umstaetter@jpl.nasa.gov; massimo.tinto@jpl.nasa.gov
NR 37
TC 7
Z9 7
U1 0
U2 0
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD APR
PY 2008
VL 77
IS 8
AR 082002
DI 10.1103/PhysRevD.77.082002
PG 19
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 295EN
UT WOS:000255457900004
ER
PT J
AU Berg, RF
Moldover, MR
Yao, MW
Zimmerli, GA
AF Berg, Robert F.
Moldover, Michael R.
Yao, Minwu
Zimmerli, Gregory A.
TI Shear thinning near the critical point of xenon
SO PHYSICAL REVIEW E
LA English
DT Article
ID CRITICAL FLUIDS; DROPLET MODEL; TRANSPORT-PROPERTIES; MICELLAR-SOLUTION;
VISCOSITY; FLOW; TEMPERATURE; WATER; MIXTURES; DYNAMICS
AB We measured shear thinning, a viscosity decrease ordinarily associated with complex liquids, near the critical point of xenon. The data span a wide range of reduced shear rate: 10(-3) (gamma) over dot tau < 700, where (gamma) over dot tau is the shear rate scaled by the relaxation time tau of critical fluctuations. The measurements had a temperature resolution of 0.01 mK and were conducted in microgravity aboard the Space Shuttle Columbia to avoid the density stratification caused by Earth's gravity. The viscometer measured the drag on a delicate nickel screen as it oscillated in the xenon at amplitudes 3 mu m < x(0) < 430 mu m and frequencies 1 Hz < omega/2 pi < 5 Hz. To separate shear thinning from other nonlinearities, we computed the ratio of the viscous force on the screen at (gamma) over dot tau to the force at (gamma) over dot tau approximate to 0: C(gamma) F(x(0), omega tau, (gamma) over dot tau)/F (x(0), omega tau, 0). At low frequencies, (omega tau)(2) < (gamma) over dot tau, C(gamma) depends only on (gamma) over dot tau, as predicted by dynamic critical scaling. At high frequencies, (omega tau)(2) > (gamma) over dot tau, C gamma depends also on both x(0) and omega. The data were compared with numerical calculations based on the Carreau-Yasuda relation for complex fluids: eta((gamma) over dot)/ eta(0) = [1 + A(gamma)|(gamma) over dot tau|](-x eta/(3+x eta)), where x eta = 0.069 is the critical exponent for viscosity and mode-coupling theory predicts A(gamma)= 0.121. For xenon we find A(gamma) = 0.137 +/- 0.029, in agreement with the mode coupling value. Remarkably, the xenon data close to the critical temperature T(c) were independent of the cooling rate (both above and below T(c)) and these data were symmetric about T(c) to within a temperature scale factor. The scale factors for the magnitude of the oscillator's response differed from those for the oscillator's phase; this suggests that the surface tension of the two-phase domains affected the drag on the screen below T(c).
C1 [Berg, Robert F.; Moldover, Michael R.] Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA.
[Yao, Minwu] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Zimmerli, Gregory A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Berg, RF (reprint author), Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA.
RI Moldover, Michael/E-6384-2013
NR 51
TC 5
Z9 5
U1 1
U2 6
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1539-3755
J9 PHYS REV E
JI Phys. Rev. E
PD APR
PY 2008
VL 77
IS 4
AR 041116
DI 10.1103/PhysRevE.77.041116
PN 1
PG 23
WC Physics, Fluids & Plasmas; Physics, Mathematical
SC Physics
GA 295ED
UT WOS:000255456900019
PM 18517587
ER
PT J
AU Schindler, K
Hesse, M
AF Schindler, Karl
Hesse, Michael
TI Formation of thin bifurcated current sheets by quasisteady compression
SO PHYSICS OF PLASMAS
LA English
DT Article
ID COLLISIONLESS MAGNETIC RECONNECTION; ELECTRIC-CURRENT SHEET; SUBSTORM
GROWTH-PHASE; PLASMA SHEET; MAGNETOTAIL; FIELD
AB Thin current sheets with half-widths in the range of about 10 or less ion inertial lengths (or ion gyroradii) have been identified as the sites of important dynamical phenomena in space plasmas. Recent space observations established that thin current sheets often have a bifurcated (double-peaked) current density. Earlier suggestions of possible bifurcation mechanisms are based on the presence of microfluctuations, magnetic reconnection, or a normal magnetic field component or assumed simplified models of adiabatic dynamics. Despite these efforts, the cause (or causes) of the formation of thin bifurcated current sheets and the conditions under which they form have remained unclear. In this paper, we identify quasisteady compression of a plane, initially wide collisionless current sheet as an effective physical mechanism for the formation of thin bifurcated current sheets. Our main tool is electromagnetic particle simulation. The initial sheet has a singly peaked current and a half-width that is five times larger than the ion inertial length. This sheet is quasisteadily compressed by external forces. A three-scale structure develops and the current bifurcates during compression. It is shown that the bifurcation, pressure anisotropy, and other major properties of the embedded current sheet can be understood in terms of basic physical principles, such as electric field shielding and momentum conservation. Sufficient conditions for bifurcation of symmetric current sheets are presented. They suggest that bifurcation must generally occur by quasisteady compression if the (singly peaked) initial current sheet is sufficiently wide. (c) 2008 American Institute of Physics.
C1 [Schindler, Karl] Ruhr Univ Bochum, D-44780 Bochum, Germany.
[Hesse, Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Schindler, K (reprint author), Ruhr Univ Bochum, D-44780 Bochum, Germany.
RI Hesse, Michael/D-2031-2012; NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
NR 40
TC 12
Z9 12
U1 0
U2 1
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 1070-664X
J9 PHYS PLASMAS
JI Phys. Plasmas
PD APR
PY 2008
VL 15
IS 4
AR 042902
DI 10.1063/1.2907359
PG 9
WC Physics, Fluids & Plasmas
SC Physics
GA 295EB
UT WOS:000255456700044
ER
PT J
AU Zenitani, S
Hesse, M
AF Zenitani, S.
Hesse, M.
TI The role of the Weibel instability at the reconnection jet front in
relativistic pair plasma reconnection (vol 15, art no 022101, 2008)
SO PHYSICS OF PLASMAS
LA English
DT Correction
C1 [Zenitani, S.; Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zenitani, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM zenitani@lssp-mail.gsfc.nasa.gov
RI Hesse, Michael/D-2031-2012; NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
NR 1
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 1070-664X
J9 PHYS PLASMAS
JI Phys. Plasmas
PD APR
PY 2008
VL 15
IS 4
AR 049901
DI 10.1063/1.2891088
PG 1
WC Physics, Fluids & Plasmas
SC Physics
GA 295EB
UT WOS:000255456700061
ER
PT J
AU Tomasko, MG
Doose, L
Engel, S
Dafoe, LE
West, R
Lemmon, M
Karkoschka, E
See, C
AF Tomasko, M. G.
Doose, L.
Engel, S.
Dafoe, L. E.
West, R.
Lemmon, M.
Karkoschka, E.
See, C.
TI A model of Titan's aerosols based on measurements made inside the
atmosphere
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Titan; aerosols; Huygens; atmosphere
ID T-MATRIX; SCATTERING; PARTICLES; DESCENT; SPHERES; WAVELENGTH; PROBE;
HAZE
AB The descent imager/spectral radiometer (DISR) instrument aboard the Huygens probe into the atmosphere of Titan measured the brightness of sunlight using a complement of spectrometers, photometers, and cameras that covered the spectral range from 350 to 1600 nm, looked both upward and downward, and made measurements at altitudes from 150 km to the surface. Measurements from the upward-looking visible and infrared spectrometers are described in Tomasko et al. [2008a. Measurements of methane absorption by the descent imager/spectral radiometer (DISR) during its descent through Titan's atmosphere. Planet. Space Sci., this volume]. Here, we very briefly review the measurements by the violet photometers, the downward-looking visible and infrared spectrometers, and the upward-looking solar aureole (SA) camera. Taken together, the DISR measurements constrain the vertical distribution and wavelength dependence of opacity, single-scattering albedo, and phase function of the aerosols in Titan's atmosphere.
Comparison of the inferred aerosol properties with computations of scattering from fractal aggregate particles indicates the size and shape of the aerosols. We find that the aggregates require monomers of radius 0.05 mu m or smaller and that the number of monomers in the loose aggregates is roughly 3000 above 60 km. The single-scattering albedo, of the aerosols above 140 kin altitude is similar to that predicted for some tholins measured in laboratory experiments, although we find that the single-scattering albedo of the aerosols increases with depth into the atmosphere between 140 and 80km altitude, possibly due to condensation of other gases on the haze particles. The number density of aerosols is about 5/cm(3) at 80 km altitude, and decreases with a scale height of 65 km to higher altitudes. The aerosol opacity above 80 km varies as the wavelength to the -2.34 power between 350 and 1600 nm.
Between 80 and 30 km the cumulative aerosol opacity increases linearly with increasing depth in the atmosphere. The total aerosol opacity in this altitude range varies as the wavelength to the -1.41 power. The single-scattering phase function of the aerosols in this region is also consistent with the fractal particles found above 60 km.
In the lower 30 km of the atmosphere, the wavelength dependence of the aerosol opacity varies as the wavelength to the -0.97 power, much less than at higher altitudes. This suggests that the aerosols here grow to still larger sizes, possibly by incorporation of methane into the aerosols. Here the cumulative opacity also increases linearly with depth, but at some wavelengths the rate is slightly different than above 30 km altitude.
For purely fractal particles in the lowest few km, the intensity looking upward opposite to the azimuth of the sun decreases with increasing zenith angle faster than the observations in red light if the single-scattering albedo is assumed constant with altitude at these low altitudes. This discrepancy can be decreased if the single-scattering albedo decreases with altitude in this region. A possible explanation is that the brightest aerosols near 30 km altitude contain significant amounts of methane, and that the decreasing albedo at lower altitudes may reflect the evaporation of some of the methane as the aerosols fall into dryer layers of the atmosphere. An alternative explanation is that there may be spherical particles in the bottom few kilometers of the atmosphere. Published by Elsevier Ltd.
C1 [Tomasko, M. G.; Doose, L.; Engel, S.; Dafoe, L. E.; Karkoschka, E.; See, C.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[West, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lemmon, M.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
RP Tomasko, MG (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
EM mtomasko@lpl.arizona.edu
RI Lemmon, Mark/E-9983-2010
OI Lemmon, Mark/0000-0002-4504-5136
NR 20
TC 130
Z9 130
U1 3
U2 23
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD APR
PY 2008
VL 56
IS 5
BP 669
EP 707
DI 10.1016/j.pss.2007.11.019
PG 39
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 296VS
UT WOS:000255574500009
ER
PT J
AU Witasse, O
Huber, L
Zender, J
Lebreton, JP
Beebe, R
Heather, D
Matson, DL
Zarnecki, J
Wheadon, J
Trautner, R
Tomasko, M
Stoppato, PL
Simoes, F
See, C
Perez-Ayucar, M
Pennanech, C
Niemann, H
McFarlane, L
Leese, M
Kazeminejad, B
Israel, G
Hathi, B
Hagermann, A
Haberman, J
Fulchignoni, M
Ferri, F
Dutta-Roy, R
Doose, L
Demick-Montelara, J
Colombatti, G
Brun, JF
Bird, M
Atkinson, D
Aboudan, A
AF Witasse, Olivier
Huber, Lyle
Zender, Joe
Lebreton, Jean-Pierre
Beebe, Reta
Heather, David
Matson, Dennis L.
Zarnecki, John
Wheadon, Joe
Trautner, Roland
Tomasko, Marty
Stoppato, Piero Leon
Simoes, Fernando
See, Chuck
Perez-Ayucar, Miguel
Pennanech, Cyril
Niemann, Hasso
McFarlane, Lisa
Leese, Mark
Kazeminejad, Bobby
Israel, Guy
Hathi, Brijen
Hagermann, Axel
Haberman, John
Fulchignoni, Marcello
Ferri, Francesca
Dutta-Roy, Robindro
Doose, Lyn
Demick-Montelara, Jaime
Colombatti, Giacomo
Brun, Jean-Francis
Bird, Michael
Atkinson, David
Aboudan, Alessio
TI The Huygens scientific data archive: Technical overview
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Cassini/Huygens mission; data archiving; Titan
ID TITAN; DESCENT; SURFACE; WINDS; PROBE
AB The Cassini/Huygens. mission was launched in October 1997, and during the third orbit around Saturn, the Huygens probe was released on course to enter Titan's atmosphere. During the descent, six science instruments provided in situ and remote sensing measurements of Titan's atmosphere and surface. Doppler tracking was performed with two Earth-based radio telescopes, and a Very Long Base Interferometry (VLBI) experiment was carried out. Data acquisition began around 1500 km altitude and continued throughout the 2 h and 30 min descent and for 1 h and 12 min after landing. This unique set of data is available in the ESA Planetary Science Archive (PSA) and mirror imaged in the NASA Planetary Data System (PDS). This paper presents an overview of the process the Huygens Data Archiving Working Group followed to develop and ingest the data set. A description of the data sets is also given. (C) 2007 Elsevier Ltd. All rights reserved.
C1 [Witasse, Olivier; Zender, Joe; Lebreton, Jean-Pierre; Heather, David; Trautner, Roland; Perez-Ayucar, Miguel] European Space Agcy, Res & Sci Support Dept, ESTEC, NL-2200 AG Noordwijk, Netherlands.
[Huber, Lyle; Beebe, Reta] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Matson, Dennis L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zarnecki, John; Leese, Mark; Hathi, Brijen; Hagermann, Axel] Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England.
[Wheadon, Joe] ESOC, ESA, D-64293 Darmstadt, Germany.
[Tomasko, Marty; See, Chuck; McFarlane, Lisa; Doose, Lyn] Kuiper LPL, Tucson, AZ 85721 USA.
[Stoppato, Piero Leon; Ferri, Francesca; Colombatti, Giacomo; Aboudan, Alessio] Univ Padua, CISAS G Colombo, I-35131 Padua, Italy.
[Pennanech, Cyril; Brun, Jean-Francis] CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France.
[Niemann, Hasso; Haberman, John; Demick-Montelara, Jaime] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20117 USA.
[Kazeminejad, Bobby] GSOC, Deutsch Zentrum Luft & Raumfahrt, D-82234 Wesssling, Germany.
[Fulchignoni, Marcello] Observ Paris, LESIA, F-92195 Meudon, France.
[Dutta-Roy, Robindro; Bird, Michael] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Atkinson, David] Univ Idaho, Dept Elect & Comp Engn, Moscow, ID 83844 USA.
[Simoes, Fernando] IPSL CNRS, CETP, F-94107 St Maur, France.
RP Witasse, O (reprint author), European Space Agcy, Res & Sci Support Dept, ESTEC, NL-2200 AG Noordwijk, Netherlands.
EM owitasse@rssd.esa.int
RI Simoes, Fernando/D-7731-2012
NR 7
TC 1
Z9 1
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 APR
PY 2008
VL 56
IS 5
BP 770
EP 777
DI 10.1016/j.pss.2007.10.007
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 296VS
UT WOS:000255574500014
ER
PT J
AU Gillespie, TW
Foody, GM
Rocchini, D
Giorgi, AP
Saatchi, S
AF Gillespie, Thomas W.
Foody, Giles M.
Rocchini, Duccio
Giorgi, Ana Paula
Saatchi, Sassan
TI Measuring and modelling biodiversity from space
SO PROGRESS IN PHYSICAL GEOGRAPHY
LA English
DT Review
DE biogeography; conservation planning; diversity modelling; remote
sensing; species distribution modelling
ID PLANT-SPECIES RICHNESS; RESOLUTION SATELLITE DATA; LAND-COVER
CLASSIFICATION; REGIONAL-SCALE ANALYSIS; TROPICAL RAIN-FORESTS;
REMOTELY-SENSED DATA; SPATIAL-RESOLUTION; SPECTRAL-RESOLUTION;
BETA-DIVERSITY; CONSERVATION PRIORITIES
AB The Earth is undergoing an accelerated rate of native ecosystem conversion and degradation and there is increased interest in measuring and modelling biodiversity from space. Biogeographers have a long-standing interest in measuring patterns of species occurrence and distributional movements and an interest in modelling species distributions and patterns of diversity. Much progress has been made in identifying plant species from space using high-resolution satellites (QuickBird, IKONOS), while the measurement of species movements has become commonplace with the ARGOS satellite tracking system which has been used to track the movements of thousands of individual animals. There have been significant advances in land-cover classifications by combining data from multi-passive and active sensors, and new classification techniques. Species distribution modelling has been growing at a striking rate and the incorporation of spaceborne data on climate, topography, land cover, and vegetation structure has great potential to improve models. There have been significant advances in modelling species richness, alpha diversity, and beta diversity using multisensors to quantify land-cover classifications and landscape metrics, measures of productivity, and measures of heterogeneity. Remote sensing of nature reserves can provide natural resources managers with near real-time data within and around reserves that can be used to support conservation efforts anywhere in the world. Future research should focus on incorporating recent spaceborne sensors, more extensive integration of available spaceborne imagery, and the collection and dissemination of high-quality field data. This will improve our understanding of the distribution of life on earth.
C1 [Gillespie, Thomas W.; Giorgi, Ana Paula] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA.
[Foody, Giles M.] Univ Nottingham, Sch Geog, Nottingham NG7 2RD, England.
[Rocchini, Duccio] Univ Siena, Dipartimento Sci Ambientali G Sarfatti, I-53100 Siena, Italy.
[Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gillespie, TW (reprint author), Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA.
EM tg@geog.ucla.edu
RI Rocchini, Duccio/B-6742-2011;
OI Rocchini, Duccio/0000-0003-0087-0594
NR 147
TC 163
Z9 174
U1 9
U2 79
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0309-1333
J9 PROG PHYS GEOG
JI Prog. Phys. Geogr.
PD APR
PY 2008
VL 32
IS 2
BP 203
EP 221
DI 10.1177/0309133308093606
PG 19
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA 345IG
UT WOS:000258989200004
ER
PT J
AU Bauer, JM
Choi, YJ
Weissman, PR
Stansberry, JA
Fernandez, YR
Roe, HG
Buratti, BJ
Sung, HI
AF Bauer, James M.
Choi, Young-Jun
Weissman, Paul R.
Stansberry, John A.
Fernandez, Yanga R.
Roe, Henry G.
Buratti, Bonnie J.
Sung, Hyun-Il
TI The large-grained dust coma of 174P/Echeclus
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID SPITZER-SPACE-TELESCOPE; DEEP-IMPACT; ABSOLUTE CALIBRATION; INFRARED
PHOTOMETRY; HALE-BOPP; COMETS; CENTAURS; NUCLEUS; OBJECTS; 2060-CHIRON
AB On 2005 December 30, Y.- J. Choi and P. R. Weissman discovered that the formerly dormant Centaur 2000 EC98 was in strong outburst. Previous observations by P. Rousselot et al. spanning a 3-year period indicated a lack of coma down to the 27 mag arcsec(-2) level. We present Spitzer Space Telescope MIPS observations of this newly active Centaur - now known as 174P/Echeclus ( 2000 EC98) - or 60558 Echeclus - taken in 2006 late February. The images show strong signal at both the 24 and 70 mu m bands and reveal an extended coma about 2' in diameter. Analyses yield estimates of the coma signal contribution that are in excess of 90% of the total signal in the 24 mu m band. Dust production estimates ranging from 1.7 - 4 x 10(2) kg s(-1) are on the order of 30 times that seen in other Centaurs. Simultaneous visible-wavelength observations were also obtained with Palomar Observatory's 200-inch telescope, the 1.8-m Vatican Advanced Technology Telescope, the Bohyunsan Optical Astronomy Observatory (BOAO) 1.8-m telescope, and Table Mountain Observatory's 0.6-m telescope, revealing a coma morphology nearly identical to the mid-IR observations. The grain size distribution derived from the data yields a log particle mass power-law with slope parameter alpha = -0.87 +/- 0.07, and is consistent with steady cometary activity, such as that observed during the Stardust spacecraft's encounter at 81P/Wild 2, and not with an impact-driven event, such as that caused by the Deep Impact experiment.
C1 [Bauer, James M.; Choi, Young-Jun; Weissman, Paul R.; Buratti, Bonnie J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Stansberry, John A.] Univ Arizona, Steward Observ, Tucson, AZ USA.
[Fernandez, Yanga R.] Univ Cent Florida, Dept Phys, Orlando, FL USA.
[Roe, Henry G.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Sung, Hyun-Il] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
RP Bauer, JM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA.
OI Fernandez, Yanga/0000-0003-1156-9721
NR 55
TC 17
Z9 17
U1 0
U2 0
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD APR
PY 2008
VL 120
IS 866
BP 393
EP 404
DI 10.1086/587552
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 290KF
UT WOS:000255121000005
ER
PT J
AU Chuss, DT
Wollack, EJ
Moseley, SH
Withington, S
Saklatvala, G
AF Chuss, David T.
Wollack, Edward J.
Moseley, S. Harvey
Withington, Stafford
Saklatvala, George
TI Diffraction considerations for planar detectors in the few-mode limit
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID TELESCOPE; ARRAYS; CAMERA
AB Filled arrays of bolometers are currently being employed for use in astronomy from the far-infrared through millimeter portion of the electromagnetic spectrum. Because of the large range of wavelengths for which such detectors are applicable, the size of a pixel (p) relative to the wavelength (lambda) will vary according to the specific application of a given available technology. As the pixel size becomes comparable to a wavelength of the absorbed radiation, correlations in the radiation field at the pixel can affect the imaging properties of the system independent of the correlations introduced by the front-end optics. We study the dependence of image fidelity and induced polarization on the size of the pixel by employing a formalism in which diffraction due to the pixel boundary is treated by propagating the second-order statistical correlations of the radiation field through an optical system. We construct simulated polarized images of square pixels for various ratios of p/lambda. For the limit in which few modes are supported by the pixel (p/lambda less than or similar to 1), we find that the diffraction due to the pixel edges is nonnegligible and hence must be considered along with the telescope diffraction pattern in modeling the ultimate spatial resolution of an imaging system. For the case in which the pixel is over-moded (p/lambda >> 1), the geometric limit is approached as expected. This technique provides a quantitative approach to understand and optimize the imaging properties of planar detectors in the few-mode limit.
C1 [Chuss, David T.; Wollack, Edward J.; Moseley, S. Harvey] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD USA.
[Withington, Stafford; Saklatvala, George] Univ Cambridge, Cavevdish Lab, Cambridge CB3 OHE, England.
RP Chuss, DT (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD USA.
EM David.T.Chuss@nasa.gov; Edward.J.Wollack@nasa.gov;
Harvey.Moseley@nasa.gov; stafford@mrao.cam.ac.uk
RI Moseley, Harvey/D-5069-2012; Chuss, David/D-8281-2012; Wollack,
Edward/D-4467-2012
OI Wollack, Edward/0000-0002-7567-4451
NR 13
TC 10
Z9 10
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD APR
PY 2008
VL 120
IS 866
BP 430
EP 438
DI 10.1086/587494
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 290KF
UT WOS:000255121000008
ER
PT J
AU Weinstein, SA
Lundgren, PR
AF Weinstein, Stuart A.
Lundgren, Paul R.
TI Finite fault modeling in a tsunami warning center context
SO PURE AND APPLIED GEOPHYSICS
LA English
DT Article
DE Finite fault modeling; earthquake rupture history; tsunami warning
center
ID STRONG-MOTION; MANTLE MAGNITUDE; RUPTURE HISTORY; EARTHQUAKE; INVERSION;
CALIFORNIA; RECORDS; WAVES
AB The US NOAA/NWS tsunami warning centers have relied on earthquake location and depth, and scalar measures of earthquake size and slowness to assess the potential for the generation of a destructive tsunami by an earthquake. Recent earthquakes, such as Peru 2001, Sumatra 2004 and the Java 2006, manifest some of the difficulties the warning centers face as they try to cope with unusual earthquakes. We have undertaken a study of a simple teleseismic waveform inverse model and applied it to the earthquakes of June 23, 2001 in Peru and of July 17, 2006 in Java. Synthetic numerical experiments suggest that the most salient features of the rupture history of an earthquake can be recovered. Furthermore the calculations can be conducted quickly enough to be useful in a warning center context.
We have applied our technique to the Peru 2001 and recent Java 2006 earthquakes. Our overall results are consistent with those obtained from other studies. The results show why the Peru event initially looked slow to the US tsunami warning centers and that the Java event is a truly slow or tsunami earthquake. Clearly, the warning centers stand to benefit from an increased understanding of the earthquakes they monitor. Furthermore, better knowledge of the slip distribution along a fault will improve tsunami wave-height forecasts.
C1 [Weinstein, Stuart A.] Richard H Hagemeyers Pacific Tsunami Warning Ctr, Ewa Beach, HI 96706 USA.
[Lundgren, Paul R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Weinstein, SA (reprint author), Richard H Hagemeyers Pacific Tsunami Warning Ctr, Ewa Beach, HI 96706 USA.
EM stuart.weinstein@noaa.gov
NR 21
TC 5
Z9 5
U1 0
U2 1
PU SPRINGER BASEL AG
PI BASEL
PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND
SN 0033-4553
EI 1420-9136
J9 PURE APPL GEOPHYS
JI Pure Appl. Geophys.
PD APR
PY 2008
VL 165
IS 3-4
BP 451
EP 474
DI 10.1007/s00024-008-0316-x
PG 24
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 301AA
UT WOS:000255867100002
ER
PT J
AU Parker, J
Lyzenga, G
Norton, C
Zuffada, C
Glasscoe, M
Lou, J
Donnellan, A
AF Parker, Jay
Lyzenga, Gregory
Norton, Charles
Zuffada, Cinzia
Glasscoe, Margaret
Lou, John
Donnellan, Andrea
TI Geophysical finite-element simulation tool (GeoFEST): Algorithms and
validation for quasistatic regional faulted crust problems
SO PURE AND APPLIED GEOPHYSICS
LA English
DT Article
AB GeoFEST (Geophysical Finite Element Simulation Tool) is a two- and three-dimensional finite element software package for the modeling of solid stress and strain in geophysical and other continuum domain applications. It is one of the featured high-performance applications of the NASA QuakeSim project. The program is targeted to be compiled and run on UNIX systems, and is running on diverse systems including sequential and message-passing parallel systems. Solution to the elliptical partial differential equations is obtained by finite element basis sampling, resulting in a sparse linear system primarily solved by conjugate gradient iteration to a tolerance level; on sequential systems a Crout factorization for the direct inversion of the linear system is also supported. The physics models supported include isotropic linear elasticity and both Newtonian and power-law viscoelasticity, via implicit quasi-static time stepping. In addition to triangular, quadrilateral, tetrahedral and hexahedral continuum elements, GeoFEST supports split-node faulting, body forces, and surface tractions. This software and related mesh refinement strategies have been validated on a variety of test cases with rigorous comparison to analytical solutions. These include a box-shaped domain with imposed motion on one surface, a pair of strike slip faults in stepover arrangement, and two community-agreed benchmark cases: a strike slip fault in an enclosing box, and a quarter-domain circular fault problem. Scientific applications of the code include the modeling of static and transient co- and post-seismic earth deformation, Earth response to glacial, atmospheric and hydrological loading, and other scenarios involving the bulk deformation of geologic media.
C1 [Parker, Jay; Lyzenga, Gregory; Norton, Charles; Zuffada, Cinzia; Glasscoe, Margaret; Lou, John; Donnellan, Andrea] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Parker, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Jay.W.Parker@jpl.nasa.gov
NR 12
TC 7
Z9 7
U1 0
U2 1
PU BIRKHAUSER VERLAG AG
PI BASEL
PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND
SN 0033-4553
J9 PURE APPL GEOPHYS
JI Pure Appl. Geophys.
PD APR
PY 2008
VL 165
IS 3-4
BP 497
EP 521
DI 10.1007/s00024-008-0325-9
PG 25
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 301AA
UT WOS:000255867100004
ER
PT J
AU Simpson, JR
Landman, D
Giroux, R
Zeisset, M
Hall, B
Rhew, RD
AF Simpson, James R.
Landman, Drew
Giroux, Rupert
Zeisset, Michelle
Hall, Brian
Rhew, Ray D.
TI Adapting second-order response surface designs to specific needs
SO QUALITY AND RELIABILITY ENGINEERING INTERNATIONAL
LA English
DT Article
DE response surface methodology; second-order designs; Box Behnken;
prediction variance; Monte Carlo simulation; desirable design properties
AB Experimental design strategies most often involve an initial choice of a classic factorial or response surface design and adapt that design to meet restrictions or unique requirements of the system under study. One such experience is described here, in which the objective was to develop an efficient experimental design strategy that would facilitate building second-order response models with excellent prediction capabilities. In development, careful consideration was paid to the desirable properties of response surface designs. Once developed, the proposed design was evaluated using Monte Carlo simulation to prove the concept, a pilot implementation of the design carried out to evaluate the accuracy of the response models, and a set of validation runs enacted to look for potential weaknesses in the approach. The purpose of the exercise was to develop a procedure to efficiently and effectively calibrate strain-gauge balances to be used in wind tunnel testing. The current calibration testing procedure is based on a time-intensive one-factor-at-a-time method. In this study, response surface methods were used to reduce the number of calibration runs required during the labor-intensive heavy load calibration, to leverage the prediction capabilities of response surface designs, and to provide an estimate of uncertainty for the calibration models. Results of the three-phased approach for design evaluation are presented. The new calibration process will require significantly fewer tests to achieve the same or improved levels of precision in balance calibration. Copyright (C) 2008 John Wiley & Sons, Ltd.
C1 [Simpson, James R.; Giroux, Rupert; Zeisset, Michelle] Florida State Univ, Tallahassee, FL 32310 USA.
[Landman, Drew] Old Dominion Univ, Norfolk, VA 23665 USA.
[Hall, Brian; Rhew, Ray D.] NASA Langley, Hampton, VA 23605 USA.
RP Simpson, JR (reprint author), Florida State Univ, Tallahassee, FL 32310 USA.
NR 11
TC 8
Z9 8
U1 0
U2 1
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND
SN 0748-8017
J9 QUAL RELIAB ENG INT
JI Qual. Reliab. Eng. Int.
PD APR
PY 2008
VL 24
IS 3
BP 331
EP 349
DI 10.1002/qre.900
PG 19
WC Engineering, Multidisciplinary; Engineering, Industrial; Operations
Research & Management Science
SC Engineering; Operations Research & Management Science
GA 292YY
UT WOS:000255303200007
ER
PT J
AU Zeng, XP
AF Zeng, Xiping
TI The influence of radiation on ice crystal spectrum in the upper
troposphere
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE cirrus; subvisual cloud; precipitation
ID VAPOR-SPHERICAL MODEL; TERMINAL VELOCITIES; HYDROMETEOR GROWTH; CIRRUS
CLOUDS; PARTICLES; WATER; CONDENSATION; ATMOSPHERES; CONVECTION;
KINETICS
AB This theoretical study is carried out to investigate the effect of radiation on ice crystal spectrum in the upper troposphere. First, an explicit expression is obtained for the ice crystal growth rate that takes account of radiative and kinetic effects. Second, the expression is used to quantitatively analyse how radiation broadens the ice crystal spectrum and then to reveal a new precipitation mechanism in the upper troposphere and the stratosphere. Third, the radiative effect is used to explain the subvisual clouds near the tropopause. Copyright (C) 2008 Royal Meteorological Society.
C1 [Zeng, Xiping] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Zeng, Xiping] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Greenbelt, MD USA.
RP Zeng, XP (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Mail Code 613-1, Greenbelt, MD 20771 USA.
EM zeng@agnes.gsfc.nasa.gov
NR 37
TC 3
Z9 3
U1 0
U2 2
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-9009
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2008
VL 134
IS 632
BP 609
EP 620
DI 10.1002/qj.226
PN A
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 349PI
UT WOS:000259292600005
ER
PT J
AU Foellmi, C
Koenigsberger, G
Georgiev, L
Toledano, O
Marchenko, SV
Massey, P
Dall, TH
Moffat, AFJ
Morrell, N
Corcoran, M
Kaufer, A
Naze, Y
Pittard, J
St-Louis, N
Fullerton, A
Massa, D
Pollock, AMT
AF Foellmi, C.
Koenigsberger, G.
Georgiev, L.
Toledano, O.
Marchenko, S. V.
Massey, P.
Dall, T. H.
Moffat, A. F. J.
Morrell, N.
Corcoran, M.
Kaufer, A.
Naze, Y.
Pittard, J.
St-Louis, N.
Fullerton, A.
Massa, D.
Pollock, A. M. T.
TI New insights into the nature of the SMC WR/LBV binary HD 5980
SO REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA
LA English
DT Article
DE binaries : close; stars : individual (HD 5980); stars : mass loss
ID SMALL-MAGELLANIC-CLOUD; WOLF-RAYET BINARY; COLLIDING STELLAR WINDS;
SYSTEM HD 5980; SPECTROSCOPIC MICROSCOPE; FUSE OBSERVATIONS; STAR
HD-5980; V444 CYGNI; COMPONENTS; EMISSION
AB We present the results of optical wavelength observations of the unusual SMC eclipsing binary system HD 5980 obtained in 1999 and 2004-2005. Radial velocity curves for the erupting LBV/WR object (star A) and its close WR-like companion (star B) are obtained by deblending the variable emission-line profiles of NIV and NV lines. The derived masses M-A = 58 - 79 M-circle dot and M-B = 51 - 67 M-circle dot, are more consistent with the the stars' location near the top of the HRD than previous estimates. The presence of a wind-wind interaction region is inferred from the orbital phase-dependent behavior of He I P Cygni absorption components. The emission-line intensities continued with the declining trend previously seen in UV spectra. The behavior of the photospheric absorption lines is consistent with the results of Schweickhardt (2000) who concludes that the third object in the combined spectrum, star C, is also a binary system with P-starC similar to 96.5 days, e=0.83.
C1 [Foellmi, C.] Domaine Univ, Lab AstrOPhys Grenoble, F-38400 St Martin Dheres, France.
[Corcoran, M.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Foellmi, C.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Dall, T. H.] Gemini Obs, Hilo, HI 96720 USA.
[Fullerton, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Georgiev, L.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Kaufer, A.] European So Observ, Santiago 19, Chile.
[Koenigsberger, G.; Toledano, O.] Univ Nacl Autonoma Mexico, Inst Ciencias Fis, Cuernavaca 62210, Morelos, Mexico.
[Marchenko, S. V.] Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA.
[Massa, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Massey, P.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Morrell, N.] Carneige Obs, Las Campanas Obs, La Serena, Chile.
[Naze, Y.] Univ Liege, Inst Astrophys & Gepphys, B-4000 Liege, Belgium.
[Pittard, J.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England.
[Pollock, A. M. T.] European Space Agcy, XMM Newton SOC, European Space Astron Ctr, Madrid 28691, Spain.
RP Foellmi, C (reprint author), Domaine Univ, Lab AstrOPhys Grenoble, 414 Rue Piscine, F-38400 St Martin Dheres, France.
EM cedric.foellmi@obs.ujf-grenoble.fr; gloria@fis.unam.mx;
georgiev@dastroscu.unam.mx; toledano@hotmail.com; sergey@astro.wku.edu;
Phil.Massey@lowell.edu; tdall@gemini.edu; moffat@astro.umontreal.ca;
nidia@leoeps1.lco.cl; Michael.F.Corcoran.1@gsfc.nasa.gov;
akaufer@eso.org; naze@astro.ulg.ac.be; jmp@ast.leeds.ac.uk;
st-louis@astro.umontreal.ca; fullerton@4stsci.edu;
massa@taotaomona.gsfc.nasa.gov; Andy.Pollock@sciops.esa.int
OI Pittard, Julian/0000-0003-2244-5070; Naze, Yael/0000-0003-4071-9346
NR 43
TC 20
Z9 21
U1 2
U2 2
PU UNIV NACIONAL AUTONOMA MEXICO, INST DE ASTRONOMIA
PI MEXICO CITY
PA APDO POSTAL 70-264, MEXICO CITY 04510, MEXICO
SN 0185-1101
J9 REV MEX ASTRON ASTR
JI Rev. Mex. Astron. Astrofis.
PD APR
PY 2008
VL 44
IS 1
BP 3
EP 27
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 285DY
UT WOS:000254758700001
ER
PT J
AU Kiang, NY
AF Kiang, Nancy Y.
TI The color of plants on other worlds
SO SCIENTIFIC AMERICAN
LA English
DT Article
C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Kiang, NY (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
NR 0
TC 4
Z9 4
U1 3
U2 12
PU SCI AMERICAN INC
PI NEW YORK
PA 415 MADISON AVE, NEW YORK, NY 10017 USA
SN 0036-8733
J9 SCI AM
JI Sci.Am.
PD APR
PY 2008
VL 298
IS 4
BP 48
EP 55
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 280RY
UT WOS:000254445100028
PM 18380141
ER
PT J
AU Zhang, KQ
Simard, M
Ross, M
Rivera-Monroy, VH
Houle, P
Ruiz, P
Twilley, RR
Whelan, KRT
AF Zhang, Keqi
Simard, Marc
Ross, Michael
Rivera-Monroy, Victor H.
Houle, Patricia
Ruiz, Pablo
Twilley, Robert R.
Whelan, Kevin R. T.
TI Airborne laser scanning quantification of disturbances from hurricanes
and lightning strikes to mangrove forests in Everglades National Park,
USA
SO SENSORS
LA English
DT Article
DE airborne light detection and ranging (LIDAR); digital canopy model
(DCM); forest disturbance; mangrove; hurricane; lightning strike;
Everglades
ID REGENERATION; VEGETATION; SEEDLINGS; SALINITY; BIOMASS; MODEL; LIDAR
AB Airborne light detection and ranging ( LIDAR) measurements derived before and after Hurricanes Katrina and Wilma ( 2005) were used to quantify the impact of hurricanes and lightning strikes on the mangrove forest at two sites in Everglades National Park ( ENP). Analysis of LIDAR measurements covering 61 and 68 ha areas of mangrove forest at the Shark River and Broad River sites showed that the proportion of high tree canopy detected by the LIDAR after the 2005 hurricane season decreased significantly due to defoliation and breakage of branches and trunks, while the proportion of low canopy and the ground increased drastically. Tall mangrove forests distant from tidal creeks suffered more damage than lower mangrove forests adjacent to the tidal creeks. The hurricanes created numerous canopy gaps, and the number of gaps per square kilometer increased from about 400 similar to 500 to 4000 after Katrina and Wilma. The total area of gaps in the forest increased from about 1 similar to 2% of the total forest area to 12%. The relative contribution of hurricanes to mangrove forest disturbance in ENP is at least 2 times more than that from lightning strikes. However, hurricanes and lightning strikes disturb the mangrove forest in a related way. Most seedlings in lightning gaps survived the hurricane impact due to the protection of trees surrounding the gaps, and therefore provide an important resource for forest recovery after the hurricane. This research demonstrated that LIDAR is an effective remote sensing tool to quantify the effects of disturbances such as hurricanes and lightning strikes in the mangrove forest.
C1 [Zhang, Keqi; Ross, Michael; Houle, Patricia; Ruiz, Pablo] Florida Int Univ, Dept Environm Studies, Miami, FL 33199 USA.
[Zhang, Keqi; Houle, Patricia] Florida Int Univ, Int Hurricane Res Ctr, Miami, FL 33199 USA.
[Simard, Marc] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ross, Michael; Ruiz, Pablo] Florida Int Univ, SE Environm Res Ctr, Miami, FL 33199 USA.
[Rivera-Monroy, Victor H.; Twilley, Robert R.] Louisiana State Univ, Wetland Biogeochem Inst, Dept Oceanog & Coastal Sci, Baton Rouge, LA 70803 USA.
[Whelan, Kevin R. T.] Natl Pk Serv, S Florida & Caribbean Network, Inventory & Monitoring Program, Miami, FL 33157 USA.
RP Zhang, KQ (reprint author), Florida Int Univ, Dept Environm Studies, Miami, FL 33199 USA.
EM zhangk@fiu.edu
RI Rivera-Monroy, Victor/G-7329-2011; Simard, Marc/H-3516-2013
OI Simard, Marc/0000-0002-9442-4562
NR 39
TC 24
Z9 26
U1 2
U2 11
PU MOLECULAR DIVERSITY PRESERVATION INT
PI BASEL
PA MATTHAEUSSTRASSE 11, CH-4057 BASEL, SWITZERLAND
SN 1424-8220
J9 SENSORS-BASEL
JI Sensors
PD APR
PY 2008
VL 8
IS 4
BP 2262
EP 2292
DI 10.3390/s8042262
PG 31
WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation
SC Chemistry; Electrochemistry; Instruments & Instrumentation
GA 312AV
UT WOS:000256642400012
PM 27879821
ER
PT J
AU Sun, CJ
Wang, YQ
Zhang, CJ
Zhou, E
Su, J
AF Sun, Changjie
Wang, Youqi
Zhang, Congjian
Zhou, Eric
Su, Ji
TI A modified self-consistent computational model for an electrostrictive
graft elastomer
SO SMART MATERIALS & STRUCTURES
LA English
DT Article
ID FIELD
AB An electrostrictive graft elastomer, as recently developed by NASA, is a type of electro-active polymer. In this paper, a 2D computational model with a self-consistent boundary is developed. Firstly, three-dimensional deformations, induced by both bending angle and dihedral torsional angle changes, are projected onto a two-dimensional plane. Using both theoretical and numerical analyses, the projected 2D equilibrium bending angle is shown to have the same value as the 3D equilibrium bending angle. The 2D equivalent bending stiffness is derived using a series model based upon the fact that both bending and dihedral torsion produce a configurational change. Equivalent stiffness is justified by polymer chain end-to-end distance characteristics. Secondly, a self-consistent scheme is developed to eliminate the boundary effect. Eight images of the unit cell are created peripherally, with the original unit cell in the center. Thus the boundary can only affect the rotation of the eight images, not the central unit cell. A computational model is employed to determine the electromechanical properties of the electrostrictive graft elastomer. Relations between electric field induced strain and electric field strength are calculated. The effect of molecular scale factors, such as free volume fraction, graft weight percentage and graft orientation, are also discussed.
C1 [Sun, Changjie; Wang, Youqi; Zhang, Congjian; Zhou, Eric] Kansas State Univ, Dept Mech & Nucl Engn, Manhattan, KS 66506 USA.
[Su, Ji] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Wang, YQ (reprint author), Kansas State Univ, Dept Mech & Nucl Engn, Manhattan, KS 66506 USA.
EM Wang@mne.ksu.edu
NR 10
TC 4
Z9 4
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0964-1726
J9 SMART MATER STRUCT
JI Smart Mater. Struct.
PD APR
PY 2008
VL 17
IS 2
AR 025007
DI 10.1088/0964-1726/17/2/025007
PG 8
WC Instruments & Instrumentation; Materials Science, Multidisciplinary
SC Instruments & Instrumentation; Materials Science
GA 276XF
UT WOS:000254176300007
ER
PT J
AU Cadavid, AC
Lawrence, JK
Ruzmaikin, A
AF Cadavid, A. C.
Lawrence, J. K.
Ruzmaikin, A.
TI Principal components and independent component analysis of solar and
space data
SO SOLAR PHYSICS
LA English
DT Article; Proceedings Paper
CT 3rd Solar Image Processing Workshop
CY SEP, 2006
CL Trinity Coll, Dublin, ISRAEL
HO Trinity Coll
DE Methods : statistical; Sun : magnetic field
ID MAGNETIC-FIELD FLUCTUATIONS; LONGITUDES; ROTATION; MODES; WIND
AB Principal components analysis (PCA) and independent component analysis (ICA) are used to identify global patterns in solar and space data. PCA seeks orthogonal modes of the two-point correlation matrix constructed from a data set. It permits the identification of structures that remain coherent and correlated or that recur throughout a time series. ICA seeks for maximally independent modes and takes into account all order correlations of the data. We apply PCA to the interplanetary magnetic field polarity near 1 AU and to the 3.25R(circle dot) source-surface fields in the solar corona. The rotations of the two-sector structures of these systems vary together to high accuracy during the active interval of solar cycle 23. We then use PCA and ICA to hunt for preferred longitudes in northern hemisphere Carrington maps of magnetic fields.
C1 [Cadavid, A. C.; Lawrence, J. K.] Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA.
[Ruzmaikin, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Cadavid, AC (reprint author), Calif State Univ Northridge, Dept Phys & Astron, 18111 Nordhoff St, Northridge, CA 91330 USA.
EM ana.cadavid@csun.edu
NR 18
TC 12
Z9 12
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD APR
PY 2008
VL 248
IS 2
BP 247
EP 261
DI 10.1007/s11207-007-9026-2
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 290IE
UT WOS:000255115700005
ER
PT J
AU Conlon, PA
Gallagher, PT
McAteer, RTJ
Ireland, J
Young, CA
Kestener, P
Hewett, RJ
Maguire, K
AF Conlon, P. A.
Gallagher, P. T.
McAteer, R. T. J.
Ireland, J.
Young, C. A.
Kestener, P.
Hewett, R. J.
Maguire, K.
TI Multifractal properties of evolving active regions
SO SOLAR PHYSICS
LA English
DT Article; Proceedings Paper
CT 3rd Solar Image Processing Workshop
CY SEP, 2006
CL Trinity Coll, Dublin, ISRAEL
HO Trinity Coll
DE active regions; magnetic fields; turbulence
ID SOLAR MAGNETIC-FIELDS; FLUX; MAGNETOGRAMS; MODEL
AB Magnetohydrodynamic turbulence is thought to be responsible for producing complex, multiscale magnetic field distributions in solar active regions. Here we explore the multiscale properties of a number of evolving active regions using magnetograms from the Michelson Doppler Imager (MDI) on the Solar and Heliospheric Observatory (SOHO). The multifractal spectrum was obtained by using a modified box-counting method to study the relationship between magnetic-field multifractality and region evolution and activity. The initial emergence of each active region was found to be accompanied by characteristic changes in the multifractal spectrum. Specifically, the range of multifractal structures (D (div)) was found to increase during emergence, as was their significance or support (C (div)). Following this, a decrease in the range in multifractal structures occurred as the regions evolved to become large-scale, coherent structures. From the small sample considered, evidence was found for a direct relationship between the multifractal properties of the flaring regions and their flaring rate.
C1 [Conlon, P. A.; Gallagher, P. T.] Trinity Coll Dublin, Astrophys Res Grp, Sch Phys, Dublin 2, Ireland.
[McAteer, R. T. J.] Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ireland, J.; Young, C. A.] NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Greenbelt, MD 20771 USA.
[Kestener, P.] CEA Saclay, DSM, DAPNIA, SEDI, F-91191 Gif Sur Yvette, France.
[Hewett, R. J.] Univ Illinois, Dept Comp Sci, Urbana, IL 61801 USA.
[Maguire, K.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
RP Conlon, PA (reprint author), Trinity Coll Dublin, Astrophys Res Grp, Sch Phys, Dublin 2, Ireland.
EM conlon.paul@gmail.com
RI McAteer, R. T. James/D-3736-2011; Gallagher, Peter/C-7717-2011
OI Gallagher, Peter/0000-0001-9745-0400
NR 26
TC 36
Z9 37
U1 1
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD APR
PY 2008
VL 248
IS 2
BP 297
EP 309
DI 10.1007/s11207-007-9074-7
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 290IE
UT WOS:000255115700008
ER
PT J
AU Jones, HP
Chapman, GA
Harvey, KL
Pap, JM
Preminger, DG
Turmon, MJ
Walton, SR
AF Jones, H. P.
Chapman, G. A.
Harvey, K. L.
Pap, J. M.
Preminger, D. G.
Turmon, M. J.
Walton, S. R.
TI A comparison of feature classification methods for modeling solar
irradiance variation
SO SOLAR PHYSICS
LA English
DT Article; Proceedings Paper
CT 3rd Solar Image Processing Workshop
CY SEP, 2006
CL Trinity Coll, Dublin, ISRAEL
HO Trinity Coll
DE solar irradiance; Sunspots; active regions; photosphere; data analysis
ID SPECTRAL IRRADIANCE; CLIMATE-CHANGE; CYCLES 21-23; VARIABILITY;
RECONSTRUCTION; SOLAR-CYCLE-23; LUMINOSITY; SUN
AB Physical understanding of total and spectral solar irradiance variation depends upon establishing a connection between the temporal variability of spatially resolved solar structures and spacecraft observations of irradiance. One difficulty in comparing models derived from different data sets is that the many ways for identifying solar features such as faculae, sunspots, quiet Sun, and various types of "network" are not necessarily consistent. To learn more about classification differences and how they affect irradiance models, feature "masks" are compared as derived from five current methods: multidimensional histogram analysis of NASA/National Solar Observatory/Kitt Peak spectromagnetograph data, statistical pattern recognition applied to SOHO/Michelson Doppler Imager photograms and magnetograms, threshold masks allowing for influence of spatial surroundings applied to NSO magnetograms, and "one-trigger" and "three-trigger" algorithms applied to California State University at Northridge Cartesian Full Disk Telescope intensity observations. In general all of the methods point to the same areas of the Sun for labeling sunspots and active-region faculae, and available time series of area measurements from the methods correlate well with each other and with solar irradiance. However, some methods include larger label sets, and there are important differences in detail, with measurements of sunspot area differing by as much as a factor of two. The methods differ substantially regarding inclusion of fine spatial scale in the feature definitions. The implications of these differences for modeling solar irradiance variation are discussed.
C1 [Jones, H. P.] Natl Solar Observ, Tucson, AZ 85726 USA.
[Chapman, G. A.; Preminger, D. G.; Walton, S. R.] Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA.
[Harvey, K. L.] Solar Phys Res Corp, Tucson, AZ USA.
[Pap, J. M.] NASA, Goddard Space Flight Ctr, UMBC, Goddard Earth Sci & Technol Inst, Greenbelt, MD 20771 USA.
[Turmon, M. J.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Jones, HP (reprint author), Natl Solar Observ, POB 26732, Tucson, AZ 85726 USA.
EM hjones@nso.edu
NR 31
TC 12
Z9 12
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD APR
PY 2008
VL 248
IS 2
BP 323
EP 337
DI 10.1007/s11207-007-9069-4
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 290IE
UT WOS:000255115700010
ER
PT J
AU Young, CA
Gallagher, PT
AF Young, C. Alex
Gallagher, Peter T.
TI Multiscale edge detection in the corona
SO SOLAR PHYSICS
LA English
DT Article; Proceedings Paper
CT 3rd Solar Image Processing Workshop
CY SEP, 2006
CL Trinity Coll, Dublin, ISRAEL
HO Trinity Coll
DE Sun : corona; Sun : coronal mass ejections (CMEs); techniques : image
processing
ID MASS EJECTIONS
AB Coronal Mass Ejections (CMEs) are challenging objects to detect using automated techniques, due to their high velocity and diffuse, irregular morphology. A necessary step to automating the detection process is to first remove the subjectivity introduced by the observer used in the current, standard, CME detection and tracking method. Here we describe and demonstrate a multiscale edge detection technique that addresses this step and could serve as one part of an automated CME detection system. This method provides a way to objectively define a CME front with associated error estimates. These fronts can then be used to extract CME morphology and kinematics. We apply this technique to a CME observed on 18 April 2000 by the Large Angle Solar COronagraph experiment (LASCO) C2/C3 and a CME observed on 21 April 2002 by LASCO C2/C3 and the Transition Region and Coronal Explorer (TRACE). For the two examples in this work, the heights determined by the standard manual method are larger than those determined with the multiscale method by approximate to 10% using LASCO data and approximate to 20% using TRACE data.
C1 [Young, C. Alex] NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Greenbelt, MD 20771 USA.
[Gallagher, Peter T.] Trinity Coll Dublin, Astrophys Res Grp, Sch Phys, Dublin 2, Ireland.
RP Young, CA (reprint author), NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Greenbelt, MD 20771 USA.
EM c.alex.young@nasa.gov
RI Gallagher, Peter/C-7717-2011
OI Gallagher, Peter/0000-0001-9745-0400
NR 19
TC 18
Z9 18
U1 1
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD APR
PY 2008
VL 248
IS 2
BP 457
EP 469
DI 10.1007/s11207-008-9177-9
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 290IE
UT WOS:000255115700018
ER
PT J
AU Kaiser, ML
Kucera, TA
Davila, JM
Cyr, OCS
Guhathakurta, M
Christian, E
AF Kaiser, M. L.
Kucera, T. A.
Davila, J. M.
Cyr, O. C. St.
Guhathakurta, M.
Christian, E.
TI The STEREO Mission: An introduction
SO SPACE SCIENCE REVIEWS
LA English
DT Editorial Material
DE CME; solar; three-dimensional
AB The twin STEREO spacecraft were launched on October 26, 2006, at 00:52 UT from Kennedy Space Center aboard a Delta 7925 launch vehicle. After a series of highly eccentric Earth orbits with apogees beyond the moon, each spacecraft used close flybys of the moon to escape into orbits about the Sun near 1 AU. Once in heliospheric orbit, one spacecraft trails Earth while the other leads. As viewed from the Sun, the two spacecraft separate at approximately 44 to 45 degrees per year. The purposes of the STEREO Mission are to understand the causes and mechanisms of coronal mass ejection (CME) initiation and to follow the propagation of CMEs through the inner heliosphere to Earth. Researchers will use STEREO measurements to study the mechanisms and sites of energetic particle acceleration and to develop three-dimensional (3-D) time-dependent models of the magnetic topology, temperature, density and velocity of the solar wind between the Sun and Earth. To accomplish these goals, each STEREO spacecraft is equipped with an almost identical set of optical, radio and in situ particles and fields instruments provided by U.S. and European investigators. The SECCHI suite of instruments includes two white light coronagraphs, an extreme ultraviolet imager and two heliospheric white light imagers which track CMEs out to 1 AU. The IMPACT suite of instruments measures in situ solar wind electrons, energetic electrons, protons and heavier ions. IMPACT also includes a magnetometer to measure the in situ magnetic field strength and direction. The PLASTIC instrument measures the composition of heavy ions in the ambient plasma as well as protons and alpha particles. The S/WAVES instrument uses radio waves to track the location of CME-driven shocks and the 3-D topology of open field lines along which flow particles produced by solar flares. Each of the four instrument packages produce a small real-time stream of selected data for purposes of predicting space weather events at Earth. NOAA forecasters at the Space Environment Center and others will use these data in their space weather forecasting and their resultant products will be widely used throughout the world. In addition to the four instrument teams, there is substantial participation by modeling and theory oriented teams. All STEREO data are freely available through individual Web sites at the four Principal Investigator institutions as well as at the STEREO Science Center located at NASA Goddard Space Flight Center.
C1 [Kaiser, M. L.; Kucera, T. A.; Davila, J. M.; Cyr, O. C. St.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Guhathakurta, M.; Christian, E.] NASA Headquarters, Washington, DC 20024 USA.
RP Kaiser, ML (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Michael.Kaiser@nasa.gov
RI Kucera, Therese/C-9558-2012; Christian, Eric/D-4974-2012;
OI Christian, Eric/0000-0003-2134-3937; Kucera, Therese/0000-0001-9632-447X
NR 18
TC 553
Z9 568
U1 8
U2 46
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD APR
PY 2008
VL 136
IS 1-4
BP 5
EP 16
DI 10.1007/s11214-007-9277-0
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 322OC
UT WOS:000257384200002
ER
PT J
AU Biesecker, DA
Webb, DF
Cyr, OCS
AF Biesecker, D. A.
Webb, D. F.
Cyr, O. C. St.
TI STEREO space weather and the Space Weather Beacon
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE STEREO; space weather; coronal mass ejection; solar wind; forecasting
ID CORONAL MASS EJECTIONS; ADVANCED COMPOSITION EXPLORER; JANUARY 1997;
MAGNETIC CLOUD; EARTH; TIME; ELECTRON; STORMS
AB The Solar Terrestrial Relations Observatory (STEREO) is primarily a solar and interplanetary research mission, with one of the natural applications being in the area of space weather. The obvious potential for space weather applications is so great that NOAA has worked to incorporate the real-time data into their forecast center as much as possible. A subset of the STEREO data will be continuously downlinked in a real-time broadcast mode, called the Space Weather Beacon. Within the research community there has been considerable interest in conducting space weather related research with STEREO. Some of this research is geared towards making an immediate impact while other work is still very much in the research domain. There are many areas where STEREO might contribute and we cannot predict where all the successes will come. Here we discuss how STEREO will contribute to space weather and many of the specific research projects proposed to address STEREO space weather issues. The data which will be telemetered down in the Space Weather Beacon is also summarized here. Some of the lessons learned from integrating other NASA missions into the forecast center are presented. We also discuss some specific uses of the STEREO data in the NOAA Space Environment Center.
C1 [Biesecker, D. A.] NOAA, Space Environm Ctr, Boulder, CO 80305 USA.
[Webb, D. F.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02467 USA.
[Cyr, O. C. St.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Biesecker, DA (reprint author), NOAA, Space Environm Ctr, 325 Broadway, Boulder, CO 80305 USA.
EM doug.biesecker@noaa.gov
NR 54
TC 10
Z9 10
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD APR
PY 2008
VL 136
IS 1-4
BP 45
EP 65
DI 10.1007/s11214-007-9165-7
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 322OC
UT WOS:000257384200004
ER
PT J
AU Howard, RA
Moses, JD
Vourlidas, A
Newmark, JS
Socker, DG
Plunkett, SP
Korendyke, CM
Cook, JW
Hurley, A
Davila, JM
Thompson, WT
St Cyr, OC
Mentzell, E
Mehalick, K
Lemen, JR
Wuelser, JP
Duncan, DW
Tarbell, TD
Wolfson, CJ
Moore, A
Harrison, RA
Waltham, NR
Lang, J
Davis, CJ
Eyles, CJ
Mapson-Menard, H
Simnett, GM
Halain, JP
Defise, JM
Mazy, E
Rochus, P
Mercier, R
Ravet, MF
Delmotte, F
Auchere, F
Delaboudiniere, JP
Bothmer, V
Deutsch, W
Wang, D
Rich, N
Cooper, S
Stephens, V
Maahs, G
Baugh, R
McMullin, D
Carter, T
AF Howard, R. A.
Moses, J. D.
Vourlidas, A.
Newmark, J. S.
Socker, D. G.
Plunkett, S. P.
Korendyke, C. M.
Cook, J. W.
Hurley, A.
Davila, J. M.
Thompson, W. T.
St Cyr, O. C.
Mentzell, E.
Mehalick, K.
Lemen, J. R.
Wuelser, J. P.
Duncan, D. W.
Tarbell, T. D.
Wolfson, C. J.
Moore, A.
Harrison, R. A.
Waltham, N. R.
Lang, J.
Davis, C. J.
Eyles, C. J.
Mapson-Menard, H.
Simnett, G. M.
Halain, J. P.
Defise, J. M.
Mazy, E.
Rochus, P.
Mercier, R.
Ravet, M. F.
Delmotte, F.
Auchere, F.
Delaboudiniere, J. P.
Bothmer, V.
Deutsch, W.
Wang, D.
Rich, N.
Cooper, S.
Stephens, V.
Maahs, G.
Baugh, R.
McMullin, D.
Carter, T.
TI Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI)
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE solar corona; Lyot coronagraph; XUV heliograph; heliospheric imager;
coronal loops; coronal mass ejections; stereo; heliosphere
ID TRANSITION REGION; ATOMIC DATABASE; EMISSION-LINES; IMAGER; EXPLORER;
CHIANTI
AB The Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) is a five telescope package, which has been developed for the Solar Terrestrial Relation Observatory (STEREO) mission by the Naval Research Laboratory (USA), the Lockheed Solar and Astrophysics Laboratory (USA), the Goddard Space Flight Center (USA), the University of Birmingham (UK), the Rutherford Appleton Laboratory (UK), the Max Planck Institute for Solar System Research (Germany), the Centre Spatiale de Leige (Belgium), the Institut d'Optique (France) and the Institut d'Astrophysique Spatiale (France). SECCHI comprises five telescopes, which together image the solar corona from the solar disk to beyond 1 AU. These telescopes are: an extreme ultraviolet imager (EUVI: 1-1.7 R-circle dot), two traditional Lyot coronagraphs (COR1: 1.5-4 R-circle dot and COR2: 2.5-15 R-circle dot) and two new designs of heliospheric imagers (HI-1: 15-84 R-circle dot and HI-2: 66-318 R-circle dot). All the instruments use 2048x2048 pixel CCD arrays in a backside-in mode. The EUVI backside surface has been specially processed for EUV sensitivity, while the others have an anti-reflection coating applied. A multi-tasking operating system, running on a PowerPC CPU, receives commands from the spacecraft, controls the instrument operations, acquires the images and compresses them for downlink through the main science channel (at compression factors typically up to 20x) and also through a low bandwidth channel to be used for space weather forecasting (at compression factors up to 200x). An image compression factor of about 10x enable the collection of images at the rate of about one every 2-3 minutes. Identical instruments, except for different sizes of occulters, are included on the STEREO-A and STEREO-B spacecraft.
C1 [Howard, R. A.; Moses, J. D.; Vourlidas, A.; Newmark, J. S.; Socker, D. G.; Plunkett, S. P.; Korendyke, C. M.; Cook, J. W.; Hurley, A.] USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA.
[Davila, J. M.; Thompson, W. T.; St Cyr, O. C.; Mentzell, E.; Mehalick, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20742 USA.
[Lemen, J. R.; Wuelser, J. P.; Duncan, D. W.; Tarbell, T. D.; Wolfson, C. J.; Moore, A.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Harrison, R. A.; Waltham, N. R.; Lang, J.; Davis, C. J.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 OQX, Oxon, England.
[Eyles, C. J.; Mapson-Menard, H.; Simnett, G. M.] Univ Birmingham, Astrophys & Space Res Grp, Birmingham B15 2TT, W Midlands, England.
[Halain, J. P.; Defise, J. M.; Mazy, E.; Rochus, P.] Univ Liege, Ctr Spatiale Liege, B-4031 Angleur, Belgium.
[Auchere, F.; Delaboudiniere, J. P.] Ctr Univ Orsay, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Bothmer, V.] Univ Gottingen, Inst Astrophys, Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany.
[Deutsch, W.] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany.
[Wang, D.; Rich, N.] Interferometr Inc, Herndon, VA USA.
[Cooper, S.; Stephens, V.; Maahs, G.] HYTEC Inc, Los Alamos, NM 87544 USA.
[Baugh, R.; McMullin, D.; Carter, T.] Praxis Inc, Alexandria, VA 22303 USA.
RP Howard, RA (reprint author), USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA.
EM russ.howard@nrl.navy.mil
RI Vourlidas, Angelos/C-8231-2009; Thompson, William/D-7376-2012; Scott,
Christopher/H-8664-2012;
OI Vourlidas, Angelos/0000-0002-8164-5948; Scott,
Christopher/0000-0001-6411-5649; Auchere, Frederic/0000-0003-0972-7022
NR 25
TC 762
Z9 775
U1 8
U2 41
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD APR
PY 2008
VL 136
IS 1-4
BP 67
EP 115
DI 10.1007/s11214-008-9341-4
PG 49
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 322OC
UT WOS:000257384200005
ER
PT J
AU Luhmann, JG
Curtis, DW
Schroeder, P
McCauley, J
Lin, RP
Larson, DE
Bale, SD
Sauvaud, JA
Aoustin, C
Mewaldt, RA
Cummings, AC
Stone, EC
Davis, AJ
Cook, WR
Kecman, B
Wiedenbeck, ME
von Rosenvinge, T
Acuna, MH
Reichenthal, LS
Shuman, S
Wortman, KA
Reames, DV
Mueller-Mellin, R
Kunow, H
Mason, GM
Walpole, P
Korth, A
Sanderson, TR
Russell, CT
Gosling, JT
AF Luhmann, J. G.
Curtis, D. W.
Schroeder, P.
McCauley, J.
Lin, R. P.
Larson, D. E.
Bale, S. D.
Sauvaud, J. -A.
Aoustin, C.
Mewaldt, R. A.
Cummings, A. C.
Stone, E. C.
Davis, A. J.
Cook, W. R.
Kecman, B.
Wiedenbeck, M. E.
von Rosenvinge, T.
Acuna, M. H.
Reichenthal, L. S.
Shuman, S.
Wortman, K. A.
Reames, D. V.
Mueller-Mellin, R.
Kunow, H.
Mason, G. M.
Walpole, P.
Korth, A.
Sanderson, T. R.
Russell, C. T.
Gosling, J. T.
TI STEREO IMPACT investigation goals, measurements, and data products
overview
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE STEREO; coronal mass ejection; solar energetic particles; suprathermal
electrons; solar wind electrons; interplanetary magnetic field;
multipoint heliospheric measurements
ID CORONAL MASS EJECTIONS; SOLAR ENERGETIC PARTICLES; INTERPLANETARY
MAGNETIC-FIELD; COROTATING INTERACTION REGIONS; HYDROMAGNETIC WAVE
EXCITATION; ADVANCED COMPOSITION EXPLORER; INTER-PLANETARY SHOCK;
HEAT-FLUX DROPOUTS; 1 AU; 3-DIMENSIONAL PROPAGATION
AB The IMPACT (In situ Measurements of Particles And CME Transients) investigation on the STEREO mission was designed and developed to provide multipoint solar wind and suprathermal electron, interplanetary magnetic field, and solar energetic particle information required to unravel the nature of coronal mass ejections and their heliospheric consequences. IMPACT consists of seven individual sensors which are packaged into a boom suite, and a SEP suite. This review summarizes the science objectives of IMPACT, the instruments that comprise the IMPACT investigation, the accommodation of IMPACT on the STEREO twin spacecraft, and the overall data products that will flow from the IMPACT measurements. Accompanying papers in this volume of Space Science Reviews highlight the individual sensor technical details and capabilities, STEREO project plans for the use of IMPACT data, and modeling activities for IMPACT (and other STEREO) data interpretation.
C1 [Luhmann, J. G.; Curtis, D. W.; Schroeder, P.; McCauley, J.; Lin, R. P.; Larson, D. E.; Bale, S. D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Sauvaud, J. -A.; Aoustin, C.] CESR, F-31028 Toulouse 4, France.
[Mewaldt, R. A.; Cummings, A. C.; Stone, E. C.; Davis, A. J.; Cook, W. R.; Kecman, B.] CALTECH, Pasadena, CA 91125 USA.
[Wiedenbeck, M. E.] Jet Prop Lab, Pasadena, CA 91109 USA.
[von Rosenvinge, T.; Acuna, M. H.; Reichenthal, L. S.; Shuman, S.; Wortman, K. A.; Reames, D. V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mueller-Mellin, R.; Kunow, H.; Mason, G. M.] Univ Kiel, D-24118 Kiel, Germany.
[Mason, G. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Walpole, P.] Univ Maryland, College Pk, MD 20742 USA.
[Korth, A.] Max Planck Inst Sonnensyst Forsch, Lindau, Germany.
[Sanderson, T. R.] ESA, Res & Sci Support Div, Noordwijk, Netherlands.
[Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Gosling, J. T.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
RP Luhmann, JG (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM jgluhman@ss1.berkeley.edu
RI Bale, Stuart/E-7533-2011
OI Bale, Stuart/0000-0002-1989-3596
NR 167
TC 136
Z9 137
U1 2
U2 9
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD APR
PY 2008
VL 136
IS 1-4
BP 117
EP 184
DI 10.1007/s11214-007-9170-x
PG 68
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 322OC
UT WOS:000257384200006
ER
PT J
AU Acuna, MH
Curtis, D
Scheifele, JL
Russell, CT
Schroeder, P
Szabo, A
Luhmann, JG
AF Acuna, M. H.
Curtis, D.
Scheifele, J. L.
Russell, C. T.
Schroeder, P.
Szabo, A.
Luhmann, J. G.
TI The STEREO/IMPACT magnetic field experiment
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE STEREO mission; IMPACT; space weather; interplanetary medium; solar
physics
ID HYDROMAGNETIC WAVE EXCITATION; INTERPLANETARY TRAVELING SHOCKS;
RANKINE-HUGONIOT PROBLEM; SOLAR-WIND; ION-ACCELERATION; BOW SHOCK;
MAGNETOMETERS; TURBULENCE; EVOLUTION; UPSTREAM
AB The magnetometer on the STEREO mission is one of the sensors in the IMPACT instrument suite. A single, triaxial, wide-range, low-power and noise fluxgate magnetometer of traditional design-and reduced volume configuration-has been implemented in each spacecraft. The sensors are mounted on the IMPACT telescoping booms at a distance of similar to 3 m from the spacecraft body to reduce magnetic contamination. The electronics have been designed as an integral part of the IMPACT Data Processing Unit, sharing a common power converter and data/command interfaces. The instruments cover the range +/- 65,536 nT in two intervals controlled by the IDPU (+/- 512 nT; +/- 65,536 nT). This very wide range allows operation of the instruments during all phases of the mission, including Earth flybys as well as during spacecraft test and integration in the geomagnetic field. The primary STEREO/IMPACT science objectives addressed by the magnetometer are the study of the interplanetary magnetic field (IMF), its response to solar activity, and its relationship to solar wind structure. The instruments were powered on and the booms deployed on November 1, 2006, seven days after the spacecraft were launched, and are operating nominally. A magnetic cleanliness program was implemented to minimize variable spacecraft fields and to ensure that the static spacecraft-generated magnetic field does not interfere with the measurements.
C1 [Acuna, M. H.; Scheifele, J. L.; Szabo, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Curtis, D.; Schroeder, P.; Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
RP Acuna, MH (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM mario.acuna@nasa.gov
NR 45
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PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD APR
PY 2008
VL 136
IS 1-4
BP 203
EP 226
DI 10.1007/s11214-007-9259-2
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 322OC
UT WOS:000257384200008
ER
PT J
AU Mason, GM
Korth, A
Walpole, PH
Desai, MI
Von Rosenvinge, TT
Shuman, SA
AF Mason, G. M.
Korth, A.
Walpole, P. H.
Desai, M. I.
Von Rosenvinge, T. T.
Shuman, S. A.
TI The Suprathermal Ion Telescope (SIT) for the IMPACT/SEP investigation
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE solar energetic particles (SEPs); cosmic rays; shock acceleration; CMEs
ID ENERGETIC PARTICLE EVENTS; HE-3-RICH SOLAR-FLARES; COROTATING
INTERACTION REGIONS; INTERPLANETARY SHOCKS; HEAVY-IONS; 1 AU; SPECTRAL
PROPERTIES; SEED POPULATION; HIGH-ENERGIES; ACCELERATION
AB The Solar-Terrestrial Relations Observatory (STEREO) mission addresses critical problems of the physics of explosive disturbances in the solar corona, and their propagation and interactions in the interplanetary medium between the Sun and Earth. The In-Situ-Measurements of Particles and CME Transients (IMPACT) investigation observes the consequences of these disturbances and other transients at 1 AU. The generation of energetic particles is a fundamentally important feature of shock-associated Coronal Mass Ejections (CMEs) and other transients in the interplanetary medium. Multiple sensors within the IMPACT suite measure the particle population from energies just above the solar wind up to hundreds of MeV/nucleon. This paper describes a portion of the IMPACT Solar Energetic Particles (SEP) package, the Suprathermal Ion Telescope (SIT) which identifies the heavy ion composition from the suprathermal through the energetic particle range (similar to few 10 s of keV/nucleon to several MeV/nucleon). SIT will trace and identify processes that energize low energy ions, and characterize their transport in the interplanetary medium. SIT is a time-of-flight mass spectrometer with high sensitivity designed to derive detailed multi-species particle spectra with a cadence of 60 s, thereby enabling detailed studies of shock-accelerated and other energetic particle populations observed at 1 AU.
C1 [Mason, G. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Korth, A.] Max Planck Inst Sonnesyst Forsch, Lindau, Germany.
[Walpole, P. H.] Univ Maryland, College Pk, MD 20742 USA.
[Desai, M. I.] SW Res Inst, San Antonio, TX 78238 USA.
[Von Rosenvinge, T. T.; Shuman, S. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Mason, GM (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM glenn.mason@jhup1.edu
NR 49
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PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD APR
PY 2008
VL 136
IS 1-4
BP 257
EP 284
DI 10.1007/s11214-006-9087-9
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 322OC
UT WOS:000257384200011
ER
PT J
AU Mewaldt, RA
Cohen, CMS
Cook, WR
Cummings, AC
Davis, AJ
Geier, S
Kecman, B
Klemic, J
Labrador, AW
Leske, RA
Miyasaka, H
Nguyen, V
Ogliore, RC
Stone, EC
Radocinski, RG
Wiedenbeck, ME
Hawk, J
Shuman, S
von Rosenvinge, TT
Wortman, K
AF Mewaldt, R. A.
Cohen, C. M. S.
Cook, W. R.
Cummings, A. C.
Davis, A. J.
Geier, S.
Kecman, B.
Klemic, J.
Labrador, A. W.
Leske, R. A.
Miyasaka, H.
Nguyen, V.
Ogliore, R. C.
Stone, E. C.
Radocinski, R. G.
Wiedenbeck, M. E.
Hawk, J.
Shuman, S.
von Rosenvinge, T. T.
Wortman, K.
TI The Low-Energy Telescope (LET) and SEP Central electronics for the
STEREO mission
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE space vehicles : instruments; instrumentation : detectors; Sun :
particle emission; Sun : coronal mass ejections; Sun : flares;
acceleration of particles
ID COROTATING INTERACTION REGIONS; SOLAR PARTICLE EVENTS; ADVANCED
COMPOSITION EXPLORER; RAY ISOTOPE SPECTROMETER; CHARGE STATES;
COSMIC-RAYS; TERMINATION SHOCK; HE-3-RICH EVENTS; NEURAL-NETWORKS;
MAGNETIC-FIELD
AB The Low-Energy Telescope (LET) is one of four sensors that make up the Solar Energetic Particle (SEP) instrument of the IMPACT investigation for NASA's STEREO mission. The LET is designed to measure the elemental composition, energy spectra, angular distributions, and arrival times of H to Ni ions over the energy range from similar to 3 to similar to 30 MeV/nucleon. It will also identify the rare isotope (3)He and trans-iron nuclei with 30 <= Z <= 83. The SEP measurements from the two STEREO spacecraft will be combined with data from ACE and other 1-AU spacecraft to provide multipoint investigations of the energetic particles that result from interplanetary shocks driven by coronal mass ejections (CMEs) and from solar flare events. The multipoint in situ observations of SEPs and solar-wind plasma will complement STEREO images of CMEs in order to investigate their role in space weather. Each LET instrument includes a sensor system made up of an array of 14 solid-state detectors composed of 54 segments that are individually analyzed by custom Pulse Height Analysis System Integrated Circuits (PHASICs). The signals from four PHASIC chips in each LET are used by a Minimal Instruction Set Computer (MISC) to provide onboard particle identification of a dozen species in similar to 12 energy intervals at event rates of similar to 1,000 events/sec. An additional control unit, called SEP Central, gathers data from the four SEP sensors, controls the SEP bias supply, and manages the interfaces to the sensors and the SEP interface to the Instrument Data Processing Unit (IDPU). This article outlines the scientific objectives that LET will address, describes the design and operation of LET and the SEP Central electronics, and discusses the data products that will result.
C1 [Mewaldt, R. A.; Cohen, C. M. S.; Cook, W. R.; Cummings, A. C.; Davis, A. J.; Geier, S.; Kecman, B.; Klemic, J.; Labrador, A. W.; Leske, R. A.; Miyasaka, H.; Nguyen, V.; Ogliore, R. C.; Stone, E. C.] CALTECH, Pasadena, CA 91125 USA.
[Radocinski, R. G.; Wiedenbeck, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hawk, J.; Shuman, S.; von Rosenvinge, T. T.; Wortman, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Mewaldt, RA (reprint author), CALTECH, Pasadena, CA 91125 USA.
EM rmewaldt@sr1.caltech.edu
NR 101
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U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD APR
PY 2008
VL 136
IS 1-4
BP 285
EP 362
DI 10.1007/s11214-007-9288-x
PG 78
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 322OC
UT WOS:000257384200012
ER
PT J
AU von Rosenvinge, TT
Reames, DV
Baker, R
Hawk, J
Nolan, JT
Ryan, L
Shuman, S
Wortman, KA
Mewaldt, RA
Cummings, AC
Cook, WR
Labrador, AW
Leske, RA
Wiedenbeck, ME
AF von Rosenvinge, T. T.
Reames, D. V.
Baker, R.
Hawk, J.
Nolan, J. T.
Ryan, L.
Shuman, S.
Wortman, K. A.
Mewaldt, R. A.
Cummings, A. C.
Cook, W. R.
Labrador, A. W.
Leske, R. A.
Wiedenbeck, M. E.
TI The High Energy Telescope for STEREO
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE space instrumentation; STEREO mission; energetic particles; coronal mass
ejections; particle acceleration
ID STORM PARTICLES; SOLAR; EXPLORER; EVENTS
AB The IMPACT investigation for the STEREO Mission includes a complement of Solar Energetic Particle instruments on each of the two STEREO spacecraft. Of these instruments, the High Energy Telescopes (HETs) provide the highest energy measurements. This paper describes the HETs in detail, including the scientific objectives, the sensors, the overall mechanical and electrical design, and the on-board software. The HETs are designed to measure the abundances and energy spectra of electrons, protons, He, and heavier nuclei up to Fe in interplanetary space. For protons and He that stop in the HET, the kinetic energy range corresponds to similar to 13 to 40 MeV/n. Protons that do not stop in the telescope (referred to as penetrating protons) are measured up to similar to 100 MeV/n, as are penetrating He. For stopping He, the individual isotopes (3)He and (4)He can be distinguished. Stopping electrons are measured in the energy range similar to 0.7-6 MeV.
C1 [von Rosenvinge, T. T.; Reames, D. V.; Baker, R.; Hawk, J.; Nolan, J. T.; Ryan, L.; Shuman, S.; Wortman, K. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mewaldt, R. A.; Cummings, A. C.; Cook, W. R.; Labrador, A. W.; Leske, R. A.] CALTECH, Pasadena, CA 91125 USA.
[Wiedenbeck, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP von Rosenvinge, TT (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Tycho.T.vonRosenvinge@nasa.gov
NR 18
TC 40
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U1 0
U2 2
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD APR
PY 2008
VL 136
IS 1-4
BP 391
EP 435
DI 10.1007/s11214-007-9300-5
PG 45
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 322OC
UT WOS:000257384200014
ER
PT J
AU Galvin, AB
Kistler, LM
Popecki, MA
Farrugia, CJ
Simunac, KDC
Ellis, L
Mobius, E
Lee, MA
Boehm, M
Carroll, J
Crawshaw, A
Conti, M
Demaine, P
Ellis, S
Gaidos, JA
Googins, J
Granoff, M
Gustafson, A
Heirtzler, D
King, B
Knauss, U
Levasseur, J
Longworth, S
Singer, K
Turco, S
Vachon, P
Vosbury, M
Widholm, M
Blush, LM
Karrer, R
Bochsler, P
Daoudi, H
Etter, A
Fischer, J
Jost, J
Opitz, A
Sigrist, M
Wurz, P
Klecker, B
Ertl, M
Seidenschwang, E
Wimmer-Schweingruber, RF
Koeten, M
Thompson, B
Steinfeld, D
AF Galvin, A. B.
Kistler, L. M.
Popecki, M. A.
Farrugia, C. J.
Simunac, K. D. C.
Ellis, L.
Moebius, E.
Lee, M. A.
Boehm, M.
Carroll, J.
Crawshaw, A.
Conti, M.
Demaine, P.
Ellis, S.
Gaidos, J. A.
Googins, J.
Granoff, M.
Gustafson, A.
Heirtzler, D.
King, B.
Knauss, U.
Levasseur, J.
Longworth, S.
Singer, K.
Turco, S.
Vachon, P.
Vosbury, M.
Widholm, M.
Blush, L. M.
Karrer, R.
Bochsler, P.
Daoudi, H.
Etter, A.
Fischer, J.
Jost, J.
Opitz, A.
Sigrist, M.
Wurz, P.
Klecker, B.
Ertl, M.
Seidenschwang, E.
Wimmer-Schweingruber, R. F.
Koeten, M.
Thompson, B.
Steinfeld, D.
TI The Plasma and Suprathermal Ion Composition (PLASTIC) investigation on
the STEREO observatories
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE STEREO; solar wind; plasma; suprathermal; composition; time-of-flight
spectrometer; coronal mass ejections; multipoint spacecraft observations
ID COROTATING INTERACTION REGIONS; SOLAR ENERGETIC PARTICLE; CORONAL MASS
EJECTIONS; WIND STREAM INTERFACES; THIN CARBON FOILS; CHARGE STATES;
ELECTRON-EMISSION; PICKUP IONS; INTERPLANETARY SHOCKS; CALIBRATION
SYSTEM
AB The Plasma and Suprathermal Ion Composition (PLASTIC) investigation provides the in situ solar wind and low energy heliospheric ion measurements for the NASA Solar Terrestrial Relations Observatory Mission, which consists of two spacecraft (STEREO-A, STEREO-B). PLASTIC-A and PLASTIC-B are identical. Each PLASTIC is a time-of-flight/energy mass spectrometer designed to determine the elemental composition, ionic charge states, and bulk flow parameters of major solar wind ions in the mass range from hydrogen to iron. PLASTIC has nearly complete angular coverage in the ecliptic plane and an energy range from similar to 0.3 to 80 keV/e, from which the distribution functions of suprathermal ions, including those ions created in pick-up and local shock acceleration processes, are also provided.
C1 [Galvin, A. B.; Kistler, L. M.; Popecki, M. A.; Farrugia, C. J.; Simunac, K. D. C.; Ellis, L.; Moebius, E.; Lee, M. A.; Boehm, M.; Carroll, J.; Crawshaw, A.; Conti, M.; Demaine, P.; Ellis, S.; Gaidos, J. A.; Googins, J.; Granoff, M.; Gustafson, A.; Heirtzler, D.; King, B.; Knauss, U.; Levasseur, J.; Longworth, S.; Singer, K.; Turco, S.; Vachon, P.; Vosbury, M.; Widholm, M.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Galvin, A. B.; Kistler, L. M.; Farrugia, C. J.; Simunac, K. D. C.; Moebius, E.; Lee, M. A.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA.
[Blush, L. M.; Karrer, R.; Bochsler, P.; Daoudi, H.; Etter, A.; Fischer, J.; Jost, J.; Opitz, A.; Sigrist, M.; Wurz, P.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland.
[Klecker, B.; Ertl, M.; Seidenschwang, E.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Wimmer-Schweingruber, R. F.; Koeten, M.] Univ Kiel, Inst Expt & Appl Phys, Extraterr Phys, D-24098 Kiel, Germany.
[Thompson, B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Steinfeld, D.] Orbital Sci Corp, Greenbelt, MD 20770 USA.
RP Galvin, AB (reprint author), Univ New Hampshire, Inst Study Earth Oceans & Space, SSC Morse Hall, Durham, NH 03824 USA.
EM toni.galvin@unh.edu
RI Galvin, Antoinette/A-6114-2013; Thompson, Barbara/C-9429-2012;
OI Moebius, Eberhard/0000-0002-2745-6978
NR 103
TC 217
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U1 2
U2 14
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD APR
PY 2008
VL 136
IS 1-4
BP 437
EP 486
DI 10.1007/s11214-007-9296-x
PG 50
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 322OC
UT WOS:000257384200015
ER
PT J
AU Bougeret, JL
Goetz, K
Kaiser, ML
Bale, SD
Kellogg, PJ
Maksimovic, M
Monge, N
Monson, SJ
Astier, PL
Davy, S
Dekkali, M
Hinze, JJ
Manning, RE
Aguilar-Rodriguez, E
Bonnin, X
Briand, C
Cairns, IH
Cattell, CA
Cecconi, B
Eastwood, J
Ergun, RE
Fainberg, J
Hoang, S
Huttunen, KEJ
Krucker, S
Lecacheux, A
MacDowall, RJ
Macher, W
Mangeney, A
Meetre, CA
Moussas, X
Nguyen, QN
Oswald, TH
Pulupa, M
Reiner, MJ
Robinson, PA
Rucker, H
Salem, C
Santolik, O
Silvis, JM
Ullrich, R
Zarka, P
Zouganelis, I
AF Bougeret, J. L.
Goetz, K.
Kaiser, M. L.
Bale, S. D.
Kellogg, P. J.
Maksimovic, M.
Monge, N.
Monson, S. J.
Astier, P. L.
Davy, S.
Dekkali, M.
Hinze, J. J.
Manning, R. E.
Aguilar-Rodriguez, E.
Bonnin, X.
Briand, C.
Cairns, I. H.
Cattell, C. A.
Cecconi, B.
Eastwood, J.
Ergun, R. E.
Fainberg, J.
Hoang, S.
Huttunen, K. E. J.
Krucker, S.
Lecacheux, A.
MacDowall, R. J.
Macher, W.
Mangeney, A.
Meetre, C. A.
Moussas, X.
Nguyen, Q. N.
Oswald, T. H.
Pulupa, M.
Reiner, M. J.
Robinson, P. A.
Rucker, H.
Salem, C.
Santolik, O.
Silvis, J. M.
Ullrich, R.
Zarka, P.
Zouganelis, I.
TI S/WAVES: The radio and plasma wave investigation on the STEREO Mission
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE solar radioastronomy; space instrumentation
ID CORONAL MASS EJECTIONS; THERMAL NOISE SPECTROSCOPY; WIND ELECTRON
PARAMETERS; STOCHASTIC-GROWTH THEORY; CLUMPY LANGMUIR-WAVES; EARTHS BOW
SHOCK; SOLAR-WIND; 1 AU; INTERPLANETARY MEDIUM; HARMONIC EMISSION
AB This paper introduces and describes the radio and plasma wave investigation on the STEREO Mission: STEREO/WAVES or S/WAVES. The S/WAVES instrument includes a suite of state-of-the-art experiments that provide comprehensive measurements of the three components of the fluctuating electric field from a fraction of a hertz up to 16 MHz, plus a single frequency channel near 30 MHz. The instrument has a direction finding or goniopolarimetry capability to perform 3D localization and tracking of radio emissions associated with streams of energetic electrons and shock waves associated with Coronal Mass Ejections (CMEs). The scientific objectives include: (i) remote observation and measurement of radio waves excited by energetic particles throughout the 3D heliosphere that are associated with the CMEs and with solar flare phenomena, and (ii) in-situ measurement of the properties of CMEs and interplanetary shocks, such as their electron density and temperature and the associated plasma waves near 1 Astronomical Unit (AU). Two companion papers provide details on specific aspects of the S/WAVES instrument, namely the electric antenna system (Bale et al., Space Sci. Rev., 2007) and the direction finding technique (Cecconi et al., Space Sci. Rev., 2007).
C1 [Bougeret, J. L.; Maksimovic, M.; Monge, N.; Astier, P. L.; Davy, S.; Dekkali, M.; Manning, R. E.; Bonnin, X.; Briand, C.; Cecconi, B.; Hoang, S.; Lecacheux, A.; Mangeney, A.; Nguyen, Q. N.; Zarka, P.; Zouganelis, I.] Observ Paris, UMR CNRS 8109, LESIA, F-92195 Meudon, France.
[Goetz, K.; Kellogg, P. J.; Monson, S. J.; Hinze, J. J.; Cattell, C. A.; Silvis, J. M.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Kaiser, M. L.; Fainberg, J.; MacDowall, R. J.; Meetre, C. A.; Reiner, M. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bale, S. D.; Aguilar-Rodriguez, E.; Eastwood, J.; Huttunen, K. E. J.; Krucker, S.; Pulupa, M.; Salem, C.; Ullrich, R.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Bale, S. D.; Pulupa, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Cairns, I. H.; Robinson, P. A.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
[Ergun, R. E.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Macher, W.; Oswald, T. H.; Rucker, H.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria.
[Moussas, X.] Univ Athens, Dept Phys, Sect Astrophys Astron & Mech, Athens, Greece.
[Reiner, M. J.] Catholic Univ Amer, Washington, DC 20064 USA.
[Santolik, O.] Charles Univ Prague, Fac Math & Phys, Prague, Czech Republic.
[Santolik, O.] CAS, IAP, Prague, Czech Republic.
RP Maksimovic, M (reprint author), Observ Paris, UMR CNRS 8109, LESIA, F-92195 Meudon, France.
EM milan.maksimovic@obspm.fr
RI Bale, Stuart/E-7533-2011; MacDowall, Robert/D-2773-2012; Kilpua,
Emilia/G-8994-2012; Santolik, Ondrej/F-7766-2014;
OI Bale, Stuart/0000-0002-1989-3596; Cattell, Cynthia/0000-0002-3805-320X;
Pulupa, Marc/0000-0002-1573-7457; Cairns, Iver/0000-0001-6978-9765
NR 89
TC 188
Z9 189
U1 1
U2 9
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD APR
PY 2008
VL 136
IS 1-4
BP 487
EP 528
DI 10.1007/s11214-007-9298-8
PG 42
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 322OC
UT WOS:000257384200016
ER
PT J
AU Aschwanden, MJ
Burlaga, LF
Kaiser, ML
Ng, CK
Reames, DV
Reiner, MJ
Gombosi, TI
Lugaz, N
Manchester, W IV
Roussev, II
Zurbuchen, TH
Farrugia, CJ
Galvin, AB
Lee, MA
Linker, JA
Mikic, Z
Riley, P
Alexander, D
Sandman, AW
Cook, JW
Howard, RA
Odstrcil, D
Pizzo, VJ
Kota, J
Liewer, PC
Luhmann, JG
Inhester, B
Schwenn, RW
Solanki, SK
Vasyliunas, VM
Wiegelmann, T
Blush, L
Bochsler, P
Cairns, IH
Robinson, PA
Bothmer, V
Kecskemety, K
Llebaria, A
Maksimovic, M
Scholer, M
Wimmer-Schweingruber, RF
AF Aschwanden, Markus J.
Burlaga, L. F.
Kaiser, M. L.
Ng, C. K.
Reames, D. V.
Reiner, M. J.
Gombosi, T. I.
Lugaz, N.
Manchester, W., IV
Roussev, I. I.
Zurbuchen, T. H.
Farrugia, C. J.
Galvin, A. B.
Lee, M. A.
Linker, J. A.
Mikic, Z.
Riley, P.
Alexander, D.
Sandman, A. W.
Cook, J. W.
Howard, R. A.
Odstrcil, D.
Pizzo, V. J.
Kota, J.
Liewer, P. C.
Luhmann, J. G.
Inhester, B.
Schwenn, R. W.
Solanki, S. K.
Vasyliunas, V. M.
Wiegelmann, T.
Blush, L.
Bochsler, P.
Cairns, I. H.
Robinson, P. A.
Bothmer, V.
Kecskemety, K.
Llebaria, A.
Maksimovic, M.
Scholer, M.
Wimmer-Schweingruber, R. F.
TI Theoretical modeling for the STEREO mission
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE STEREO mission; solar corona; solar wind; coronal mass ejection (CME);
solar filaments; heliosphere; interplanetary shocks; interplanetary
particle beams; solar energetic particle events (SEP); solar flares;
space weather; stereoscopy; 3D reconstruction techniques; white-light
emission; EUV emission; interplanetary radio emission
ID CORONAL MASS EJECTIONS; SOLAR RADIO-BURSTS; ACTIVE-REGION LOOPS; SPACE
WEATHER EVENT; WHITE-LIGHT IMAGES; MAGNETIC-FLUX ROPE; AB-INITIO
APPROACH; GLOBAL MHD MODEL; WHOLE SUN MONTH; 3-DIMENSIONAL PROPAGATION
AB We summarize the theory and modeling efforts for the STEREO mission, which will be used to interpret the data of both the remote-sensing (SECCHI, SWAVES) and in-situ instruments (IMPACT, PLASTIC). The modeling includes the coronal plasma, in both open and closed magnetic structures, and the solar wind and its expansion outwards from the Sun, which defines the heliosphere. Particular emphasis is given to modeling of dynamic phenomena associated with the initiation and propagation of coronal mass ejections (CMEs). The modeling of the CME initiation includes magnetic shearing, kink instability, filament eruption, and magnetic reconnection in the flaring lower corona. The modeling of CME propagation entails interplanetary shocks, interplanetary particle beams, solar energetic particles (SEPs), geoeffective connections, and space weather. This review describes mostly existing models of groups that have committed their work to the STEREO mission, but is by no means exhaustive or comprehensive regarding alternative theoretical approaches.
C1 [Aschwanden, Markus J.] Lockheed Martin ATC, Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Burlaga, L. F.; Kaiser, M. L.; Ng, C. K.; Reames, D. V.; Reiner, M. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gombosi, T. I.; Lugaz, N.; Manchester, W., IV; Roussev, I. I.; Zurbuchen, T. H.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Farrugia, C. J.; Galvin, A. B.; Lee, M. A.] Univ New Hampshire, Durham, NH 03824 USA.
[Linker, J. A.; Mikic, Z.; Riley, P.] SAIC, San Diego, CA 92121 USA.
[Alexander, D.; Sandman, A. W.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA.
[Cook, J. W.; Howard, R. A.] USN, Res Lab, Washington, DC 20375 USA.
[Odstrcil, D.; Pizzo, V. J.] NOAA, SEC, Boulder, CO 80303 USA.
[Kota, J.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Liewer, P. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Inhester, B.; Schwenn, R. W.; Solanki, S. K.; Vasyliunas, V. M.; Wiegelmann, T.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Blush, L.; Bochsler, P.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland.
[Cairns, I. H.; Robinson, P. A.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
[Bothmer, V.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Kecskemety, K.] HKFI RMKI, H-1525 Budapest, Hungary.
[Llebaria, A.] CNRS, Astron Spatiale Lab, F-13376 Marseille, France.
[Maksimovic, M.] Observ Paris, CNRS, F-92195 Meudon, France.
[Maksimovic, M.] Observ Paris, LESIA, F-92195 Meudon, France.
[Scholer, M.] Max Planck Inst Extraterr Phys, Ctr Interdisciplinary Plasma Sci, D-85740 Munich, Germany.
[Wimmer-Schweingruber, R. F.] Univ Kiel, Phys IEAP, D-24118 Kiel, Germany.
RP Aschwanden, MJ (reprint author), Lockheed Martin ATC, Solar & Astrophys Lab, 3251 Hanover St, Palo Alto, CA 94304 USA.
EM aschwanden@1msa1.com
RI Lugaz, Noe/C-1284-2008; Roussev, Ilia/E-9141-2011; Gombosi,
Tamas/G-4238-2011; Manchester, Ward/I-9422-2012; Galvin,
Antoinette/A-6114-2013; Solanki, Sami/E-2487-2013
OI Cairns, Iver/0000-0001-6978-9765; Lugaz, Noe/0000-0002-1890-6156;
Gombosi, Tamas/0000-0001-9360-4951; Solanki, Sami/0000-0002-3418-8449
NR 218
TC 21
Z9 22
U1 1
U2 4
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD APR
PY 2008
VL 136
IS 1-4
BP 565
EP 604
DI 10.1007/s11214-006-9027-8
PG 40
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 322OC
UT WOS:000257384200019
ER
PT J
AU Eichstedt, J
Thompson, WT
Cyr, OCS
AF Eichstedt, J.
Thompson, W. T.
Cyr, O. C. St.
TI STEREO ground segment, science operations, and data archive
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE STEREO; space weather; science operations; data archive; solar
observations
ID SYSTEM
AB Vitally important to the success of any mission is the ground support system used for commanding the spacecraft, receiving the telemetry, and processing the results. We describe the ground system used for the STEREO mission, consisting of the Mission Operations Center, the individual Payload Operations Centers for each instrument, and the STEREO Science Center, together with mission support from the Flight Dynamics Facility, Deep Space Mission System, and the Space Environment Center. The mission planning process is described, as is the data flow from spacecraft telemetry to processed science data to long-term archive. We describe the online resources that researchers will be able to use to access STEREO planning resources, science data, and analysis software. The STEREO Joint Observations Program system is described, with instructions on how observers can participate. Finally, we describe the near-real-time processing of the "space weather beacon" telemetry, which is a low telemetry rate quicklook product available close to 24 hours a day, with the intended use of space weather forecasting.
C1 [Thompson, W. T.] NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Greenbelt, MD 20771 USA.
[Eichstedt, J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Thompson, WT (reprint author), NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Code 671, Greenbelt, MD 20771 USA.
EM William.T.Thompson.1@gsfc.nasa.gov
RI Thompson, William/D-7376-2012
NR 6
TC 4
Z9 4
U1 0
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD APR
PY 2008
VL 136
IS 1-4
BP 605
EP 626
DI 10.1007/s11214-007-9249-4
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 322OC
UT WOS:000257384200020
ER
PT J
AU Peticolas, LM
Craig, N
Kucera, T
Michels, DJ
Gerulskis, J
MacDowall, RJ
Beisser, K
Chrissotimos, C
Luhmann, JG
Galvin, AB
Ratta, L
Drobnes, E
Mendez, BJ
Hill, S
Marren, K
Howard, R
AF Peticolas, L. M.
Craig, N.
Kucera, T.
Michels, D. J.
Gerulskis, J.
MacDowall, R. J.
Beisser, K.
Chrissotimos, C.
Luhmann, J. G.
Galvin, A. B.
Ratta, L.
Drobnes, E.
Mendez, B. J.
Hill, S.
Marren, K.
Howard, R.
TI The solar terrestrial relations observatory (STEREO) Education and
Outreach (E/PO) program
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE education; outreach; Sun : coronal mass ejections (CMEs); Sun : magnetic
fields; Sun : particle emission; Sun : solar-terrestrial relations
AB The STEREO mission's Education and Outreach (E/PO) program began early enough its team benefited from many lessons learned as NASA's E/PO profession matured. Originally made up of discrete programs, by launch the STEREO E/PO program had developed into a quality suite containing all the program elements now considered standard: education workshops, teacher/student guides, national and international collaboration, etc. The benefit of bringing so many unique programs together is the resulting diverse portfolio, with scientists, E/PO professionals, and their education partners all of whom can focus on excellent smaller programs. The drawback is a less cohesive program nearly impossible to evaluate in its entirety with the given funding. When individual components were evaluated, we found our programs mostly made positive impact. In this paper, we elaborate on the programs, hoping that others will effectively use or improve upon them. When possible, we indicate the programs' effects on their target audiences.
C1 [Peticolas, L. M.; Craig, N.; Luhmann, J. G.; Mendez, B. J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Kucera, T.; MacDowall, R. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Michels, D. J.; Howard, R.] USN, Res Lab, Ctr Space Res, Washington, DC 20375 USA.
[Gerulskis, J.] Christa McAuliffe Planetarium, Concord, NH 03301 USA.
[Beisser, K.; Marren, K.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Chrissotimos, C.] Sci Syst & Applicat Inc, Cranbury, NJ 08512 USA.
[Galvin, A. B.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Ratta, L.] Integrated Commun Technol Inc, Greenbelt, MD 20770 USA.
[Drobnes, E.] ADNEt Syst Inc, Rockville, MD 20852 USA.
[Hill, S.] RS Informat Syst, Greenbelt, MD 20771 USA.
RP Peticolas, LM (reprint author), Univ Calif Berkeley, Space Sci Lab, 77 Gauss Way, Berkeley, CA 94720 USA.
EM laura@ssl.berkeley.edu
RI Kucera, Therese/C-9558-2012; MacDowall, Robert/D-2773-2012;
OI Kucera, Therese/0000-0001-9632-447X
NR 10
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD APR
PY 2008
VL 136
IS 1-4
BP 627
EP 646
DI 10.1007/s11214-007-9287-y
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 322OC
UT WOS:000257384200021
ER
PT J
AU Kohout, T
Kletetschka, G
Donadini, F
Fuller, M
Herrero-Bervera, E
AF Kohout, T.
Kletetschka, G.
Donadini, F.
Fuller, M.
Herrero-Bervera, E.
TI Analysis of the natural remanent magnetization of rocks by measuring the
efficiency ratio through alternating field demagnetization spectra
SO STUDIA GEOPHYSICA ET GEODAETICA
LA English
DT Article
DE REM; efficiency of magnetization; coercivity; shock remanence; SRM
ID DEPENDENCE; PLOTS
AB The REM(AF) method is a new tool for the analysis of the origin and alternating field demagnetization coercivity spectra of the remanent magnetization. We applied this method on precambrian Gila diabase sheets from Arizona in order to identify the high coercivity magnetic carrier, and on artificially shocked Rowley Regis basalt from UK in order to analyze the effect of the shock on the natural remanent magnetization.
In the Gila diabase the high coercivity magnetic component was identified to be most likely represented by the acicular magnetite (increase in the efficiency ratio in the high coercivity region).
In the Rowley Regis basalt, the REM(AF) analysis revealed that comparing to NRM, the shock produced a different distribution of the AF demagnetization coercivity spectra due to the occurrence of the Shock Remanent Magnetization.
C1 [Kohout, T.; Donadini, F.] Univ Helsinki, Dept Phys, Helsinki, Finland.
[Kohout, T.; Donadini, F.] Charles Univ Prague, Dept Appl Geophys, Prague 12843 2, Czech Republic.
[Kohout, T.; Kletetschka, G.] Acad Sci Czech Republic, Inst Geol, Prague 16500 6, Czech Republic.
[Kletetschka, G.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Kletetschka, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Donadini, F.] Univ Calif San Diego, Scripps Inst Oceanog, San Diego, CA 92103 USA.
[Fuller, M.; Herrero-Bervera, E.] Univ Hawaii Manoa, HIGP SOEST, Honolulu, HI 96822 USA.
RP Kohout, T (reprint author), Univ Helsinki, Dept Phys, POB 64, Helsinki, Finland.
EM tomas.kohout@helsinki.fi
RI Kohout, Tomas/C-1394-2008; Kletetschka, Gunther/C-9996-2011
OI Kohout, Tomas/0000-0003-4458-3650; Kletetschka,
Gunther/0000-0002-0645-9037
NR 19
TC 2
Z9 2
U1 0
U2 7
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0039-3169
J9 STUD GEOPHYS GEOD
JI Stud. Geophys. Geod.
PD APR
PY 2008
VL 52
IS 2
BP 225
EP 235
DI 10.1007/s11200-008-0015-1
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 315UY
UT WOS:000256906900006
ER
PT J
AU Adachi, T
Kletetschka, G
AF Adachi, T.
Kletetschka, G.
TI Impact-pressure controlled orientation of shatter cone magnetizations in
Sierra Madera, Texas, USA
SO STUDIA GEOPHYSICA ET GEODAETICA
LA English
DT Article
DE shatter cones; demagnetization; remagnetization; impact crater; shock
fractures; magnetism; magnetic efficiency; magnetic signatures; magnetic
anomaly; Mars
ID VREDEFORT METEORITE CRATER; SHOCK METAMORPHISM; SOUTH-AFRICA; QUARTZ;
ROCKS; ORIGIN
AB A suite of Sierra Madera Impact deformed rocks was studied and magnetic analyses were performed. We characterized the magnetic signatures of two locations, sites A and B that have different physical characteristics of shock fractured structures as well as the magnetic signatures. Shatter cone at site A has a fine-scale (few to similar to 10 mm) distributed array of complete shatter cones with sharp apex. Natural remanent magnetization (NRM) of site A shatter cone is distributed within the plane that is perpendicular to the apexes of the cones. Shatter cone at site B shows no apparent cone shape or apex, instead, a relatively larger scale and multiple striated joint set (MSJS) and sinusoidal continuous peak. NRM of site B shatter cone is clustered along the apexes. The difference in magnetization direction is a likely indicator of the shock pressure where parallel to apex indicates pressures larger than 10 GPa and perpendicular to apex indicate pressures less than 10 GPa. Intensities of NRM and saturation isothermal remanent magnetization (SIRM) contrast and fluctuate within a shatter cone as well as in between two sites. We observed a random orientation of magnetic vector directions and amplitudes changing over small scales leading to the absence of coherent macro-scale signature.
C1 [Adachi, T.; Kletetschka, G.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Adachi, T.; Kletetschka, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kletetschka, G.] Acad Sci Czech Republic, Inst Geol, Prague 16500 6, Czech Republic.
RP Adachi, T (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
EM tomoko.adachi@ssedmail.gsfc.nasa.gov
RI Kletetschka, Gunther/C-9996-2011
OI Kletetschka, Gunther/0000-0002-0645-9037
NR 27
TC 2
Z9 2
U1 0
U2 9
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0039-3169
J9 STUD GEOPHYS GEOD
JI Stud. Geophys. Geod.
PD APR
PY 2008
VL 52
IS 2
BP 237
EP 254
DI 10.1007/s11200-008-0016-0
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 315UY
UT WOS:000256906900007
ER
PT J
AU Andersen, O
Berry, P
Freeman, J
Lemoine, FG
Lutsckhe, S
Jakobsen, F
Butts, M
AF Andersen, Ole
Berry, Philippa
Freeman, Jennifer
Lemoine, Frank G.
Lutsckhe, S.
Jakobsen, Flemming
Butts, Michael
TI Satellite altimetry and GRACE gravimetry for studies of annual water
storage variations in Bangladesh
SO TERRESTRIAL ATMOSPHERIC AND OCEANIC SCIENCES
LA English
DT Article; Proceedings Paper
CT International Workshop on Coast and Land Applications of Satellite
Altimetry
CY JUL 21-22, 2006
CL Beijing, PEOPLES R CHINA
SP Chinese Acad Surveying & Mapping, Natl Chiao Tung Univ, Asia GIS & GPS Co, Chung Hsing Surv Co, Huanyu Surv Engn Cons, Real World Engn Cons
DE altimetry; grace; river-level; ground water
ID GRAVITY-FIELD
AB Four different data sources have been compared with respect to observations of the annual water storage variations in the region of Bangladesh. Data from satellite altimeters and river gauges estimates the variation in surface water storage in the major rivers of Bangladesh.
The GRACE satellites measure the integrated mass change and hence the terrestrial soil moisture variations, which can also be estimated by a hydrological model (GLDAS). These types of observations enable the derivation of the integrated water storage in the entire region of Bangladesh.
For all data types, the annual signal has been estimated from a common dataset spanning the period 2003 and 2004. All four different data observe that water storage in Bangladesh is largely dominated by an annual signal with a phase peaking in early September. The annual variations in river level peaks roughly two weeks earlier than terrestrial soil moisture observations by GRACE observations and GLDAS model output.
C1 [Andersen, Ole] DTU, Danish Natl Space Ctr, DK-2100 Copenhagen, Denmark.
[Berry, Philippa; Freeman, Jennifer] De Montfort Univ, EAPRS Lab, Leicester LE1 9BH, Leics, England.
[Lemoine, Frank G.; Lutsckhe, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Jakobsen, Flemming; Butts, Michael] DHI Water & Environm, DK-2970 Horsholm, Denmark.
RP Andersen, O (reprint author), DTU, Danish Natl Space Ctr, DK-2100 Copenhagen, Denmark.
EM oa@space.dtu.dk
RI Lemoine, Frank/D-1215-2013; Andersen, Ole /H-7481-2016
OI Andersen, Ole /0000-0002-6685-3415
NR 15
TC 10
Z9 12
U1 2
U2 10
PU CHINESE GEOSCIENCE UNION
PI TAIPEI
PA PO BOX 23-59, TAIPEI 10764, TAIWAN
SN 1017-0839
J9 TERR ATMOS OCEAN SCI
JI Terr. Atmos. Ocean. Sci.
PD APR
PY 2008
VL 19
IS 1-2
BP 47
EP 52
DI 10.3319/TAO.2008.19.1-2.47(SA)
PG 6
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences;
Oceanography
SC Geology; Meteorology & Atmospheric Sciences; Oceanography
GA 300WQ
UT WOS:000255856500005
ER
PT J
AU Bauschlicher, CW
Lawson, JW
AF Bauschlicher, Charles W., Jr.
Lawson, John W.
TI Current-voltage curves for molecular junctions: the issue of the basis
set for the metal contacts
SO THEORETICAL CHEMISTRY ACCOUNTS
LA English
DT Article
DE DFT; Greens Functions; current-voltage curves; molecular electronics
ID EFFECTIVE CORE POTENTIALS; ELECTRONIC DEVICES; CONDUCTANCE; FORMALISM;
TRANSPORT; EXCHANGE; ENERGY; WIRES
AB We present current-voltage (I-V) curves for a chain of six Au atoms and for benzene-1,4-dithiol between two Au (111) surfaces computed using a self-consistent, non-equilibrium, Green's Functions approach in conjunction with a density functional theory (DFT) description of the extended molecule. The solutions are expanded in Gaussian basis sets. In an attempt to improve the description of the molecule-surface bond, we consider one- and two-layer clusters of metal atoms in the extended molecule. To avoid non-physical charging of the bulk metal clusters we add a shift to the diagonal elements of the Fock Matrix of the metal atoms in the DFT treatment; this can be viewed as correcting the self-energies or shifting the Fermi level. The Au-6 cluster with the full minimal basis set represents a compromise between accuracy and cost. The Au-31(12/19) two-layer cluster results are of about the same quality as the one-layer Au-21 cluster, but allows one to study more binding sites. Using a double zeta basis set for three of the top-layer Au atoms of the Au-31(12/19) cluster yields result similar to the all minimal basis set, while using all double zeta atoms yields inferior results.
C1 [Bauschlicher, Charles W., Jr.; Lawson, John W.] NASA, Ames Res Ctr, Ctr Adv Mat & Devices, Moffett Field, CA 94035 USA.
RP Bauschlicher, CW (reprint author), NASA, Ames Res Ctr, Ctr Adv Mat & Devices, Mail Stop 230-3, Moffett Field, CA 94035 USA.
EM Charles.W.Bauschlicher@nasa.gov; John.W.Lawson@nasa.gov
NR 30
TC 1
Z9 1
U1 1
U2 5
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1432-881X
J9 THEOR CHEM ACC
JI Theor. Chem. Acc.
PD APR
PY 2008
VL 119
IS 5-6
BP 429
EP 435
DI 10.1007/s00214-007-0398-z
PG 7
WC Chemistry, Physical
SC Chemistry
GA 280DY
UT WOS:000254406400003
ER
PT J
AU Kehrer, K
Graf, B
Roeder, WP
AF Kehrer, Kristen
Graf, Brian
Roeder, William P.
TI Global positioning system (GPS) precipitable water in forecasting
lightning at Spaceport Canaveral
SO WEATHER AND FORECASTING
LA English
DT Article
ID VAPOR
AB This paper evaluates the use of precipitable water (PW) from the global positioning system (GPS) in lightning prediction. Additional independent verification of an earlier model is performed. This earlier model used binary logistic regression with the following four predictor variables optimally selected from a candidate list of 23 candidate predictors: the current precipitable water value for a given time of the day, the change in GPS PW over the past 9 h, the K index, and the electric field mill value. The K index was used as a measure of atmospheric stability, which, of the traditional stability measures, has been shown to work best in the area and season under study. This earlier model was not optimized for any specific forecast interval, but showed promise for 6- and 1.5-h forecasts. Two new models were developed and verified. These new models were optimized for two operationally significant forecast intervals. The first model was optimized for the 0.5-h lightning advisories issued by the U. S. Air Force's 45th Weather Squadron. An additional 1.5 h was allowed for sensor dwell, communication, calculation, analysis, and advisory decision by the forecaster. Therefore, the 0.5-h advisory model became a 2-h forecast model for lightning within the 45th Weather Squadron advisory areas. The second model was optimized for major ground processing operations supported by the 45th Weather Squadron, which can require lightning forecasts with a lead time of up to 7.5 h. Using the same 1.5-h lag as in the other new model, this became a 9-h forecast model for lightning within 37 km (20 n mi) of the 45th Weather Squadron advisory areas. The two new models were built using binary logistic regression and a list of 26 candidate predictor variables: the current GPS PW value, the K index, and 24 candidate variables of the change in GPS PW levels over 0.5-h increments up to 12 h. The new 2-h model found the following four predictors to be statistically significant, listed in decreasing order of contribution to the forecast: the 0.5-h change in GPS PW, the 7.5-h change in GPS PW, the current GPS PW value, and the K index. The new 9-h forecast model found the following five independent variables to be statistically significant, listed in decreasing order of contribution to the forecast: the current GPS PW value, the 8.5-h change in GPS PW, the 3.5-h change in GPS PW, the 12-h change in GPS PW, and the K index. In both models, the GPS PW parameters had better correlation to the lightning forecast than did the K index, a widely used thunderstorm index. Possible future improvements to this study are discussed.
C1 [Kehrer, Kristen; Graf, Brian] NASA, Kennedy Space Ctr, FL 32899 USA.
[Roeder, William P.] Patrick AFB, Miami, FL USA.
RP Kehrer, K (reprint author), NASA, Mail Stop EA-C, Kennedy Space Ctr, FL 32899 USA.
EM kristen.c.kehrer@nasa.gov
NR 19
TC 2
Z9 2
U1 1
U2 1
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0882-8156
J9 WEATHER FORECAST
JI Weather Forecast.
PD APR
PY 2008
VL 23
IS 2
BP 219
EP 232
DI 10.1175/2007WAF2006105.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 289TT
UT WOS:000255077500002
ER
PT J
AU Herring, GC
Popovic, S
AF Herring, G. C.
Popovic, S.
TI Microwave air breakdown enhanced with metallic initiators
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID DISCHARGE
AB We have determined X-band (9.4 GHz) electric field strengths required to obtain air breakdown at atmospheric pressure in the presence of metallic initiators, which are irradiated with repetitive (30 pulses/s) microwave pulses of 3 mu s duration and 200 kW peak power. Using a half-wavelength initiator, a factor of 40 reduction (compared to no initiator) was observed in the electric field required to achieve breakdown. The present measurements are compared to a previously published model for air breakdown, which was originally validated with S-band (3 GHz) frequencies and single 40 mu s pulses. We find good agreement between this previous model and our present measurements of breakdown with X-band frequencies and repetitive 3 mu s pulses. (C) 2008 American Institute of Physics.
C1 [Herring, G. C.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Popovic, S.] Old Dominion Univ, Dept Phys, Norfolk, VA 23529 USA.
RP Herring, GC (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM gregory.c.herring@nasa.gov
NR 11
TC 4
Z9 5
U1 0
U2 1
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0003-6951
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD MAR 31
PY 2008
VL 92
IS 13
AR 131501
DI 10.1063/1.2897308
PG 3
WC Physics, Applied
SC Physics
GA 283XN
UT WOS:000254669900020
ER
PT J
AU Correira, J
Aikin, AC
Grebowsky, JM
Pesnell, WD
Burrows, JP
AF Correira, J.
Aikin, A. C.
Grebowsky, J. M.
Pesnell, W. D.
Burrows, J. P.
TI Seasonal variations of magnesium atoms in the mesosphere-thermosphere
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID UPPER-ATMOSPHERE; POTASSIUM LAYER; IONOSPHERE; MODEL; IRON; IONS; MG;
CHEMISTRY; ARECIBO; MIDDLE
AB UV radiances from the Global Ozone Monitoring Experiment (GOME) spectrometer on the ERS-2 satellite are used to determine long-term dayside temporal variations of the total vertical column density below 795 km of the meteoric metal species Mg and Mg+ in the upper atmosphere. The GOME instrument has the ability to observe the ground state transition lines of Mg I at 285.2 nm and resolve the Mg II at 280 nm. A retrieval algorithm has been developed to determine column densities and applied to the years 1996-1997. Results show the middle latitude dayside Mg+ peaks in total vertical content during the summer, while neutral Mg demonstrates a much more subtle maximum in summer. Dayside trends are opposite previous midlatitude nighttime lidar observations, with the exception of calcium. The Mg+/Mg ratio has a seasonal variation, reaching a maximum in the summer. The total content of Mg+ is twice that of neutral Mg.
C1 [Correira, J.; Aikin, A. C.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Grebowsky, J. M.; Pesnell, W. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Burrows, J. P.] Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany.
RP Correira, J (reprint author), Catholic Univ Amer, Dept Phys, 200 Hannan Hall,620 Michigan Ave NE, Washington, DC 20064 USA.
EM john.correira@gmail.com; aikin@comcast.net; joseph.m.grebowsky@nasa.gov;
william.d.pesnell@nasa.gov
RI Pesnell, William/D-1062-2012; Grebowsky, Joseph/I-7185-2013; Burrows,
John/B-6199-2014
OI Pesnell, William/0000-0002-8306-2500; Burrows, John/0000-0002-6821-5580
NR 34
TC 8
Z9 8
U1 0
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 29
PY 2008
VL 35
IS 6
AR L06103
DI 10.1029/2007GL033047
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 281XM
UT WOS:000254532200003
ER
PT J
AU Fan, CJ
Schulze-Makuch, D
Fairen, AG
Wolff, JA
AF Fan, Chaojun
Schulze-Makuch, Dirk
Fairen, Alberto G.
Wolff, John A.
TI A new hypothesis for the origin and redistribution of sulfates in the
equatorial region of western Mars
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MERIDIANI-PLANUM; OMEGA/MARS EXPRESS; MARTIAN CLIMATE; LANDING SITE;
SULFUR; SPECTROMETER; DEPOSITS; BASALT; OCEANS; CRATER
AB The formation of sulfates on Mars has been under debate since they were identified by several Mars missions starting from the 1970s. We propose that sulfates formed as evaporites in enclosed standing bodies of water in the Valles Marineris area following the early alteration of Martian basaltic crust, were then elevated by the Tharsis uplift, and transported together with rock materials to Meridiani Planum by periodic outbursts of water, where they were deposited as sediments. The proposed model comprehensively addresses all forms of sulfate occurrences near the equator in the western Martian hemisphere and relates it to physiographic processes (volcanic, tectonic and sedimentary) affecting the Martian surface.
C1 [Fan, Chaojun; Schulze-Makuch, Dirk; Wolff, John A.] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA.
[Fairen, Alberto G.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
RP Fan, CJ (reprint author), Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA.
EM cfan1@wsu.edu
RI Fan, Chaojun/A-9966-2010;
OI Schulze-Makuch, Dirk/0000-0002-1923-9746
NR 42
TC 8
Z9 8
U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 29
PY 2008
VL 35
IS 6
AR L06201
DI 10.1029/2007GL033079
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 281XM
UT WOS:000254532200004
ER
PT J
AU Ma, Q
Tipping, RH
Leforestier, C
AF Ma, Q.
Tipping, R. H.
Leforestier, C.
TI Temperature dependences of mechanisms responsible for the water-vapor
continuum absorption. I. Far wings of allowed lines
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID POTENTIAL FUNCTIONS; ROTATIONAL BANDS; LIQUID WATER; SHAPE THEORY; CM-1;
H2O; CO2; SPECTROSCOPY; REGION; ENERGY
AB It is well known that the water-vapor continuum plays an important role in the radiative balance in the Earth's atmosphere. This was first discovered by Elsasser almost 70 years ago, and since that time there has been a large body of work, both experimental and theoretical, on this topic. It has been experimentally shown that for ambient atmospheric conditions, the continuum absorption scales quadratically with the H(2)O number density and has a strong, negative temperature dependence (T dependence). Over the years, there have been three different theoretical mechanisms postulated: Far wings of allowed transitions, water dimers, and collision-induced absorption. Despite the improvements in experimental data, at present there is no consensus on which mechanism is primarily responsible for the absorption. The first mechanism proposed was the accumulation of the far-wing absorption of the strong allowed transitions. Later, absorption by water dimers was proposed and this mechanism provides a qualitative explanation for the strong, negative T dependence. Recently, some atmospheric modelers have proposed that collision-induced absorption is one of the major contributors. However, based on improvements in the theoretical calculation of accurate far-wing line shapes, ab initio dimer calculations, and theoretical collision-induced absorptions, it is now generally accepted that the dominant mechanism for the absorption in the infrared (IR) windows is that due to the far wings. Whether this is true for other spectral regions is not presently established. Although all these three mechanisms have a negative T dependence, their T dependences will be characterized by individual features. To analyze the characteristics of the latter will enable one to assess their roles with more certainty. In this paper, we present a detailed study of the T dependence of the far-wing absorption mechanism. We will then compare our theoretical calculations with the most recent and accurate experimental data in the IR windows. The results of our calculations are found to agree very well with measurements in the 800-1200 cm(-1) region. We conclude from this work that the T dependence in the IR window region predicted by the far-wing theory is negative and moderately strong. Its pattern is not simple and it could vary significantly as the frequency of interest varies. (C) 2008 American Institute of Physics.
C1 [Ma, Q.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Ma, Q.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA.
[Tipping, R. H.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Leforestier, C.] Univ Montpellier 2, CNRS, UMR, CC 1501, F-34095 Montpellier, France.
RP Ma, Q (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM qma@giss.nasa.gov
NR 38
TC 31
Z9 38
U1 1
U2 3
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-9606
J9 J CHEM PHYS
JI J. Chem. Phys.
PD MAR 28
PY 2008
VL 128
IS 12
AR 124313
DI 10.1063/1.2839604
PG 17
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 281ZK
UT WOS:000254537200026
PM 18376925
ER
PT J
AU Seo, KW
Wilson, CR
Han, SC
Waliser, DE
AF Seo, K. W.
Wilson, C. R.
Han, S. C.
Waliser, D. E.
TI Gravity Recovery and Climate Experiment (GRACE) alias error from ocean
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
ID GRAVIMETRY; TIDES; MODEL
AB Gravity Recovery and Climate Experiment (GRACE) is able to observe interannual and longer-period mass redistribution driven by climate changes. However, alias errors due to inaccurate ocean tide models may contaminate these signals. To quantify this problem, we estimate alias contamination due to expected errors in eight tidal constituents (Q(1), O-1, P-1, K-1, N-2, M-2, S-2, and K-2) for the period August 2002 to February 2006. Differences between GOT00.2 and TPXO6.2 tide models are used as estimates of tide model errors. The alias estimate is based on an approximate method employing least squares fits of spherical harmonics to potential differences between the two GRACE satellites. Results from this method are similar to previous estimates, confirming this is a useful and efficient way to study the alias problem. New findings are (1) the period of the M2 tide alias is about 140 d, much longer than the predicted period (13.5 d) because of monthly sampling of the 13.5-d period; (2) there are two alias periods for K1 (one about (0 d and one longer than 7 years); and (3) the slow decay in the GRACE orbit causes tide component aliases to differ from pure frequencies as the orbit evolves. We also find that aliases can contaminate in both space and time and thus may affect estimates of mass changes over land. Finally, we compare the simulated S2 alias with the estimated S2 alias in GRACE data. They are similar, but our approximate method appears to overestimate alias error over high-latitude oceans and along certain coastlines while underestimating error over low-latitude oceans.
C1 [Seo, K. W.; Waliser, D. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wilson, C. R.] Univ Texas Austin, Jackson Sch Geosci, Dept Geol Sci, Austin, TX 78712 USA.
[Han, S. C.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA.
RP Seo, KW (reprint author), Korea Polar Res Inst, 504 Get Pearl Tower, Inchon 406840, South Korea.
RI Han, Shin-Chan/A-2022-2009
NR 20
TC 17
Z9 20
U1 1
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9313
EI 2169-9356
J9 J GEOPHYS RES-SOL EA
JI J. Geophys. Res.-Solid Earth
PD MAR 28
PY 2008
VL 113
IS B3
AR B03405
DI 10.1029/2006JB004747
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 281YF
UT WOS:000254534100001
ER
PT J
AU Gjerloev, JW
Hoffman, RA
Sigwarth, JB
Frank, LA
Baker, JBH
AF Gjerloev, J. W.
Hoffman, R. A.
Sigwarth, J. B.
Frank, L. A.
Baker, J. B. H.
TI Typical auroral substorm: A bifurcated oval
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID HEIGHT-INTEGRATED CONDUCTIVITY; UV; MORPHOLOGY; IMAGER; SYSTEM; SECTOR;
ARCS; DMSP
AB Utilizing global auroral images obtained by Polar Visible Imaging System Earth Camera, we have analyzed the UV emissions from 116 auroral substorms. The events selected were fairly isolated and had to expand from a localized onset. It was found that essentially all auroral events fulfilling these simple criteria expand into the Akasofu (1964) bulge-type aurora. Averaged auroral emission patterns were compiled for 11 time steps of the substorm covering 20 min prior to the onset until well into the recovery phase. This compilation required a three-step normalization technique, one temporal based on the expansion time and two spatial, magnetic local time and latitude. These average patterns were then fit to either a single or double Gaussian distribution in latitude for each of 24 magnetic local times. On the basis of this analysis we made the following conclusions. The normalization technique is highly efficient in maintaining the key features in the individual auroral emission patterns, even though the individual events varied significantly in intensity, size, position, and lifetime. Thus our normalization results quantitatively validate the Akasofu (1964) assumption that key auroral features exist in the bulge-type auroral substorm. After the substorm onset the auroral oval becomes clearly bifurcated consisting of two components: the oval aurora in the latitude range of the preonset oval and expanding primarily eastward postmidnight, and the bulge aurora, which emerges out of the oval, expanding poleward and both east and west in MLT. The oval aurora decay faster than the bulge emissions indicating that the decays have separate time constants. Owing to the pronounced difference in the spatiotemporal behavior of the two auroral components we suggest that their sources are quasi-independent.
C1 [Gjerloev, J. W.; Baker, J. B. H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Hoffman, R. A.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
[Sigwarth, J. B.] NASA, Goddard Space Flight Ctr, Div Off, Heliophys Div, Greenbelt, MD 20771 USA.
[Frank, L. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
RP Gjerloev, JW (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM jesper.gjerloev@jhuapl.edu
NR 33
TC 11
Z9 12
U1 1
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR 28
PY 2008
VL 113
IS A3
AR A03211
DI 10.1029/2007JA012431
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 281YI
UT WOS:000254534400001
ER
PT J
AU Araneda, JA
Marsch, E
Vinas, AF
AF Araneda, Jaime A.
Marsch, Eckart
Vinas, Adolfo F. -
TI Proton core heating and beam formation via parametrically unstable
Alfven-cyclotron waves
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID SOLAR-WIND; VELOCITY DISTRIBUTIONS; PLASMA
AB Vlasov theory and one-dimensional hybrid simulations are used to study the effects that compressible fluctuations driven by parametric instabilities Alfven-cyclotron waves have on proton velocity distributions. Field-aligned proton beams are generated during the saturation phase of the wave-particle interaction, with a drift speed which is slightly greater than the Alfven speed and is maintained until the end of the simulation. The main part of the distribution becomes anisotropic due to phase mixing as is typically observed in the velocity distributions measured in the fast solar wind. We identify the key instabilities and also find that, even in the parameter regime where fluid theory appears to be appropriate, strong kinetic effects still prevail.
C1 [Araneda, Jaime A.] Univ Concepcion, Dept Fis, Concepcion 4070386, Chile.
[Marsch, Eckart] Max Planck Inst, Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Vinas, Adolfo F. -] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Araneda, JA (reprint author), Univ Concepcion, Dept Fis, Concepcion 4070386, Chile.
EM jaraneda@udec.cl
RI Araneda, Jaime/J-9245-2015
NR 28
TC 88
Z9 88
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 MAR 28
PY 2008
VL 100
IS 12
AR 125003
DI 10.1103/PhysRevLett.100.125003
PG 4
WC Physics, Multidisciplinary
SC Physics
GA 281CK
UT WOS:000254473800038
PM 18517877
ER
PT J
AU Dyudina, UA
Ingersoll, AP
Ewald, SP
Vasavada, AR
West, RA
Del Genio, AD
Barbara, JM
Porco, CC
Achterberg, RK
Flasar, FM
Simon-Miller, AA
Fletcher, LN
AF Dyudina, Ulyana A.
Ingersoll, Andrew P.
Ewald, Shawn P.
Vasavada, Ashwin R.
West, Robert A.
Del Genio, Anthony D.
Barbara, John M.
Porco, Carolyn C.
Achterberg, Richard K.
Flasar, F. Michael
Simon-Miller, Amy A.
Fletcher, Leigh N.
TI Dynamics of Saturn's south polar vortex
SO SCIENCE
LA English
DT Article
C1 [Dyudina, Ulyana A.; Ingersoll, Andrew P.; Ewald, Shawn P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Vasavada, Ashwin R.; West, Robert A.; Fletcher, Leigh N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Del Genio, Anthony D.; Barbara, John M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Porco, Carolyn C.] Space Sci Inst, Boulder, CO 80301 USA.
[Achterberg, Richard K.; Flasar, F. Michael; Simon-Miller, Amy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fletcher, Leigh N.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England.
RP Dyudina, UA (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM ulyana@gps.caltech.edu
RI Fletcher, Leigh/D-6093-2011; Flasar, F Michael/C-8509-2012; Del Genio,
Anthony/D-4663-2012; Simon, Amy/C-8020-2012
OI Fletcher, Leigh/0000-0001-5834-9588; Del Genio,
Anthony/0000-0001-7450-1359; Simon, Amy/0000-0003-4641-6186
NR 5
TC 19
Z9 19
U1 1
U2 4
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD MAR 28
PY 2008
VL 319
IS 5871
BP 1801
EP 1801
DI 10.1126/science.1153633
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 279ZF
UT WOS:000254394000039
PM 18369142
ER
PT J
AU Gavriil, FP
Gonzalez, ME
Gotthelf, EV
Kaspi, VM
Livingstone, MA
Woods, PM
AF Gavriil, F. P.
Gonzalez, M. E.
Gotthelf, E. V.
Kaspi, V. M.
Livingstone, M. A.
Woods, P. M.
TI Magnetar-like emission from the young pulsar in Kes 75
SO SCIENCE
LA English
DT Article
ID X-RAY PULSAR; SOFT GAMMA-REPEATERS; TRANSIENT MAGNETAR; XTE J1810-197;
RADIO PULSARS; NEUTRON-STARS; SPIN-DOWN; BURSTS; FIELD; 1E-1048.1-5937
AB We report the detection of magnetar- like x- ray bursts from the young pulsar PSR J1846- 0258, at the center of the supernova remnant Kes 75. This pulsar, long thought to be exclusively rotation- powered, has an inferred surface dipolar magnetic field of 4.9 x 10(13) gauss, which is higher than those of the vast majority of rotation- powered pulsars, but lower than those of the approximately 12 previously identified magnetars. The bursts were accompanied by a sudden flux increase and an unprecedented change in timing behavior. These phenomena lower the magnetic and rotational thresholds associated with magnetar- like behavior and suggest that in neutron stars there exists a continuum of magnetic activity that increases with inferred magnetic field strength.
C1 [Gavriil, F. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gavriil, F. P.] Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA.
[Gonzalez, M. E.; Kaspi, V. M.; Livingstone, M. A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Gotthelf, E. V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Kaspi, V. M.; Woods, P. M.] Dynetics, Huntsville, AL 35806 USA.
[Woods, P. M.] Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
RP Gavriil, FP (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
EM fotis.p.gavriil@nasa.gov
NR 30
TC 113
Z9 113
U1 0
U2 1
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD MAR 28
PY 2008
VL 319
IS 5871
BP 1802
EP 1805
DI 10.1126/science.1153465
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 279ZF
UT WOS:000254394000040
PM 18292305
ER
PT J
AU Livesey, NJ
Filipiak, MJ
Froidevaux, L
Read, WG
Lambert, A
Santee, ML
Jiang, JH
Pumphrey, HC
Waters, JW
Cofield, RE
Cuddy, DT
Daffer, WH
Drouin, BJ
Fuller, RA
Jarnot, RF
Jiang, YB
Knosp, BW
Li, QB
Perun, VS
Schwartz, MJ
Snyder, WV
Stek, PC
Thurstans, RP
Wagner, PA
Avery, M
Browell, EV
Cammas, JP
Christensen, LE
Diskin, GS
Gao, RS
Jost, HJ
Loewenstein, M
Lopez, JD
Nedelec, P
Osterman, GB
Sachse, GW
Webster, CR
AF Livesey, N. J.
Filipiak, M. J.
Froidevaux, L.
Read, W. G.
Lambert, A.
Santee, M. L.
Jiang, J. H.
Pumphrey, H. C.
Waters, J. W.
Cofield, R. E.
Cuddy, D. T.
Daffer, W. H.
Drouin, B. J.
Fuller, R. A.
Jarnot, R. F.
Jiang, Y. B.
Knosp, B. W.
Li, Q. B.
Perun, V. S.
Schwartz, M. J.
Snyder, W. V.
Stek, P. C.
Thurstans, R. P.
Wagner, P. A.
Avery, M.
Browell, E. V.
Cammas, J. -P.
Christensen, L. E.
Diskin, G. S.
Gao, R. -S.
Jost, H. -J.
Loewenstein, M.
Lopez, J. D.
Nedelec, P.
Osterman, G. B.
Sachse, G. W.
Webster, C. R.
TI Validation of Aura Microwave Limb Sounder O-3 and CO observations in the
upper troposphere and lower stratosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID MOZAIC AIRBORNE PROGRAM; DIAL MEASUREMENTS; WATER-VAPOR; EOS MLS; OZONE;
TRANSPORT; AIRCRAFT; AIR; RETRIEVAL; SATELLITE
AB Global satellite observations of ozone and carbon monoxide from the Microwave Limb Sounder (MLS) on the EOS Aura spacecraft are discussed with emphasis on those observations in the 215-100 hPa region (the upper troposphere and lower stratosphere). The precision, resolution and accuracy of the data produced by the MLS "version 2.2'' processing algorithms are discussed and quantified. O-3 accuracy is estimated at similar to 40 ppbv + 5% (similar to 20 ppbv + 20% at 215 hPa) while the CO accuracy is estimated at similar to 30 ppbv + 30% for pressures of 147 hPa and less. Comparisons with expectations and other observations show good agreements for the O3 product, generally consistent with the systematic errors quoted above. In the case of CO, a persistent factor of similar to 2 high bias is seen at 215 hPa. However, the morphology is shown to be realistic, consistent with raw MLS radiance data, and useful for scientific study. The MLS CO data at higher altitudes are shown to be consistent with other observations.
C1 [Livesey, N. J.; Froidevaux, L.; Read, W. G.; Lambert, A.; Santee, M. L.; Jiang, J. H.; Waters, J. W.; Cofield, R. E.; Cuddy, D. T.; Daffer, W. H.; Drouin, B. J.; Fuller, R. A.; Jarnot, R. F.; Jiang, Y. B.; Knosp, B. W.; Li, Q. B.; Perun, V. S.; Schwartz, M. J.; Snyder, W. V.; Stek, P. C.; Thurstans, R. P.; Wagner, P. A.; Christensen, L. E.; Osterman, G. B.; Webster, C. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Filipiak, M. J.; Pumphrey, H. C.] Univ Edinburgh, Sch Geosci, Edinburgh EH8 9YL, Midlothian, Scotland.
[Avery, M.; Browell, E. V.; Diskin, G. S.; Sachse, G. W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Cammas, J. -P.; Nedelec, P.] CNRS, UMR5560, Lab Aerol, F-31400 Toulouse, France.
[Gao, R. -S.] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Jost, H. -J.] Novawave Technol, Redwood City, CA 94065 USA.
[Loewenstein, M.; Lopez, J. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Livesey, NJ (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-701, Pasadena, CA 91109 USA.
EM nathaniel.j.livesey@jpl.nasa.gov
RI Gao, Ru-Shan/H-7455-2013; Schwartz, Michael/F-5172-2016; Manager, CSD
Publications/B-2789-2015
OI Schwartz, Michael/0000-0001-6169-5094;
NR 35
TC 122
Z9 124
U1 2
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 27
PY 2008
VL 113
IS D15
AR D15S02
DI 10.1029/2007JD008805
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 281XS
UT WOS:000254532800001
ER
PT J
AU Tzortziou, M
Krotkov, NA
Cede, A
Herman, JR
Vasilkov, A
AF Tzortziou, Maria
Krotkov, Nickolay A.
Cede, Alexander
Herman, Jay R.
Vasilkov, Alexander
TI A new technique for retrieval of tropospheric and stratospheric ozone
profiles using sky radiance measurements at multiple view angles:
Application to a Brewer spectrometer
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID AEROSOL OPTICAL DEPTH; SHADOW-BAND RADIOMETER; DOBSON
SPECTROPHOTOMETERS; O-3 PROFILES; RADIATIVE-TRANSFER; SATELLITE DATA; UV
IRRADIANCE; LIDAR; GOME; VARIABILITY
AB This paper describes and applies a new technique for retrieving diurnal variability in tropospheric ozone vertical distribution using ground-based measurements of ultraviolet sky radiances. The measured radiances are obtained by a polarization-insensitive modified Brewer double spectrometer located at Goddard Space Flight Center, in Greenbelt, Maryland, USA. Results demonstrate that the Brewer angular (0-72 degrees viewing zenith angle) and spectral (303-320 nm) measurements of sky radiance in the solar principal plane provide sufficient information to derive tropospheric ozone diurnal variability. In addition, the Brewer measurements provide stratospheric ozone vertical distributions at least twice per day near sunrise and sunset. Frequent measurements of total column ozone amounts from direct-sun observations are used as constraints in the retrieval. The vertical ozone profile resolution is shown in terms of averaging kernels to yield at least four points in the troposphere-low stratosphere, including good information in Umkehr layer 0 (0-5 km). The focus of this paper is on the derivation of stratospheric and tropospheric ozone profiles using both simulated and measured radiances. We briefly discuss the necessary modifications of the Brewer spectrometer that were used to eliminate instrumental polarization sensitivity so that accurate sky radiances can be obtained in the presence of strong Rayleigh scattering and aerosols. The results demonstrate that including a site-specific and time-dependent aerosol correction, based on Brewer direct-sun observations of aerosol optical thickness, is critical to minimize the sky radiance residuals as a function of observing angle in the optimal estimation inversion algorithm and improve the accuracy of the retrieved ozone profile.
C1 [Tzortziou, Maria; Cede, Alexander] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Tzortziou, Maria; Krotkov, Nickolay A.; Cede, Alexander; Herman, Jay R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Krotkov, Nickolay A.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA.
[Vasilkov, Alexander] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Tzortziou, M (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
EM maria.a.tzortziou@nasa.gov
RI Krotkov, Nickolay/E-1541-2012;
OI Krotkov, Nickolay/0000-0001-6170-6750; Herman, Jay/0000-0002-9146-1632
NR 49
TC 3
Z9 3
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 27
PY 2008
VL 113
IS D6
AR D06304
DI 10.1029/2007JD009093
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 281XP
UT WOS:000254532500001
ER
PT J
AU Davila, AF
Gomez-Silva, B
de los Rios, A
Ascaso, C
Olivares, H
Mckay, CP
Wierzchos, J
AF Davila, Alfonso F.
Gomez-Silva, Benito
de los Rios, Asuncion
Ascaso, Carmen
Olivares, Hector
Mckay, Christopher P.
Wierzchos, Jacek
TI Facilitation of endolithic microbial survival in the hyperarid core of
the Atacama Desert by mineral deliquescence
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Article
ID WATER RELATIONS; PHOTOSYNTHESIS; MARS; CHROOCOCCIDIOPSIS; METEORITES;
CHILE; LIFE
AB The hyperarid core of the Atacama Desert is considered the dry limit for life on Earth. Soils in this region have very low abundance of heterotrophic bacteria and are practically barren of photosynthetic microorganisms because of the extreme dry conditions (<= 2 mm a(-1) rainfall). However, relatively abundant endolithic communities of cyanobacteria (Chroococcidiopsis) occur within halite crusts in paleolake evaporitic deposits. By means of continuous monitoring of the microclimate conditions ( temperature, relative humidity, water vapor density, wetness, and photosynthetically active radiation) inside and around the halite crusts, we demonstrate here that water vapor condenses within the pore space of the halite at relative humidity ( RH) levels that otherwise hinder the occurrence of liquid water in the surrounding environment. Water condensation occurs at RH > 75%, which corresponds to the deliquescence point of halite. We have estimated a total of 57 deliquescence events (i.e., water condensation) within the halite crusts, as opposed to only 1 liquid water event outside. These wet events resulted in a total of 213.8 h of potential photosynthetic activity for the endolithic microorganisms versus only 6 h for organisms outside the halite crusts. Halite crusts may therefore represent the last available niche for photosynthetic activity in extreme arid environments on Earth.
C1 [Davila, Alfonso F.; Mckay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Gomez-Silva, Benito; Olivares, Hector] Univ Antofagasta, Dept Biomed, Antofagasta, Chile.
[Gomez-Silva, Benito; Olivares, Hector] Univ Antofagasta, Inst Desierto, Antofagasta, Chile.
[de los Rios, Asuncion; Ascaso, Carmen] CSIC, CCMA, Inst Recursos Nat, E-28006 Madrid, Spain.
[Wierzchos, Jacek] Univ Lleida, Serv Microscopia Elect, E-25198 Lleida, Spain.
RP Davila, AF (reprint author), NASA, Ames Res Ctr, MS 245-3,Moffett Field, Moffett Field, CA 94035 USA.
EM alfonso.fernandez-davila-1@nasa.gov
RI Wierzchos, Jacek/F-7036-2011; Ascaso, Carmen/F-5369-2011; Davila,
Alfonso/A-2198-2013; de los Rios, Asuncion/L-3694-2014
OI Wierzchos, Jacek/0000-0003-3084-3837; Ascaso,
Carmen/0000-0001-9665-193X; Davila, Alfonso/0000-0002-0977-9909; de los
Rios, Asuncion/0000-0002-0266-3516
NR 21
TC 61
Z9 62
U1 4
U2 30
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-BIOGEO
JI J. Geophys. Res.-Biogeosci.
PD MAR 27
PY 2008
VL 113
IS G1
AR G01028
DI 10.1029/2007JG000561
PG 9
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 281XU
UT WOS:000254533000001
ER
PT J
AU Styers-Barnett, DJ
Ellison, SP
Mehl, BP
Westlake, BC
House, RL
Park, C
Wise, KE
Papanikolas, JM
AF Styers-Barnett, David J.
Ellison, Stephen P.
Mehl, Brian P.
Westlake, Brittany C.
House, Ralph L.
Park, Cheol
Wise, Kristopher E.
Papanikolas, John M.
TI Exciton dynamics and biexciton formation in single-walled carbon
nanotubes studied with femtosecond transient absorption spectroscopy
SO JOURNAL OF PHYSICAL CHEMISTRY C
LA English
DT Article
ID SEMICONDUCTOR QUANTUM DOTS; OPTICAL SPECTROSCOPY; ULTRAFAST RELAXATION;
CARRIER DYNAMICS; RAMAN-SCATTERING; POLYMER; STATES; MOLECULES;
CHEMISTRY; KINETICS
AB We used femtosecond transient absorption (TA) spectroscopy to examine the excited state dynamics of single-walled carbon nanotube (SWNT) bundles embedded in polymer matrices. The SWNTs were excited by a femtosecond pump pulse centered at either 1800, 900, or 550 nm and probed using a white-light continuum extending from 400 to 750 nm. We observed a structured TA spectrum consisting of a series of narrow induced transmission (IT) and induced absorption (IA) bands. The TA spectrum, which is independent of excitation wavelength, appeared on a time scale shorter than our instrument response (200 fs) and persisted for up to 100 ps. TA spectra obtained at a series of pump-probe delay times provided a window through which to monitor the exciton dynamics. We observed three distinct spectral signatures in the time-dependent data: (1) the decay of a broad photobleach, (2) the biphasic decay of narrow IT and IA features, and (3) a dynamical spectral shift of IA bands. These processes were attributed to plasmon relaxation, electron-hole recombination, and lattice relaxation associated with exciton self-trapping, respectively. Analysis of the transient spectrum suggested that it arose from a nonlinear optical response of the SWNT, where excitons produced by the pump pulse modified the transition frequencies of subsequent carrier excitations. The result was a series of IT bands (bleaches) at the ground state absorption frequencies, and associated with each was a corresponding red-shifted absorption band. These induced absorptions were attributed to the formation of biexcitons, four-particle excitations that are produced through the sequential excitation of two closely spaced electron-hole pairs.
C1 [Styers-Barnett, David J.; Ellison, Stephen P.; Mehl, Brian P.; Westlake, Brittany C.; House, Ralph L.; Papanikolas, John M.] Univ N Carolina, Dept Chem, Venable & Kenan Labs, Chapel Hill, NC 27599 USA.
[Park, Cheol; Wise, Kristopher E.] NASA, Langley Res Ctr, Natl Inst Aerosp, Hampton, VA 23681 USA.
RP Papanikolas, JM (reprint author), Univ N Carolina, Dept Chem, Venable & Kenan Labs, CB 3290, Chapel Hill, NC 27599 USA.
EM John_Papanikolas@unc.edu
NR 86
TC 32
Z9 33
U1 3
U2 44
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1932-7447
J9 J PHYS CHEM C
JI J. Phys. Chem. C
PD MAR 27
PY 2008
VL 112
IS 12
BP 4507
EP 4516
DI 10.1021/jp7099256
PG 10
WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science,
Multidisciplinary
SC Chemistry; Science & Technology - Other Topics; Materials Science
GA 290FM
UT WOS:000255108700014
ER
PT J
AU Bhushan, B
Galasso, B
Bignardi, C
Nguyen, CV
Dai, LM
Qu, LT
AF Bhushan, Bharat
Galasso, Barbara
Bignardi, Cristina
Nguyen, Cattien V.
Dai, Liming
Qu, Liangti
TI Adhesion, friction and wear on the nanoscale of MWNT tips and SWNT and
MWNT arrays
SO NANOTECHNOLOGY
LA English
DT Article
ID SCANNING PROBE MICROSCOPY; CARBON NANOTUBE FILMS; CERAMIC-MATRIX
NANOCOMPOSITES; ATOMIC-FORCE MICROSCOPY; FIELD-EMISSION; TRIBOLOGICAL
PROPERTIES; POLYMER COMPOSITES; LATERAL RESOLUTION; AFM PROBES;
FABRICATION
AB The nanotribological characterization of carbon nanotubes is fundamental for the exploration of new sliding applications. In this study, a comprehensive investigation of adhesion, friction and wear of a multiwalled nanotube (MWNT) tip, and SWNT (single-walled nanotube) and MWNT arrays has been carried out. A nonlinear response of the MWNT tip is observed when the tip is brought into and out of contact with various surfaces. A nonlinear response occurs due to the buckling of the nanotube and its subsequent sliding on the surface. In addition to the role of surface chemistry, it can also explain the relatively high value of the coefficient of friction obtained on different surfaces, as compared to that of Si and Si(3)N(4) tips. The adhesion and friction studies carried out on SWNT and MWNT arrays using Si tips show that SWNT arrays, compared to MWNT arrays, exhibit lower values, possibly due to lower van der Waals forces as a result of lower packing density and higher flexibility. The wear tests conducted with the MWNT tip and a Si tip on a gold film, at two normal loads, show less damage of the surface when the MWNT tip is used because of the MWNT acting as a compliant spring, absorbing part of the load. Wear tests conducted with a Si tip on SWNT and MWNT arrays show that the arrays do not wear. The tip wear and the friction force in the SWNT array are lower, because of lower adhesion and higher flexibility of the SWNTs, which causes less opposition to the motion of the tip.
C1 [Bhushan, Bharat] Ohio State Univ, Nanotribol Lab Informat Storage, Columbus, OH 43210 USA.
[Bhushan, Bharat] Ohio State Univ, MEMS NEMS, Columbus, OH 43210 USA.
[Galasso, Barbara; Bignardi, Cristina] Politecn Torino, Dipartimento Meccan, I-10129 Turin, Italy.
[Nguyen, Cattien V.] NASA, Ames Res Ctr, ELORET, Moffett Field, CA 94035 USA.
[Dai, Liming; Qu, Liangti] Univ Dayton, Res Inst, Dept Chem & Mat Engn, Dayton, OH 45469 USA.
RP Bhushan, B (reprint author), Ohio State Univ, Nanotribol Lab Informat Storage, 201 W 19th Ave, Columbus, OH 43210 USA.
RI Bhushan, Bharat/A-9684-2013
OI Bhushan, Bharat/0000-0001-7161-6601
NR 69
TC 13
Z9 13
U1 4
U2 16
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
J9 NANOTECHNOLOGY
JI Nanotechnology
PD MAR 26
PY 2008
VL 19
IS 12
AR 125702
DI 10.1088/0957-4484/19/12/125702
PG 10
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 276WK
UT WOS:000254174200024
PM 21817743
ER
PT J
AU Ho, CM
Morabito, DD
Woo, R
AF Ho, C. M.
Morabito, D. D.
Woo, R.
TI Solar corona effects on angle of arrival fluctuations for microwave
telecommunication links during superior solar conjunction
SO RADIO SCIENCE
LA English
DT Article
AB During the superior solar conjunction of spacecraft, the transmitted signals from a spacecraft to the Earth ground station graze the region near the Sun's photospheric surface, passing through dense and turbulent regions of solar-charged particles. Phase changes due to solar coronal irregularities cause raypath wandering, wavefront tilting, and fluctuations in the apparent angle of arrival when observed from the Earth. This study presents a first theoretical investigation of solar wind and solar coronal effects on the angle of arrival fluctuations for RF signals. On the basis of the Chandrasekhar relationship between phase and angular fluctuations, an analytical integrating solution for angle of arrival fluctuations is derived by applying solar corona and plasma irregularity spectrum models. It is found that angular fluctuations rapidly decrease with increasing heliocentric distance at a rate of similar to r(-5.5) and also decrease with increasing frequency at a rate of similar to 1/f(2). It is found that when using K(a) band at alpha = 0.4 degrees (r = 1.6 solar radii), there is a 19 millidegrees (mdeg) angular scattering, corresponding to a 9 dB gain degradation. In comparison, lower-frequency X and S band signals undergo much worse degradation effects. Beyond alpha = 2 degrees (r > 8 solar radii), angular fluctuations at microwave frequency bands can almost be neglected (theta(RMS) < 1 mdeg). A solution to minimize this degradation is to use K(a)- or higher-frequency bands for the telecommunication link during periods of solar conjunction. This study not only quantifies the angular fluctuations caused by solar corona irregularities but also provides an effective method for diagnosing the plasma density fluctuations in a region very close to the solar photospheric surface.
C1 [Ho, C. M.; Morabito, D. D.; Woo, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ho, CM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM cmho@mail.jpl.nasa.gov
NR 16
TC 2
Z9 2
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 MAR 26
PY 2008
VL 43
IS 2
AR RS2003
DI 10.1029/2007RS003620
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 281YM
UT WOS:000254534800001
ER
PT J
AU Anderson, MS
AF Anderson, Mark S.
TI Nearfield surface enhanced spectroscopy using targeted nanoparticle
deposition
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID ATOMIC-FORCE MICROSCOPE; RAMAN-SCATTERING; FIELD
AB Surface enhanced spectroscopy is demonstrated by depositing gold nanoparticles on a surface using an atomic force microscope. A modified dip pen nanolithography process is used to place particles directly on to a target. Near-field optical enhancement is demonstrated for Raman and infrared spectroscopies and is applicable for fluorescence spectroscopy. This approach provides localized, near-field spectroscopy with subdiffraction limit resolution and a general method for fabricating plasmonic device structures. (C) 2008 American Institute of Physics.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Anderson, MS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM mark.s.anderson@jpl.nasa.gov
NR 16
TC 13
Z9 13
U1 0
U2 5
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0003-6951
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD MAR 24
PY 2008
VL 92
IS 12
AR 123101
DI 10.1063/1.2891085
PG 3
WC Physics, Applied
SC Physics
GA 281PJ
UT WOS:000254510300072
ER
PT J
AU Hubbard, SM
Cress, CD
Bailey, CG
Raffaelle, RP
Bailey, SG
Wilt, DM
AF Hubbard, S. M.
Cress, C. D.
Bailey, C. G.
Raffaelle, R. P.
Bailey, S. G.
Wilt, D. M.
TI Effect of strain compensation on quantum dot enhanced GaAs solar cells
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID INTERMEDIATE BAND
AB GaP tensile strain compensation ( SC ) layers were introduced into GaAs solar cells enhanced with a five layer stack of InAs quantum dots (QDs ). One sun air mass zero illuminated current- voltage curves show that SC results in improved conversion efficiency and reduced dark current. The strain compensated QD solar cell shows a slight increase in short circuit current compared to a baseline GaAs cell due to sub- GaAs bandgap absorption by the InAs QD. Quantum efficiency and electroluminescence were also measured and provide further insight to the improvements due to SC. (C) 2008 American Institute of Physics.
C1 [Hubbard, S. M.; Cress, C. D.; Bailey, C. G.; Raffaelle, R. P.] Rochester Inst Technol, Nanopower Res Lab, Dept Phys, Rochester, NY 14623 USA.
[Bailey, S. G.; Wilt, D. M.] NASA, Glenn Res Ctr, Photovolta & Power Technol Branch, Cleveland, OH 44135 USA.
RP Hubbard, SM (reprint author), Rochester Inst Technol, Nanopower Res Lab, Dept Phys, 85 Lomb Mem Dr, Rochester, NY 14623 USA.
EM smhsps@rit.edu
RI Cress, Cory/A-8673-2009;
OI Cress, Cory/0000-0001-7563-6693
NR 19
TC 228
Z9 228
U1 6
U2 64
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0003-6951
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD MAR 24
PY 2008
VL 92
IS 12
AR 123512
DI 10.1063/1.2903699
PG 3
WC Physics, Applied
SC Physics
GA 281PJ
UT WOS:000254510300099
ER
PT J
AU Kumar, S
Gao, J
Zmuidzinas, J
Mazin, BA
Leduc, HG
Day, PK
AF Kumar, Shwetank
Gao, Jiansong
Zmuidzinas, Jonas
Mazin, Benjamin A.
LeDuc, Henry G.
Day, Peter K.
TI Temperature dependence of the frequency and noise of superconducting
coplanar waveguide resonators
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID KINETIC INDUCTANCE DETECTORS; MICROWAVE SQUID MULTIPLEXER; PHOTON;
CAVITY; QUBIT
AB We present measurements of the temperature and power dependence of the resonance frequency and frequency noise of superconducting niobium thin-film coplanar waveguide resonators carried out at temperatures well below the superconducting transition (T-c=9.2 K). The noise decreases by nearly two orders of magnitude as the temperature is increased from 120 to 1200 mK, while the variation of the resonance frequency with temperature over this range agrees well with the standard two-level system (TLS) model for amorphous dielectrics. These results support the hypothesis that TLSs are responsible for the noise in superconducting microresonators and have important implications for resonator applications such as qubits and photon detectors. (C) 2008 American Institute of Physics.
C1 [Kumar, Shwetank; Gao, Jiansong; Zmuidzinas, Jonas; Mazin, Benjamin A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[LeDuc, Henry G.; Day, Peter K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kumar, S (reprint author), CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
EM jonas@caltech.edu
RI Mazin, Ben/B-8704-2011
OI Mazin, Ben/0000-0003-0526-1114
NR 28
TC 35
Z9 35
U1 1
U2 10
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0003-6951
EI 1077-3118
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD MAR 24
PY 2008
VL 92
IS 12
AR 123503
DI 10.1063/1.2894584
PG 3
WC Physics, Applied
SC Physics
GA 281PJ
UT WOS:000254510300090
ER
PT J
AU Vallisneri, M
Crowder, J
Tinto, M
AF Vallisneri, Michele
Crowder, Jeff
Tinto, Massimo
TI Sensitivity and parameter-estimation precision for alternate LISA
configurations
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
AB We describe a simple framework to assess the LISA scientific performance (more specifically, its sensitivity and expected parameter-estimation precision for prescribed gravitational-wave signals) under the assumption of failure of one or two inter-spacecraft laser measurements (links) and of one to four intra-spacecraft laser measurements. We apply the framework to the simple case of measuring the LISA sensitivity to monochromatic circular binaries, and the LISA parameter-estimation precision for the gravitational-wave polarization angle of these systems. Compared to the six-link baseline configuration, the five-link case is characterized by a small loss in signal-to-noise ratio (SNR) in the high-frequency section of the LISA band; the four-link case shows a reduction by a factor of root 2 at low frequencies, and by up to similar to 2 at high frequencies. The uncertainty in the estimate of polarization, as computed in the Fisher-matrix formalism, also worsens when moving from six to five, and then to four links: this can be explained by the reduced SNR available in those configurations (except for observations shorter than three months, where five and six links do better than four even with the same SNR). In addition, we prove (for generic signals) that the SNR and Fisher matrix are invariant with respect to the choice of a basis of TDI observables; rather, they depend only on which inter-spacecraft and intra-spacecraft measurements are available.
C1 [Vallisneri, Michele; Crowder, Jeff; Tinto, Massimo] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Vallisneri, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Michele.Vallisneri@jpl.nasa.gov
NR 24
TC 12
Z9 12
U1 1
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 MAR 21
PY 2008
VL 25
IS 6
AR 065005
DI 10.1088/0264-9381/25/6/065005
PG 17
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA 276OA
UT WOS:000254150700006
ER
PT J
AU Ajello, JM
Gustin, J
Stewart, I
Larsen, K
Esposito, L
Pryor, W
McClintock, W
Stevens, MH
Malone, CP
Dziczek, D
AF Ajello, Joseph M.
Gustin, Jacques
Stewart, Ian
Larsen, Kristopher
Esposito, Larry
Pryor, Wayne
McClintock, William
Stevens, Michael H.
Malone, Charles P.
Dziczek, Dariusz
TI Titan airglow spectra from the Cassini Ultraviolet Imaging Spectrograph:
FUV disk analysis
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ELECTRON-IMPACT; INFRARED OBSERVATIONS; VOYAGER-1 ENCOUNTER; EUV
EMISSION; ATMOSPHERE; SYSTEM
AB We present a spectral analysis of the far ultraviolet (FUV: 1150-1900 angstrom) disk airglow observations of Titan's atmosphere by the Cassini Ultraviolet Imaging Spectrograph (UVIS). The FUV spectrum consists of emissions from the Lyman-Birge-Hopfield (LBH) band system of N-2 excited by photoelectrons (a (1)Pi(g) -> X (1)Sigma(+)(g)), N I multiplets from solar photodissociative excitation of N-2, resonantly scattered solar H Ly-alpha and sunlight reflected by N-2 in the mesosphere-stratosphere and modified by aerosols (e. g., tholins) and hydrocarbon absorption. Below 1450 angstrom, the strongest emissions arise from H Ly-a with an intensity of 208 Rayleighs (R), LBH bands with an intensity of 43 R, and the N I multiplets with a combined intensity of 16 R. Above 1450 angstrom, most of the UVIS signal is due to reflected sunlight. Mixing ratios of tholins, C2H2, C2H4 and C4H2 have been derived from the reflected sunlight using a Rayleigh scattering model. The derived mixing ratios are in good agreement with Voyager infrared observations and with FUV photochemical models, assuming solar energy deposition above 1450 angstrom occurs near 250 km (Wilson and Atreya, 2004). We also present the first geometric albedo measurement of Titan from 1500-1900 angstrom.
C1 [Ajello, Joseph M.; Malone, Charles P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dziczek, Dariusz] Nicholas Copernicus Univ, PL-87100 Torun, Poland.
[Gustin, Jacques; Stewart, Ian; Larsen, Kristopher; Esposito, Larry; McClintock, William] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA.
[Pryor, Wayne] Cent Arizona Coll, Dept Sci, Coolidge, AZ 85228 USA.
[Stevens, Michael H.] Natl Res Lab, Space Sci Div, Washington, DC 20375 USA.
RP Ajello, JM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM joseph.m.ajello@jpl.nasa.gov
RI Malone, Charles/A-6294-2010; Dziczek, Dariusz/G-3620-2014;
OI Malone, Charles/0000-0001-8418-1539; Stevens,
Michael/0000-0003-1082-8955
NR 26
TC 28
Z9 28
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 21
PY 2008
VL 35
IS 6
AR L06102
DI 10.1029/2007GL032315
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 281TO
UT WOS:000254522000002
ER
PT J
AU Ajello, JM
Aguilar, A
Mangina, RS
James, GK
Geissler, P
Trafton, L
AF Ajello, Joseph M.
Aguilar, Alejandro
Mangina, Rao S.
James, Geoffrey K.
Geissler, Paul
Trafton, Laurence
TI Middle UV to near-IR spectrum of electron-excited SO2
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID ULTRAVIOLET IMAGING SPECTROSCOPY; CROSS-SECTIONS; IOS ATMOSPHERE; ATOMIC
OXYGEN; O-I; IMPACT; EMISSION; EXCITATION; MODEL; HYDROGEN
AB We investigated the electron impact-induced fluorescence spectrum of SO2 to provide excitation cross sections for modeling Io's emission spectrum and analyzing Cassini Imaging Science Subsystem observations. The electron-excited middle-ultraviolet visible optical near-infrared (VOIR) emission spectrum of SO2 gas was generated in the laboratory and studied from 2000 to 11,000 angstrom at a resolution of Delta lambda similar to 2.5 angstrom full width at half maximum (FWHM). The VOIR laboratory spectrum longward of 6000 angstrom consists entirely of S I, II and O I, II multiplets for electron impact energies above similar to 15 eV. Between 2000 and 6000 angstrom, we find previously identified molecular bands from both SO and SO2. This work represents a significant improvement in spectral resolution over our earlier work done at 18 angstrom FWHM. From a measurement of the medium-resolution spectrum, we provide detailed 25- and 100-eV emission cross sections for spectral features from 2000 to 11,000 angstrom. On the basis of these data, we suggest future ground-based and satellite telescopic observations in the VOIR that are of promise for understanding Io's atmosphere.
C1 [Ajello, Joseph M.; Aguilar, Alejandro; Mangina, Rao S.; James, Geoffrey K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Geissler, Paul] US Geol Survey, Flagstaff, AZ 86001 USA.
[Trafton, Laurence] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
RP Ajello, JM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM geoffrey.james@jpl.nasa.gov
NR 37
TC 4
Z9 4
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAR 21
PY 2008
VL 113
IS E3
AR E03002
DI 10.1029/2007JE002921
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 281VC
UT WOS:000254526000001
ER
PT J
AU Ziaeepour, H
Holland, ST
Boyd, PT
Page, K
Oates, S
Markwardt, CB
Meszaros, P
Gehrels, N
Marshall, FE
Cummings, J
Goad, M
AF Ziaeepour, Houri
Holland, Stephen T.
Boyd, Patricia T.
Page, Kim
Oates, Samantha
Markwardt, Craig B.
Meszaros, Peter
Gehrels, Neil
Marshall, Francis E.
Cummings, Jay
Goad, Mike
TI GRB 060607A: a gamma-ray burst with bright asynchronous early X-ray and
optical emissions
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE shock waves; gamma-rays : bursts
ID SWIFT XRT DATA; ULTRARELATIVISTIC SHOCKS; PARTICLE-ACCELERATION;
RELATIVISTIC SHOCKS; SPECTRAL EVOLUTION; WEIBEL INSTABILITY; AFTERGLOW
EMISSION; FERMI ACCELERATION; TEMPORAL STRUCTURE; ROBOTIC TELESCOPE
AB The early optical emission of the moderately high redshift (z = 3.08) GRB 060607A shows a remarkable broad and strong peak with a rapid rise and a relatively slow power-law decay. It is not coincident with the strong early-time flares seen in the X-ray and gamma-ray energy bands. There is weak evidence for variability superposed on this dominant component in several optical bands that can be related to flares in high-energy bands. While for a small number of gamma-ray bursts (GRBs), well-sampled optical flares have been observed simultaneously with X-ray and gamma-ray pulses, GRB 060607A is one of the few cases where the early optical emission shows no significant evidence for correlation with the prompt emission. In this work we first report in detail the broad-band observations of this burst by Swift. Then by applying a simple model for the dynamics and the synchrotron radiation of a relativistic shock, we show that the dominant component of the early emissions in optical wavelengths has the same origin as the tail emission produced after the main gamma-ray activity. The most plausible explanation for the peak in the optical light curve seems to be the cooling of the prompt after the main collisions, shifting the characteristic synchrotron frequency to the optical bands. The fact that the early emission in X-ray does not show a steep decay, like what is observed in many other GRBs, is further evidence for slow cooling of the prompt shell within this GRB. It seems that the cooling process requires a steepening of the electron energy distribution and/or a break in this distribution at high energies. From simultaneous gamma-ray emission during the first flare, the behaviour of hardness ratio, and the lack of spectral features, we conclude that the X-ray flares are due to the collision of late shells rather than late reprocessing of the central engine activities. The sharp break in the X-ray light curve at few thousands of seconds after the trigger, is not observed in the infrared/optical/ultraviolet bands, and therefore cannot be a jet break. Either the X-ray break is due to a change in the spectrum of the accelerated electrons or the lack of an optical break is due to the presence of a related delayed response component.
C1 [Ziaeepour, Houri; Oates, Samantha] Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Holland, Stephen T.; Gehrels, Neil] 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.; Marshall, Francis E.; Cummings, Jay] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Boyd, Patricia T.; Markwardt, Craig B.] NASA, Goddard Space Flight Ctr, Lab Astroparticle Phys, Greenbelt, MD 20771 USA.
[Page, Kim; Goad, Mike] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Meszaros, Peter] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
RP Ziaeepour, H (reprint author), Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
EM hz@mssl.ucl.ac.uk
RI Boyd, Patricia/D-3274-2012; Gehrels, Neil/D-2971-2012
NR 85
TC 18
Z9 18
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 21
PY 2008
VL 385
IS 1
BP 453
EP 467
DI 10.1111/j.1365-2966.2008.12859.x
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 287KR
UT WOS:000254916500036
ER
PT J
AU Rodgers, SD
Charnley, SB
AF Rodgers, S. D.
Charnley, S. B.
TI Nitrogen superfractionation in dense cloud cores
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE astrochemistry; molecular processes; meteors, meteoriods; ISM :
molecules
ID INTERPLANETARY DUST PARTICLES; ISOTOPIC COMPOSITION; INTERSTELLAR
CLOUDS; DISSOCIATIVE RECOMBINATION; GAS TEMPERATURE; ORGANIC-MATTER;
STAR-FORMATION; FRACTIONATION; METEORITES; ABUNDANCES
AB We report new calculations of interstellar N-15-fractionation. Previously, we have shown that large enhancements of N-15/N-14 can occur in cold, dense gas where CO is frozen out, but that the existence of an NH + N channel in the dissociative recombination of N2H+ severely curtails the fractionation. In the light of recent experimental evidence that this channel is in fact negligible, we have reassessed the N-15 chemistry in dense cloud cores. We consider the effects of temperatures below 10 K, and of the presence of large amounts of atomic nitrogen. We also show how the temporal evolution of gas-phase isotope ratios is preserved as spatial heterogeneity in ammonia ice mantles, as monolayers deposited at different times have different isotopic compositions. We demonstrate that the upper layers of this ice may have N-15/N-14 ratios an order of magnitude larger than the underlying elemental value. Converting our ratios to delta-values, we obtain delta N-15 > 3000% in the uppermost layer, with values as high as 10 000% in some models. We suggest that this material is the precursor to the N-15 'hotspots' recently discovered in meteorites and IDPs.
C1 NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA.
RP Rodgers, SD (reprint author), NASA, Ames Res Ctr, Div Space Sci & Astrobiol, MS 245-3, Moffett Field, CA 94035 USA.
EM rogers@dusty.arc.nasa.gov
RI Charnley, Steven/C-9538-2012
NR 37
TC 48
Z9 48
U1 0
U2 5
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 21
PY 2008
VL 385
IS 1
BP L48
EP L52
DI 10.1111/j.1745-3933.2008.00431.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 287KR
UT WOS:000254916500055
ER
PT J
AU Sotin, C
Tobie, G
AF Sotin, Christophe
Tobie, Gabriel
TI Planetary science - Titan's hidden ocean
SO SCIENCE
LA English
DT Editorial Material
C1 [Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tobie, Gabriel] Univ Nantes, Lab Planetol & Geodynam, F-44322 Nantes, France.
RP Sotin, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM csotin@jpl.nasa.gov; gabriel.tobie@univ-nantes.fr
NR 7
TC 12
Z9 13
U1 1
U2 4
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD MAR 21
PY 2008
VL 319
IS 5870
BP 1629
EP 1630
DI 10.1126/science.1155964
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 276VR
UT WOS:000254172300028
PM 18356514
ER
PT J
AU Lorenz, RD
Stiles, BW
Kirk, RL
Allison, MD
del Marmo, PP
Iess, L
Lunine, JI
Ostro, SJ
Hensley, S
AF Lorenz, Ralph D.
Stiles, Bryan W.
Kirk, Randolph L.
Allison, Michael D.
del Marmo, Paolo Persi
Iess, Luciano
Lunine, Jonathan I.
Ostro, Steven J.
Hensley, Scott
TI Titan's rotation reveals an internal ocean and changing zonal winds
SO SCIENCE
LA English
DT Article
ID GALILEAN SATELLITES; SURFACE
AB Cassini radar observations of Saturn's moon Titan over several years show that its rotational period is changing and is different from its orbital period. The present- day rotation period difference from synchronous spin leads to a shift of similar to 0.36 per year in apparent longitude and is consistent with seasonal exchange of angular momentum between the surface and Titan's dense superrotating atmosphere, but only if Titan's crust is decoupled from the core by an internal water ocean like that on Europa.
C1 [Lorenz, Ralph D.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA.
[Stiles, Bryan W.; Ostro, Steven J.; Hensley, Scott] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kirk, Randolph L.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Allison, Michael D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[del Marmo, Paolo Persi; Iess, Luciano] Univ Roma La Sapienza, I-00184 Rome, Italy.
[Lunine, Jonathan I.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
RP Lorenz, RD (reprint author), Johns Hopkins Univ, Appl Phys Lab, Dept Space, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM ralph.lorenz@jhuapl.edu
RI IESS, Luciano/F-4902-2011; Lorenz, Ralph/B-8759-2016
OI IESS, Luciano/0000-0002-6230-5825; Lorenz, Ralph/0000-0001-8528-4644
FU Intramural NIH HHS
NR 23
TC 114
Z9 116
U1 3
U2 12
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD MAR 21
PY 2008
VL 319
IS 5870
BP 1649
EP 1651
DI 10.1126/science.1151639
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 276VR
UT WOS:000254172300035
PM 18356521
ER
PT J
AU Reichle, RH
Crow, WT
Keppenne, CL
AF Reichle, Rolf H.
Crow, Wade T.
Keppenne, Christian L.
TI An adaptive ensemble Kalman filter for soil moisture data assimilation
SO WATER RESOURCES RESEARCH
LA English
DT Article
ID ERROR COVARIANCE PARAMETERS; LAND DATA ASSIMILATION; ALGORITHM; IMPACT
AB In a 19- year twin experiment for the Red- Arkansas river basin we assimilate synthetic surface soil moisture retrievals into the NASA Catchment land surface model. We demonstrate how poorly specified model and observation error parameters affect the quality of the assimilation products. In particular, soil moisture estimates from data assimilation are sensitive to observation and model error variances and, for very poor input error parameters, may even be worse than model estimates without data assimilation. Estimates of surface heat fluxes and runoff are at best marginally improved through the assimilation of surface soil moisture and tend to have large errors when the assimilation system operates with poor input error parameters. We present a computationally affordable, adaptive assimilation system that continually adjusts model and observation error parameters in response to internal diagnostics. The adaptive filter can identify model and observation error variances and provide generally improved assimilation estimates when compared to the non- adaptive system.
C1 [Reichle, Rolf H.; Keppenne, Christian L.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Crow, Wade T.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD USA.
[Reichle, Rolf H.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Keppenne, Christian L.] Sci Applicat Int Corp, Beltsville, MD USA.
RP Reichle, RH (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM rolf.reichle@nasa.gov
RI Reichle, Rolf/E-1419-2012
NR 33
TC 88
Z9 88
U1 2
U2 17
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 MAR 21
PY 2008
VL 44
IS 3
AR W03423
DI 10.1029/2007WR006357
PG 13
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 281WM
UT WOS:000254529600004
ER
PT J
AU Eriksen, HK
Jewell, JB
Dickinson, C
Banday, AJ
Gorski, KM
Lawrence, CR
AF Eriksen, H. K.
Jewell, J. B.
Dickinson, C.
Banday, A. J.
Gorski, K. M.
Lawrence, C. R.
TI Joint Bayesian component separation and CMB power spectrum estimation
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic microwave background; cosmology : observations; methods :
numerical
ID MICROWAVE BACKGROUND ANISOTROPY; PROBE WMAP OBSERVATIONS; SKY MAPS;
FOREGROUNDS; POLARIZATION; TEMPERATURE; RADIATION; TEMPLATE; EMISSION;
FASTICA
AB We describe and implement an exact, flexible, and computationally efficient algorithm for joint component separation and CMB power spectrum estimation, building on a Gibbs sampling framework. Two essential new features are ( 1) conditional sampling of foreground spectral parameters and ( 2) joint sampling of all amplitude-type degrees of freedom ( e. g., CMB, foreground pixel amplitudes, and global template amplitudes) given spectral parameters. Given a parametric model of the foreground signals, we estimate efficiently and accurately the exact joint foreground-CMB posterior distribution and, therefore, all marginal distributions such as the CMB power spectrum or foreground spectral index posteriors. The main limitation of the current implementation is the requirement of identical beam responses at all frequencies, which restricts the analysis to the lowest resolution of a given experiment. We outline a future generalization to multiresolution observations. To verify the method, we analyze simple models and compare the results to analytical predictions. We then analyze a realistic simulation with properties similar to the 3 yr WMAP data, downgraded to a common resolution of 3 degrees FWHM. The results from the actual 3 yr WMAP temperature analysis are presented in a companion Letter.
C1 [Eriksen, H. K.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Eriksen, H. K.] Univ Oslo, Ctr Math Appl, N-0316 Oslo, Norway.
[Jewell, J. B.; Dickinson, C.; Gorski, K. M.; Lawrence, C. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Banday, A. J.] Max Planck Inst Astrophys, D-85741 Munich, Germany.
[Gorski, K. M.] Warsaw Univ Observat, PL-00478 Warsaw, Poland.
RP Eriksen, HK (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, N-0315 Oslo, Norway.
EM h.k.k.eriksen@astro.uio.no
NR 30
TC 85
Z9 86
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2008
VL 676
IS 1
BP 10
EP 32
DI 10.1086/525277
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 275QG
UT WOS:000254086100002
ER
PT J
AU Assef, RJ
Kochanek, CS
Brodwin, M
Brown, MJI
Caldwell, N
Cool, RJ
Eisenhardt, P
Eisenstein, D
Gonzalez, AH
Jannuzi, BT
Jones, C
McKenzie, E
Murray, SS
Stern, D
AF Assef, R. J.
Kochanek, C. S.
Brodwin, M.
Brown, M. J. I.
Caldwell, N.
Cool, R. J.
Eisenhardt, P.
Eisenstein, D.
Gonzalez, A. H.
Jannuzi, B. T.
Jones, C.
McKenzie, E.
Murray, S. S.
Stern, D.
TI Low-resolution spectral templates for galaxies from 0.2 to 10 mu m
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : distances and redshifts; galaxies : luminosity function, mass
function; galaxies : photometry
ID DIGITAL SKY SURVEY; INFRARED ARRAY CAMERA; SPITZER-SPACE-TELESCOPE;
BROAD-BAND PHOTOMETRY; STAR-FORMING GALAXIES; LYMAN BREAK GALAXIES; IRAC
SHALLOW SURVEY; WIDE-FIELD SURVEY; LUMINOSITY FUNCTION;
ENERGY-DISTRIBUTIONS
AB We built an optimal basis of low- resolution templates for galaxies over the wavelength range from 0.2 to 10 mu m using a variant of the algorithm presented by Budavari and coworkers. We derived them using 11 bands of photometry from the NDWFS, FLAMEX, zBootes, and IRAC Shallow surveys for 16,033 galaxies in the NDWFS Bootes field with spectroscopic redshifts measured by the AGN and Galaxy Evolution Survey. We also developed algorithms to accurately determine photometric redshifts, K-corrections, and bolometric luminosities using these templates. Our photometric redshifts have an accuracy of sigma(z)/(1+z) = 0.04 when clipped to the best 95%. We used these templates to study the spectral type distribution in the field and to estimate luminosity functions of galaxies as a function of redshift and spectral type. In particular, we note that the 5 - 8 mu m color distribution of galaxies is bimodal, much like the optical g - r colors.
C1 [Assef, R. J.; Kochanek, C. S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Brodwin, M.; Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
[Caldwell, N.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cool, R. J.; Eisenstein, D.] Univ Arizona, Steward Observ, Tucson, AZ 85121 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Jannuzi, B. T.] Kitt Peak Natl Observ, Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[McKenzie, E.] Colgate Univ, Dept Phys & Astron, Hamilton, NY 13346 USA.
RP Assef, RJ (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
RI Brown, Michael/B-1181-2015
OI Brown, Michael/0000-0002-1207-9137
NR 63
TC 45
Z9 45
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2008
VL 676
IS 1
BP 286
EP 303
DI 10.1086/527533
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 275QG
UT WOS:000254086100020
ER
PT J
AU Beirao, P
Brandl, BR
Appleton, PN
Groves, B
Armus, L
Schreiber, NMF
Smith, JD
Charmandaris, V
Houck, JR
AF Beirao, P.
Brandl, B. R.
Appleton, P. N.
Groves, B.
Armus, L.
Schreiber, N. M. Foerster
Smith, J. D.
Charmandaris, V.
Houck, J. R.
TI Spatially resolved spitzer IRS spectroscopy of the central region of M82
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : individual (M82); galaxies : starburst; infrared : galaxies
ID STARBURST GALAXY M82; AROMATIC-HYDROCARBON EMISSION; RESOLUTION X-RAY;
INFRARED SPECTROGRAPH; INTERSTELLAR DUST; STAR-FORMATION; MU-M;
MIDINFRARED SPECTROSCOPY; MOLECULAR-HYDROGEN; SPACE-TELESCOPE
AB We present high spatial resolution ( similar to 35 pc) 5-38 mu m spectra of the central region of M82, taken with the Spitzer Infrared Spectrograph. From these spectra we determined the fluxes and equivalent widths ( EWs) of key diagnostic features, such as the [Ne-II] 12.8 mu m, [Ne-III] 15.5 mu m, and H-2 S(1) 17.03 mu m lines, and the broad mid-IR polycyclic aromatic hydrocarbon (PAH) emission features in six representative regions and analyzed the spatial distribution of these lines and their ratios across the central region. We find a good correlation of the dust extinction with the CO 1-0 emission. The PAH emission follows closely the ionization structure along the galactic disk. The observed variations of the diagnostic PAH ratios across M82 can be explained by extinction effects, within systematic uncertainties. The 16-18 mu m PAH complex is very prominent, and its EW is enhanced outward from the galactic plane. We interpret this as a consequence of the variation of the UV radiation field. The EWs of the 11.3 mu m PAH feature and the H-2 S( 1) line correlate closely, and we conclude that shocks in the outflow regions have no measurable influence on the H-2 emission. The [ Ne-III]/[ Ne-II] ratio is on average low, at similar to 0.18, and shows little variations across the plane, indicating that the dominant stellar population is evolved ( 5-6 Myr) and well distributed. There is a slight increase of the ratio with distance from the galactic plane of M82, which we attribute to a decrease in gas density. Our observations indicate that the star formation rate has decreased significantly in the last 5 Myr. The quantities of dust and molecular gas in the central area of the galaxy argue against starvation and for negative feedback processes, observable through the strong extraplanar outflows.
C1 [Beirao, P.; Brandl, B. R.; Groves, B.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Appleton, P. N.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA.
[Armus, L.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Schreiber, N. M. Foerster] Max Planck Inst Extraterr Phys, Garching, Germany.
[Smith, J. D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Charmandaris, V.] Fdn Res & Technol Hellas, IESL, GR-71110 Iraklion, Greece.
[Houck, J. R.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
RP Beirao, P (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
RI Charmandaris, Vassilis/A-7196-2008;
OI Charmandaris, Vassilis/0000-0002-2688-1956; Appleton,
Philip/0000-0002-7607-8766
NR 67
TC 33
Z9 33
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2008
VL 676
IS 1
BP 304
EP 316
DI 10.1086/527343
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 275QG
UT WOS:000254086100021
ER
PT J
AU Hwang, U
Petre, R
Flanagan, KA
AF Hwang, Una
Petre, Robert
Flanagan, Kathryn A.
TI X-ray-emitting ejecta in Puppis A observed with Suzaku
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE supernova remnants; X-rays : individual (Puppis A); X-rays : ISM
ID CORE-COLLAPSE SUPERNOVAE; LARGE-MAGELLANIC-CLOUD; CYGNUS LOOP; NEUTRAL
HYDROGEN; PLASMA STRUCTURE; REMNANT PUPPIS; MASSIVE STARS; RICH EJECTA;
NUCLEOSYNTHESIS; SPECTROSCOPY
AB We report the detection and localization of X-ray-emitting ejecta in the middle-aged Galactic supernova remnant Puppis A using five observations with the Suzaku X-Ray Imaging Spectrometer to survey the eastern and middle portions of the remnant. Aroughly 3' x 5', double-peaked region in the north center is found to be highly enriched in Si and other elements relative to the rest of the remnant. The X-ray-fitted abundances are otherwise well below the solar values. While the ejecta-enhanced regions show some variation of relative element abundances, there is little evidence for a very strong enhancement of one element over the others in the imaged portion of the remnant, except possibly for a region of O and Ne enhancement in the remnant's south center. There is no general spatial correlation between the compact [OIII]-emitting ejecta knots seen optically and the abundance enhancements seen in X-rays, although they are located in the same vicinity. The map of fitted column density shows strong variations across the remnant that echo earlier X-ray spectral hardness maps. The ionization age (as fitted for single-temperature models) is sharply higher in a ridge behind the northeast-east boundary of the remnant, and is probably related to the strong molecular cloud interaction along that boundary. The temperature map, by comparison, shows relatively weak variations.
C1 [Hwang, Una; Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hwang, Una] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Flanagan, Kathryn A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Hwang, U (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
RI XRAY, SUZAKU/A-1808-2009
NR 40
TC 27
Z9 27
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 MAR 20
PY 2008
VL 676
IS 1
BP 378
EP 389
DI 10.1086/528925
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 275QG
UT WOS:000254086100027
ER
PT J
AU Alcala, JM
Spezzi, L
Chapman, N
Evans, NJ
Huard, TL
Jorgensen, JK
Merin, B
Stapelfeldt, KR
Covino, E
Frasca, A
Gandolfi, D
Oliveira, I
AF Alcala, Juan M.
Spezzi, Loredana
Chapman, Nicholas
Evans, Neal J.
Huard, Tracy L.
Jorgensen, Jes K.
Merin, Bruno
Stapelfeldt, Karl R.
Covino, Elvira
Frasca, Antonio
Gandolfi, Davide
Oliveira, Isa
TI The Spitzer c2d survey of large, nearby, interstellar clouds. X. The
Chamaeleon II pre-main-sequence population as observed with IRAC and
MIPS
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE circumstellar matter; infrared : stars; planetary systems :
protoplanetary disks; stars : formation; stars : low-mass; brown dwarfs;
stars : pre-main-sequence
ID T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; YOUNG STELLAR OBJECTS;
HERBIG-HARO OBJECTS; ALL-SKY SURVEY; MASS-LOSS RATES; DARK-CLOUD;
MOLECULAR CLOUDS; FORMING REGION; BROWN DWARF
AB We discuss the results from the combined IRAC and MIPS c2d Spitzer Legacy survey observations and complementary optical and NIR data of the Chamaeleon II (Cha II) dark cloud. We perform a census of the young population in an area of similar to 1.75 deg(2) and study the spatial distribution and properties of the cloud members and candidate pre-main-sequence (PMS) objects and their circumstellar matter. Our census is complete down to the substellar regime (M approximate to 0.03 M-circle dot). From the analysis of the volume density of the PMS objects and candidates we find two groups of objects with volume densities higher than 25 M-circle dot pc(-3) and 5-10 members each. A multiplicity fraction of about 13% +/- 3% is observed for objects with separations 0.8 '' < theta < 6.0 '' (142-1065 AU). No evidence for variability between the two epochs of the c2d IRAC data set, Delta t similar to 6 hr, is detected. We estimate a star formation efficiency of 1%-4%, consistent with the estimates for Taurus and Lupus, but lower than for Cha I. This might mean that different star formation activities in the Chamaeleon clouds reflect a different history of star formation. We also find that Cha II is turning some 6-7 M-circle dot into stars every Myr, which is low in comparison with the star formation rate in other c2d clouds. The disk fraction of 70%-80% that we estimate in Cha II is much higher than in other star-forming regions and indicates that the population in this cloud is dominated by objects with active accretion. Finally, the Cha II outflows are discussed; a new Herbig-Haro outflow, HH 939, driven by the classical T Tauri star Sz 50, has been discovered.
C1 [Alcala, Juan M.; Spezzi, Loredana; Covino, Elvira] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy.
[Spezzi, Loredana; Frasca, Antonio; Gandolfi, Davide] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy.
[Chapman, Nicholas] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Evans, Neal J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Huard, Tracy L.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Jorgensen, Jes K.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Merin, Bruno] European Space Agcy, Res & Sci Support Dept ESTEC, NL-2200 AG Noordwijk, Netherlands.
[Merin, Bruno; Oliveira, Isa] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Stapelfeldt, Karl R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Oliveira, Isa] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Alcala, JM (reprint author), Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy.
EM alcala@oacn.inaf.it; chapman@astro.umd.edu; nje@astro.as.utexas.edu;
thuard@cfa.harvard.edu; jes@astro.uni-bonn.de; bmerin@rssd.esa.int;
krs@exoplanet.jpl.nasa.gov; afr@oact.inaf.it; isa@gps.caltech.edu
RI Stapelfeldt, Karl/D-2721-2012;
OI Alcala, Juan Manuel/0000-0001-8657-095X; Frasca,
Antonio/0000-0002-0474-0896; Covino, Elvira/0000-0002-6187-6685;
Gandolfi, Davide/0000-0001-8627-9628; Merin, Bruno/0000-0002-8555-3012
NR 114
TC 57
Z9 57
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 MAR 20
PY 2008
VL 676
IS 1
BP 427
EP 463
DI 10.1086/527315
PG 37
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 275QG
UT WOS:000254086100033
ER
PT J
AU Roberge, A
Weinberger, AJ
AF Roberge, Aki
Weinberger, Alycia J.
TI Debris disks around nearby stars with circumstellar gas
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared : stars; planetary systems : formation;
stars : early-type
ID A-SHELL STARS; BETA-PICTORIS; DUST; EMISSION; CATALOG; SYSTEM; EXCESS
AB We conducted a survey for infrared excess emission from 16 nearby main-sequence shell stars using the Multiband Imaging Photometer for Spitzer (MIPS) on the Spitzer Space Telescope. Shell stars are early-type stars with narrow absorption lines in their spectra that appear to arise from circumstellar (CS) gas. Four of the 16 stars in our survey showed excess emission at 24 and 70 mu m characteristic of cool CS dust and are likely to be edge-on debris disks. Including previously known disks, it appears that the fraction of protoplanetary and debris disks among the main-sequence shell stars is at least 48% +/- 14%. While dust in debris disks has been extensively studied, relatively little is known about their gas content. In the case of beta Pictoris, extensive observations of gaseous species have provided insights into the dynamics of the CS material and surprises about the composition of the CS gas coming from young planetesimals. To understand the coevolution of gas and dust through the terrestrial planet formation phase, we need to study the gas in additional debris disks. The new debris disk candidates from this Spitzer survey double the number of systems in which the gas can be observed right now with sensitive line-of-sight absorption spectroscopy.
C1 [Roberge, Aki] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Weinberger, Alycia J.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
RP Roberge, A (reprint author), NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA.
EM Aki.Roberge@nasa.gov; aweinberger@ciw.edu
RI Roberge, Aki/D-2782-2012;
OI Roberge, Aki/0000-0002-2989-3725; Weinberger, Alycia/0000-0001-6654-7859
NR 30
TC 21
Z9 21
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2008
VL 676
IS 1
BP 509
EP 517
DI 10.1086/527314
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 275QG
UT WOS:000254086100037
ER
PT J
AU Shkolnik, E
Bohlender, DA
Walker, GAH
Cameron, AC
AF Shkolnik, Evgenya
Bohlender, David A.
Walker, Gordon A. H.
Cameron, Andrew Collier
TI The on/off nature of star-planet interactions
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; radiation mechanisms : nonthermal; stars : activity;
stars : chromospheres; stars : individual (tau Boo, HD 179949, HD
209458, HD 189733, HD 217107, HD 149143); stars : late-type
ID CA-II H; METALLICITY-BIASED SEARCH; EXTRASOLAR GIANT PLANETS; TRANSITING
HOT JUPITERS; K-STAR; SPECTROPOLARIMETRIC OBSERVATIONS; CHROMOSPHERIC
ACTIVITY; MAGNETIC-FIELD; HOST STARS; TAU-BOOTIS
AB Evidence suggesting an observable magnetic interaction between a star and its hot Jupiter appears as a cyclic variation of stellar activity synchronized to the planet's orbit. In this study we monitored the chromospheric activity using several stellar activity indicators of seven stars with hot Jupiters using new high-resolution echelle spectra collected with ESPaDOnS over a few nights in 2005 and 2006 from the CFHT (Ca II H lambda 3968, K lambda 3933, the Ca II infrared triplet [IRT] lambda 8662 line, H alpha lambda 6563, and He I lambda 5876). Synchronicity of the Ca II H and K emission of HD 179949 with its planet's orbit is clearly seen in four out of six epochs, while rotational modulation with P(rot) = 7 days is apparent in the other two seasons. We observe a similar phenomenon on upsilon And. This on/off nature of star-planet interaction (SPI) in the two systems is likely a function of the changing stellar magnetic field structure throughout its activity cycle. Variability in the transiting system HD 189733 is likely associated with an active region rotating with the star; however, the flaring in excess of the rotational modulation may be associated with its hot Jupiter. As for HD 179949, the peak variability as measured by the mean absolute deviation ( MAD) for both HD 189733 and tau Boo leads the subplanetary longitude by similar to 70 degrees. The tentative correlation between this activity and the ratio of M(p) sin i to the planet's rotation period, a quantity proportional to the hot Jupiter's magnetic moment, first presented by Shkolnik and coworkers remains viable. This work furthers the characterization of SPI, improving its potential as a probe of extrasolar planetary magnetic fields.
C1 [Shkolnik, Evgenya] Univ Hawaii Manoa, Inst Astron, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
[Bohlender, David A.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Cameron, Andrew Collier] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
RP Shkolnik, E (reprint author), Univ Hawaii Manoa, Inst Astron, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
EM shkolnik@ifa.hawaii.edu; david.bohlender@nrc-cnrc.gc.ca;
gordonwa@uvic.ca; acc4@st-andrews.ac.uk
OI Cameron, Andrew/0000-0002-8863-7828
NR 51
TC 113
Z9 113
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2008
VL 676
IS 1
BP 628
EP 638
DI 10.1086/527351
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 275QG
UT WOS:000254086100047
ER
PT J
AU Winebarger, AR
Warren, HP
Falconer, DA
AF Winebarger, Amy R.
Warren, Harry P.
Falconer, David A.
TI Modeling X-ray loops and EUV "moss" in an active region core
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE sun : corona
ID TRANSITION-REGION; CORONAL-EXPLORER; MAGNETIC-FIELD; TRACE; TEMPERATURE;
TELESCOPE; EMISSION; DYNAMICS
AB The soft X-ray intensity of loops in active region cores and the corresponding footpoint, or moss, intensity observed in the EUV remain steady for several hours of observation. The steadiness of the emission has prompted many to suggest that the heating in these loops must also be steady, although no direct comparison between the observed X-ray and EUV intensities and the steady heating solutions of the hydrodynamic equations has yet been made. In this paper we perform these simulations and simultaneously model the X-ray and EUV moss intensities in one active region core with steady uniform heating. To perform this task, we introduce a new technique to constrain the model parameters using the measured EUV footpoint intensity to infer a heating rate. Using an ensemble of loop structures derived from magnetic field extrapolation of photospheric field, we associate each field line with an EUV moss intensity, then determine the steady uniform heating rate on that field line that reproduces the observed EUV intensity within 5% for a specific cross-sectional area, or filling factor. We then calculate the total X-ray filter intensities from all loops in the ensemble and compare this to the observed X-ray intensities. We complete this task iteratively to determine the filling factor that returns the best match to the observed X-ray intensities. We find that a filling factor of 8% and loops that expand with height provides the best agreement with the intensity in two X-ray filters, although the simulated SXT Al12 intensity is 147% the observed intensity and the SXT AlMg intensity is 80% the observed intensity. From this solution we determine the required heating rate scales as (B) over bar L-0.29(-0:95). Finally, we discuss the future potential of this type of modeling, such as the ability to use density measurements to fully constrain filling factor, and its shortcomings, such as the requirement to use potential field extrapolations to approximate the coronal field.
C1 [Winebarger, Amy R.] Alabama A&M Univ, Normal, AL 35762 USA.
[Warren, Harry P.] USN, Res Lab, Washington, DC 20375 USA.
[Falconer, David A.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA.
RP Winebarger, AR (reprint author), Alabama A&M Univ, 4900 Meridian St,POB 1268, Normal, AL 35762 USA.
EM winebarger@physics.aamu.edu; hwarren@nrl.navy.mil;
david.falconer@msfc.nasa.gov
NR 28
TC 23
Z9 24
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 MAR 20
PY 2008
VL 676
IS 1
BP 672
EP 679
DI 10.1086/527291
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 275QG
UT WOS:000254086100051
ER
PT J
AU Liu, W
Petrosian, V
Dennis, BR
Jiang, YW
AF Liu, Wei
Petrosian, Vahe
Dennis, Brian R.
Jiang, Yan Wei
TI Double coronal hard and soft X-ray source observed by RHESSI: Evidence
for magnetic reconnection and particle acceleration in solar flares
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; Sun : corona; Sun : flares; Sun : X-rays,
gamma rays
ID STOCHASTIC ACCELERATION; ELECTRON ACCELERATION; ATOMIC DATABASE;
EMISSION-LINES; LOOP; SPECTRA; BURSTS; ENERGY; CHIANTI; EVENTS
AB We present data analysis and interpretation of an M1.4 class flare observed with the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) on 2002 April 30. This event, with its footpoints occulted by the solar limb, exhibits a rarely observed, but theoretically expected, double-source structure in the corona. The two coronal sources, observed over the 6-30 keV range, appear at different altitudes and show energy-dependent structures with the higher energy emission being closer together. Spectral analysis implies that the emission at higher energies in the inner region between the two sources is mainly nonthermal, while the emission at lower energies in the outer region is primarily thermal. The two sources are both visible for about 12 minutes and have similar light curves and power-law spectra above about 20 keV. These observations suggest that the magnetic reconnection site lies between the two sources. Bidirectional outflows of the released energy in the form of turbulence and/or particles from the reconnection site could be the source of the observed radiation. The spatially resolved thermal emission below about 15 keV, on the other hand, indicates that the lower source has a larger emission measure but a lower temperature than the upper source. This is likely the result of the differences in the magnetic field and plasma density of the two sources.
C1 [Liu, Wei; Dennis, Brian R.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Liu, Wei; Petrosian, Vahe; Jiang, Yan Wei] Stanford Univ, Dept Phys, Ctr Space Sci & Astrophys, Stanford, CA 94305 USA.
RP Liu, W (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Code 671, Greenbelt, MD 20771 USA.
EM weiliu@helio.gsfc.nasa.gov
RI Dennis, Brian/C-9511-2012
NR 50
TC 63
Z9 64
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2008
VL 676
IS 1
BP 704
EP 716
DI 10.1086/527538
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 275QG
UT WOS:000254086100054
ER
PT J
AU Chandra, D
Sharma, A
Chellappa, R
Cathey, WN
Lynch, FE
Bowman, RC
Wermer, JR
Paglieri, SN
AF Chandra, Dhanesh
Sharma, Archana
Chellappa, Raja
Cathey, William N.
Lynch, Franklin E.
Bowman, Robert C., Jr.
Wermer, Joseph R.
Paglieri, Stephen N.
TI Hydriding and structural characteristics of thermally cycled and
cold-worked V-0.5 at.%C alloy
SO JOURNAL OF ALLOYS AND COMPOUNDS
LA English
DT Article
DE metal hydrides; domain structure; thermal cycling; cold-working; V-0.5
at.%C alloy
ID METAL-HYDROGEN SYSTEMS; X-RAY-DIFFRACTION; INTERMETALLIC COMPOUND; H
SYSTEMS; HYSTERESIS; VANADIUM; THERMODYNAMICS; ABSORPTION; PRESSURE;
NIOBIUM
AB High pressure hydrides Of V0.995C0.005 were thermally cycled between beta(2)- and gamma-phases hydrides for potential use in cryocoolers/heat pumps for space applications. The effect of addition of carbon to vanadium, on the plateau enthalpies of the high pressure beta(2) + gamma region is minimal. This is in contrast to the calculated plateau enthalpies for low pressure (a + 01) mixed phases which showed a noticeable lowering of the values. Thermal cycling between beta(2)-and gamma-phase hydrides increased the absorption pressures but desorption pressure did not change significantly and the free energy loss due to hysteresis also increased. Hydriding of the alloy with prior cold-work increased the pressure hysteresis significantly and lowered the hydrogen capacity. In contrast to the alloy without any prior straining (as-cast), desorption pressure of the alloy with prior cold-work also decreased significantly. Microstrains, (1/2), in the beta(2)-phase lattice of the thermally cycled hydrides decreased after 778 cycles and the domain sizes increased. However, in the gamma-phase, both the microstrains and the domain sizes decreased after thermal cycling indicating no particle size effect. The dehydrogenated alpha-phase after 778 thermal cycles also showed residual microstrains. in the lattice, similar to those observed in intermetallic hydrides. The effect of thermal cycling (up to 4000 cycles between beta(2)- and gamma-phases) and cold working on absorption/desorption pressures, hydrogen storage capacity, microstrains, long-range strains, and domain sizes of beta(2)- and gamma-phase hydrides Of V0.995C0.005 alloys are presented. Published by Elsevier B.V.
C1 [Chandra, Dhanesh; Sharma, Archana; Chellappa, Raja; Cathey, William N.] Univ Nevada, Reno, NV 89557 USA.
[Lynch, Franklin E.] HCI, Littleton, CO 80125 USA.
[Bowman, Robert C., Jr.] NASA, Jet Propuls Lab, Pasadena, CA 91109 USA.
[Wermer, Joseph R.; Paglieri, Stephen N.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Chandra, D (reprint author), Univ Nevada, Reno, NV 89557 USA.
EM dchandra@unr.edu
OI Bowman, Robert/0000-0002-2114-1713
NR 66
TC 21
Z9 21
U1 1
U2 5
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0925-8388
J9 J ALLOY COMPD
JI J. Alloy. Compd.
PD MAR 20
PY 2008
VL 452
IS 2
BP 312
EP 324
DI 10.1016/j.jallcom.2006.11.078
PG 13
WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy &
Metallurgical Engineering
SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering
GA 275UI
UT WOS:000254096800024
ER
PT J
AU Swain, MR
Vasisht, G
Tinetti, G
AF Swain, Mark R.
Vasisht, Gautam
Tinetti, Giovanna
TI The presence of methane in the atmosphere of an extrasolar planet
SO NATURE
LA English
DT Article
ID GIANT PLANETS; TRANSMISSION SPECTRA; LIGHT CURVES; WATER-VAPOR; HD
189733B; HD-189733; DYNAMICS; 209458B; TRANSIT; SYSTEM
AB Molecules present in the atmospheres of extrasolar planets are expected to influence strongly the balance of atmospheric radiation, to trace dynamical and chemical processes, and to indicate the presence of disequilibrium effects. As molecules have the potential to reveal atmospheric conditions and chemistry, searching for them is a high priority. The rotational - vibrational transition bands of water, carbon monoxide and methane are anticipated to be the primary sources of non- continuum opacity in hot- Jupiter planets(1-3). As these bands can overlap in wavelength, and the corresponding signatures from them are weak, decisive identification requires precision infrared spectroscopy. Here we report a near- infrared transmission spectrum of the planet HD 189733b that shows the presence of methane. Additionally, a resolved water vapour band at 1.9 mu m confirms the recent claim(4) of water in this object. On thermochemical grounds, carbon monoxide is expected to be abundant in the upper atmosphere of hot- Jupiter planets, but is not identifiable here; therefore the detection of methane rather than carbon monoxide in such a hot planet(5,6) could signal the presence of a horizontal chemical gradient away from the permanent dayside, or it may imply an ill- understood photochemical mechanism that leads to an enhancement of methane.
C1 [Swain, Mark R.; Vasisht, Gautam] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tinetti, Giovanna] UCL, Dept Phys & Astron, London WC1E 6BT, England.
RP Swain, MR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Mark.R.Swain@jpl.nasa.gov
OI Tinetti, Giovanna/0000-0001-6058-6654
NR 25
TC 321
Z9 324
U1 5
U2 27
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD MAR 20
PY 2008
VL 452
IS 7185
BP 329
EP 331
DI 10.1038/nature06823
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 276BX
UT WOS:000254117400041
PM 18354477
ER
PT J
AU Uno, I
Yumimoto, K
Shimizu, A
Hara, Y
Sugimoto, N
Wang, Z
Liu, Z
Winker, DM
AF Uno, I.
Yumimoto, K.
Shimizu, A.
Hara, Y.
Sugimoto, N.
Wang, Z.
Liu, Z.
Winker, D. M.
TI 3D structure of Asian dust transport revealed by CALIPSO lidar and a
4DVAR dust model
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
AB We present detailed 3D structure of Asian dust outflow from a dust source region to the northwestern Pacific ocean retrieved by NASA/CALIOP onboard CALIPSO and results simulated by a four-dimensional variational (4DVAR) data assimilation version of a dust transport model (RC4) based on the NIES Lidar network. The modeled and CALIOP dust extinction showed good agreement, both for horizontal scale (600-1200 km) and vertical depth (1600-3600 m) near the dust source regions. Cross-section analyses of CALIOP and RC4 assisted by forward trajectory revealed that dust from the Gobi Desert on 5 May traveled approximately 1000-1500 km/day to the east and passed over Japan on 8 May. The elevated dust subsequently passed to the Pacific Ocean while maintaining the major dust layer height of 2500-4000 m MSL trapped within the potential temperature of 302-306 K. Results of our analyses demonstrate the importance of integration of CALIOP measurement and the dust model for clarifying the overall structure of an Asian dust event.
C1 Kyushu Univ, Res Inst Appl Mech, Fukuoka 812, Japan.
[Yumimoto, K.] Kyushu Univ, Dept Earth Syst Sci & Technol, Fukuoka 812, Japan.
[Shimizu, A.; Hara, Y.; Sugimoto, N.] Natl Inst Environm Study, Tsukuba, Ibaraki 3058506, Japan.
[Liu, Z.] Natl Inst Atmosphere, Hampton, VA 23666 USA.
[Wang, Z.] Chinese Acad Sci, Inst Atmospher Phys, Beijing 100029, Peoples R China.
[Winker, D. M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Yumimoto, K.] Kyushu Univ, Dept Earth Syst Sci & Technol, Fukuoka 8168580, Japan.
RP Uno, I (reprint author), Kyushu Univ, Res Inst Appl Mech, Fukuoka 812, Japan.
EM uno@riam.kyushu-u.ac.jp
RI Wang, Zifa/B-5192-2008; Kyushu, RIAM/F-4018-2015; U-ID,
Kyushu/C-5291-2016; Liu, Zhaoyan/A-9604-2009; Shimizu,
Atsushi/C-2810-2009; Liu, Zhaoyan/B-1783-2010; Uno, Itsushi/B-5952-2011;
Wang, ZF/D-7202-2012; Wang, Zifa/B-5799-2011; Yumimoto,
Keiya/G-1345-2012; Sugimoto, Nobuo/C-5189-2015
OI Shimizu, Atsushi/0000-0002-7306-7412; Liu, Zhaoyan/0000-0003-4996-5738;
Wang, ZF/0000-0002-7062-6012; Yumimoto, Keiya/0000-0002-3465-0613;
Sugimoto, Nobuo/0000-0002-0545-1316
NR 9
TC 51
Z9 51
U1 2
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 19
PY 2008
VL 35
IS 6
AR L06803
DI 10.1029/2007GL032329
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA 281TC
UT WOS:000254520800001
ER
PT J
AU Wu, SL
Mickley, LJ
Leibensperger, EM
Jacob, DJ
Rind, D
Streets, DG
AF Wu, Shiliang
Mickley, Loretta J.
Leibensperger, Eric M.
Jacob, Daniel J.
Rind, David
Streets, David G.
TI Effects of 2000-2050 global change on ozone air quality in the United
States
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TROPICAL TROPOSPHERIC OZONE; SURFACE OZONE; CLIMATE-CHANGE; ISOPRENE
EMISSION; GODDARD-INSTITUTE; MODEL; POLLUTION; DISTRIBUTIONS;
SENSITIVITY; CHEMISTRY
AB We investigate the effects on U. S. ozone air quality from 2000 - 2050 global changes in climate and anthropogenic emissions of ozone precursors by using a global chemical transport model ( GEOS- Chem) driven by meteorological fields from the NASA Goddard Institute for Space Studies general circulation model ( NASA/ GISS GCM). We follow the Intergovernmental Panel on Climate Change A1B scenario and separate the effects from changes in climate and anthropogenic emissions through sensitivity simulations. The 2000 - 2050 changes in anthropogenic emissions reduce the U. S. summer daily maximum 8- hour ozone by 2 - 15 ppb, but climate change causes a 2 - 5 ppb positive offset over the Midwest and northeastern United States, partly driven by decreased ventilation from convection and frontal passages. Ozone pollution episodes are far more affected by climate change than mean values, with effects exceeding 10 ppb in the Midwest and northeast. We find that ozone air quality in the southeast is insensitive to climate change, reflecting compensating effects from changes in isoprene emission and air pollution meteorology. We define a " climate change penalty'' as the additional emission controls necessary to meet a given ozone air quality target. We find that a 50% reduction in U. S. NOx emissions is needed in the 2050 climate to reach the same target in the Midwest as a 40% reduction in the 2000 climate. Emission controls reduce the magnitude of this climate change penalty and can even turn it into a climate benefit in some regions.
C1 [Wu, Shiliang; Mickley, Loretta J.; Leibensperger, Eric M.; Jacob, Daniel J.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Rind, David] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Streets, David G.] Argonne Natl Lab, Argonne, IL 60439 USA.
RP Wu, SL (reprint author), Harvard Univ, Sch Engn & Appl Sci, Pierce Hall,20 Oxford St, Cambridge, MA 02138 USA.
EM s.wu@post.harvard.edu
RI Mickley, Loretta/D-2021-2012; Chem, GEOS/C-5595-2014;
OI Mickley, Loretta/0000-0002-7859-3470; Streets, David/0000-0002-0223-1350
NR 64
TC 126
Z9 127
U1 2
U2 34
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 19
PY 2008
VL 113
IS D6
AR D06302
DI 10.1029/2007JD008917
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 281UC
UT WOS:000254523400002
ER
PT J
AU Stockli, R
Lawrence, DM
Niu, GY
Oleson, KW
Thornton, PE
Yang, ZL
Bonan, GB
Denning, AS
Running, SW
AF Stoeckli, R.
Lawrence, D. M.
Niu, G. -Y.
Oleson, K. W.
Thornton, P. E.
Yang, Z. -L.
Bonan, G. B.
Denning, A. S.
Running, S. W.
TI Use of FLUXNET in the community land model development
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Article
ID SURFACE PARAMETRIZATION SCHEMES; ATMOSPHERE COUPLING EXPERIMENT;
CARBON-DIOXIDE EXCHANGE; ENERGY-BALANCE CLOSURE; MIXED HARDWOOD FOREST;
CLIMATE SYSTEM MODEL; INTERANNUAL VARIATION; SPRUCE FOREST;
GLOBAL-MODELS; WATER
AB The Community Land Model version 3 (CLM3.0) simulates land-atmosphere exchanges in response to climatic forcings. CLM3.0 has known biases in the surface energy partitioning as a result of deficiencies in its hydrological and biophysical parameterizations. Such models, however, need to be robust for multidecadal global climate simulations. FLUXNET now provides an extensive data source of carbon, water and energy exchanges for investigating land processes, and it encompasses a global range of ecosystem-climate interactions. Data from 15 FLUXNET sites are used to identify and improve model deficiencies. Including a prognostic aquifer, a bare soil evaporation resistance formulation and numerous other changes in the model result in a significantly improved soil hydrology and energy partitioning. Terrestrial water storage increased by up to 300 mm in warm climates and decreased in cold climates. Nitrogen control of photosynthesis is revealed as another missing process in the model. These improvements increase the correlation coefficient of hourly and monthly latent heat fluxes from a range of 0.5-0.6 to the range of 0.7-0.9. RMSE of the simulated sensible heat fluxes decrease by 20-50%. Primary production is overestimated during the wet season in mediterranean and tropical ecosystems. This might be related to missing carbon-nitrogen dynamics as well as to site-specific parameters. The new model (CLM3.5) with an improved terrestrial water cycle should lead to more realistic land-atmosphere exchanges in coupled simulations. FLUXNET is found to be a valuable tool to develop and validate land surface models prior to their application in computationally expensive global simulations.
C1 [Stoeckli, R.; Denning, A. S.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Stoeckli, R.] MeteoSwiss, Climate Serv, Fed Off Meteorol & Climatol, CH-8044 Zurich, Switzerland.
[Stoeckli, R.] NASA, Goddard Space Flight Ctr, Earth Observ, Greenbelt, MD 20771 USA.
[Lawrence, D. M.; Oleson, K. W.; Thornton, P. E.; Bonan, G. B.] Natl Ctr Atmospher Res, Terr Sci Sect, Boulder, CO 80305 USA.
[Niu, G. -Y.; Yang, Z. -L.] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA.
[Running, S. W.] Univ Montana, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA.
RP Stockli, R (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
EM reto.stoeckli@meteoswiss.ch
RI Oleson, Keith/A-9328-2008; Lawrence, David/C-4026-2011; Yang,
Zong-Liang/B-4916-2011; Thornton, Peter/B-9145-2012; Denning,
Scott/F-4974-2011; Niu, Guo-Yue/B-8317-2011; Vuichard,
Nicolas/A-6629-2011
OI Lawrence, David/0000-0002-2968-3023; Thornton,
Peter/0000-0002-4759-5158; Denning, Scott/0000-0003-3032-7875;
NR 84
TC 127
Z9 130
U1 5
U2 45
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-8953
J9 J GEOPHYS RES-BIOGEO
JI J. Geophys. Res.-Biogeosci.
PD MAR 19
PY 2008
VL 113
IS G1
AR G01025
DI 10.1029/2007JG000562
PG 19
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 281UE
UT WOS:000254523600001
ER
PT J
AU Khazanov, GV
Tel'nikhin, AA
Kronberg, TK
AF Khazanov, G. V.
Tel'nikhin, A. A.
Kronberg, T. K.
TI Dynamic theory of relativistic electrons stochastic heating by whistler
mode waves with application to the Earth magnetosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID CHAOTIC MOTION; ACCELERATION; PARTICLE; FIELD; SCATTERING; PACKET
AB In the Hamiltonian approach, electron motion in a coherent packet of the whistler mode waves propagating along the direction of an ambient magnetic field is studied. The physical processes by which these particles are accelerated to high energy are established. Equations governing particle motion are transformed into a closed pair of nonlinear difference equations. The solutions of these equations show there exists a threshold in initial electron energy, below which electron motion is regular and above which electron motion is stochastic. Particle energy spectra and pitch angle electron scattering are described by the Fokker-Planck-Kolmogorov equations. A calculation of the stochastic diffusion of electrons due to a spectrum of whistler modes is presented. The parametric dependence of the diffusion coefficients on the plasma particle density, magnitude of wave field, and the strength of magnetic field is studied. It is shown that significant pitch angle diffusion occurs for the Earth radiation belt electrons with energies from a few keV up to a few MeV.
C1 [Khazanov, G. V.] NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
[Tel'nikhin, A. A.; Kronberg, T. K.] Altai State Univ, Dept Phys, Barnaul 656049, Russia.
RP Khazanov, GV (reprint author), NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM george.khazanov@nsstc.nasa.gov; tatiana.kronberg@list.ru
NR 26
TC 8
Z9 8
U1 0
U2 1
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 MAR 19
PY 2008
VL 113
IS A3
AR A03207
DI 10.1029/2007JA012488
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 281VM
UT WOS:000254527000001
ER
PT J
AU Grefenstette, BW
Smith, DM
Dwyer, JR
Fishman, GJ
AF Grefenstette, B. W.
Smith, D. M.
Dwyer, J. R.
Fishman, G. J.
TI Time evolution of terrestrial gamma ray flashes
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
AB We present a study of the time evolution of TGFs observed by both RHESSI and BATSE and compare the data with Monte Carlo simulations of relativistic runaway electron avalanches that record the time of flight for individual photons. Our analysis of the RHESSI data shows that the average delay between the main, hard peak and the secondary, soft tail in the RHESSI data is 28 +/- 3 mu s. We show that this is consistent with Compton downscattering of hard photons in the atmosphere in our simulations when the source region is located at or below 21 km, which is consistent with previous spectroscopic analysis of the RHESSI data. We also show that the much longer delays (nominally 100 mu s) reported for the BATSE TGFs can be understood by the same simulations that are consistent with the RHESSI data once the effects of instrumental deadtime are considered.
C1 [Grefenstette, B. W.; Smith, D. M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Dwyer, J. R.] Florida Inst Technol, Dept Space Sci, Melbourne, FL 32901 USA.
[Fishman, G. J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Grefenstette, BW (reprint author), Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, 1156 High St, Santa Cruz, CA 95064 USA.
EM bwgref@scipp.ucsc.edu
NR 11
TC 41
Z9 42
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 18
PY 2008
VL 35
IS 6
AR L06802
DI 10.1029/2007GL032922
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 281TB
UT WOS:000254520700004
ER
PT J
AU Skofronick-Jackson, G
Heymsfield, A
Holthaus, E
Albers, C
Kim, MJ
AF Skofronick-Jackson, Gail
Heymsfield, Andrew
Holthaus, Eric
Albers, Cerese
Kim, Min-Jeong
TI Nonspherical and spherical characterization of ice in Hurricane Erin for
wideband passive microwave comparisons
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID PART I; MODEL; APPROXIMATION; VERIFICATION; TEMPERATURE; RADIOMETER;
PARTICLES; EVOLUTION
AB In order to better understand the characteristics and physical-to-radiative relationships of frozen hydrometeors in hurricane systems, computed brightness temperatures (TB) from 10.7 to 183 +/- 10 GHz were compared with radiometric observations of Hurricane Erin (2001) from the NASA ER-2 aircraft. The focus was on the high frequencies (>= 85 GHz) that are particularly sensitive to frozen hydrometeors. In order to initialize the cloud profiles used in the radiative transfer calculations, data from airborne radars, dropsondes, and cloud models were used. Three different ice habit and size parameterizations were used with these cloud profiles to obtain the particle radiative signatures including (1) spherical particles with size distributions derived from in situ observations, (2) spherical "fluffy" snow and graupel particles with modified Marshall-Palmer size distributions, and (3) a non-spherical bullet rosette habit where the radiation attributes (scattering, absorption, and asymmetry properties) were computed using the Discrete Dipole Approximation. In addition, three different reflectivity to ice water content (Z-IWC) relationships were used with the three habit and size parameterizations to provide a measure of the sensitivity of the Z-IWC relationship. This work showed that both the scattering and asymmetry coefficients, along with the ice water content in each layer, play an important role in determining the resultant high frequency brightness temperatures. All low frequency (< 40 GHz) calculations matched the observations with correlation coefficients greater than 0.9. At higher frequencies (> 90 GHz), correlation coefficients ranged from 0.7 to 0.92. Comparing between the three ice habit and size parameterizations showed less than a 0.2 difference in correlation coefficient, while the comparisons between the three Z-IWC relationships caused changes of up to 0.15 in the correlation coefficients, but they had a significant effect on the mean differences between the observations and the calculations.
C1 [Skofronick-Jackson, Gail] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Heymsfield, Andrew] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Holthaus, Eric] Columbia Univ, New York, NY USA.
[Albers, Cerese] Florida State Univ, Tallahassee, FL 32306 USA.
[Kim, Min-Jeong] NOAA, Camp Springs, MD USA.
RP Skofronick-Jackson, G (reprint author), NASA, Goddard Space Flight Ctr, Code 614-6,Bldg 33,RoomA428, Greenbelt, MD 20771 USA.
EM gail.s.jackson@nasa.gov
RI Heymsfield, Andrew/E-7340-2011; Skofronick-Jackson, Gail/D-5354-2012
NR 33
TC 8
Z9 8
U1 0
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 18
PY 2008
VL 113
IS D6
AR D06201
DI 10.1029/2007JD008866
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 281UB
UT WOS:000254523300002
ER
PT J
AU Asner, GP
Hughes, RF
Vitousek, PM
Knapp, DE
Kennedy-Bowdoin, T
Boardman, J
Martin, RE
Eastwood, M
Green, RO
AF Asner, Gregory P.
Hughes, R. Flint
Vitousek, Peter M.
Knapp, David E.
Kennedy-Bowdoin, Ty
Boardman, Joseph
Martin, Roberta E.
Eastwood, Michael
Green, Robert O.
TI Invasive plants transform the three-dimensional structure of rain
forests
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE biological invasion; Hawaii; imaging spectroscopy; LiDAR; tropical
forest
ID GINGER HEDYCHIUM-GARDNERIANUM; BIOLOGICAL INVASION; HAWAIIAN FORESTS;
GLOBAL CHANGE; ECOSYSTEM; LIGHT; GRASS; GAPS
AB Biological invasions contribute to global environmental change, but the dynamics and consequences of most invasions are difficult to assess at regional scales. We deployed an airborne remote sensing system that mapped the location and impacts of five highly invasive plant species across 221,875 ha of Hawaiian ecosystems, identifying four distinct ways that these species transform the three-dimensional (3D) structure of native rain forests. In lowland to montane forests, three invasive tree species replace native midcanopy and understory plants, whereas one understory invader excludes native species at the ground level. A fifth invasive nitrogen-fixing tree, in combination with a midcanopy alien tree, replaces native plants at all canopy levels in lowland forests. We conclude that this diverse array of alien plant species, each representing a different growth form or functional type, is changing the fundamental 3D structure of native Hawaiian rain forests. Our work also demonstrates how an airborne mapping strategy can identify and track the spread of certain invasive plant species, determine ecological consequences of their proliferation, and provide detailed geographic information to conservation and management efforts.
C1 [Asner, Gregory P.; Knapp, David E.; Kennedy-Bowdoin, Ty; Martin, Roberta E.] Carnegie Inst Washington, Dept Global Ecol, Stanford, CA 94305 USA.
[Hughes, R. Flint] US Forest Serv, Inst Pacific Isl Forestry, Hilo, HI 96720 USA.
[Vitousek, Peter M.] Stanford Univ, Dept Biol Sci, Stanford, CA 94305 USA.
[Boardman, Joseph] Analyt Imaging & Geophys LLC, Boulder, CO 80303 USA.
[Eastwood, Michael; Green, Robert O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Asner, GP (reprint author), Carnegie Inst Washington, Dept Global Ecol, Stanford, CA 94305 USA.
EM gpa@stanford.edu
RI Asner, Gregory/G-9268-2013
OI Asner, Gregory/0000-0001-7893-6421
NR 30
TC 110
Z9 112
U1 10
U2 79
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 MAR 18
PY 2008
VL 105
IS 11
BP 4519
EP 4523
DI 10.1073/pnas.0710811105
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 278DH
UT WOS:000254263300079
PM 18316720
ER
PT J
AU Hayes, DJ
Cohen, WB
Sader, SA
Irwin, DE
AF Hayes, Daniel J.
Cohen, Warren B.
Sader, Steven A.
Irwin, Daniel E.
TI Estimating proportional change in forest cover as a continuous variable
from multi-year MODIS data
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE MODIS; regression models; tropical forests; land cover and land use
change
ID RESOLUTION IMAGING SPECTRORADIOMETER; NOAA AVHRR DATA; SATELLITE DATA;
TROPICAL DEFORESTATION; VEGETATION INDEXES; BIOSPHERE RESERVE; BRAZILIAN
AMAZON; LANDSAT; IMAGERY; SCALE
AB This article describes a series of fundamental analyses designed to test and compare the utility of various MODIS data and products for detecting land cover change over a large area of the tropics. The approach for estimating proportional forest cover change as a continuous variable was based on a reduced major axis regression model. The model relates multispectral and multi-temporal MODIS data, transformed to optimize the spectral detection of vegetation changes, to reference change data sets derived from a Landsat data record for several study sites across the Central American region. Three MODIS data sets with diverse attributes were evaluated on model consistency, prediction accuracy and practical utility in estimating change in forest cover over multiple time intervals and spatial extents.
A spectral index based on short-wave infrared information (normalized difference moisture index), calculated from half-kilometer Calibrated Radiances data sets, generally showed the best relationships with the reference data and the lowest model prediction errors at individual study areas and time intervals. However, spectral indices based on atmospherically corrected surface reflectance data, as with the Vegetation Indices and Nadir Bidirectional Reflectance Distribution Function - Adjusted Reflectance (NBAR) data sets, produced consistent model parameters and accurate forest cover change estimates when modeling over multiple time intervals. Models based on anniversary date acquisitions of the one-kilometer resolution NBAR product proved to be the most consistent and practical to implement. Linear regression models based on spectral indices that correlate with change in the brightness, greenness and wetness spectral domains of these data estimated proportional change in forest cover with less than 10% prediction error over the full spatial and temporal extent of this study. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Hayes, Daniel J.] Oregon State Univ, Dept Forest Sci, Corvallis, OR 97331 USA.
[Cohen, Warren B.] US Forest Serv, Pacific NW Res Stn, Forestry Sci Lab, Corvallis, OR 97331 USA.
[Sader, Steven A.] Univ Maine, Sch Forest Resources, Orono, ME 04469 USA.
[Irwin, Daniel E.] NASA, George C Marshall Space Flight Ctr, Global Hydrol & Climate Ctr, Huntsville, AL 35805 USA.
RP Hayes, DJ (reprint author), Oregon State Univ, Dept Forest Sci, 321 Richardson Hall, Corvallis, OR 97331 USA.
EM Daniel.Hayes@Oregonstate.edu
RI Hayes, Daniel/B-8968-2012
NR 48
TC 27
Z9 27
U1 0
U2 8
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 MAR 18
PY 2008
VL 112
IS 3
BP 735
EP 749
DI 10.1016/j.rse.2007.06.003
PG 15
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 280RK
UT WOS:000254443700010
ER
PT J
AU Del Castillo, CE
Miller, RL
AF Del Castillo, Carlos E.
Miller, Richard L.
TI On the use of ocean color remote sensing to measure the transport of
dissolved organic carbon by the Mississippi River Plume
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE CDOM; DOC; SeaWiFS; ocean color; river transport; Mississippi River
ID WEST FLORIDA SHELF; BIOOPTICAL PROPERTIES; MATTER; WATERS; CHLOROPHYLL;
ABSORPTION; FLUORESCENCE; ALGORITHMS
AB We investigated the use of ocean color remote sensing to measure the transport of dissolved organic carbon (DOC) by the Mississippi River to the Gulf of Mexico. From 2000 to 2005 we recorded surface measurements of DOC, colored dissolved organic matter (CDOM), salinity, and water-leaving radiances during five cruises to the Mississippi River Plume. These measurements were used to develop empirical relationships to derive DOC, CDOM, and salinity from monthly composites of SeaWiFS imagery collected from 1998 through 2005. We compared our remote sensing estimates of river flow and DOC transport with data collected by the United States Geological Survey (USGS) from 1998 through 2005. Our remote sensing estimates of river flow and DOC transport correlated well (r(2) similar to 0.70) with the USGS data. Our remote sensing estimates and USGS field data showed low variability in DOC concentrations in the river end-member (7-11%), and high seasonal variability in river flow (similar to 50%). Therefore, changes in river flow control the variability in DOC transport, indicating that the remote sensing estimate of river flow is the most critical element of our DOC transport measurement. We concluded that it is possible to use this method to estimate DOC transport by other large rivers if there are data on the relationship between CDOM, DOC, and salinity in the river plume. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Del Castillo, Carlos E.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20707 USA.
[Miller, Richard L.] NASA, Stennis Space Ctr, MS USA.
RP Del Castillo, CE (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20707 USA.
EM carlos.del.castillo@jhuapl.edu
RI Liu, Cheng-Chien/E-4859-2011; Del Castillo, Carlos/N-2601-2013
NR 24
TC 65
Z9 67
U1 3
U2 23
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 MAR 18
PY 2008
VL 112
IS 3
BP 836
EP 844
DI 10.1016/j.rse.2007.06.015
PG 9
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 280RK
UT WOS:000254443700017
ER
PT J
AU Wulder, MA
White, JC
Goward, SN
Masek, JG
Irons, JR
Herold, M
Cohen, WB
Loveland, TR
Woodcock, CE
AF Wulder, Michael A.
White, Joanne C.
Goward, Samuel N.
Masek, Jeffrey G.
Irons, James R.
Herold, Martin
Cohen, Warren B.
Loveland, Thomas R.
Woodcock, Curtis E.
TI Landsat continuity: Issues and opportunities for land cover monitoring
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Landsat; landsat data continuity mission; large area; land cover;
monitoring; change detection; remote sensing
ID TERM ACQUISITION PLAN; EARTH OBSERVATION; ADVISORY-COMMITTEE; SATELLITE
DATA; LARGE AREAS; ASTER; IMAGERY; VALIDATION; MISSION; POLICY
AB Initiated in 1972, the Landsat program has provided a continuous record of earth observation for 35 years. The assemblage of Landsat spatial, spectral, and temporal resolutions, over a reasonably sized image extent, results in imagery that can be processed to represent land cover over large areas with an amount of spatial detail that is absolutely unique and indispensable for monitoring, management, and scientific activities. Recent technical problems with the two existing Landsat satellites, and delays in the development and launch of a successor, increase the likelihood that a gap in Landsat continuity may occur. In this communication, we identify the key features of the Landsat program that have resulted in the extensive use of Landsat data for large area land cover mapping and monitoring. We then augment this list of key features by examining the data needs of existing large area land cover monitoring programs. Subsequently, we use this list as a basis for reviewing the current constellation of earth observation satellites to identify potential alternative data sources for large area land cover applications. Notions of a virtual constellation of satellites to meet large area land cover mapping and monitoring needs are also presented. Finally, research priorities that would facilitate the integration of these alternative data sources into existing large area land cover monitoring programs are identified. Continuity of the Landsat program and the measurements provided are critical for scientific, environmental, economic, and social purposes. It is difficult to overstate the importance of Landsat; there are no other systems in orbit, or planned for launch in the short-term, that can duplicate or approach replication, of the measurements and information conferred by Landsat. While technical and political options are being pursued, there is no satellite image data stream poised to enter the National Satellite Land Remote Sensing Data Archive should system failures occur to Landsat-5 and -7. Crown Copyright (C) 2007 Published by Elsevier Inc. All rights reserved.
C1 [Wulder, Michael A.; White, Joanne C.] Nat Resources Canada, Pacific Forestry Ctr, Canadian Forest Serv, Victoria, BC V8Z 1M5, Canada.
[Goward, Samuel N.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Masek, Jeffrey G.; Irons, James R.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Herold, Martin] FSU Jena, Dept Geog, GOFC GOLD Land Cover Project Off, Jena, Germany.
[Cohen, Warren B.] USDA, Forest Serv, PNW Res Stn, Corvallis, OR 97331 USA.
[Loveland, Thomas R.] US Geol Survey, Ctr Earth Observat & Sci EROS, Sioux Falls, SD 57198 USA.
[Woodcock, Curtis E.] Boston Univ, Dept Geog, Boston, MA 02215 USA.
RP Wulder, MA (reprint author), Nat Resources Canada, Pacific Forestry Ctr, Canadian Forest Serv, 506 W Burnside Rd, Victoria, BC V8Z 1M5, Canada.
EM mwulder@nrcan.ge.ca
RI Masek, Jeffrey/D-7673-2012; Irons, James/D-8535-2012; Herold,
Martin/F-8553-2012; Wulder, Michael/J-5597-2016;
OI Herold, Martin/0000-0003-0246-6886; Wulder, Michael/0000-0002-6942-1896;
White, Joanne/0000-0003-4674-0373
NR 90
TC 190
Z9 200
U1 12
U2 81
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 MAR 18
PY 2008
VL 112
IS 3
BP 955
EP 969
DI 10.1016/j.rse.2007.07.004
PG 15
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 280RK
UT WOS:000254443700027
ER
PT J
AU Huang, CQ
Song, K
Kim, S
Townshend, JRG
Davis, P
Masek, JG
Goward, SN
AF Huang, Chengquan
Song, Kuan
Kim, Sunghee
Townshend, John R. G.
Davis, Paul
Masek, Jeffrey G.
Goward, Samuel N.
TI Use of a dark object concept and support vector machines to automate
forest cover change analysis
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE forest cover change; training data automation; integrated forest index;
Landsat; SVM
ID REMOTELY-SENSED DATA; ACCURACY ASSESSMENT; LANDSAT DATA; CLASSIFICATION
ACCURACY; TROPICAL DEFORESTATION; ATMOSPHERIC CORRECTION;
SPATIAL-RESOLUTION; MODIS DATA; REFLECTANCE; ALGORITHM
AB An automated method was developed for mapping forest cover change using satellite remote sensing data sets. This multi-temporal classification method consists of a training data automation (TDA) procedure and uses the advanced support vector machines (SVM) algorithm. The TDA procedure automatically generates training data using input satellite images and existing land cover products. The derived high quality training data allow the SVM to produce reliable forest cover change products. This approach was tested in 19 study areas selected from major forest biomes across the globe. In each area a forest cover change map was produced using a pair of Landsat images acquired around 1990 and 2000. High resolution IKONOS images and independently developed reference data sets were available for evaluating the derived change products in 7 of those areas. The overall accuracy values were over 90% for 5 areas, and were 89.4% and 89.6% for the remaining two areas. The user's and producer's accuracies of the forest loss class were over 80% for all 7 study areas, demonstrating that this method is especially effective for mapping major disturbances with low commission errors. IKONOS images were also available in the remaining 12 study areas but they were either located in non-forest areas or in forest areas that did not experience forest cover change between 1990 and 2000. For those areas the IKONOS images were used to assist visual interpretation of the Landsat images in assessing the derived change products. This visual assessment revealed that for most of those areas the derived change products likely were as reliable as those in the 7 areas where accuracy assessment was conducted. The results also suggest that images acquired during leaf-off seasons should not be used in forest cover change analysis in areas where deciduous forests exist. Being highly automatic and with demonstrated capability to produce reliable change products, the TDA-SVM method should be especially usefial for quantifying forest cover change over large areas. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Huang, Chengquan; Song, Kuan; Townshend, John R. G.; Davis, Paul; Goward, Samuel N.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Song, Kuan; Kim, Sunghee; Davis, Paul] Univ Maryland, Inst Adv Comp Studies, College Pk, MD 20742 USA.
[Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Huang, CQ (reprint author), Univ Maryland, Dept Geog, 2181 LeFrak Hall, College Pk, MD 20742 USA.
EM cqhuang@umd.edu
RI Masek, Jeffrey/D-7673-2012;
OI Huang, Chengquan/0000-0003-0055-9798
NR 65
TC 106
Z9 123
U1 7
U2 41
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 MAR 18
PY 2008
VL 112
IS 3
BP 970
EP 985
DI 10.1016/j.rse.2007.07.023
PG 16
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 280RK
UT WOS:000254443700028
ER
PT J
AU Cho, HM
Yang, P
Kattawar, GW
Nasiri, SL
Hu, YX
Minnis, P
Trepte, C
Winker, D
AF Cho, Hyoun-Myoung
Yang, Ping
Kattawar, George W.
Nasiri, Shaima L.
Hu, Yongxiang
Minnis, Patrick
Trepte, Charles
Winker, David
TI Depolarization ratio and attenuated backscatter for nine cloud types:
Analyses based on collocated CALIPSO lidar and MODIS measurements
SO OPTICS EXPRESS
LA English
DT Article
ID ICE CRYSTALS; WATER-VAPOR; AEROSOL; MISSION
AB This paper reports on the relationship between lidar backscatter and the corresponding depolarization ratio for nine types of cloud systems. The data used in this study are the lidar returns measured by the CloudAerosol Lidar with Orthogonal Polarization (CALIOP) aboard the CloudAerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) satellite and the collocated cloud products derived from the observations made by the Moderate Resolution Imaging Spectroradiometer (MODIS) aboard Aqua satellite. Specifically, the operational MODIS cloud optical thickness and cloud-top pressure products are used to classify cloud types on the basis of the International Satellite Cloud Climatology Project (ISCCP) cloud classification scheme. While the CALIPSO observations provide information for up to 10 cloud layers, in the present study only the uppermost clouds are considered. The layer-averaged attenuated backscatter (gamma) and layer-averaged depolarization ratio (delta) from the CALIPSO measurements show both water-and ice-phase features for global cirrus, cirrostratus, and deep convective cloud classes. Furthermore, we screen both the MODIS and CALIPSO data to eliminate cases in which CALIPSO detected two-or multi-layered clouds. It is shown that low gamma values corresponding to uppermost thin clouds are largely eliminated in the CALIPSO delta-gamma relationship for single-layered clouds. For mid-latitude and polar regions corresponding, respectively, to latitude belts 30 degrees-60 degrees and 60 degrees-90 degrees in both the hemispheres, a mixture of water and ice is also observed in the case of the altostratus class. MODIS cloud phase flags are also used to screen ice clouds. The resultant water clouds flagged by the MODIS algorithm show only water phase feature in the delta-gamma relation observed by CALIOP; however, in the case of the ice clouds flagged by the MODIS algorithm, the co-existence of ice-and water-phase clouds is still observed in the CALIPSO delta-gamma relationship.
(C)2008 Optical Society of America.
C1 [Cho, Hyoun-Myoung; Yang, Ping; Nasiri, Shaima L.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[Kattawar, George W.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
[Hu, Yongxiang; Minnis, Patrick; Trepte, Charles; Winker, David] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Yang, P (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
EM pyang@ariel.met.tamu.edu
RI Yang, Ping/B-4590-2011; Nasiri, Shaima/C-8044-2011; Hu,
Yongxiang/K-4426-2012; Minnis, Patrick/G-1902-2010
OI Minnis, Patrick/0000-0002-4733-6148
NR 29
TC 33
Z9 37
U1 4
U2 16
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 MAR 17
PY 2008
VL 16
IS 6
BP 3931
EP 3948
DI 10.1364/OE.16.003931
PG 18
WC Optics
SC Optics
GA 276DL
UT WOS:000254121400050
PM 18542490
ER
PT J
AU Savchenkov, AA
Rubiola, E
Matsko, AB
Ilchenko, VS
Maleki, L
AF Savchenkov, Anatoliy A.
Rubiola, Enrico
Matsko, Andrey B.
Ilchenko, Vladimir S.
Maleki, Lute
TI Phase noise of whispering gallery photonic hyper-parametric microwave
oscillators
SO OPTICS EXPRESS
LA English
DT Article
ID OPTOELECTRONIC OSCILLATOR; MODULATIONAL INSTABILITY; FREQUENCY
REFERENCES; MODE RESONATORS; FIBER; GENERATION; STABILITY; CAVITY; LASER
AB We report on the experimental study of phase noise properties of a high frequency photonic microwave oscillator based on four wave mixing in calcium fluoride whispering gallery mode resonators. Specifically, the oscillator generates similar to 8.5 GHz signals with -120 dBc/Hz at 100 kHz from the carrier. The floor of the phase noise is limited by the shot noise of the signal received at the photodetector. We argue that the performance of the oscillator can be significantly improved if one uses extremely high finesse resonators, increases the input optical power, supersaturates the oscillator, and suppresses the residual stimulated Raman scattering in the resonator. We also disclose a method of extremely sensitive measurement of the integral dispersion of millimeter scale dielectric resonators. (C) 2008 Optical Society of America.
C1 [Savchenkov, Anatoliy A.; Rubiola, Enrico; Matsko, Andrey B.; Ilchenko, Vladimir S.; Maleki, Lute] OEwaves Inc, Pasadena, CA 91106 USA.
[Rubiola, Enrico; Maleki, Lute] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Rubiola, Enrico] FEMTO ST Inst, CNRS, UMR 6174, Besancon, France.
RP Savchenkov, AA (reprint author), OEwaves Inc, 1010 E Union St, Pasadena, CA 91106 USA.
EM Andrey.Matsko@oewaves.com
NR 29
TC 48
Z9 48
U1 0
U2 14
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 MAR 17
PY 2008
VL 16
IS 6
BP 4130
EP 4144
DI 10.1364/OE.16.004130
PG 15
WC Optics
SC Optics
GA 276DL
UT WOS:000254121400070
PM 18542510
ER
PT J
AU Kim, H
Kim, HI
Johnson, PV
Beegle, LW
Beauchamp, JL
Goddard, WA
Kanik, I
AF Kim, Hyungjun
Kim, Hugh I.
Johnson, Paul V.
Beegle, Luther W.
Beauchamp, J. L.
Goddard, William A.
Kanik, Isik
TI Experimental and theoretical investigation into the correlation between
mass and ion mobility for choline and other ammonium cations in N-2
SO ANALYTICAL CHEMISTRY
LA English
DT Article
ID ELECTROSPRAY-IONIZATION; GAS-PHASE; AMINO-ACIDS; SPECTROMETRY;
SEPARATION; COLLISIONS; BIOMOLECULES; PEPTIDES; ENERGIES; CLUSTERS
AB A number of tertiary amine and quaternary ammonium cations spanning a mass range of 60-146 amu (trimethylamine, tetramethylammonium, trimethylethylammonium, N,N-dimethylaminoethanol, choline, N,N-dimethylglycine, betaine, acetylcholine, (3-carboxypropyl)trimethylammonium) were investigated using electrospray ionization ion mobility spectrometry. Measured ion mobilities demonstrate a high correlation between mass and mobility in N-2. In addition, identical mobilities within experimental uncertainties are observed for structurally dissimilar ions with similar ion masses. For example, dimethylethylammonium (88 amu) cations and protonated N,N-dimethylaminoethanol cations (90 amu) show identical mobilities (1.93 cm(2) V-1 s(-1)) though N,N-dimethylaminoethanol contains a hydroxyl functional group while dimethylethylammonium only contains alkyl groups. Computational analysis was performed using the modified trajectory (TJ) method with nonspherical N-2 molecules as the drift gas. The sensitivity of the ammonium cation collision cross sections to the details of the ion-neutral interactions was investigated and compared to other classes of organic molecules (carboxylic acids and abiotic amino acids). The specific charge distribution of the molecular ions in the investigated mass range has an insignificant affect on the collision cross section.
C1 [Kim, Hugh I.; Johnson, Paul V.; Beegle, Luther W.; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kim, Hyungjun; Goddard, William A.] CALTECH, Beckman Inst, Mat & Proc Simulat Ctr, Pasadena, CA 91125 USA.
[Kim, Hugh I.; Beauchamp, J. L.] CALTECH, Arthur Amos Noyes Lab Chem Phys, Pasadena, CA 91125 USA.
RP Beegle, LW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Luther.Beegle@jpl.nasa.gov
RI Beegle, Luther/A-6354-2010; Kim, Hugh/G-4476-2011; Kim,
Hyungjun/B-4527-2013; Johnson, Paul/D-4001-2009
OI Johnson, Paul/0000-0002-0186-8456
NR 44
TC 28
Z9 28
U1 1
U2 20
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0003-2700
EI 1520-6882
J9 ANAL CHEM
JI Anal. Chem.
PD MAR 15
PY 2008
VL 80
IS 6
BP 1928
EP 1936
DI 10.1021/ac701888e
PG 9
WC Chemistry, Analytical
SC Chemistry
GA 274QX
UT WOS:000254017000012
PM 18278882
ER
PT J
AU Sullivan, RM
Ghosn, LJ
Lerch, BA
AF Sullivan, Roy M.
Ghosn, Louis J.
Lerch, Bradley A.
TI A general tetrakaidecahedron model for open-celled foams
SO INTERNATIONAL JOURNAL OF SOLIDS AND STRUCTURES
LA English
DT Article
DE foam material; elastic material; energy methods; elongated tetrakaideca
hedron; elongated Kelvin model
ID ELASTIC PROPERTIES
AB A micro-mechanics model for non-isotropic, open-celled foams is developed using an elongated tetrakaidecahedron (Kelvin model) as the repeating unit cell. Assuming the cell edges possess axial and bending rigidity, the mechanics of deformation of the elongated tetrakaidecahedron lead to a set of equations for the Young's modulus, Poisson's ratio and tensile strength of the foam in the principal material directions. These equations are written as a function of the cell edge lengths and cross-section properties, the inclination angle and the strength and stiffness of the solid material. This micro-mechanics model employs an elongated Kelvin model geometry which is more general than that employed by previous authors, as the size and shape of the repeating unit cell are defined by specifying three independent dimensions. As a result, the model accounts for an additional variation in the unit cell shape which is not accounted for in the previous models. The effect of this additional shape parameter on the non-isotropic stiffness and strength behavior is demonstrated and the advantages of this more general micro-mechanics model are illustrated. Published by Elsevier Ltd.
C1 [Sullivan, Roy M.; Ghosn, Louis J.; Lerch, Bradley A.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
RP Sullivan, RM (reprint author), NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
EM roy.sullivan@grc.nasa.gov
NR 13
TC 59
Z9 61
U1 2
U2 21
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0020-7683
J9 INT J SOLIDS STRUCT
JI Int. J. Solids Struct.
PD MAR 15
PY 2008
VL 45
IS 6
BP 1754
EP 1765
DI 10.1016/j.ijsolstr.2007.10.028
PG 12
WC Mechanics
SC Mechanics
GA 270DO
UT WOS:000253700500013
ER
PT J
AU Killian, JL
Zuckerman, NB
Niemann, DL
Ribaya, BP
Rahman, M
Espinosa, R
Meyyappan, M
Nguyen, CV
AF Killian, Jessica L.
Zuckerman, Nathaniel B.
Niemann, Darrell L.
Ribaya, Bryan P.
Rahman, Mahmud
Espinosa, Robert
Meyyappan, M.
Nguyen, Cattien V.
TI Field emission properties of carbon nanotube pillar arrays
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID FILM ELECTRON EMITTERS; MICROSCOPY
AB Carbon nanotube pillar arrays (CPAs) for cold field emission applications were grown directly on polished 70/30 at. % NiCr alloy surfaces patterned by photolithography. A carbon nanotube (CNT) pillar is a localized, vertically aligned, and well-ordered group of multiwalled CNTs resulting from van der Waals forces within high-density CNT growth. The edge effect, in which the applied electric field is enhanced along the edge of each pillar, is primarily responsible for the excellent emission properties of CPAs. We achieved efficient emission with turn-on fields as low as 0.9 V/mu m and stable current densities as high as 10 mA/cm(2) at an applied macroscopic field of 5.7 V/mu m. We investigated the effects of pillar aspect ratio, density, and spacing on CPA field emission and quantified the edge effect with respect to pillar aspect ratio through modeling. We also investigated the field emission stability and found substantial improvement with CPAs compared to continuous and patterned CNT films. (c) 2008 American Institute of Physics.
C1 [Killian, Jessica L.; Zuckerman, Nathaniel B.; Nguyen, Cattien V.] ELORET Corp, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Killian, Jessica L.; Zuckerman, Nathaniel B.] San Jose State Univ, Dept Chem, San Jose, CA 95192 USA.
[Niemann, Darrell L.; Ribaya, Bryan P.; Rahman, Mahmud] Santa Clara Univ, Electron Devices Lab, Dept Elect Engn, Santa Clara, CA 95053 USA.
[Espinosa, Robert] InXitu Inc, Mountain View, CA 94043 USA.
RP Nguyen, CV (reprint author), ELORET Corp, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM cvnguyen@mail.arc.nasa.gov
NR 28
TC 31
Z9 31
U1 0
U2 14
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-8979
J9 J APPL PHYS
JI J. Appl. Phys.
PD MAR 15
PY 2008
VL 103
IS 6
AR 064312
DI 10.1063/1.2870931
PG 7
WC Physics, Applied
SC Physics
GA 281ZH
UT WOS:000254536900108
ER
PT J
AU Steinke, IP
Ruden, PP
Ni, X
Morkoc, H
Son, KA
AF Steinke, I. P.
Ruden, P. P.
Ni, X.
Morkoc, H.
Son, K. -A.
TI Current versus voltage characteristics of GaN/AlGaN/GaN double
heterostructures with varying AlGaN thickness and composition under
hydrostatic pressure
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID 2-DIMENSIONAL ELECTRON GASES; PIEZOELECTRIC POLARIZATION;
UNIAXIAL-STRESS; CONDUCTIVITY; GAN
AB We have studied current versus voltage characteristics of n-GaN/u-AlGaN/n-GaN double heterostructure devices under hydrostatic pressure up to 500 MPa. Devices were grown on c-plane sapphire substrates by organometallic vapor phase epitaxy using epitaxial layer overgrowth. The effect of AlGaN layer thickness and composition on the pressure sensitivity was investigated. For a fixed applied bias, we found that the current decreases approximately linearly in magnitude with increasing hydrostatic pressure over the range of voltages and pressures applied. The decrease in current magnitude can be attributed to piezoelectric effects and is consistent with model calculations. The polarization charge densities at the GaN/AlGaN interfaces change with hydrostatic pressure, which in turn modifies the internal potential barrier. Changes in the AlGaN layer thickness and composition also modify the interfacial polarization, with thicker AlGaN layers and higher AlN content increasing the effect of pressure on the observed current versus voltage characteristics. The strain gauge factors obtained for these devices range from similar to 200 to 800. (c) 2008 American Institute of Physics.
C1 [Steinke, I. P.; Ruden, P. P.] Univ Minnesota, Dept Elect & Comp Engn, Minneapolis, MN 55455 USA.
[Ni, X.; Morkoc, H.] Virginia Commonwealth Univ, Dept Elect Engn, Richmond, VA 23284 USA.
[Son, K. -A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Steinke, IP (reprint author), Univ Minnesota, Dept Elect & Comp Engn, Minneapolis, MN 55455 USA.
EM stei0194@umn.edu
RI Ni, Xianfeng/A-1635-2011
NR 17
TC 3
Z9 3
U1 0
U2 14
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-8979
J9 J APPL PHYS
JI J. Appl. Phys.
PD MAR 15
PY 2008
VL 103
IS 6
AR 064502
DI 10.1063/1.2844484
PG 6
WC Physics, Applied
SC Physics
GA 281ZH
UT WOS:000254536900118
ER
PT J
AU Wu, LG
Wang, B
AF Wu, Liguang
Wang, Bin
TI What has changed the proportion of intense hurricanes in the last 30
years?
SO JOURNAL OF CLIMATE
LA English
DT Article
ID VERTICAL WIND SHEAR; TROPICAL CYCLONES; ATLANTIC; INCREASE; CLIMATE;
MODEL
AB The recently reported increase in the proportion of intense hurricanes is considerably larger than those projected by the maximum potential intensity (MPI) theory and the results of numerical simulation. To reconcile this discrepancy, the authors examined the best-track datasets for the North Atlantic (NA), western North Pacific (WNP), and eastern North Pacific (ENP) basins. It was found that the changes in the tropical cyclone formation locations and prevailing tracks may have contributed to the changes in the proportion of the intense hurricanes over the past 30 yr. The authors suggest that the changes in the formation locations and prevailing tracks have a profound impact on the basinwide tropical cyclone intensity. Thus, how the atmospheric circulation in the tropical cyclone basins responds to the global warming may be a critical factor in understanding the impacts of global warming on tropical cyclone intensity.
C1 [Wu, Liguang] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20071 USA.
[Wu, Liguang] Univ Maryland, Goddard Earth & Technol Ctr, Baltimore, MD 21201 USA.
[Wang, Bin] Univ Hawaii Manoa, Dept Meteorol, Honolulu, HI 96822 USA.
[Wang, Bin] Univ Hawaii Manoa, IPRC, Honolulu, HI 96822 USA.
[Wang, Bin] Ocean Univ China, Coll Phys & Environm Oceanog, Qingdao 266003, Peoples R China.
RP Wu, LG (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613-1, Greenbelt, MD 20071 USA.
EM liguang@agnes.gsfc.nasa.gov
NR 25
TC 27
Z9 31
U1 0
U2 6
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 15
PY 2008
VL 21
IS 6
BP 1432
EP 1439
DI 10.1175/2007JCLI1715.1
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 280IY
UT WOS:000254421100017
ER
PT J
AU Erickson, DJ
Mills, RT
Gregg, J
Blasing, TJ
Hoffman, FM
Andres, RJ
Devries, M
Zhu, Z
Kawa, SR
AF Erickson, D. J., III
Mills, R. T.
Gregg, J.
Blasing, T. J.
Hoffman, F. M.
Andres, R. J.
Devries, M.
Zhu, Z.
Kawa, S. R.
TI An estimate of monthly global emissions of anthropogenic CO(2): Impact
on the seasonal cycle of atmospheric CO(2)
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Article
ID CARBON-DIOXIDE EMISSIONS; TRANSPORT; LAND
AB Monthly estimates of the global emissions of anthropogenic CO(2) are presented. Approximating the seasonal CO(2) emission cycle using a 2-harmonic Fourier series with coefficients as a function of latitude, the annual fluxes are decomposed into monthly flux estimates based on data for the United States and applied globally. These monthly anthropogenic CO(2) flux estimates are then used to model atmospheric CO(2) concentrations using meteorological fields from the NASA GEOS-4 data assimilation system. We find that the use of monthly resolved fluxes makes a significant difference in the seasonal cycle of atmospheric CO(2) in and near those regions where anthropogenic CO(2) is released to the atmosphere. Local variations of 2-6 ppmv CO(2) in the seasonal cycle amplitude are simulated; larger variations would be expected if smaller source-receptor distances could be more precisely specified using a more refined spatial resolution. We also find that in the midlatitudes near the sources, synoptic scale atmospheric circulations are important in the winter and that boundary layer venting and diurnal rectifier effects are more important in the summer. These findings have implications for inverse-modeling efforts that attempt to estimate surface source/sink regions especially when the surface sinks are colocated with regions of strong anthropogenic CO(2) emissions.
C1 [Erickson, D. J., III; Mills, R. T.; Hoffman, F. M.; Devries, M.] Oak Ridge Natl Lab, Div Math & Comp Sci, Computat Earth Sci Grp, Oak Ridge, TN 37831 USA.
[Erickson, D. J., III] Duke Univ, Nicholas Sch Environm & Earth Sci, Durham, NC USA.
[Gregg, J.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Blasing, T. J.; Andres, R. J.] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA.
[Devries, M.] Vanderbilt Univ, Sch Engn, Nashville, TN USA.
[Zhu, Z.; Kawa, S. R.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
RP Erickson, DJ (reprint author), Oak Ridge Natl Lab, Div Math & Comp Sci, Computat Earth Sci Grp, Oak Ridge, TN 37831 USA.
RI Gregg, Jay/C-6732-2011; Blasing, T/B-9498-2012; ANDRES,
ROBERT/B-9786-2012; Kawa, Stephan/E-9040-2012; Hoffman,
Forrest/B-8667-2012;
OI Gregg, Jay/0000-0003-3946-3099; Hoffman, Forrest/0000-0001-5802-4134;
ANDRES, ROBERT/0000-0001-8781-4979
NR 23
TC 15
Z9 15
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-BIOGEO
JI J. Geophys. Res.-Biogeosci.
PD MAR 15
PY 2008
VL 113
IS G1
AR G01023
DI 10.1029/2007JG000435
PG 10
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 276TQ
UT WOS:000254166400002
ER
PT J
AU Jolliff, JK
Kindle, JC
Penta, B
Helber, R
Lee, ZP
Shulman, I
Arnone, R
Rowley, CD
AF Jolliff, Jason K.
Kindle, John C.
Penta, Bradley
Helber, Robert
Lee, Zhongping
Shulman, Igor
Arnone, Robert
Rowley, Clark D.
TI On the relationship between satellite-estimated bio-optical and thermal
properties in the Gulf of Mexico
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Review
ID DISSOLVED ORGANIC-MATTER; WEST FLORIDA SHELF; SEA-SURFACE TEMPERATURE;
NITRATE-DEPLETION TEMPERATURES; MISSISSIPPI RIVER PLUME; OCEAN-COLOR
DATA; CHLOROPHYLL-A; PHYTOPLANKTON BIOMASS; CONTINENTAL-MARGIN;
LIGHT-ABSORPTION
AB Three years of Sea-viewing Wide Field-of-view Sensor (SeaWiFS) ocean color data were combined with three-dimensional thermal fields generated by the U. S. Navy's Modular Ocean Data Assimilation System (MODAS) in order to examine the interdependencies between bio-optical fields and their relationship to seasonal and mesoscale changes in upper ocean thermal structure. The combined data set suggests that the oceanic boundary layer within the Gulf of Mexico may be broadly defined by two seasonally occurring bio-thermal periods. A winter mixing period, characterized by net heat losses to the atmosphere, deepening of the isothermal layer depth, and annual maxima of satellite-estimated colored detrital matter (CDM) absorption coefficients and surface pigment concentration, was followed by a thermally stratified period characterized by net surface ocean heating, reduced isothermal layer depths, and annual minima in surface bio-optical fields. Variability in the interdependencies of ocean color products was used to diagnose an attendant shift in the size-structure of surface phytoplankton communities as well as identify CDM as the constituent responsible for the majority of blue-light absorption in Gulf of Mexico surface waters. The mesoscale circulation, as resolved by MODAS thermal fields into cold and warm-core eddies, appears to significantly modulate the seasonal bio-optical cycle of CDM absorption and surface pigment concentration. An empirical model was developed to describe CDM absorption as a function of upper ocean thermal energy. The model accounted for nearly half the variance in the satellite-estimate of this bio-optical variable. Large mismatches between the model and satellite data implied episodes of shelf water export to the deep Gulf of Mexico.
C1 [Jolliff, Jason K.; Kindle, John C.; Penta, Bradley; Helber, Robert; Lee, Zhongping; Shulman, Igor; Arnone, Robert; Rowley, Clark D.] USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA.
RP Jolliff, JK (reprint author), USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA.
EM jason.jolliff@nrlssc.navy.mil
OI Rowley, Clark/0000-0003-3496-6404
NR 136
TC 11
Z9 11
U1 1
U2 7
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 MAR 15
PY 2008
VL 113
IS G1
AR G01024
DI 10.1029/2006JG000373
PG 27
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 276TQ
UT WOS:000254166400001
ER
PT J
AU Bhatt, RT
Choi, SR
Cosgriff, LM
Fox, DS
Lee, KN
AF Bhatt, Ramakrishna T.
Choi, Sung R.
Cosgriff, Laura M.
Fox, Dennis-S.
Lee, Kang N.
TI Impact resistance of environmental barrier coated SiC/SiC composites
SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES
MICROSTRUCTURE AND PROCESSING
LA English
DT Article
DE impact; EBC coatings; SiC/SiC composites; mechanical properties; NDE
ID SIO2 SCALE VOLATILITY; SILICON-CARBIDE; COMBUSTION CONDITIONS; COATINGS;
DAMAGE; OXIDATION; MULLITE; MODEL
AB Impact performance of 2D woven SiC/SiC composites coated with 225 and 525 mu m thick environmental barrier coating (EBC) was investigated. The composites were fabricated by melt infiltration and the EBC was deposited by plasma spray. Impact tests were conducted at room temperature and at 1316 degrees C in air using 1.59 mm diameter steel-balls at projectile velocities ranging from 110 to 375 m/s. Both microscopy and non-destructive evaluation (NDE) methods were used to determine the extent of damage in the substrate and coating with increasing projectile velocity. The impacted specimens were tensile tested at room temperature to determine their residual mechanical properties. At projectile velocities less than 125 m/s, no detectable internal damage was noticed in the MI SiC/SiC composites coated with 525 mu m EBC. With increase in projectile velocity beyond this value. spallation of EBC layers, delamination of fiber plies, and fiber fracture were detected. At a fixed projectile velocity, the composites coated with 525 mu m EBC showed less damage than those coated with 225 mu m EBC. Both types of coated composites retained a large fraction of the baseline proper-ties of the as-fabricated composites and exhibited non-brittle failure after impact testing. Furnace exposure of impacted specimens in a moisture environment at 1316 degrees C for 500 h indicated that the through-the-thickness cracks in the coating and delamination cracks in the substrate generated after impact testing acted as conduits for internal oxidation. (C) 2007 Elsevier B.V. All rights reserved.
C1 [Bhatt, Ramakrishna T.; Fox, Dennis-S.] NASA Glenn Res Ctr, USA Vehicle Technol Directorate, Cleveland, OH 44135 USA.
[Choi, Sung R.] Naval Air Syst Command, Patuxent River, MD 20670 USA.
[Cosgriff, Laura M.] Cleveland State Univ, Cleveland, OH 44115 USA.
[Lee, Kang N.] Rolls Royce Corp, Indianapolis, IN 46206 USA.
RP Bhatt, RT (reprint author), NASA Glenn Res Ctr, USA Vehicle Technol Directorate, Cleveland, OH 44135 USA.
EM Ramakrishna.T.Bhatt@nasa.gov
NR 20
TC 24
Z9 27
U1 4
U2 37
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0921-5093
J9 MAT SCI ENG A-STRUCT
JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process.
PD MAR 15
PY 2008
VL 476
IS 1-2
BP 8
EP 19
DI 10.1016/j.msea.2007.04.067
PG 12
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 270AX
UT WOS:000253693200002
ER
PT J
AU Bhatt, RT
Choi, SR
Cosgriff, LM
Fox, DS
Lee, KN
AF Bhatt, Ramakrishna T.
Choi, Sung R.
Cosgriff, Laura M.
Fox, Dennis S.
Lee, Kang N.
TI Impact resistance of uncoated SiC/SiC composites
SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES
MICROSTRUCTURE AND PROCESSING
LA English
DT Article
DE impact; SiC/SiC composite; NDE; mechanical properties
ID ENVIRONMENTAL BARRIER COATINGS; SIO2 SCALE VOLATILITY; COMBUSTION
CONDITIONS; SILICON-NITRIDE; DAMAGE BEHAVIOR; MODEL
AB Two-dimensional woven SiC/SiC composites fabricated by melt infiltration method were impact tested at room temperature and at 1316 degrees C in air using 1.59-mm diameter steel-ball projectiles at velocities ranging from 115 to 400 m/s. The extent of substrate damage with increasing projectile velocity was imaged and analyzed using optical and scanning electron microscopy, and non-destructive evaluation (NDE) methods such as pulsed thermography, and computed tomography. The impacted specimens were tensile tested at room temperature to determine their residual mechanical properties. Results indicate that at 115 m/s projectile velocity, the composite showed no noticeable surface or internal damage and retained its as-fabricated mechanical properties. As the projectile velocity increased above this value, the internal damage increased and mechanical properties degraded. At velocities >300 m/s, the projectile penetrated through the composite, but the composite retained similar to 50% of the ultimate tensile strength of the as-fabricated composite and exhibited non-brittle failure. Predominant internal damages are delamination of fiber plies, fiber fracture and matrix shearing, (C) 2007 Elsevier B.V. All rights reserved.
C1 [Bhatt, Ramakrishna T.; Fox, Dennis S.] NASA Glenn Res Ctr, USA Vehicle Technol Directorate, Cleveland, OH 44135 USA.
[Choi, Sung R.] Naval Air Syst Command, Patuxent River, MD 20670 USA.
[Cosgriff, Laura M.] Cleveland State Univ, Cleveland, OH 44115 USA.
[Lee, Kang N.] Rolls Royce Corp, Indianapolis, IN 46206 USA.
RP Bhatt, RT (reprint author), NASA Glenn Res Ctr, USA Vehicle Technol Directorate, Cleveland, OH 44135 USA.
EM Ramakrishna.T.Bhatt@nasa.gov
NR 20
TC 20
Z9 22
U1 1
U2 9
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0921-5093
J9 MAT SCI ENG A-STRUCT
JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process.
PD MAR 15
PY 2008
VL 476
IS 1-2
BP 20
EP 28
DI 10.1016/j.msea.2007.04.066
PG 9
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 270AX
UT WOS:000253693200003
ER
PT J
AU Bansal, NP
Zhu, DM
AF Bansal, Narottam P.
Zhu, Dongming
TI Thermal properties of oxides with magnetoplumbite structure for advanced
thermal barrier coatings
SO SURFACE & COATINGS TECHNOLOGY
LA English
DT Article
DE magnetoplumbite oxides; thermal conductivity; thermal expansion; thermal
barrier coatings; doping
ID LANTHANUM HEXAALUMINATE; CONDUCTIVITY
AB Oxides having magnetoplumbite structure are promising candidate materials for applications as high temperature thermal barrier coatings because of their high thermal stability, high thermal expansion, and low thermal conductivity. In this study, powders of LaMgAl11O19, GdMgAl11O19, SmMgAl11O19, and Gd0.7Yb0.3MgAl11O19 magnetoplumbite oxides were synthesized by citric acid sol-gel method and hot-pressed into disk specimens. The thermal expansion coefficients (CTE) of these oxide materials were measured from room temperature to 1500 degrees C. The average CTE value was found to be similar to 9.6 x 10(-6)/C. Thermal conductivity of these magnetoplumbite-based oxide materials was also evaluated using steady-state laser heat flux test method. The effects of doping on thermal properties were also examined. Thermal conductivity of the doped Gd0.7Yb0.3MgAl11O19 composition was found to be lower than that of the undoped GdMgAl11O19. In contrast, thermal expansion coefficient was found to be independent of the oxide composition and appears to be controlled by the magnetoplumbite crystal structure. Preliminary results of thermal conductivity testing at 1600 degrees C for LaMgAl11O19 and LaMnAl11O19 magnetoplumbite oxide coatings plasma-sprayed on NiCrAlY/Rene N5 superalloy substrates are also presented. The plasma-sprayed coatings did not sinter even. at temperatures as high as 1600 degrees C. Published by Elsevier B.V.
C1 NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
[Zhu, Dongming] Glenn Res Ctr, US Army Lab, Vehicle Technol Directorate, Cleveland, OH 44135 USA.
RP Bansal, NP (reprint author), NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
EM Narottam.P.Bansal@nasa.gov
NR 15
TC 56
Z9 64
U1 2
U2 40
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0257-8972
J9 SURF COAT TECH
JI Surf. Coat. Technol.
PD MAR 15
PY 2008
VL 202
IS 12
BP 2698
EP 2703
DI 10.1016/j.surfcoat.2007.09.048
PG 6
WC Materials Science, Coatings & Films; Physics, Applied
SC Materials Science; Physics
GA 279PT
UT WOS:000254367800025
ER
PT J
AU Garcia, M
Peters-Lidard, CD
Goodrich, DC
AF Garcia, Matthew
Peters-Lidard, Christa D.
Goodrich, David C.
TI Spatial interpolation of precipitation in a dense gauge network for
monsoon storm events in the southwestern United States
SO WATER RESOURCES RESEARCH
LA English
DT Article
ID MESOSCALE CONVECTIVE SYSTEMS; NORTH-AMERICAN MONSOON; MULTIQUADRIC
INTERPOLATION; ALPINE PRECIPITATION; RAINFALL VARIABILITY;
HIGH-RESOLUTION; POINT RAINFALL; UNCERTAINTY; MODEL; SCALE
AB Inaccuracy in spatially distributed precipitation fields can contribute significantly to the uncertainty of hydrological states and fluxes estimated from land surface models. This paper examines the results of selected interpolation methods for both convective and mixed/stratiform events that occurred during the North American monsoon season over a dense gauge network at the U. S. Department of Agriculture Agricultural Research Service Walnut Gulch Experimental Watershed in the southwestern United States. The spatial coefficient of variation for the precipitation field is employed as an indicator of event morphology, and a gauge clustering factor CF is formulated as a new, scale-independent measure of network organization. We consider that CF < 0 ( a more distributed gauge network) will produce interpolation errors by reduced resolution of the precipitation field and that CF > 0 ( clustering in the gauge network) will produce errors because of reduced areal representation of the precipitation field. Spatial interpolation is performed using both inverse-distance-weighted (IDW) and multiquadric-biharmonic (MQB) methods. We employ ensembles of randomly selected network subsets for the statistical evaluation of interpolation errors in comparison with the observed precipitation. The magnitude of interpolation errors and differences in accuracy between interpolation methods depend on both the density and the geometrical organization of the gauge network. Generally, MQB methods outperform IDW methods in terms of interpolation accuracy under all conditions, but it is found that the order of the IDW method is important to the results and may, under some conditions, be just as accurate as the MQB method. In almost all results it is demonstrated that the inverse-distance-squared method for spatial interpolation, commonly employed in operational analyses and for engineering assessments, is inferior to the ID- cubed method, which is also more computationally efficient than the MQB method in studies of large networks.
C1 [Garcia, Matthew] Univ Maryland Baltimore Cty, Good Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Garcia, Matthew; Peters-Lidard, Christa D.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
[Goodrich, David C.] ARS, SW Watershed Res Ctr, USDA, Tucson, AZ 85719 USA.
RP Garcia, M (reprint author), Univ Maryland Baltimore Cty, Good Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
EM matthew.garcia@nasa.gov
RI Goodrich, David/B-1763-2009; Garcia, Matthew/K-9286-2013; Peters-Lidard,
Christa/E-1429-2012
OI Goodrich, David/0000-0001-7735-1448; Garcia,
Matthew/0000-0002-9637-4204; Peters-Lidard, Christa/0000-0003-1255-2876
NR 63
TC 33
Z9 34
U1 1
U2 12
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 MAR 15
PY 2008
VL 44
IS 5
AR W05S13
DI 10.1029/2006WR005788
PG 14
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 276UZ
UT WOS:000254170300001
ER
PT J
AU Korotova, GI
Sibeck, DG
Rosenberg, T
AF Korotova, G. I.
Sibeck, D. G.
Rosenberg, T.
TI Seasonal dependence of Interball flux transfer events
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID INTERPLANETARY MAGNETIC-FIELD; MAGNETOPAUSE; RECONNECTION
AB J. Raeder ( 2006) presented the results of a global magnetohydrodynamic simulation indicating that flux transfer events ( FTEs) form solely in the winter hemisphere and move poleward in the direction of the background magnetosheath flow during periods of strongly southward interplanetary magnetic field ( IMF) orientation. This paper presents results from a statistical survey of flux transfer FTEs observed on the mid-latitude northern and southern magnetopause by the magnetometer on the Interball-1 spacecraft over the course of its five-year mission from 1995 to 1999. Interball-1 observations confirm that FTEs exhibit a strong tendency to occur in the winter hemisphere.
C1 [Rosenberg, T.] Univ Maryland, IPST, College Pk, MD 20742 USA.
[Sibeck, D. G.] NASA GSFC, Greenbelt, MD 20723 USA.
[Korotova, G. I.] IZMIRAN, Troitsk 142190, Russia.
RP Korotova, GI (reprint author), Univ Maryland, IPST, College Pk, MD 20742 USA.
EM korotova@excite.com
RI Sibeck, David/D-4424-2012
NR 19
TC 6
Z9 6
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 14
PY 2008
VL 35
IS 5
AR L05106
DI 10.1029/2008GL033254
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 276TG
UT WOS:000254165400007
ER
PT J
AU Mackenzie, RA
Iess, L
Tortora, P
Rappaport, NJ
AF Mackenzie, R. A.
Iess, L.
Tortora, P.
Rappaport, N. J.
TI A non-hydrostatic Rhea
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
AB Radiometric data obtained during Cassini's close flyby of Rhea, on 26 November 2005, has been subject to several published analyses aiming to determine the satellite's mass and quadrupole gravity moments. Combining aspects of two of these analyses we present our best, unbiased estimates of the gravity field parameters and point out how the constraint of hydrostatic equilibrium adopted by previous analysts affects the results. We present solutions based on a broad range of geophysical assumptions, such as the presence of degree 3 and 4 gravity field constrained at different levels. The result is a balanced approach which describes our current knowledge of Rhea's gravity field. In the case of a gravity field limited to second degree harmonics the most reliable estimates are GM = 153.9398 +/- 0.0008 km(3) s(-2), 10(6) J(2) = 931.0 +/- 12.0, 10(6) C(22) = 237.2 +/- 4.5, and 10(6) S(22) = 3.8 +/- 3.8.
C1 [Iess, L.] Univ Roma La Sapienza, Dipartimento Ingn Aerosp & Astronaut, I-00185 Rome, Italy.
[Tortora, P.] Univ Bologna, Fac Ingn 2, DIEM, I-47100 Forli, Italy.
[Mackenzie, R. A.; Rappaport, N. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mackenzie, RA (reprint author), European Space Technol Ctr, Robert Bosch Str 5, D-64293 Darmstadt, Germany.
EM ruaraidh.mackenzie@esa.int
RI IESS, Luciano/F-4902-2011; Tortora, Paolo/J-6191-2012
OI IESS, Luciano/0000-0002-6230-5825; Tortora, Paolo/0000-0001-9259-7673
NR 5
TC 12
Z9 12
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 14
PY 2008
VL 35
IS 5
AR L05204
DI 10.1029/2007GL032898
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 276TG
UT WOS:000254165400005
ER
PT J
AU Stammerjohn, SE
Martinson, DG
Smith, RC
Yuan, X
Rind, D
AF Stammerjohn, S. E.
Martinson, D. G.
Smith, R. C.
Yuan, X.
Rind, D.
TI Trends in Antarctic annual sea ice retreat and advance and their
relation to El Nino-Southern Oscillation and Southern Annular Mode
variability
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID HEMISPHERE CLIMATE-CHANGE; ATMOSPHERIC CIRCULATION; PENINSULA REGION;
BELLINGSHAUSEN SEAS; SPATIAL PATTERNS; OCEAN CLIMATE; ENSO; TEMPERATURE;
PRECIPITATION; IMPACT
AB Previous studies have shown strong contrasting trends in annual sea ice duration and in monthly sea ice concentration in two regions of the Southern Ocean: decreases in the western Antarctic Peninsula/southern Bellingshausen Sea ( wAP/sBS) region and increases in the western Ross Sea ( wRS) region. To better understand the evolution of these regional sea ice trends, we utilize the full temporal ( quasi-daily) resolution of satellite-derived sea ice data to track spatially the annual ice edge advance and retreat from 1979 to 2004. These newly analyzed data reveal that sea ice is retreating 31 +/- 10 days earlier and advancing 54 +/- 9 days later in the wAP/sBS region ( i.e., total change over 1979 - 2004), whereas in the wRS region, sea ice is retreating 29 +/- 6 days later and advancing 31 +/- 6 days earlier. Changes in the wAP/sBS and wRS regions, particularly as observed during sea ice advance, occurred in association with decadal changes in the mean state of the Southern Annular Mode ( SAM; negative in the 1980s and positive in the 1990s) and the high-latitude response to El Nino - Southern Oscillation ( ENSO). In general, the high-latitude ice-atmosphere response to ENSO was strongest when - SAM was coincident with El Nino and when +SAM was coincident with La Nina, particularly in the wAP/sBS region. In total, there were 7 of 11 -SAMs between 1980 and 1990 and the 7 of 10 +SAMs between 1991 and 2000 that were associated with consistent decadal sea ice changes in the wAP/sBS and wRS regions, respectively. Elsewhere, ENSO/SAM-related sea ice changes were not as consistent over time ( e. g., western Weddell, Amundsen, and eastern Ross Sea region), or variability in general was high ( e. g., central/ eastern Weddell and along East Antarctica).
C1 [Stammerjohn, S. E.; Martinson, D. G.; Yuan, X.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Stammerjohn, S. E.; Martinson, D. G.] Columbia Univ, Dept Earth & Environm Sci, New York, NY USA.
[Smith, R. C.] Univ Calif Santa Barbara, Inst Computat Earth Syst Sci, Santa Barbara, CA 93106 USA.
[Smith, R. C.] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
[Rind, D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Stammerjohn, SE (reprint author), Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
EM sstammerjohn@giss.nasa.gov
OI STAMMERJOHN, SHARON/0000-0002-1697-8244
NR 84
TC 261
Z9 268
U1 3
U2 84
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 MAR 14
PY 2008
VL 113
IS C3
AR C03S90
DI 10.1029/2007JC004269
PG 20
WC Oceanography
SC Oceanography
GA 276UB
UT WOS:000254167600003
ER
PT J
AU Bonifacie, M
Jendrzejewski, N
Agrinier, P
Humler, E
Coleman, M
Javoy, M
AF Bonifacie, M.
Jendrzejewski, N.
Agrinier, P.
Humler, E.
Coleman, M.
Javoy, M.
TI The chlorine isotope composition of Earth's mantle
SO SCIENCE
LA English
DT Article
ID SEA-FLOOR SERPENTINITES; MIDOCEAN RIDGE BASALTS; OCEANIC-CRUST; BENEATH;
BEHAVIOR; FLUIDS; FRACTIONATION; ASSIMILATION; EVAPORITES; ATLANTIC
AB Chlorine stable isotope compositions ( delta Cl-37) of 22 mid- ocean ridge basalts ( MORBs) correlate with Cl content. The high-delta Cl-37, Cl- rich basalts are highly contaminated by Cl- rich materials ( seawater, brines, or altered rocks). The low-delta(37) Cl, Cl- poor basalts approach the composition of uncontaminated, mantle- derived magmas. Thus, most or all oceanic lavas are contaminated to some extent during their emplacement. MORB- source mantle has delta(37) Cl <= -1.6 per mil (%), which is significantly lower than that of surface reservoirs (similar to 0 parts per thousand not equal). This isotopic difference between the surface and deep Earth results from net Cl isotopic fractionation ( associated with removal of Cl from the mantle and its return by subduction over Earth history) and/ or the addition ( to external reservoirs) of a late volatile supply that is Cl-37- enriched.
C1 [Bonifacie, M.; Jendrzejewski, N.; Agrinier, P.; Humler, E.; Javoy, M.] Inst Phys Globe, CNRS INSU, UMR 7154, F-75251 Paris 05, France.
[Bonifacie, M.; Jendrzejewski, N.; Agrinier, P.; Javoy, M.] UPD, CNRS INSU, UMR 7154, F-75251 Paris, France.
[Bonifacie, M.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Humler, E.] Univ Nantes, Lab Planetol & Geodynam, CNRS, UMR 6112, F-44322 Nantes 3, France.
[Coleman, M.] Univ Reading, Sch Human & Environm Sci, Reading RG6 6AB, Berks, England.
[Coleman, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bonifacie, M (reprint author), Inst Phys Globe, CNRS INSU, UMR 7154, 4 Pl Jussieu, F-75251 Paris 05, France.
EM bonifaci@gps.caltech.edu
RI Bonifacie, Magali/A-5656-2011; Coleman, Max/A-1303-2007
OI Coleman, Max/0000-0002-5514-1826
NR 26
TC 50
Z9 50
U1 2
U2 37
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD MAR 14
PY 2008
VL 319
IS 5869
BP 1518
EP 1520
DI 10.1126/science.1150988
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 273PI
UT WOS:000253943800036
PM 18339936
ER
PT J
AU Farrell, WM
Stubbs, TJ
Halekas, JS
Delory, GT
Collier, MR
Vondrak, RR
Lin, RP
AF Farrell, W. M.
Stubbs, T. J.
Halekas, J. S.
Delory, G. T.
Collier, M. R.
Vondrak, R. R.
Lin, R. P.
TI Loss of solar wind plasma neutrality and affect on surface potentials
near the lunar terminator and shadowed polar regions
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID IN-CELL SIMULATIONS; WAKE; EXPANSION; VACUUM
AB As the solar wind is absorbed on the lunar dayside, a clear and obvious plasma void is created in the anti-solar direction that extends many lunar radii behind the Moon. Plasma adjacent to this void will expand into the depleted region and this process is modeled here using a particle-in-cell code. It is found that thermal electrons will diffuse into the void ahead of the ions, creating a break in plasma quasi-neutrality. In essence, immediately trailing behind the lunar terminator/ polar regions, there is a magnetic-field aligned E-field peaking near 400 mV/ m associated with a standing double-layer, this layer consisting of fast thermal electrons ( electron cloud) moving into the central void ahead of an ion-enhanced layer. We demonstrate that the surface locations that are incident with the electron cloud ( just nightside of the terminator) will develop enhanced negative surface potentials due to the dominance of electron currents. Such regions of large negative potentials near the lunar poles are of interest, especially given NASA's recent announcement of a lunar outpost at the south polar Aitken Basin.
C1 [Farrell, W. M.; Stubbs, T. J.; Collier, M. R.; Vondrak, R. R.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Halekas, J. S.; Delory, G. T.; Lin, R. P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Stubbs, T. J.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA.
RP Farrell, WM (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Code 661, Greenbelt, MD 20771 USA.
EM william.farrell@gsfc.nasa.gov
RI Collier, Michael/I-4864-2013; Stubbs, Timothy/I-5139-2013; Farrell,
William/I-4865-2013;
OI Collier, Michael/0000-0001-9658-6605; Stubbs,
Timothy/0000-0002-5524-645X; Halekas, Jasper/0000-0001-5258-6128
NR 14
TC 20
Z9 20
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 13
PY 2008
VL 35
IS 5
AR L05105
DI 10.1029/2007GL032653
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 276TF
UT WOS:000254165200002
ER
PT J
AU Yan, XH
Jo, YH
Jiang, L
Wan, ZW
Liu, WT
Li, Y
Zhan, JM
Du, T
AF Yan, Xiao-Hai
Jo, Young-Heon
Jiang, Lide
Wan, Zhenwen
Liu, W. Timothy
Li, Yan
Zhan, Jiemin
Du, Tao
TI Impact of the Three Gorges Dam water storage on the Yangtze River
outflow into the East China Sea
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
AB The role of the Three Gorges Dam Water Storage ( TGDWS) in changing salinity in the East China Sea ( ECS) near the Yangtze River Estuary ( YRE) was investigated using a multi-sensor remote sensing technique, namely the salt steric height anomaly, calculated from Sea Surface Height Anomaly ( SSHA) and Sea Surface Temperature ( SST) data. The patterns of the salt steric height anomaly near the YRE agreed well with the in situ Sea Surface Salinity ( SSS) measurements. In order to examine the changes in stability in the mixed layer near the YRE due to TGDWS, the time series of the steric height anomaly ratio ( R(s)') between heat and salt at three locations were estimated. The R(s)' was strongly associated with a coastal upwelling in the ECS, because the reduced freshwater outflow gives rise to changes of both mixed layer depth and surface current patterns off the YRE.
C1 [Yan, Xiao-Hai; Jo, Young-Heon; Jiang, Lide; Du, Tao] Univ Delaware, Grad Coll Marine & Earth Studies, Ctr Remote Sensing, Newark, DE 19716 USA.
[Yan, Xiao-Hai; Wan, Zhenwen; Li, Yan] Xiamen Univ, State Key Lab Marine Environm Sci, Xiamen 361005, Peoples R China.
[Liu, W. Timothy] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhan, Jiemin] Zhongshan Univ, Dept Appl Mech & Engn, Guangzhou 510275, Peoples R China.
RP Yan, XH (reprint author), Univ Delaware, Grad Coll Marine & Earth Studies, Ctr Remote Sensing, Newark, DE 19716 USA.
EM xiaohai@udel.edu
RI Li, Y/G-3453-2010; Jiang, Lide/G-2041-2010
OI Jiang, Lide/0000-0002-9883-4411
NR 13
TC 11
Z9 11
U1 3
U2 26
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 13
PY 2008
VL 35
IS 5
AR L05610
DI 10.1029/2007GL032908
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 276TF
UT WOS:000254165200004
ER
PT J
AU O'Neill, NT
Eck, TF
Reid, JS
Smirnov, A
Pancrati, O
AF O'Neill, N. T.
Eck, T. F.
Reid, J. S.
Smirnov, A.
Pancrati, O.
TI Coarse mode optical information retrievable using ultraviolet to
short-wave infrared sun photometry: Application to United Arab Emirates
unified aerosol experiment data
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID DEPTH; SPHEROIDS
AB The United Arab Emirates Unified Aerosol experiment provided a unique opportunity for testing aerosol retrieval algorithms in conditions where the optical influence of coarse mode particles was significant. Comparisons between Aerosol Robotic Network (AERONET) Sun photometry retrievals of a previously reported spectral deconvolution algorithm (SDA) and surface-based microphysical and optical measurements showed levels of correlation suggestive of moderate vertical homogeneity for (extensive) measures of fine and coarse mode aerosol particles and stronger vertical homogeneity for indicators of (intensive) aerosol type. An extension of the SDA into the short-wave infrared (SDA+) was developed in order to exploit the enhanced coarse mode information available in new AERONET instruments which include a 1.64 mu m channel. Comparisons between values of coarse mode Angstrom exponent alpha(c) (1.64 mu m)) retrieved from SDA+ and effective (coarse mode) radius derived from AERONET inversions showed moderate but significant correlations. Correlations between coarse mode effective radius derived from alpha(c) (1.64 mu m) and surface-based volume mean diameter estimates underscored the physical significance of the spectral retrievals and suggested moderate vertical homogeneity in terms of coarse mode particle size.
C1 [O'Neill, N. T.; Pancrati, O.] Univ Sherbrooke, CARTEL, Sherbrooke, PQ J1K 2R1, Canada.
[Eck, T. F.; Smirnov, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Reid, J. S.] Naval Res Lab, Monterey, CA 93943 USA.
[Eck, T. F.; Smirnov, A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
RP O'Neill, NT (reprint author), Univ Sherbrooke, CARTEL, Sherbrooke, PQ J1K 2R1, Canada.
EM norm.oneill@usherbrooke.ca
RI ECK, THOMAS/D-7407-2012; Smirnov, Alexander/C-2121-2009; Reid,
Jeffrey/B-7633-2014
OI Smirnov, Alexander/0000-0002-8208-1304; Reid,
Jeffrey/0000-0002-5147-7955
NR 10
TC 9
Z9 9
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 13
PY 2008
VL 113
IS D5
AR D05212
DI 10.1029/2007JD009052
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 276TL
UT WOS:000254165900004
ER
PT J
AU Vorotnikov, VS
Smith, CW
Hu, Q
Szabo, A
Skoug, RM
Cohen, CMS
AF Vorotnikov, Vasiliy S.
Smith, Charles W.
Hu, Qiang
Szabo, Adam
Skoug, Ruth M.
Cohen, Christina M. S.
TI Automated shock detection and analysis algorithm for space weather
application
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID ADVANCED COMPOSITION EXPLORER; RANKINE-HUGONIOT PROBLEM; RADIATION BELT
FORMATION; INTERPLANETARY SHOCKS; MAGNETIC-FIELDS; WIND; ACCELERATION
AB [1] Space weather applications have grown steadily as real-time data have become increasingly available. Numerous industrial applications have arisen with safeguarding of the power distribution grids being a particular interest. NASA uses short-term and long-term space weather predictions in its launch facilities. Researchers studying ionospheric, auroral, and magnetospheric disturbances use real-time space weather services to determine launch times. Commercial airlines, communication companies, and the military use space weather measurements to manage their resources and activities. As the effects of solar transients upon the Earth's environment and society grow with the increasing complexity of technology, better tools are needed to monitor and evaluate the characteristics of the incoming disturbances. A need is for automated shock detection and analysis methods that are applicable to in situ measurements upstream of the Earth. Such tools can provide advance warning of approaching disturbances that have significant space weather impacts. Knowledge of the shock strength and speed can also provide insight into the nature of the approaching solar transient prior to arrival at the magnetopause. We report on efforts to develop a tool that can find and analyze shocks in interplanetary plasma data without operator intervention. This method will run with sufficient speed to be a practical space weather tool providing useful shock information within 1 min of having the necessary data to ground. The ability to run without human intervention frees space weather operators to perform other vital services. We describe ways of handling upstream data that minimize the frequency of false positive alerts while providing the most complete description of approaching disturbances that is reasonably possible.
C1 [Vorotnikov, Vasiliy S.] Univ New Hampshire, Dept Chem Engn, Durham, NH USA.
[Hu, Qiang] Univ New Hampshire, Inst Geophys, Durham, NH USA.
[Smith, Charles W.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Szabo, Adam] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Skoug, Ruth M.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Cohen, Christina M. S.] CALTECH, Space Radiat Lab, Pasadena, CA USA.
RP Vorotnikov, VS (reprint author), Univ New Hampshire, Dept Chem Engn, Durham, NH USA.
NR 39
TC 12
Z9 13
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD MAR 13
PY 2008
VL 6
IS 3
AR S03002
DI 10.1029/2007SW000358
PG 12
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 276UU
UT WOS:000254169800001
ER
PT J
AU Taktakishvili, A
Kuznetsova, MM
Hesse, M
Fok, MC
Rastaetter, L
Maddox, M
Chulaki, A
Toth, G
Gombosi, TI
De Zeeuw, DL
AF Taktakishvili, A.
Kuznetsova, M. M.
Hesse, M.
Fok, M. -C.
Rastaetter, L.
Maddox, M.
Chulaki, A.
Toth, G.
Gombosi, T. I.
De Zeeuw, D. L.
TI Role of periodic loading-unloading in the magnetotail versus
interplanetary magnetic field B(z) flipping in the ring current buildup
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID MODEL
AB Introducing kinetic corrections into the to BATSRUS code in the magnetotail region leads to fast reconnection rates observed in kinetic simulations and quasi-periodic loading-unloading cycles in the magnetotail during a long period of steady southward interplanetary magnetic field (IMF) B(z) (Kuznetsova et al., 2006, 2007). We use the global MHD code BATSRUS output to drive the Fok Ring Current (FRC) model, which then exhibits quasi-periodic oscillations of geosynchronous energetic particle fluxes, similar to "sawtooth'' injection profiles. We compare these results with the results of the FRC model driven by BATSRUS for periodically flipping IMF Bz component, without kinetic corrections. The comparison shows the dominant role of quasi-periodic loading-unloading in the tail over the role of flipping IMF Bz component in the formation of geosynchronous fluxes for various energies. This same result is confirmed by the analysis of particle number and energy content within geosynchronous orbit.
C1 [Taktakishvili, A.; Kuznetsova, M. M.; Hesse, M.; Fok, M. -C.; Rastaetter, L.; Maddox, M.; Chulaki, A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Toth, G.; Gombosi, T. I.; De Zeeuw, D. L.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA.
RP Taktakishvili, A (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
EM staktak@lssp-mail.gsfc.nasa.gov
RI Gombosi, Tamas/G-4238-2011; De Zeeuw, Darren/F-3667-2011; Hesse,
Michael/D-2031-2012; Rastaetter, Lutz/D-4715-2012; Kuznetsova,
Maria/F-6840-2012; Fok, Mei-Ching/D-1626-2012; Toth, Gabor/B-7977-2013
OI Gombosi, Tamas/0000-0001-9360-4951; Rastaetter,
Lutz/0000-0002-7343-4147; Toth, Gabor/0000-0002-5654-9823
NR 12
TC 1
Z9 1
U1 0
U2 0
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 MAR 12
PY 2008
VL 113
IS A3
AR A03206
DI 10.1029/2007JA012845
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 276UM
UT WOS:000254168800003
ER
PT J
AU Quillen, AC
Bland-Hawthorn, J
Green, JD
Smith, JD
Prasad, DA
Alonso-Herrero, A
Cleary, K
Brookes, MH
Lawrence, CR
AF Quillen, Alice C.
Bland-Hawthorn, Joss
Green, Joel D.
Smith, J. D.
Prasad, D. Amelia
Alonso-Herrero, Almudena
Cleary, Kieran
Brookes, Mairi H.
Lawrence, Charles R.
TI Spitzer Space Telescope Infrared Spectrograph mapping of the central kpc
of Centaurus A
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE ISM : jets and outflows; galaxies : individual : NGC 5128; galaxies :
ISM; galaxies : jets; galaxies : nuclei; galaxies : structure
ID WARM MOLECULAR-HYDROGEN; RADIO GALAXY CENTAURUS; X-RAY-EMISSION;
SEYFERT-GALAXIES; INTERSTELLAR-MEDIUM; LINE DIAGNOSTICS; SPECTROSCOPY;
NUCLEUS; GAS; KINEMATICS
AB We report on the results of spectroscopic mapping observations carried out in the central kpc of Centaurus A (NGC 5128) over the 5.2-15 and 20-36 mu m spectral regions using the Infrared Spectrograph onboard the Spitzer Space Telescope. The 500-pc bipolar dust shell discovered by Quillen et al. is even more clearly seen in the 11.3-mu m dust emission feature than previous broad-band imaging. The pure rotational lines of molecular hydrogen other than the S(0) line are detected above the dusty disc and associated with the oval dust shell. The molecular hydrogen transitions indicate the presence of warm gas at temperatures 250-720 K. The ratio of the surface brightnesses in the dust emission features at 7.7 and 11.3 mu m and the ratio of the [Ne II](12.8 mu m) and 11.3-mu m dust emission feature are lower in the 500-pc dust shell than in the star-forming disc. The clearer shell morphology at 11.3 mu m, warm molecular hydrogen emission in the shell, and variation in line ratios in the shell compared to those in the disc, confirm spectroscopically that this shell is a separate coherent entity and is unlikely to be a chance superposition of dust filaments. The physical conditions in the shell are most similar to Galactic supernova remnants where blast waves encounter molecular clouds. The lines requiring the highest level of ionization, [Ne V](24.318 mu m) and [O IV](25.890 mu m), are detected 20-25 arcsec north-east and south-west of the nucleus and at position angles near the radio jet axis. Fine-structure line ratios and limits from this region suggest that the medium is a low-density one and illuminated by a hard radiation field at low ionization parameter. These higher S molecular hydrogen pure rotational transitions are also particularly bright in the same region as the [O IV] and [Ne V] emission. This suggests that the gas associated with the dust shell has been excited near the jet axis and is part of an ionization cone.
C1 [Quillen, Alice C.; Green, Joel D.; Prasad, D. Amelia] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Bland-Hawthorn, Joss] Anglo Australian Observ, Epping, NSW 2121, Australia.
[Bland-Hawthorn, Joss] Univ Sydney, Sch Phys, Inst Astron, Sydney, NSW 2006, Australia.
[Smith, J. D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Alonso-Herrero, Almudena] CSIC, Inst Estructura Mat, Dept Astrofis Mol & Infrarroja, E-28006 Madrid, Spain.
[Brookes, Mairi H.; Lawrence, Charles R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Quillen, AC (reprint author), Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
EM aquillen@pas.rochester.edu; jbh@aao.gov.au; joel@pas.rochester.edu;
jdsmith@as.arizona.edu; aalonso@damir.iem.csic.es
RI Alonso-Herrero, Almudena/H-1426-2015
OI Alonso-Herrero, Almudena/0000-0001-6794-2519
NR 38
TC 9
Z9 9
U1 0
U2 1
PU BLACKWELL PUBLISHING
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 11
PY 2008
VL 384
IS 4
BP 1469
EP 1482
DI 10.1111/j.1365-2966.2007.12768.x
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 270HK
UT WOS:000253711700021
ER
PT J
AU Damineli, A
Hillier, DJ
Corcoran, MF
Stahl, O
Levenhagen, RS
Leister, NV
Groh, JH
Teodoro, M
Colombo, JFA
Gonzalez, F
Arias, J
Levato, H
Grosso, M
Morrell, N
Gamen, R
Wallerstein, G
Niemela, V
AF Damineli, A.
Hillier, D. J.
Corcoran, M. F.
Stahl, O.
Levenhagen, R. S.
Leister, N. V.
Groh, J. H.
Teodoro, M.
Colombo, J. F. Albacete
Gonzalez, F.
Arias, J.
Levato, H.
Grosso, M.
Morrell, N.
Gamen, R.
Wallerstein, G.
Niemela, V.
TI The periodicity of the eta Carinae events
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars : general; stars : individual : eta Carinae; stars : binary
ID 2003.5 MINIMUM; HOMUNCULUS NEBULA; SPECTROSCOPY; VARIABILITY;
INTERFEROMETRY; EMISSION; SPECTRA; BINARY; EJECTA
AB Extensive spectral observations of eta Carinae over the last cycle, and particularly around the 2003.5 low-excitation event, have been obtained. The variability of both narrow and broad lines, when combined with data taken from two earlier cycles, reveal a common and well-defined period. We have combined the cycle lengths derived from the many lines in the optical spectrum with those from broad-band X-rays, optical and near-infrared observations, and obtained a period length of P-pres = 2022.7 +/- 1.3 d. Spectroscopic data collected during the last 60 yr yield an average period of P-avg = 2020 +/- 4 d, consistent with the present-day period. The period cannot have changed by more than Delta P/P = 0.0007 since 1948. This confirms the previous claims of a true, stable periodicity, and gives strong support to the binary scenario. We have used the disappearance of the narrow component of He I 6678 to define the epoch of the Cycle 11 minimum, T-0 = JD 245 2819.8. The next event is predicted to occur on 2009 January 11 (+/- 2 d). The dates for the start of the minimum in other spectral features and broad-bands are very close to this date, and have well-determined time-delays from the He I epoch.
C1 [Damineli, A.; Levenhagen, R. S.; Leister, N. V.; Groh, J. H.; Teodoro, M.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfericas, BR-05508900 Sao Paulo, Brazil.
[Hillier, D. J.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Corcoran, M. F.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Corcoran, M. F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Corcoran, M. F.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Stahl, O.] Univ Heidelberg, ZAH, D-69117 Heidelberg, Germany.
[Colombo, J. F. Albacete] UNLP, FCAGLP, Buenos Aires, DF, Argentina.
[Gonzalez, F.; Levato, H.; Grosso, M.; Gamen, R.] Complejo Astron El Leoncito, San Juan, Argentina.
[Arias, J.] Univ La Serena, Dept Fis, La Serena, Chile.
[Morrell, N.] Carnegie Observ, Las Campanas Observ, La Serena, Chile.
[Wallerstein, G.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
RP Damineli, A (reprint author), Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfericas, Rua Matao 1226,Cidade Univ, BR-05508900 Sao Paulo, Brazil.
EM damineli@astro.iag.usp.br
RI Damineli, Augusto/D-8210-2012; Levenhagen, Ronaldo/A-1043-2008; Teodoro,
Mairan/H-9123-2013; Gamen, Roberto/A-1728-2015
OI Damineli, Augusto/0000-0002-7978-2994; Levenhagen,
Ronaldo/0000-0003-2499-9325;
NR 33
TC 72
Z9 72
U1 0
U2 3
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 MAR 11
PY 2008
VL 384
IS 4
BP 1649
EP 1656
DI 10.1111/j.1365-2966.2007.12815.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 270HK
UT WOS:000253711700038
ER
PT J
AU Shi, C
Yan, H
Gu, C
Ghosh, D
Seballos, L
Chen, SW
Zhang, JZ
Chen, B
AF Shi, Chao
Yan, He
Gu, Claire
Ghosh, Debraj
Seballos, Leo
Chen, Shaowei
Zhang, Jin Z.
Chen, Bin
TI A double substrate "sandwich" structure for fiber surface enhanced Raman
scattering detection
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID OPTICAL-FIBER; SILVER; SPECTROSCOPY; PROBES; RESONANCE; SENSORS; TIPS
AB A double substrate "sandwiching" structure has been designed and tested for molecular detection using surface enhanced Raman scattering (SERS). With silver (Ag) nanoparticles as SERS substrates and rhodamine 6G (R6G) as a test molecule, the results show that the "sandwich" configuration exhibits significantly higher SERS enhancement compared to just one of the substrates or a simple sum of the signals from the two separate substrates. The improved SERS sensitivity is attributed to a stronger electromagnetic field enhancement by the double substrate sandwich structure. (C) 2008 American Institute of Physics.
C1 [Shi, Chao; Yan, He; Gu, Claire] Univ Calif Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95064 USA.
[Ghosh, Debraj; Seballos, Leo; Chen, Shaowei; Zhang, Jin Z.] Univ Calif Santa Cruz, Dept Chem & Biochem, Santa Cruz, CA 95064 USA.
[Chen, Bin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Gu, C (reprint author), Univ Calif Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95064 USA.
EM chaoshi@soe.ucsc.edu; claire@soe.ucsc.edu; zhang@chemistry.ucsc.edu
RI Chen, Shaowei/B-5171-2013
OI Chen, Shaowei/0000-0002-3668-8551
NR 29
TC 35
Z9 37
U1 3
U2 20
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0003-6951
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD MAR 10
PY 2008
VL 92
IS 10
AR 103107
DI 10.1063/1.2883957
PG 3
WC Physics, Applied
SC Physics
GA 274GH
UT WOS:000253989300107
ER
PT J
AU Ackermann, M
Adams, J
Ahrens, J
Andeen, K
Auffenberg, J
Bai, X
Baret, B
Barwick, SW
Bay, R
Beattie, K
Becka, T
Becker, JK
Becker, KH
Beimforde, M
Berghaus, P
Berley, D
Bernardini, E
Bertrand, D
Besson, DZ
Blaufuss, E
Boersma, DJ
Bohm, C
Bolmont, J
Boser, S
Botner, O
Bouchta, A
Braun, J
Burgess, T
Castermans, T
Chirkin, D
Christy, B
Clem, J
Cowen, DF
D'Agostino, MV
Davour, A
Day, CT
De Clercq, C
Demirors, L
Descamps, F
Desiati, P
De Vries-Uiterweerd, G
DeYoung, T
Diaz-Velez, JC
Dreyer, J
Dumm, JP
Duvoort, MR
Edwards, WR
Ehrlich, R
Eisch, J
Ellsworth, RW
Evenson, PA
Fadiran, O
Fazely, AR
Filimonov, K
Finley, C
Foerster, MM
Fox, BD
Franckowiak, A
Franke, R
Gaisser, TK
Gallagher, J
Ganugapati, R
Geenen, H
Gerhardt, L
Goldschmidt, A
Goodman, JA
Gozzini, R
Griesel, T
Gross, A
Grullon, S
Gunasingha, RM
Gurtner, M
Ha, C
Hallgren, A
Halzen, F
Han, K
Hanson, K
Hardtke, D
Hardtke, R
Hasegawa, Y
Hauschildt, T
Heise, J
Helbing, K
Hellwig, M
Herquet, P
Hill, GC
Hodges, J
Hoffman, KD
Hommez, B
Hoshina, K
Hubert, D
Hughey, B
Hulss, JP
Hulth, PO
Hultqvist, K
Hundertmark, S
Inaba, M
Ishihara, A
Jacobsen, J
Japaridze, GS
Johansson, H
Joseph, JM
Kampert, KH
Kappes, A
Karg, T
Karle, A
Kawai, H
Kelley, JL
Kiryluk, J
Kislat, F
Kitamura, N
Klein, SR
Klepser, S
Kohnen, G
Kolanoski, H
Kopke, L
Kowalski, M
Kowarik, T
Krasberg, M
Kuehn, K
Kuwabara, T
Labare, M
Laihem, K
Landsman, H
Lauer, R
Leich, H
Leier, D
Liubarsky, I
Lundberg, J
Lunemann, J
Madsen, J
Maruyama, R
Mase, K
Matis, HS
McCauley, T
McParland, CP
Meagher, K
Meli, A
Messarius, T
Meszaros, P
Miyamoto, H
Montaruli, T
Morey, A
Morse, R
Movit, SM
Muenich, K
Nahnhauer, R
Nam, JW
Niessen, P
Nygren, DR
Olivas, A
Ono, M
Patton, S
Heros, CPDL
Piegsa, A
Pieloth, D
Pohl, AC
Porrata, R
Pretz, J
Price, PB
Przybylski, GT
Rawlins, K
Razzaque, S
Redl, P
Resconi, E
Rhode, W
Ribordy, M
Rizzo, A
Robbins, S
Robbins, WJ
Roth, P
Rothmaier, F
Rott, C
Roucelle, C
Rutledge, D
Ryckbosch, D
Sander, HG
Sarkar, S
Satalecka, K
Schlenstedt, S
Schmidt, T
Schneider, D
Schultz, O
Seckel, D
Semburg, B
Seo, SH
Sestayo, Y
Seunarine, S
Silvestri, A
Smith, AJ
Song, C
Spiczak, GM
Spiering, C
Stamatikos, M
Stanev, T
Stezelberger, T
Stokstad, RG
Stoufer, MC
Stoyanov, S
Strahler, EA
Straszheim, T
Sulanke, KH
Sullivan, GW
Sumner, TJ
Swillens, Q
Taboada, I
Tarasova, O
Tepe, A
Thollander, L
Tilav, S
Tluczykont, M
Toale, PA
Tosi, D
Turcan, D
Van Eijndhoven, N
Vandenbroucke, J
Van Overloop, A
Viscomi, V
Vogt, C
Voigt, B
Wagner, W
Walck, C
Waldmann, H
Waldenmaier, T
Walter, M
Wang, YR
Wendt, C
Wiebusch, CH
Wiedemann, C
Wikstrom, G
Williams, DR
Wischnewski, R
Wissing, H
Woschnagg, K
Xu, XW
Yodh, G
Yoshida, S
Zornoza, JD
AF Ackermann, M.
Adams, J.
Ahrens, J.
Andeen, K.
Auffenberg, J.
Bai, X.
Baret, B.
Barwick, S. W.
Bay, R.
Beattie, K.
Becka, T.
Becker, J. K.
Becker, K. -H.
Beimforde, M.
Berghaus, P.
Berley, D.
Bernardini, E.
Bertrand, D.
Besson, D. Z.
Blaufuss, E.
Boersma, D. J.
Bohm, C.
Bolmont, J.
Boeser, S.
Botner, O.
Bouchta, A.
Braun, J.
Burgess, T.
Castermans, T.
Chirkin, D.
Christy, B.
Clem, J.
Cowen, D. F.
D'Agostino, M. V.
Davour, A.
Day, C. T.
De Clercq, C.
Demiroers, L.
Descamps, F.
Desiati, P.
De Vries-Uiterweerd, G.
DeYoung, T.
Diaz-Velez, J. C.
Dreyer, J.
Dumm, J. P.
Duvoort, M. R.
Edwards, W. R.
Ehrlich, R.
Eisch, J.
Ellsworth, R. W.
Evenson, P. A.
Fadiran, O.
Fazely, A. R.
Filimonov, K.
Finley, C.
Foerster, M. M.
Fox, B. D.
Franckowiak, A.
Franke, R.
Gaisser, T. K.
Gallagher, J.
Ganugapati, R.
Geenen, H.
Gerhardt, L.
Goldschmidt, A.
Goodman, J. A.
Gozzini, R.
Griesel, T.
Gross, A.
Grullon, S.
Gunasingha, R. M.
Gurtner, M.
Ha, C.
Hallgren, A.
Halzen, F.
Han, K.
Hanson, K.
Hardtke, D.
Hardtke, R.
Hasegawa, Y.
Hauschildt, T.
Heise, J.
Helbing, K.
Hellwig, M.
Herquet, P.
Hill, G. C.
Hodges, J.
Hoffman, K. D.
Hommez, B.
Hoshina, K.
Hubert, D.
Hughey, B.
Huelss, J. -P.
Hulth, P. O.
Hultqvist, K.
Hundertmark, S.
Inaba, M.
Ishihara, A.
Jacobsen, J.
Japaridze, G. S.
Johansson, H.
Joseph, J. M.
Kampert, K. -H.
Kappes, A.
Karg, T.
Karle, A.
Kawai, H.
Kelley, J. L.
Kiryluk, J.
Kislat, F.
Kitamura, N.
Klein, S. R.
Klepser, S.
Kohnen, G.
Kolanoski, H.
Koepke, L.
Kowalski, M.
Kowarik, T.
Krasberg, M.
Kuehn, K.
Kuwabara, T.
Labare, M.
Laihem, K.
Landsman, H.
Lauer, R.
Leich, H.
Leier, D.
Liubarsky, I.
Lundberg, J.
Luenemann, J.
Madsen, J.
Maruyama, R.
Mase, K.
Matis, H. S.
McCauley, T.
McParland, C. P.
Meagher, K.
Meli, A.
Messarius, T.
Meszaros, P.
Miyamoto, H.
Montaruli, T.
Morey, A.
Morse, R.
Movit, S. M.
Muenich, K.
Nahnhauer, R.
Nam, J. W.
Niessen, P.
Nygren, D. R.
Olivas, A.
Ono, M.
Patton, S.
Heros, C. Perez De Los
Piegsa, A.
Pieloth, D.
Pohl, A. C.
Porrata, R.
Pretz, J.
Price, P. B.
Przybylski, G. T.
Rawlins, K.
Razzaque, S.
Redl, P.
Resconi, E.
Rhode, W.
Ribordy, M.
Rizzo, A.
Robbins, S.
Robbins, W. J.
Roth, P.
Rothmaier, F.
Rott, C.
Roucelle, C.
Rutledge, D.
Ryckbosch, D.
Sander, H. -G.
Sarkar, S.
Satalecka, K.
Schlenstedt, S.
Schmidt, T.
Schneider, D.
Schultz, O.
Seckel, D.
Semburg, B.
Seo, S. H.
Sestayo, Y.
Seunarine, S.
Silvestri, A.
Smith, A. J.
Song, C.
Spiczak, G. M.
Spiering, C.
Stamatikos, M.
Stanev, T.
Stezelberger, T.
Stokstad, R. G.
Stoufer, M. C.
Stoyanov, S.
Strahler, E. A.
Straszheim, T.
Sulanke, K. -H.
Sullivan, G. W.
Sumner, T. J.
Swillens, Q.
Taboada, I.
Tarasova, O.
Tepe, A.
Thollander, L.
Tilav, S.
Tluczykont, M.
Toale, P. A.
Tosi, D.
Turcan, D.
Van Eijndhoven, N.
Vandenbroucke, J.
Van Overloop, A.
Viscomi, V.
Vogt, C.
Voigt, B.
Wagner, W.
Walck, C.
Waldmann, H.
Waldenmaier, T.
Walter, M.
Wang, Y. -R.
Wendt, C.
Wiebusch, C. H.
Wiedemann, C.
Wikstroem, G.
Williams, D. R.
Wischnewski, R.
Wissing, H.
Woschnagg, K.
Xu, X. W.
Yodh, G.
Yoshida, S.
Zornoza, J. D.
CA IceCube Collaboration
TI Search for ultra-high-energy neutrinos with amanda-II
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE diffuse radiation; galaxies : active; neutrinos; telescopes
ID COSMIC-RAYS; LIMITS; SELECTION; DETECTOR; FLUX; KNEE
AB A search for diffuse neutrinos with energies in excess of 10(5) GeV is conducted with AMANDA-II data recorded between 2000 and 2002. Above 10(7) GeV, the Earth is essentially opaque to neutrinos. This fact, combined with the limited overburden of the AMANDA-II detector ( roughly 1.5 km), concentrates these ultra-high-energy neutrinos at the horizon. The primary background for this analysis is bundles of downgoing, high-energy muons from the interaction of cosmic rays in the atmosphere. No statistically significant excess above the expected background is seen in the data, and an upper limit is set on the diffuse all-flavor neutrino flux of E-2 Phi(90%CL) < 2.7x10(-7) GeV cm(-2) s(-1) sr(-1) valid over the energy range of 2x10(5) to 10(9) GeV. A number of models that predict neutrino fluxes from active galactic nuclei are excluded at the 90% confidence level.
C1 [Barwick, S. W.; Gerhardt, L.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Adams, J.; Han, K.; Seunarine, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Ahrens, J.; Gozzini, R.; Griesel, T.; Hellwig, M.; Koepke, L.; Kowarik, T.; Piegsa, A.; Rothmaier, F.; Sander, H. -G.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[Andeen, K.; Becka, T.; Boersma, D. J.; Braun, J.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Finley, C.; Ganugapati, R.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hodges, J.; Hoshina, K.; Hughey, B.; Jacobsen, J.; Kappes, A.; Karle, A.; Kelley, J. L.; Kitamura, N.; Krasberg, M.; Landsman, H.; Maruyama, R.; Montaruli, T.; Morse, R.; Schneider, D.; Song, C.; Stamatikos, M.; Strahler, E. A.; Wang, Y. -R.; Wendt, C.; Zornoza, J. D.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Auffenberg, J.; Becker, K. -H.; Franckowiak, A.; Geenen, H.; Gurtner, M.; Helbing, K.; Kampert, K. -H.; Karg, T.; Robbins, S.; Semburg, B.; Tepe, A.] Berg Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Bai, X.; Clem, J.; Demiroers, L.; Evenson, P. A.; Gaisser, T. K.; Hauschildt, T.; Kuwabara, T.; Niessen, P.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Waldenmaier, T.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bai, X.; Demiroers, L.; Hauschildt, T.; Niessen, P.; Rizzo, A.; Stanev, T.; Stoyanov, S.; Waldenmaier, T.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Baret, B.; De Clercq, C.; Hubert, D.; Kuehn, K.] Vrije Univ Brussels, Dienst ELEM, B-1050 Brussels, Belgium.
[Bay, R.; D'Agostino, M. V.; Filimonov, K.; Hardtke, D.; Morey, A.; Porrata, R.; Price, P. B.; Taboada, I.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Beattie, K.; Chirkin, D.; Day, C. T.; Edwards, W. R.; Goldschmidt, A.; Joseph, J. M.; Kiryluk, J.; Klein, S. R.; Matis, H. S.; McCauley, T.; McParland, C. P.; Nygren, D. R.; Patton, S.; Przybylski, G. T.; Roucelle, C.; Stezelberger, T.; Stokstad, R. G.; Stoufer, M. C.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Becker, J. K.; Dreyer, J.; Leier, D.; Luenemann, J.; Meli, A.; Messarius, T.; Muenich, K.; Rhode, W.] Univ Dortmund, Dept Phys, D-44221 Dortmund, Germany.
[Beimforde, M.; Kislat, F.; Kolanoski, H.; Kowalski, M.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Berghaus, P.; Bertrand, D.; Labare, M.; Swillens, Q.] Univ Libre Bruxelles, Fac Sci, B-1050 Brussels, Belgium.
[Berley, D.; Blaufuss, E.; Christy, B.; Ehrlich, R.; Ellsworth, R. W.; Goodman, J. A.; Hoffman, K. D.; Meagher, K.; Olivas, A.; Pretz, J.; Redl, P.; Roth, P.; Schmidt, T.; Smith, A. J.; Straszheim, T.; Sullivan, G. W.; Turcan, D.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Bohm, C.; Burgess, T.; Hulth, P. O.; Hultqvist, K.; Hundertmark, S.; Johansson, H.; Thollander, L.; Walck, C.; Wiedemann, C.; Wikstroem, G.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Botner, O.; Bouchta, A.; Davour, A.; Hallgren, A.; Lundberg, J.; Heros, C. Perez De Los; Pohl, A. C.] Uppsala Univ, Div High Energy Phys, S-75121 Uppsala, Sweden.
[Castermans, T.; Herquet, P.; Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Cowen, D. F.; DeYoung, T.; Foerster, M. M.; Fox, B. D.; Ha, C.; Meszaros, P.; Razzaque, S.; Robbins, W. J.; Rott, C.; Rutledge, D.; Seo, S. H.; Toale, P. A.; Viscomi, V.; Wagner, W.; Williams, D. R.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Cowen, D. F.; Meszaros, P.; Movit, S. M.; Razzaque, S.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Descamps, F.; Hommez, B.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Subatom & Radiat Phys, B-9000 Ghent, Belgium.
[De Vries-Uiterweerd, G.; Duvoort, M. R.; Heise, J.; Van Eijndhoven, N.] Univ Utrecht, Dept Phys & Astron, SRON, NL-3584 CC Utrecht, Netherlands.
[Fadiran, O.; Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Fazely, A. R.; Gunasingha, R. M.; Xu, X. W.] So Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Ackermann, M.; Bernardini, E.; Bolmont, J.; Boeser, S.; Franke, R.; Klepser, S.; Lauer, R.; Leich, H.; Nahnhauer, R.; Pieloth, D.; Satalecka, K.; Schlenstedt, S.; Spiering, C.; Sulanke, K. -H.; Tarasova, O.; Tluczykont, M.; Tosi, D.; Voigt, B.; Waldmann, H.; Walter, M.; Wischnewski, R.] DESY, D-15735 Zeuthen, Germany.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Gross, A.; Resconi, E.; Schultz, O.; Sestayo, Y.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany.
[Hardtke, R.; Madsen, J.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Hasegawa, Y.; Inaba, M.; Ishihara, A.; Kawai, H.; Mase, K.; Miyamoto, H.; Ono, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Huelss, J. -P.; Laihem, K.; Vogt, C.; Wiebusch, C. H.; Wissing, H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
[Liubarsky, I.; Sumner, T. J.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BW, England.
[Pohl, A. C.] Kalmar Univ, Sch Pure & Appl Nat Sci, S-39182 Kalmar, Sweden.
[Rawlins, K.] Univ Alaska, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland.
[Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Zornoza, J. D.] Univ Valencia, CSIC, IFIC, Valencia 46071, Spain.
RP Gerhardt, L (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
EM gerhardt@hep.ps.uci.edu
RI Zornoza, Juan de Dios/L-1604-2014; Maruyama, Reina/A-1064-2013; Song,
Chihwa/A-3455-2008; Hundertmark, Stephan/A-6592-2010; Vogt,
Christian/E-2028-2012; Wiebusch, Christopher/G-6490-2012; Kowalski,
Marek/G-5546-2012; Hallgren, Allan/A-8963-2013; Botner,
Olga/A-9110-2013; Tjus, Julia/G-8145-2012; Auffenberg, Jan/D-3954-2014;
OI Zornoza, Juan de Dios/0000-0002-1834-0690; Maruyama,
Reina/0000-0003-2794-512X; Perez de los Heros,
Carlos/0000-0002-2084-5866; Wiebusch, Christopher/0000-0002-6418-3008;
Auffenberg, Jan/0000-0002-1185-9094; Hubert, Daan/0000-0002-4365-865X;
Lauer, Robert/0000-0003-1933-7861; Sarkar, Subir/0000-0002-3542-858X
NR 56
TC 74
Z9 74
U1 1
U2 9
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2008
VL 675
IS 2
BP 1014
EP 1024
DI 10.1086/527046
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 271VT
UT WOS:000253817500006
ER
PT J
AU Rykoff, ES
Mckay, TA
Becker, MR
Evrard, A
Johnston, DE
Koester, BP
Rozo, E
Sheldon, ES
Wechsler, RH
AF Rykoff, E. S.
McKay, T. A.
Becker, M. R.
Evrard, A.
Johnston, D. E.
Koester, B. P.
Rozo, E.
Sheldon, E. S.
Wechsler, R. H.
TI Measuring the mean and scatter of the X-ray luminosity-optical richness
relation for maxBCG galaxy clusters
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE galaxies : clusters : general; X-rays : galaxies : clusters
ID DIGITAL SKY SURVEY; SPECTROSCOPIC TARGET SELECTION; WEAK-LENSING
ANALYSIS; FLUX-LIMITED SAMPLE; SUNYAEV-ZELDOVICH; REDSHIFT SURVEY; ABELL
CLUSTERS; DISTANT CLUSTERS; COOLING-CORE; DARK-MATTER
AB Determining the scaling relations between galaxy cluster observables requires large samples of uniformly observed clusters. We measure the mean X-ray luminosity-optical richness ((L) over bar (X)-(N) over bar (200)) relation for an approximately volume-limited sample of more than 17,000 optically selected clusters from the maxBCG catalog spanning the redshift range 0.1 < z < 0.3. By stacking the X-ray emission from many clusters using ROSAT All-Sky Survey data, we are able to measure mean X-ray luminosities to similar to 10% (including systematic errors) for clusters in nine independent optical richness bins. In addition, we are able to crudely measure individual X-ray emission from similar to 800 of the richest clusters. Assuming a lognormal form for the scatter in the L-X-N-200 relation, we measure sigma(ln L) = 0.86 +/- 0.03 at fixed N-200. This scatter is large enough to significantly bias the mean stacked relation. The corrected median relation can be parameterized by (L) over tilde (X) = e(alpha)((N) over bar (200)/40)(beta) x 10(42) h(-2) ergs s(-1), where alpha = 3.57 +/- 0.08 and beta = 1.82 +/- 0.05. We find that X-ray-selected clusters are significantly brighter than optically selected clusters at a given optical richness. This selection bias explains the apparently X-ray-underluminous nature of optically selected cluster catalogs.
C1 [Rykoff, E. S.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Rykoff, E. S.; McKay, T. A.; Becker, M. R.; Evrard, A.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[McKay, T. A.; Evrard, A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[McKay, T. A.; Evrard, A.] Michigan Ctr Theoret Phys, Ann Arbor, MI 48109 USA.
[Johnston, D. E.] Jet Prop Lab, Pasadena, CA 91109 USA.
[Koester, B. P.] Univ Chicago, Dept Astron, Chicago, IL 60637 USA.
[Rozo, E.] Ohio State Univ, Columbus, OH 43201 USA.
[Sheldon, E. S.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
[Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford Linear Accelerator Ctr, Stanford, CA 94305 USA.
RP Rykoff, ES (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
EM erykoff@physics.ucsb.edu
RI McKay, Timothy/C-1501-2009;
OI McKay, Timothy/0000-0001-9036-6150; Evrard, August/0000-0002-4876-956X;
Becker, Matthew/0000-0001-7774-2246
NR 106
TC 58
Z9 58
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2008
VL 675
IS 2
BP 1106
EP 1124
DI 10.1086/527537
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 271VT
UT WOS:000253817500014
ER
PT J
AU Corbet, RHD
Sokoloski, JL
Mukai, K
Markwardt, CB
Tueller, J
AF Corbet, R. H. D.
Sokoloski, J. L.
Mukai, K.
Markwardt, C. B.
Tueller, J.
TI A comparison of the variability of the symbiotic X-ray binaries GX 1+4,
4U 1954+31, and 4U 1700+24 from Swift bat and RXTE ASM observations
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries : symbiotic; stars : individual (GX 1+4, 4U 1954+31, 4U
1700+24) stars : neutron; X-rays : binaries
ID ACCRETING PULSAR GX-1+4; ALL-SKY MONITOR; NEUTRON-STAR; TIMING-EXPLORER;
ORBITAL PERIOD; 2S 0114+650; SCUTUM X-1; RED NOISE; COUNTERPARTS;
LUMINOSITY
AB We present an analysis of the X-ray variability of three symbiotic X-ray binaries, GX 1+4, 4U 1700+24, and 4U 1954+31, using observations made with the Swift Burst Alert Telescope (BAT) and the Rossi X-Ray Timing Explorer (RXTE) All-Sky Monitor (ASM). Observations of 4U 1954+31 with the Swift BAT show modulation at a period near 5 hr. Models to explain this modulation are discussed, including the presence of an exceptionally slow X-ray pulsar in the system and accretion instabilities. We conclude that the most likely interpretation is that 4U 1954+31 contains one of the slowest known X-ray pulsars. Unlike 4U 1954+31, neither GX 1+4 nor 4U 1700+24 show any evidence for modulation on a timescale of hours. An analysis of the RXTE ASM light curves of GX 1+4, 4U 1700+24, and 4U 1954+31 does not show the presence of periodic modulation in any source, with the exception of a possible detection of the 5 hr period in 4U 1954+31, although there is considerable variability on long timescales for all three sources. There is no modulation in GX 1+4 on either the optical 1161 day orbital period or a previously reported 304 day X-ray period. For 4U 1700+24 we do not confirm the 404 day X-ray period previously proposed for this source from a shorter duration ASM light curve. We conclude that all three sources have substantial low-frequency noise in their power spectra that may give the appearance of periodic modulation if this noise is not properly accounted for, particularly if short-duration light curves are examined.
C1 [Corbet, R. H. D.; Mukai, K.; Markwardt, C. B.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Corbet, R. H. D.; Mukai, K.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21228 USA.
[Sokoloski, J. L.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Markwardt, C. B.] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA.
[Tueller, J.] NASA, Goddard Space Flight Ctr, Astrophys Phys Lab, Greenbelt, MD 20771 USA.
RP Corbet, RHD (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Mail Code 662, Greenbelt, MD 20771 USA.
EM Corbet@nasa.gov
RI Tueller, Jack/D-5334-2012
NR 57
TC 25
Z9 26
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2008
VL 675
IS 2
BP 1424
EP 1435
DI 10.1086/526337
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 271VT
UT WOS:000253817500033
ER
PT J
AU Hartman, JM
Patruno, A
Chakrabarty, D
Kaplan, DL
Markwardt, CB
Morgan, EH
Ray, PS
van der Klis, M
Wijnands, R
AF Hartman, Jacob M.
Patruno, Alessandro
Chakrabarty, Deepto
Kaplan, David L.
Markwardt, Craig B.
Morgan, Edward H.
Ray, Paul S.
van der Klis, Michiel
Wijnands, Rudy
TI The long-term evolution of the spin, pulse shape, and orbit of the
accretion-powered millisecond pulsar SAX J1808.4-3658
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars : individual (SAX J1808.4-3658); stars : neutron; X-rays : stars
ID RAY-TIMING-EXPLORER; PROPORTIONAL COUNTER ARRAY; ACTIVE RADIO PULSAR;
BINARY PSR B1957+20; NEUTRON-STARS; OPTICAL COUNTERPART;
GRAVITATIONAL-RADIATION; CATACLYSMIC VARIABLES; IGR J00291+5934;
EMISSION
AB We present a 7 yr timing study of the 2.5 ms X-ray pulsar SAX J1808.4-3658, an X-ray transient with a recurrence time of approximate to 2 yr, using data from the Rossi X-Ray Timing Explorer covering four transient outbursts (1998-2005). We verify that the 401 Hz pulsation traces the spin frequency fundamental and not a harmonic. Substantial pulse shape variability, both stochastic and systematic, was observed during each outburst. Analysis of the systematic pulse shape changes suggests that, as an outburst dims, the X-ray "hot spot'' on the pulsar surface drifts longitudinally and a second hot spot may appear. The overall pulse shape variability limits the ability to measure spin frequency evolution within a given X-ray outburst (and calls previous. (nu) over dot measurements of this source into question), with typical upper limits of vertical bar(nu) over dot vertical bar less than or similar to 2.5 x 10(-14) Hz s(-1) (2 sigma). However, combining data from all the outbursts shows with high (6 sigma) significance that the pulsar is undergoing long-term spin down at a rate. (nu) over dot = (-5.6 +/- 2.0) x 10(-16) Hz s(-1), with most of the spin evolution occurring during X-ray quiescence. We discuss the possible contributions of magnetic propeller torques, magnetic dipole radiation, and gravitational radiation to the measured spin down, setting an upper limit of B < 1.5 x 10(8) G for the pulsar's surface dipole magnetic field and Q/I < 5 x 10(-9) for the fractional mass quadrupole moment. We also measured an orbital period derivative of (P) over dot(orb) (3.5 +/- 0.2) x 10(-12) s s(-1). This surprisingly large (P) over dot(orb) is reminiscent of the large and quasi-cyclic orbital period variation observed in the so-called black widow millisecond radio pulsars, which further strengthens previous speculation that SAX J1808.4-3658 may turn on as a radio pulsar during quiescence. In an appendix we derive an improved (0: 1500) source position from optical data.
C1 MIT, Dept Phys, Cambridge, MA 02139 USA.
MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands.
Univ Amsterdam, Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands.
[Markwardt, Craig B.] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA.
[Markwardt, Craig B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Ray, Paul S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
RP Hartman, JM (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA.
EM jhartman@space.mit.edu; apatruno@science.uva.nl; deepto@space.mit.edu;
craigm@milkyway.gsfc.nasa.gov; ehm@space.mit.edu; paul.ray@nrl.navy.mil;
michiel@science.uva.nl; rudy@science.uva.nl
OI Ray, Paul/0000-0002-5297-5278
NR 83
TC 104
Z9 104
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 MAR 10
PY 2008
VL 675
IS 2
BP 1468
EP 1486
DI 10.1086/527461
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 271VT
UT WOS:000253817500037
ER
PT J
AU Suchy, S
Pottschmidt, K
Wilms, J
Kreykenbohm, I
Schonherr, G
Kretschmar, P
McBride, V
Caballero, I
Rothschild, RE
Grinberg, V
AF Suchy, Slawomir
Pottschmidt, Katja
Wilms, Joern
Kreykenbohm, Ingo
Schoenherr, Gabriele
Kretschmar, Peter
McBride, Vanessa
Caballero, Isabel
Rothschild, Richard E.
Grinberg, Victoria
TI Pulse phase-resolved analysis of the high-mass X-ray binary centaurus
X-3 over two binary orbits
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars : individual (Centarus X-3); stars : magnetic fields; X-rays :
binaries; X-rays : stars
ID CYCLOTRON-LINE FEATURES; STELLAR WIND ACCRETION; TIMING-EXPLORER; VELA
X-1; CEN X-3; SCATTERING FEATURE; MAGNETIC-FIELDS; NEUTRON-STAR;
DISCOVERY; SPECTRUM
AB We present a detailed analysis of observations of the high-mass X-ray binary Cen X-3, spanning two consecutive binary orbits performed with the RXTE satellite in early March 1997. During this time Cen X-3 had a luminosity of L2-10 keV similar to (4-5) x 10(37) ergs s(-1) and a pulse period of 4.814 s. The PCA and HEXTE light curves both show a clear reduction in count rate after midorbit for both binary revolutions. We therefore analyze two broadband spectra for each orbit, before and after midorbit. Consistent with earlier observations, these four joint PCA and HEXTE spectra can be well described using a phenomenological pulsar continuum model, including an iron emission line and a cyclotron resonance-scattering feature. While no strong spectral variations were detected, the second half of orbit 2 shows a tendency toward being softer and more strongly absorbed. In order to follow the orbital phase-dependent evolution of the spectrum in greater detail, we model spectra for shorter exposures, confirming that most spectral parameters show either a gradual or sudden change for the second half of the second orbit. A comparison with a simple wind model indicates the existence of an accretion wake in this system. We also present and discuss high-resolution pulse profiles for several different energy bands, as well as their hardness ratios. PCA and HEXTE spectra were created for 24 phase bins and fitted using the same model as in the phase-averaged case. Systematic pulse phase-dependent variations of several continuum and cyclotron line parameters were detected, most notably a significant increase of the cyclotron line energy during the early rise of the main peak, followed by a gradual decrease. We show that applying a simple dipole model for the magnetic field is not sufficient to describe our data.
C1 [Suchy, Slawomir; Pottschmidt, Katja; Rothschild, Richard E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Pottschmidt, Katja] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Wilms, Joern] Astron Inst, D-96049 Bamberg, Germany.
[Kreykenbohm, Ingo; Caballero, Isabel] Inst Astron & Astrophys, Abt Astron, D-72076 Tubingen, Germany.
[Kreykenbohm, Ingo] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Schoenherr, Gabriele] Inst Astrophys, D-14482 Potsdam, Germany.
[Kretschmar, Peter] European Space Agcy, European Space Astron Ctr, Madrid 28691, Spain.
[McBride, Vanessa] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Grinberg, Victoria] Univ Munich, Fac Phys, D-80799 Munich, Germany.
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; kpottschmidt@ucsd.edu;
joern.wilms@sternwarte.uni-erlangen.de; kreyken@astro.uni-tuebingen.de;
gschoenherr@aip.de; peter.kretschmar@esa.int; vanessa@astro.soton.ac.uk;
isabel@astro.uni-tuebingende; rrothschild@ucsd.edu;
victoria.grinberg@physik.lmu.de
RI Wilms, Joern/C-8116-2013; Kreykenbohm, Ingo/H-9659-2013;
OI Wilms, Joern/0000-0003-2065-5410; Kreykenbohm, Ingo/0000-0001-7335-1803;
Kretschmar, Peter/0000-0001-9840-2048
NR 64
TC 34
Z9 34
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2008
VL 675
IS 2
BP 1487
EP 1498
DI 10.1086/527042
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 271VT
UT WOS:000253817500038
ER
PT J
AU Thommes, EW
Bryden, G
Wu, YQ
Rasio, FA
AF Thommes, Edward W.
Bryden, Geoffrey
Wu, Yanqin
Rasio, Frederic A.
TI From mean motion resonances to scattered planets: Producing the solar
system, eccentric exoplanets, and late heavy bombardments
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems : formation; solar system : formation
ID EDGEWORTH-KUIPER BELT; GIANT PLANETS; PROTOPLANETARY DISK; DYNAMICAL
INSTABILITIES; PLANETESIMAL DISK; ORBITAL EVOLUTION; DENSITY WAVES;
MIGRATION; NEPTUNE; ORIGIN
AB We show that interaction with a gas disk may produce young planetary systems with closely spaced orbits, stabilized by mean motion resonances between neighbors. On longer timescales, after the gas is gone, interaction with a remnant planetesimal disk tends to pull these configurations apart, eventually inducing dynamical instability. We find that this can lead to a variety of outcomes; some cases resemble the solar system, while others end up with high-eccentricity orbits reminiscent of the observed exoplanets. A similar mechanism has been previously suggested as the cause of the lunar late heavy bombardment. Thus, it may be that a large-scale dynamical instability, with more or less cataclysmic results, is an evolutionary step common to many planetary systems, including our own.
C1 [Thommes, Edward W.; Rasio, Frederic A.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
[Bryden, Geoffrey] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wu, Yanqin] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
RP Thommes, EW (reprint author), Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
OI Rasio, Frederic/0000-0002-7132-418X
NR 46
TC 43
Z9 43
U1 1
U2 6
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2008
VL 675
IS 2
BP 1538
EP 1548
DI 10.1086/525244
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 271VT
UT WOS:000253817500044
ER
PT J
AU Atrio-Barandela, F
Kashlinsky, A
Kocevski, D
Ebeling, H
AF Atrio-Barandela, F.
Kashlinsky, A.
Kocevski, D.
Ebeling, H.
TI Measurement of the electron-pressure profile of galaxy clusters in 3
year Wilkinson microwave anisotropy probe (WMAP) data
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmic microwave background; cosmology : observations; cosmology :
theory
ID X-RAY SEARCH; INTRACLUSTER MEDIUM; POWER SPECTRUM; MILKY-WAY; SAMPLE;
MAPS; GAS; COSMOLOGY; EINSTEIN; DENSITY
AB Using 3 year WMAP data at the locations of similar to 700 X-ray-selected clusters, we have detected the amplitude of the thermal Sunyaev-Zeldovich (TSZ) effect at the 15 sigma level, the highest statistical significance reported so far. Owing to the large size of our cluster sample, we are able to detect the corresponding cosmic microwave background distortions out to large cluster-centric radii. The region over which the TSZ signal is detected is, on average, 4 times larger in radius than the X-ray-emitting region, extending to similar to 3 h(70)(-1) Mpc. We show that an isothermal b- model does not fit the electron pressure at large radii; instead, the baryon profile is consistent with the Navarro-Frenk-White profile, which is expected for dark matter in the concordance Lambda CDM model. The Xray temperature at the virial radius of the clusters falls by a factor similar to 3-4 from the central value, depending on the cluster concentration parameter. Our results suggest that cluster dynamics at large radii is dominated by dark matter and is well described by Newtonian gravity.
C1 [Atrio-Barandela, F.] Univ Salamanca, E-37008 Salamanca, Spain.
[Kashlinsky, A.] NASA, Goddard Space Flight Ctr, SSAI, Greenbelt, MD 20771 USA.
[Kashlinsky, A.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Kocevski, D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Ebeling, H.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP Atrio-Barandela, F (reprint author), Univ Salamanca, E-37008 Salamanca, Spain.
EM atrio@usal.es
RI Atrio-Barandela, Fernando/A-7379-2017
OI Atrio-Barandela, Fernando/0000-0002-2130-2513
NR 37
TC 43
Z9 43
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 10
PY 2008
VL 675
IS 2
BP L57
EP L60
DI 10.1086/533437
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 291ZC
UT WOS:000255235100001
ER
PT J
AU Nitta, NV
Mason, GM
Wiedenbeck, ME
Cohen, CMS
Krucker, S
Hannah, IG
Shimojo, M
Shibata, K
AF Nitta, Nariaki V.
Mason, Glenn M.
Wiedenbeck, Mark E.
Cohen, Christina M. S.
Krucker, Sam
Hannah, Iain G.
Shimojo, Masumi
Shibata, Kazunari
TI Coronal jet observed by Hinode as the source of a He-3-rich solar
energetic particle event
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun : flares; Sun : particle emission; Sun : X-rays; gamma rays
ID X-RAY JETS; ISOTOPE SPECTROMETER; ELECTRON EVENTS; WIND SPACECRAFT;
TELESCOPE; MISSION; PLASMA; IMAGER; SUN; ACCELERATION
AB We study the solar source of the 3He-rich solar energetic particle (SEP) event observed on 2006 November 18. The SEP event showed a clear velocity dispersion at energies below 1 MeV nucleon(-1), indicating its solar origin. We associate the SEP event with a coronal jet in an active region at heliographic longitude of W50 degrees, as observed in soft X-rays. This jet was the only noticeable activity in full-disk X-ray images around the estimated release time of the ions. It was temporally correlated with a series of type III radio bursts detected in metric and longer wavelength ranges and was followed by a nonrelativistic electron event. The jet may be explained in terms of the model of an expanding loop reconnecting with a large-scale magnetic field, which is open to interplanetary space for the particles to be observed at 1 AU. The open field lines appear to be anchored at the boundary between the umbra and penumbra of the leading sunspot, where a brightening is observed in both soft and hard X-rays during the jet activity. Other flares in the same region possibly associated with He-3-rich SEP events were not accompanied by a jet, indicative of different origins of this type of SEP event.
C1 [Nitta, Nariaki V.] Org ADBS, Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Mason, Glenn M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Wiedenbeck, Mark E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wiedenbeck, Mark E.; Cohen, Christina M. S.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
[Krucker, Sam; Hannah, Iain G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Krucker, Sam; Shimojo, Masumi] Natl Inst Nat Sci, Natl Astron Observ Japan, Nobeyama Radio Observ, Minamimaki, Nagano 3841305, Japan.
[Shibata, Kazunari] Kyoto Univ, Kwasan Observ, Yamashina Ku, Kyoto 6078471, Japan.
[Shibata, Kazunari] Kyoto Univ, Hida Observ, Yamashina Ku, Kyoto 6078471, Japan.
RP Nitta, NV (reprint author), Org ADBS, Lockheed Martin Solar & Astrophys Lab, Bldg 252,3251 Hanover St, Palo Alto, CA 94304 USA.
EM nitta@lmsal.com
RI Hannah, Iain/F-1972-2011; Shimojo, Masumi/J-2605-2016
OI Hannah, Iain/0000-0003-1193-8603; Shimojo, Masumi/0000-0002-2350-3749
NR 31
TC 24
Z9 24
U1 0
U2 6
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 MAR 10
PY 2008
VL 675
IS 2
BP L125
EP L128
DI 10.1086/533438
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 291ZC
UT WOS:000255235100018
ER
PT J
AU Remijan, AJ
Hollis, JM
Lovas, FJ
Stork, WD
Jewell, PR
Meier, DS
AF Remijan, Anthony J.
Hollis, J. M.
Lovas, F. J.
Stork, Wilmer D.
Jewell, P. R.
Meier, D. S.
TI Detection of interstellar cyanoformaldehyde (CNCHO)
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM : abundances; ISM : clouds; ISM : individual (Sagittarius
B2(N-LMH)); ISM : molecules; radio lines : ISM
ID GREEN-BANK TELESCOPE; FORMYL CYANIDE; GALACTIC-CENTER; GLYCOLALDEHYDE;
CHOCN; MOLECULES; SPECTRUM; SUGAR; LINES; HCOCN
AB Cyanoformaldehyde (CNCHO) has been detected toward the star-forming region Sagittarius B-2(N) with the 100 m Green Bank Telescope (GBT) by means of four P-branch rotational transitions in emission, the 7(0, 7)-6(1, 6) at 8.6 GHz, the 8(0, 8)-7(1, 7) at 19.4 GHz, the 9(0, 9)-8(1, 8) at 30.3 GHz, and the 10(0, 10)-9(1, 9) at 41.3 GHz, and one P-branch transition in absorption, the 5(1, 5)-6(0, 6) at 2.1 GHz. The five b-type transitions have favorable transition line strengths (S-ij mu(2) > 10 D-2) and occur in spectral regions that have little possibility of confusion with other molecular 2 species. The transition line strengths and energy levels involved in the four cyanoformaldehyde transitions in emission are similar; however, transitions with larger beam sizes give systematically higher column densities, suggesting that CNCHO is spatially extended and not concentrated toward the Sgr B2(N-LMH) position. Moreover, with a GBT beamwidth of similar to 350'', the 5(1, 5)-6(0, 6) transition of CNCHO was detected in absorption, confirming the widespread spatial extent of this molecule. We suggest that cyanoformaldehyde is likely formed in a neutral-radical reaction of two other interstellar molecules known for widespread spatial distributions: formaldehyde (H2CO) and the cyanide (CN) radical.
C1 [Remijan, Anthony J.; Jewell, P. R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Hollis, J. M.] NASA, Goddard Space Flight Ctr, Computat & Informat Sci & Technol Off, Greenbelt, MD 20771 USA.
[Lovas, F. J.] Natl Inst Stand & Technol, Opt Technol Div, Gaithersburg, MD 20899 USA.
[Stork, Wilmer D.] Plastipak Packaging Inc, Champaign, IL 61821 USA.
[Stork, Wilmer D.] Parkland Coll, Dept Nat Sci, Champaign, IL 61821 USA.
[Meier, D. S.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
RP Remijan, AJ (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA.
NR 27
TC 23
Z9 23
U1 1
U2 4
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 10
PY 2008
VL 675
IS 2
BP L85
EP L88
DI 10.1086/533529
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 291ZC
UT WOS:000255235100008
ER
PT J
AU Prates-Clark, CD
Saatchi, SS
Agosti, D
AF Prates-Clark, Cassia Da Conceicao
Saatchi, Sassan S.
Agosti, Donat
TI Predicting geographical distribution models of high-value timber trees
in the Amazon Basin using remotely sensed data
SO ECOLOGICAL MODELLING
LA English
DT Article
DE Amazon Basin; climate variables; ecological niche; remote sensing data;
species distribution model; timber trees
ID GLOBAL LAND AREAS; RAIN-FOREST; VIROLA-SURINAMENSIS; SPECIES RICHNESS;
BRAZILIAN AMAZON; PLANT-GROWTH; CORAL-REEFS; COSTA-RICA; LEAF-AREA;
VEGETATION
AB Species distribution models were developed for three high economic value timber trees (Calophyllum brasiliensis, Carapa quianensis and Virola surinamensis) that are heavily harvested in the Amazon Basin. A combination of habitat measurements extracted from remote sensing data (MODIS, QSCAT and SRTM) and bioclimatic surfaces was examined to ascertain the most influential factors determining the occurrence of these tree species. The prediction of species' occurrence rates was tested separately for each species distribution model and the results were examined for their ability to accurately map the spatial distribution of these tree species. By evaluating the omission and commission rates we concluded that species distribution models based on remote sensing data contributed significantly in quantifying environmental properties used to summarize the ecological niche of each tree species. Specific vegetation characteristics (such as percentage of tree cover, vegetation moisture and roughness, annual NDVI and mean LAI during the dry LAI) showed the dependence of these species' occurrence in more densely vegetated forests. Areas with high leaf area (even during the dry months) and areas with high vegetation moisture were predicted as potential species habitat for C. brasiliensis. The density vegetation during the dry season and vegetation phenology were strongly correlated with climate differences, such as variations in air temperature and precipitation seasonality for V surinamensis. Lower elevation areas with more exuberant vegetation and a high greenness index were among the most important factors accounting for the geographical distribution of C. guianensis. Species distribution models are increasingly important in many fields of research and conservation. The potential of remotely sensed data to monitor environmental changes in tropical areas, along with the understanding of ecosystem function, are both critical for conservation of biodiversity and the long-term process of sustaining ecosystems. (c) 2007 Elsevier B.V All rights reserved.
C1 [Prates-Clark, Cassia Da Conceicao] Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England.
[Prates-Clark, Cassia Da Conceicao; Saatchi, Sassan S.] Univ Calif Los Angeles, Ctr Trop Res, Los Angeles, CA 90095 USA.
[Saatchi, Sassan S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Agosti, Donat] Naturmuseum Burgergemeinde Bern, CH-3005 Bern, Switzerland.
RP Prates-Clark, CD (reprint author), Univ Bristol, Sch Geog Sci, Univ Rd, Bristol BS8 1SS, Avon, England.
EM Cassia.Prates-Clark@bristol.ac.uk
OI Agosti, Donat /0000-0001-9286-1200
NR 91
TC 30
Z9 34
U1 1
U2 24
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0304-3800
EI 1872-7026
J9 ECOL MODEL
JI Ecol. Model.
PD MAR 10
PY 2008
VL 211
IS 3-4
BP 309
EP 323
DI 10.1016/j.ecolmodel.2007.09.024
PG 15
WC Ecology
SC Environmental Sciences & Ecology
GA 270DS
UT WOS:000253700900006
ER
PT J
AU Mlynczak, MG
Martin-Torres, FJ
Mertens, CJ
Marshall, BT
Thompson, RE
Kozyra, JU
Remsberg, EE
Gordley, LL
Russell, JM
Woods, T
AF Mlynczak, Martin G.
Martin-Torres, F. Javier
Mertens, Christopher J.
Marshall, B. Thomas
Thompson, R. Earl
Kozyra, Janet U.
Remsberg, Ellis E.
Gordley, Larry L.
Russell, James M., III
Woods, Thomas
TI Solar-terrestrial coupling evidenced by periodic behavior in geomagnetic
indexes and the infrared energy budget of the thermosphere
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MESOSPHERE; ENERGETICS
AB We examine time series of the daily global power (W) radiated by carbon dioxide (at 15 mm) and by nitric oxide (at 5.3 mu m) from the Earth's thermosphere between 100 km and 200 km altitude. Also examined is a time series of the daily absorbed solar ultraviolet power in the same altitude region in the wavelength span 0 to 175 nm. The infrared data are derived from the SABER instrument and the solar data are derived from the SEE instrument, both on the NASA TIMED satellite. The time series cover nearly 5 years from 2002 through 2006. The infrared and solar time series exhibit a decrease in radiated and absorbed power consistent with the declining phase of the current 11-year solar cycle. The infrared time series also exhibits high frequency variations that are not evident in the solar power time series. Spectral analysis shows a statistically significant 9-day periodicity in the infrared data but not in the solar data. A very strong 9-day periodicity is also found to exist in the time series of daily A(p) and K(p) geomagnetic indexes. These 9-day periodicities are linked to the recurrence of coronal holes on the Sun. These results demonstrate a direct coupling between the upper atmosphere of the Sun and the infrared energy budget of the thermosphere.
C1 [Mlynczak, Martin G.; Mertens, Christopher J.; Remsberg, Ellis E.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Martin-Torres, F. Javier] Analyt Serv & Mat Inc, Hampton, VA 23666 USA.
[Marshall, B. Thomas; Thompson, R. Earl; Gordley, Larry L.] G&A Tech Software, Newport News, VA 23606 USA.
[Kozyra, Janet U.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Russell, James M., III] Hampton Univ, Hampton, VA USA.
[Woods, Thomas] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
RP Mlynczak, MG (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
EM m.g.mlynczak@nasa.gov
RI Mlynczak, Martin/K-3396-2012; Martin-Torres, Francisco
Javier/G-6329-2015
OI Martin-Torres, Francisco Javier/0000-0001-6479-2236
NR 16
TC 63
Z9 63
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 8
PY 2008
VL 35
IS 5
AR L05808
DI 10.1029/2007GL032620
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 276QA
UT WOS:000254156000004
ER
PT J
AU Ren, XR
Olson, JR
Crawford, JH
Brune, WH
Mao, JQ
Long, RB
Chen, Z
Chen, G
Avery, MA
Sachse, GW
Barrick, JD
Diskin, GS
Huey, LG
Fried, A
Cohen, RC
Heikes, B
Wennberg, PO
Singh, HB
Blake, DR
Shetter, RE
AF Ren, Xinrong
Olson, Jennifer R.
Crawford, James H.
Brune, William H.
Mao, Jingqiu
Long, Robert B.
Chen, Zhong
Chen, Gao
Avery, Melody A.
Sachse, Glen W.
Barrick, John D.
Diskin, Glenn S.
Huey, L. Greg
Fried, Alan
Cohen, Ronald C.
Heikes, Brian
Wennberg, Paul O.
Singh, Hanwant B.
Blake, Donald R.
Shetter, Richard E.
TI HOx chemistry during INTEX-A 2004: Observation, model calculation, and
comparison with previous studies
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID LASER-INDUCED FLUORESCENCE; PEM-TROPICS-B; UPPER TROPOSPHERE; OZONE
PRODUCTION; BOUNDARY-LAYER; NITROUS-ACID; RURAL SITE; TRACE-P; OH;
RADICALS
AB OH and HO2 were measured with the Airborne Tropospheric Hydrogen Oxides Sensor (ATHOS) as part of a large measurement suite from the NASA DC-8 aircraft during the Intercontinental Chemical Transport Experiment-A ( INTEX-A). This mission, which was conducted mainly over North America and the western Atlantic Ocean in summer 2004, was an excellent test of atmospheric oxidation chemistry. The HOx results from INTEX-A are compared to those from previous campaigns and to results for other related measurements from INTEX-A. Throughout the troposphere, observed OH was generally 0.95 of modeled OH; below 8 km, observed HO2 was generally 1.20 of modeled HO2. This observed-to-modeled comparison is similar to that for TRACE-P, another midlatitude study for which the median observed-to-modeled ratio was 1.08 for OH and 1.34 for HO2, and to that for PEM-TB, a tropical study for which the median observed-to-modeled ratio was 1.17 for OH and 0.97 for HO2. HO2 behavior above 8 km was markedly different. The observed-to-modeled HO2 ratio increased from similar to 1.2 at 8 km to similar to 3 at 11 km with the observed-to-modeled ratio correlating with NO. Above 8 km, the observed-to-modeled HO2 and observed NO were both considerably greater than observations from previous campaigns. In addition, the observed-to-modeled HO2/OH, which is sensitive to cycling reactions between OH and HO2, increased from similar to 1.5 at 8 km to almost 3.5 at 11 km. These discrepancies suggest a large unknown HOx source and additional reactants that cycle HOx from OH to HO2. In the continental planetary boundary layer, the observed-to-modeled OH ratio increased from 1 when isoprene was less than 0.1 ppbv to over 4 when isoprene was greater than 2 ppbv, suggesting that forests throughout the United States are emitting unknown HOx sources. Progress in resolving these discrepancies requires a focused research activity devoted to further examination of possible unknown OH sinks and HOx sources.
C1 [Ren, Xinrong; Brune, William H.; Mao, Jingqiu; Long, Robert B.; Chen, Zhong] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Olson, Jennifer R.; Crawford, James H.; Chen, Gao; Avery, Melody A.; Sachse, Glen W.; Barrick, John D.; Diskin, Glenn S.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
[Huey, L. Greg] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Fried, Alan] Natl Ctr Atmospher Res, Earth Observing Lab, Boulder, CO 80307 USA.
[Cohen, Ronald C.] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA.
[Cohen, Ronald C.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Heikes, Brian] Univ Rhode Isl, Grad Sch Oceanog, Kingston, RI 02881 USA.
[Wennberg, Paul O.] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA.
[Singh, Hanwant B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Blake, Donald R.] Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA.
[Shetter, Richard E.] Univ N Dakota, Natl Suborbital Educ & Res Ctr, Grand Forks, ND 58202 USA.
RP Ren, XR (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, 4600 Rickenbacker Causeway, Miami, FL 33149 USA.
EM xren@rsmas.miami.edu
RI Mao, Jingqiu/F-2511-2010; Cohen, Ronald/A-8842-2011; Ren,
Xinrong/B-2229-2010; Wennberg, Paul/A-5460-2012; Crawford,
James/L-6632-2013; Ren, Xinrong/E-7838-2015
OI Mao, Jingqiu/0000-0002-4774-9751; Cohen, Ronald/0000-0001-6617-7691;
Crawford, James/0000-0002-6982-0934; Ren, Xinrong/0000-0001-9974-1666
NR 42
TC 105
Z9 105
U1 2
U2 39
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 8
PY 2008
VL 113
IS D5
AR D05310
DI 10.1029/2007JD009166
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 276QL
UT WOS:000254157100006
ER
PT J
AU Kedar, S
Longuet-Higgins, M
Webb, F
Graham, N
Clayton, R
Jones, C
AF Kedar, Sharon
Longuet-Higgins, Michael
Webb, Frank
Graham, Nicholas
Clayton, Robert
Jones, Cathleen
TI The origin of deep ocean microseisms in the North Atlantic Ocean
SO PROCEEDINGS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING
SCIENCES
LA English
DT Article
DE microseisms; wave-wave interaction; acoustic resonance; wave model;
Stoneley waves
ID RAYLEIGH-WAVE ATTENUATION; AMBIENT SEISMIC NOISE; SECONDARY MICROSEISMS;
AMERICA; SEA; GENERATION; STATIONS; SPECTRUM
AB Oceanic microseisms are small oscillations of the ground, in the frequency range of 0.05 0.3 Hz, associated with the occurrence of energetic ocean waves of half the corresponding frequency. In 1950, Longuet-Higgins suggested in a landmark theoretical paper that (i) microseisms originate from surface pressure oscillations caused by the interaction between oppositely travelling components with the same frequency in the ocean wave spectrum, (ii) these pressure oscillations generate seismic Stoneley waves on the ocean bottom, and (iii) when the ocean depth is comparable with the acoustic wavelength in water, compressibility must be considered. The efficiency of microseism generation thus depends on both the wave frequency and the depth of water. While the theory provided an estimate of the magnitude of the corresponding microseisms in a compressible ocean, its predictions of microseism amplitude heretofore have never been tested quantitatively. In this paper, we show a strong agreement between observed microseism and calculated amplitudes obtained by applying Longuet-Higgins' theory to hindcast ocean wave spectra from the North Atlantic Ocean. The calculated vertical displacements are compared with seismic data collected at stations in North America, Greenland, Iceland and Europe. This modelling identifies a particularly energetic source area stretching from the Labrador Sea to south of Iceland, where wind patterns are especially conducive to generating oppositely travelling waves of same period, and the ocean depth is favourable for efficient microseism generation through the 'organ pipe' resonance of the compression waves, as predicted by the theory. This correspondence between observations and the model predictions demonstrates that deep ocean nonlinear wave-wave interactions are sufficiently energetic to account for much of the observed seismic amplitudes in North America, Greenland and Iceland.
C1 [Kedar, Sharon; Webb, Frank; Jones, Cathleen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Longuet-Higgins, Michael] Univ Calif San Diego, Inst Nonlinear Sci, La Jolla, CA 92093 USA.
[Clayton, Robert] CALTECH, Seismol Lab, Pasadena, CA 91125 USA.
RP Kedar, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM sharon.kedar@jpl.nasa.gov
RI GEOFON, GlobalSeismicNetwork/E-4273-2012
NR 39
TC 131
Z9 137
U1 2
U2 18
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1364-5021
J9 P ROY SOC A-MATH PHY
JI Proc. R. Soc. A-Math. Phys. Eng. Sci.
PD MAR 8
PY 2008
VL 464
IS 2091
BP 777
EP 793
DI 10.1098/rspa.2007.0277
PG 17
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 256XM
UT WOS:000252763200014
ER
PT J
AU Paillou, P
Mitchell, K
Wall, S
Ruffie, G
Wood, C
Lorenz, R
Stofan, E
Lunine, J
Lopes, R
Encrenaz, P
AF Paillou, Philippe
Mitchell, Karl
Wall, Stephen
Ruffie, Gilles
Wood, Charles
Lorenz, Ralph
Stofan, Ellen
Lunine, Jonathan
Lopes, Rosaly
Encrenaz, Pierre
TI Microwave dielectric constant of liquid hydrocarbons: Application to the
depth estimation of Titan's lakes
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID CASSINI RADAR; SURFACE; MAPPER
AB Cassini RADAR reveals the surface of Titan since flyby Ta acquired on October 2004. The RADAR instrument discovered volcanic structures, craters, dunes, channels, lakes and seas. In particular, flyby T16 realized in July 2006 imaged tens of radar-dark features close to Titan's north pole. They are interpreted as lakes filled with liquid hydrocarbons - mainly methane, a key material in the geologic and climatic history of Titan. In order to perform quantitative analysis and modeling of the radar response of Titan's lakes, the dielectric constant of liquid hydrocarbons is a crucial parameter, in particular to estimate the radar wave attenuation. We present here first measurements of the dielectric constant of LNG ( Liquefied Natural Gas), mainly composed of methane, at Ku-band ( 10 - 13 GHz): we obtained a value epsilon = 1.75 - 0.002j. This value is used to model the radar backscattering of lakes observed during T16 flyby. Using a two-layer scattering model, we derive a relationship that is used to estimate a minimum depth for Titan's lakes. The proposed relationship is also coherent with the observation that the larger and then the deeper lakes are also the darker in radar images.
C1 [Paillou, Philippe] OASU, UMR 5804, F-33270 Floirac, France.
[Encrenaz, Pierre] LERMA, Observ Paris, F-75014 Paris, France.
[Mitchell, Karl; Wall, Stephen; Lopes, Rosaly] JPL, Pasadena, CA 91109 USA.
[Lorenz, Ralph] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Lunine, Jonathan] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Ruffie, Gilles] IMS, UMR 5218, F-33607 Pessac, France.
[Stofan, Ellen] Proxemy Res, Rectortown, VA 20140 USA.
[Wood, Charles] Planetary Sci Inst, Tucson, AZ 85719 USA.
RP Paillou, P (reprint author), OASU, UMR 5804, F-33270 Floirac, France.
RI Lorenz, Ralph/B-8759-2016; Lopes, Rosaly/D-1608-2016
OI Lorenz, Ralph/0000-0001-8528-4644; Lopes, Rosaly/0000-0002-7928-3167
NR 25
TC 26
Z9 26
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 MAR 7
PY 2008
VL 35
IS 5
AR L05202
DI 10.1029/2007GL032515
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 276PZ
UT WOS:000254155900003
ER
PT J
AU Anderson, JD
Campbell, JK
Ekelund, JE
Ellis, J
Jordan, JF
AF Anderson, John D.
Campbell, James K.
Ekelund, John E.
Ellis, Jordan
Jordan, James F.
TI Anomalous orbital-energy changes observed during spacecraft flybys of
Earth
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID GALILEO; SYSTEM
AB We report and characterize anomalous orbital-energy changes observed during six Earth flybys by the Galileo, NEAR, Cassini, Rosetta, and MESSENGER spacecraft. These anomalous energy changes are consistent with an empirical prediction formula which is proportional to the total orbital energy per unit mass and which involves the incoming and outgoing geocentric latitudes of the asymptotic spacecraft velocity vectors. We use this formula to predict a potentially detectable flyby velocity increase of less than 1 mm/s for a second Rosetta flyby on November 13, 2007.
C1 [Anderson, John D.; Campbell, James K.; Ekelund, John E.; Ellis, Jordan; Jordan, James F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Anderson, JD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 15
TC 78
Z9 78
U1 1
U2 2
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 MAR 7
PY 2008
VL 100
IS 9
AR 091102
DI 10.1103/PhysRevLett.100.091102
PG 4
WC Physics, Multidisciplinary
SC Physics
GA 271BS
UT WOS:000253764500011
PM 18352689
ER
PT J
AU Jones, GH
Roussos, E
Krupp, N
Beckmann, U
Coates, AJ
Crary, F
Dandouras, I
Dikarev, V
Dougherty, MK
Garnier, P
Hansen, CJ
Hendrix, AR
Hospodarsky, GB
Johnson, RE
Kempf, S
Khurana, KK
Krimigis, SM
Kruger, H
Kurth, WS
Lagg, A
McAndrews, HJ
Mitchell, DG
Paranicas, C
Postberg, F
Russell, CT
Saur, J
Seiss, M
Spahn, F
Srama, R
Strobel, DF
Tokar, R
Wahlund, JE
Wilson, RJ
Woch, J
Young, D
AF Jones, G. H.
Roussos, E.
Krupp, N.
Beckmann, U.
Coates, A. J.
Crary, F.
Dandouras, I.
Dikarev, V.
Dougherty, M. K.
Garnier, P.
Hansen, C. J.
Hendrix, A. R.
Hospodarsky, G. B.
Johnson, R. E.
Kempf, S.
Khurana, K. K.
Krimigis, S. M.
Krueger, H.
Kurth, W. S.
Lagg, A.
McAndrews, H. J.
Mitchell, D. G.
Paranicas, C.
Postberg, F.
Russell, C. T.
Saur, J.
Seiss, M.
Spahn, F.
Srama, R.
Strobel, D. F.
Tokar, R.
Wahlund, J. -E.
Wilson, R. J.
Woch, J.
Young, D.
TI The dust halo of Saturn's largest icy moon, Rhea
SO SCIENCE
LA English
DT Article
ID PLANETARY SATELLITES; CASSINI; MAGNETOSPHERE; CLOUDS
AB Saturn's moon Rhea had been considered massive enough to retain a thin, externally generated atmosphere capable of locally affecting Saturn's magnetosphere. The Cassini spacecraft's in situ observations reveal that energetic electrons are depleted in the moon's vicinity. The absence of a substantial exosphere implies that Rhea's magnetospheric interaction region, rather than being exclusively induced by sputtered gas and its products, likely contains solid material that can absorb magnetospheric particles. Combined observations from several instruments suggest that this material is in the form of grains and boulders up to several decimetres in size and orbits Rhea as an equatorial debris disk. Within this disk may reside denser, discrete rings or arcs of material.
C1 [Jones, G. H.; Roussos, E.; Krupp, N.; Dikarev, V.; Krueger, H.; Lagg, A.; Woch, J.] Max Planck Inst Sonnensystemforsch, D-37191 Katlenburg Lindau, Germany.
[Jones, G. H.; Coates, A. J.; McAndrews, H. J.] UCL, Mullard Space Sci Lab, Dept Space & Climate Phys, Dorking RH5 6NT, Surrey, England.
[Jones, G. H.; Coates, A. J.] UCL, Ctr Planetary Sci, London WC1E 6BT, England.
[Beckmann, U.; Dikarev, V.; Kempf, S.; Postberg, F.; Srama, R.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Crary, F.; Young, D.] SW Res Inst, San Antonio, TX 78238 USA.
[Dandouras, I.; Garnier, P.] Univ Toulouse 3, CNRS, Ctr Etud Spatiale Rayonnements, F-31400 Toulouse, France.
[Dikarev, V.] St Petersburg State Univ, Inst Astron, St Petersburg 198504, Russia.
[Dougherty, M. K.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BW, England.
[Garnier, P.; Wahlund, J. -E.] Swedish Inst Space Phys, S-75121 Uppsala, Sweden.
[Hansen, C. J.; Hendrix, A. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hospodarsky, G. B.; Kurth, W. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Johnson, R. E.] Univ Virginia, Dept Mat Sci & Engn, Charlottesville, VA 22904 USA.
[Khurana, K. K.; Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Krimigis, S. M.; Mitchell, D. G.; Paranicas, C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Krimigis, S. M.] Acad Athens, Athens 11527, Greece.
[Saur, J.] Univ Cologne, Inst Geophys & Meteorol, D-50923 Cologne, Germany.
[Seiss, M.; Spahn, F.] Univ Potsdam, AG Nichtlineare Dynam, D-14469 Potsdam, Germany.
[Strobel, D. F.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[McAndrews, H. J.; Tokar, R.; Wilson, R. J.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Jones, GH (reprint author), Max Planck Inst Sonnensystemforsch, Max Planck Str 2, D-37191 Katlenburg Lindau, Germany.
EM ghj@mssl.ucl.ac.uk
RI Roussos, Elias/H-2249-2011; Coates, Andrew/C-2396-2008; Wilson,
Rob/C-2689-2009; Jones, Geraint/C-1682-2008; Paranicas,
Christopher/B-1470-2016;
OI Jones, Geraint/0000-0002-5859-1136; Coates, Andrew/0000-0002-6185-3125;
Wilson, Rob/0000-0001-9276-2368; Paranicas,
Christopher/0000-0002-4391-8255; Dandouras, Iannis/0000-0002-7121-1118;
KEMPF, SASCHA/0000-0001-5236-3004; Hospodarsky,
George/0000-0001-9200-9878; Roussos, Elias/0000-0002-5699-0678; Kurth,
William/0000-0002-5471-6202
FU Science and Technology Facilities Council [PP/D00084X/1]
NR 22
TC 41
Z9 41
U1 1
U2 4
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD MAR 7
PY 2008
VL 319
IS 5868
BP 1380
EP 1384
DI 10.1126/science.1151524
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 270HW
UT WOS:000253712900041
PM 18323452
ER
PT J
AU Connor, BJ
Boesch, H
Toon, G
Sen, B
Miller, C
Crisp, D
AF Connor, Brian J.
Boesch, Hartmut
Toon, Geoffrey
Sen, Bhaswar
Miller, Charles
Crisp, David
TI Orbiting carbon observatory: Inverse method and prospective error
analysis
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ATMOSPHERIC CO2; WFM-DOAS; CM(-1); (CO2)-C-12-O-16
AB The objective, design, and implementation of the OCO inverse method are presented. The inverse method is the algorithm which finds the profile-weighted mean mixing ratio, X-CO2, which best fits the measured spectrum, given a "forward model'' which calculates the spectrum for a given atmospheric state, surface, and instrument properties. Minimizing bias among comparative values of X-CO2 is a critical objective. The algorithm uses an "optimal,'' maximum a posteriori inverse method, with weak a priori constraint, and employs a state vector containing atmospheric and surface properties expected to vary significantly between soundings. An extensive operational characterization and error analysis will be employed, producing quantities designed to aid atmospheric modelers in use of the OCO data. In particular, comparison to inverse models of surface CO2 flux will require use of the OCO column averaging kernel and a priori state vector. An off-line error analysis has also been developed for more detailed error studies, and its use is illustrated by prospective application to case studies of nadir observations in summer and winter at three sites. Uncertainties due to noise, geophysical variability, and spectroscopic parameters are considered in detail. At low and midlatitudes, the single-sounding errors due to these sources are expected to be similar to 0.7-0.8 ppm for high-sun conditions and similar to 1.5-2.5 ppm for low sun (winter). Errors from the same sources in semimonthly regional averages are predicted to be < 1 ppm for all conditions.
C1 [Connor, Brian J.] Natl Inst Water & Atmospher Res, Lauder, New Zealand.
[Boesch, Hartmut; Toon, Geoffrey; Sen, Bhaswar; Miller, Charles; Crisp, David] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Connor, BJ (reprint author), Natl Inst Water & Atmospher Res, Pvt Bag 50061, Lauder, New Zealand.
EM b.connor@niwa.co.nz
RI Boesch, Hartmut/G-6021-2012
NR 18
TC 89
Z9 90
U1 5
U2 18
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 6
PY 2008
VL 113
IS D5
AR D05305
DI 10.1029/2006JD008336
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 276QI
UT WOS:000254156800001
ER
PT J
AU Sayres, DS
Smith, JB
Pittman, JV
Weinstock, EM
Anderson, JG
Heymsfield, G
Li, L
Fridlind, AM
Ackerman, AS
AF Sayres, D. S.
Smith, J. B.
Pittman, J. V.
Weinstock, E. M.
Anderson, J. G.
Heymsfield, G.
Li, L.
Fridlind, A. M.
Ackerman, A. S.
TI Validation and determination of ice water content-radar reflectivity
relationships during CRYSTAL-FACE: Flight requirements for future
comparisons
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID IN-SITU DATA; RADIATIVE PROPERTIES; CIRRUS CLOUDS; PART II; LIDAR; SIZE;
VARIABILITY; RETRIEVALS; AIRCRAFT; MISSION
AB In situ measurements of cirrus ice water content (IWC) by the Harvard water vapor and total water instruments during Cirrus Regional Study of Tropical Anvils and Cirrus Layers-Florida Area Cirrus Experiment are compared with remote sensing data made by the Cloud Radar System instrument in order to derive and validate an empirical IWC-radar relflectivity Z(e) relationship. The comparisons show that for measurements of in situ IWC and remotely measured radar reflectivity, collocated within 2 km of each other, a single IWC-Z(e) relationship can be found that fits the data with an uncertainty of +/- 20-30%. A cloud resolving model shows this level of uncertainty to be consistent with sampling errors associated with comparing two measurements that are not collocated. Uncertainties are quantified in the use of in situ data to validate the retrieval algorithms used to derive the IWC of clouds from remote sensing observations, such as radar reflectivity Ze. Uncertainties are classified into instrumental uncertainties, uncertainties related to sampling errors, and uncertainties in using a single IWC-Z(e) relationship to describe a cloud.
C1 [Sayres, D. S.; Smith, J. B.; Pittman, J. V.; Weinstock, E. M.; Anderson, J. G.] Harvard Univ, Sch Med, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Fridlind, A. M.; Ackerman, A. S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Heymsfield, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Li, L.] Univ Maryland, Baltimore, MD 21250 USA.
[Pittman, J. V.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Sayres, DS (reprint author), Harvard Univ, Sch Med, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA.
EM sayres@huarp.harvard.edu
RI Ackerman, Andrew/D-4433-2012; Fridlind, Ann/E-1495-2012
OI Ackerman, Andrew/0000-0003-0254-6253;
NR 28
TC 6
Z9 6
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 6
PY 2008
VL 113
IS D5
AR D05208
DI 10.1029/2007JD008847
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 276QI
UT WOS:000254156800003
ER
PT J
AU Hwang, SJ
Bowman, RC
Reiter, JW
Rijssenbeek, J
Soloveichik, GL
Zhao, JC
Kabbour, H
Ahn, CC
AF Hwang, Son-Jong
Bowman, Robert C., Jr.
Reiter, Joseph W.
Rijssenbeek, Job
Soloveichik, Grigorii L.
Zhao, Ji-Cheng
Kabbour, Houria
Ahn, Channing C.
TI NMR confirmation for formation of [B12H12](2-) complexes during hydrogen
desorption from metal borohydrides
SO JOURNAL OF PHYSICAL CHEMISTRY C
LA English
DT Letter
ID SOLID-STATE NMR; MAGNESIUM BOROHYDRIDE; CROSS-POLARIZATION; STORAGE
MATERIALS; B12H12-2 ION; LIBH4; DECOMPOSITION; COMPOSITES; MG(BH4)(2);
ADDITIVES
AB B-11 NMR spectroscopy has been employed to identify the reaction intermediates and products formed in the amorphous phase during the thermal hydrogen desorption of metal tetrahydroborates (borohydrides) LiBH4, Mg(BH4)(2), LiSc(BH4)(4), and the mixed Ca(AIH(4))(2)-LiBH4 system. The B-11 magic angle spinning (MAS) and cross polarization magic angle spinning (CPMAS) spectral features of the amorphous intermediate species closely coincide with those of a model compound, closo-borane K2B12H12 that contains the [B12H12](2-) anion. The presence of [B12H12](2-) in the partially decomposed borohydrides was further confirmed by high-resolution solution B-11 and H-1 NMR spectra after dissolution of the intermediate desorption powders in water. The formation of the closo-borane structure is observed as a major intermediate species in all of the metal borohydride systems we have examined.
C1 [Hwang, Son-Jong] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
[Bowman, Robert C., Jr.; Reiter, Joseph W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Rijssenbeek, Job; Soloveichik, Grigorii L.; Zhao, Ji-Cheng] GE Global Res, New York, NY 12309 USA.
[Kabbour, Houria; Ahn, Channing C.] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA.
RP Hwang, SJ (reprint author), CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
RI Zhao, Ji-Cheng (JC)/H-4387-2012
OI Zhao, Ji-Cheng (JC)/0000-0002-4426-1080
NR 50
TC 207
Z9 209
U1 7
U2 60
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1932-7447
J9 J PHYS CHEM C
JI J. Phys. Chem. C
PD MAR 6
PY 2008
VL 112
IS 9
BP 3164
EP 3169
DI 10.1021/jp710894t
PG 6
WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science,
Multidisciplinary
SC Chemistry; Science & Technology - Other Topics; Materials Science
GA 267MF
UT WOS:000253512400002
ER
PT J
AU Kobayashi, DR
Polovina, JJ
Parker, DM
Kamezaki, N
Cheng, IJ
Uchida, I
Dutton, PH
Balazs, GH
AF Kobayashi, Donald R.
Polovina, Jeffrey J.
Parker, Denise M.
Kamezaki, Naoki
Cheng, I-Jiunn
Uchida, Itaru
Dutton, Peter H.
Balazs, George H.
TI Pelagic habitat characterization of loggerhead sea turtles, Caretta
caretta, in the North Pacific Ocean (1997-2006): Insights from satellite
tag tracking and remotely sensed data
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE biotelemetry; habitat use; oceanography; remote sensing; resource
utilization; satellite tracking; sea turtles
ID DIEL VERTICAL MIGRATION; FLIPPER BEAT FREQUENCY; MARINE PROTECTED AREAS;
TIGER SHARKS; SELECTIVE PREDATION; SEAGRASS ECOSYSTEM; ELECTIVITY
INDEXES; FORAGING BEHAVIOR; DIVING BEHAVIOR; ANIMAL BEHAVIOR
AB We analyzed satellite track data for 186 loggerhead sea turtles in the North Pacific Ocean using remotely sensed environmental data to characterize pelagic habitat. A large number of candidate habitat variables were merged to the satellite track data and statistically compared to background values over a large spatiotemporal grid which bounded overall occupancy. Five statistically significant variables were identified out of the 16 environmental variables examined. Two of these variables have strong seasonal, interannual, and spatial patterns (sea surface temperature and chlorophyll a concentration), while three others were primarily spatial (earth magnetic force, earth magnetic declination, and earth magnetic inclination). Habitat selectivity for these variables was quantified using preference curve methodology established in the foraging literature. The output from the selectivity curves was used to predict a multivariate loggerhead sea turtle habitat index across the pelagic North Pacific. This predicted habitat was ground-truthed with newly available satellite track data. (C) 2008 Elsevier B.V. All rights reserved.
C1 [Kobayashi, Donald R.; Polovina, Jeffrey J.; Parker, Denise M.; Balazs, George H.] NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, US Dept Commerce, Honolulu, HI 96822 USA.
[Kobayashi, Donald R.] Univ Technol Sydney, Dept Environm Sci, Broadway, NSW 2007, Australia.
[Parker, Denise M.] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA.
[Kamezaki, Naoki] Sea Turtle Assoc Japan, Osaka 5730163, Japan.
[Cheng, I-Jiunn] Natl Taiwan Ocean Univ, Inst Marine Biol, Chilung 20224, Taiwan.
[Uchida, Itaru] Port Nagoya Publ Aquarium, Minato Ku, Nagoya, Aichi 4550033, Japan.
[Dutton, Peter H.] NOAA, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, US Dept Commerce, La Jolla, CA 92037 USA.
RP Kobayashi, DR (reprint author), NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, US Dept Commerce, 2570 Dole St, Honolulu, HI 96822 USA.
EM Donald.Kobayashi@noaa.gov
NR 91
TC 54
Z9 60
U1 4
U2 52
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0981
EI 1879-1697
J9 J EXP MAR BIOL ECOL
JI J. Exp. Mar. Biol. Ecol.
PD MAR 3
PY 2008
VL 356
IS 1-2
BP 96
EP 114
DI 10.1016/j.jembe.2007.12.019
PG 19
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 284CN
UT WOS:000254683000008
ER
PT J
AU Rice, MR
Balazs, GH
AF Rice, Marc R.
Balazs, George H.
TI Diving behavior of the Hawaiian green turtle (Chelonia mydas) during
oceanic migrations
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE diving; Hawaiian islands; migration; sea turtles; TDR
ID SEA-TURTLES; ASCENSION ISLAND; DIVE PROFILES; LEPIDOCHELYS-OLIVACEA;
SATELLITE TRACKING; DEPTH DISTRIBUTION; DURATIONS; PACIFIC
AB The diving behavior of an adult female and two adult male green turtles was recorded during their roundtrip breeding migration from Laniakea, Oahu, to French Frigate Shoals in the Northwestern Hawaiian Islands. These data represent the first detailed records of diving behavior of green turtles as they migrate to their breeding grounds. All three turtles exhibited a biphasic diving behavior. During the daylight hours, diving depth was shallow (1-4 m) and duration was short (1-18 min). It was assumed that the turtles were moving deliberately toward their destination during this time. Between 1900 and 1930 h daily, the turtles began a diving pattern consisting of deep dives with a mean maximum dive depth of 35-55 m and a mean duration of 35 to 44 min. The shallow diurnal diving began between 0600 and 0700 h, after the nocturnal deep-diving pattern ended. The adult female made two dives in excess of 135 to and one male made several dives in excess of 100 in. These are the deepest dives ever recorded for a naturally diving green turtle. It took an average of 36 days for the turtles to make the trip to French Frigate Shoals and an average of 30 days to make the return trip. The deep nocturnal diving was unexpected and this behavior is in need of further investigation. (C) 2008 Elsevier B.V All rights reserved.
C1 [Rice, Marc R.] Hawaii Preparatory Acad, Kamuela, HI 96743 USA.
[Balazs, George H.] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA.
RP Rice, MR (reprint author), Hawaii Preparatory Acad, 65-1692 Kohala Mt Rd, Kamuela, HI 96743 USA.
EM mrice@hpa.edu
NR 33
TC 25
Z9 27
U1 3
U2 10
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0981
EI 1879-1697
J9 J EXP MAR BIOL ECOL
JI J. Exp. Mar. Biol. Ecol.
PD MAR 3
PY 2008
VL 356
IS 1-2
BP 121
EP 127
DI 10.1016/j.jembe.2007.12.010
PG 7
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 284CN
UT WOS:000254683000010
ER
PT J
AU Suh, JO
Tu, KN
Lutsenko, GV
Gusak, AM
AF Suh, J. O.
Tu, K. N.
Lutsenko, G. V.
Gusak, A. M.
TI Size distribution and morphology of Cu(6)Sn(5) scallops in wetting
reaction between molten solder and copper
SO ACTA MATERIALIA
LA English
DT Article
DE CU(6)Sn(5); solder wetting; ripening
ID KINETICS; ALLOY; CU
AB During the reaction between molten solder and copper, ripening and growth Of Cu(6)Sn(5) scallops take place at the solder/metal interface. An experimental study on the morphology, size distribution and growth rate Of Cu(6)Sn(5) scallops was conducted. The measured size distributions Of CU(6)Sn(5) as a function of time from top-view and cross-sectional view scanning electron microscopy images were in good agreement with the flux-driven ripening (FDR) theory. The FDR theory assumes a non-conservative ripening under a constant total interfacial area between the scallops and the solder, while the total volume of scallops increases with reaction time. The measured average radius of the scallops was proportional to the cube root of time. Comparing the experimental results and the theoretical model, the width of the liquid channel between scallops was calculated to be similar to 2.5 nm. Morphology of the scallop-type CU(6)Sn(5) was dependent to the composition of the solder. The scallop morphology became more faceted when the composition was further away from the eutectic composition. The CU(6)Sn(5) scallops with a shape close to hemispheric gave better agreement with FDR theory. The small difference between the experimental data and theory was explained by taking the noise factor into account. The modified FDR model showed even better agreement with the experimental data. (c) 2007 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Suh, J. O.; Tu, K. N.] Univ Calif Los Angeles, Dept Mat Sci & Engn, Los Angeles, CA 90095 USA.
[Lutsenko, G. V.; Gusak, A. M.] Cherkasy Natl Univ, Dept Theoret Phys, Cherkassy, Ukraine.
RP Suh, JO (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM Jong-ook.Suh@jpl.nasa.gov
RI Gusak, Andriy/F-3459-2010; Lutsenko, Galyna/C-2321-2014
OI Gusak, Andriy/0000-0002-2594-5559; Lutsenko, Galyna/0000-0002-9727-7836
NR 13
TC 64
Z9 66
U1 3
U2 23
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 MAR
PY 2008
VL 56
IS 5
BP 1075
EP 1083
DI 10.1016/j.actamat.2007.11.009
PG 9
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA 276ZU
UT WOS:000254183000017
ER
PT J
AU Davis, RB
Virgin, LN
Brown, AM
AF Davis, R. Benjamin
Virgin, Lawrence N.
Brown, Andrew M.
TI Cylindrical shell submerged in bounded acoustic media: A modal approach
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT AIAA/ASME/ASCE/AHS/ASC 48th Structures, Structural Dynamics, and
Materials Conference
CY APR 23-26, 2007
CL Honolulu, HI
SP AIAA, ASME, ASCE, AHS, ASC
ID SYSTEMS; FLUID; NOISE
AB The dynamics of a simply supported cylindrical shell submerged in liquid hydrogen and liquid oxygen are considered. The shell itself is bounded by a rigid outer cylinder with closed rigid ends. This configuration gives rise to two fluid-filled cavities-an inner cylindrical cavity. and an outer annular cavity. Such geometries are common in rocket engine design. The natural frequencies and modes of the fluid-structure system are computed by combining the rigid wall acoustic cavity modes and the in vacuo structural modes into a system of coupled ordinary differential equations. Eigenvalue veering is observed near the intersections of the curves representing natural frequencies of the rigid wall acoustic and the in vacuo structural modes. In the case of a shell submerged in liquid hydrogen, system frequencies near these intersections are as much as 30% lower than the corresponding in vacuo structural frequencies. Because of its high density, the frequency reductions in the presence of liquid oxygen are even more dramatic. The forced responses of a shell submerged in liquid hydrogen and liquid oxygen, while subject to a harmonic point excitation, are also presented. The responses in the presence of fluid are found to be quite distinct from those of the structure in vacuo.
C1 [Davis, R. Benjamin] Duke Univ, Dept Mech Engn & Mat Sci, Durham, NC 27708 USA.
[Virgin, Lawrence N.] Duke Univ, Dept Civil & Environm Engn, Durham, NC 27708 USA.
[Brown, Andrew M.] NASA, George C Marshall Space Flight Ctr, Struct & Dynam Analysis Branch, Huntsville, AL 35812 USA.
RP Davis, RB (reprint author), Duke Univ, Dept Mech Engn & Mat Sci, Durham, NC 27708 USA.
OI Davis, R Benjamin /0000-0003-4478-302X
NR 19
TC 2
Z9 2
U1 0
U2 3
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 MAR
PY 2008
VL 46
IS 3
BP 752
EP 763
DI 10.2514/1.31706
PG 12
WC Engineering, Aerospace
SC Engineering
GA 266AL
UT WOS:000253403200020
ER
PT J
AU Koch, GJ
Beyon, JY
Gibert, F
Barnes, BW
Ismail, S
Petros, M
Petzar, PJ
Yu, J
Modlin, EA
Davis, KJ
Singh, UN
AF Koch, Grady J.
Beyon, Jeffrey Y.
Gibert, Fabien
Barnes, Bruce W.
Ismail, Syed
Petros, Mulugeta
Petzar, Paul J.
Yu, Jirong
Modlin, Edward A.
Davis, Kenneth J.
Singh, Upendra N.
TI Side-line tunable laser transmitter for differential absorption lidar
measurements of CO2: design and application to atmospheric measurements
SO APPLIED OPTICS
LA English
DT Article
ID TALL TOWER; PACIFIC; FOREST
AB A 2 mu m wavelength, 90 mJ, 5 Hz pulsed Ho laser is described with wavelength control to precisely tune and lock the wavelength at a desired offset up to 2.9 GHz from the center of a CO2 absorption line. Once detuned from the line center the laser wavelength is actively locked to keep the wavelength within 1.9 MHz standard deviation about the setpoint. This wavelength control allows optimization of the optical depth for a differential absorption lidar (DIAL) measuring atmospheric CO2 concentrations. The laser transmitter has been coupled with a coherent heterodyne receiver for measurements of CO2 concentration using aerosol backscatter; wind and aerosols are also measured with the same lidar and provide useful additional information on atmospheric structure. Range-resolved CO2 measurements were made with < 2.4% standard deviation using 500 m range bins and 6.7 min (1000 pulse pairs) integration time. Measurement of a horizontal column showed a precision of the CO2 concentration to < 0.7% standard deviation using a 30 min (4500 pulse pairs) integration time, and comparison with a collocated in situ sensor showed the DIAL to measure the same trend of a diurnal variation and to detect shorter time scale CO2 perturbations. For vertical column measurements the lidar was setup at the WLEF tall tower site in Wisconsin to provide meteorological profiles and to compare the DIAL measurements with the in situ sensors distributed on the tower up to 396 m height. Assuming the DIAL column measurement extending from 153 m altitude to 1353 m altitude should agree with the tower in situ sensor at 396 m altitude, there was a 7.9 ppm rms difference between the DIAL and the in situ sensor using a 30 min rolling average on the DIAL measurement. (C) 2008 Optical Society of America.
C1 [Koch, Grady J.; Barnes, Bruce W.; Ismail, Syed; Yu, Jirong; Modlin, Edward A.; Singh, Upendra N.] NASA, Langley Res Ctr, Hampton, VA 23692 USA.
[Beyon, Jeffrey Y.] Calif State Univ Los Angeles, Dept Elect & Comp Engn, Los Angeles, CA 90032 USA.
[Gibert, Fabien; Davis, Kenneth J.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Petros, Mulugeta] Sci & Technol Corp, Hampton, VA 23666 USA.
[Petzar, Paul J.] Natl Inst Aerosp, Hampton, VA 23666 USA.
RP Koch, GJ (reprint author), NASA, Langley Res Ctr, Hampton, VA 23692 USA.
EM grady.j.koch@nasa.gov
NR 24
TC 72
Z9 76
U1 2
U2 18
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 MAR 1
PY 2008
VL 47
IS 7
BP 944
EP 956
DI 10.1364/AO.47.000944
PG 13
WC Optics
SC Optics
GA 283ZC
UT WOS:000254674000011
PM 18311266
ER
PT J
AU Muterspaugh, MW
Lane, BF
Fekel, FC
Konacki, M
Burke, BF
Kulkarni, SR
Colavita, MM
Shao, M
Wiktorowicz, SJ
AF Muterspaugh, Matthew W.
Lane, Benjamin F.
Fekel, Francis C.
Konacki, Maciej
Burke, Bernard F.
Kulkarni, S. R.
Colavita, M. M.
Shao, M.
Wiktorowicz, Sloane J.
TI Masses, luminosities, and orbital coplanarities of the mu orionis
quadruple-star system from phases differential astrometry
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE astrometry; binaries : close; binaries : visual; stars : distances;
stars : individual (delta Equ, kappa Peg, mu Orionis, V819 Her);
techniques : interferometric
ID PALOMAR TESTBED INTERFEROMETER; TRIPLE STARS; SPECKLE OBSERVATIONS;
RADIAL-VELOCITIES; BINARY; INCLINATION; ORIENTATION; TELESCOPE;
HIPPARCOS; STABILITY
AB mu Orionis was identified by spectroscopic studies as a quadruple-star system. Seventeen high-precision differential astrometry measurements of mu Ori have been collected by the Palomar High-precision Astrometric Search for Exoplanet Systems (PHASES). These show both the motion of the long-period binary orbit and short-period perturbations superimposed on that caused by each of the components in the long-period system being themselves binaries. The new measurements enable the orientations of the long-period binary and short-period subsystems to be determined. Recent theoretical work predicts the distribution of relative inclinations between inner and outer orbits of hierarchical systems to peak near 40 and 140 degrees. The degree of coplanarity of this complex system is determined, and the angle between the planes of the A-B and Aa-Ab orbits is found to be 136.7 +/- 8.3 degrees, near the predicted distribution peak at 140 degrees; this result is discussed in the context of the handful of systems with established mutual inclinations. The system distance and masses for each component are obtained from a combined fit of the PHASES astrometry and archival radial velocity observations. The component masses have relative precisions of 5% (component Aa), 15% (Ab), and 1.4% (each of Ba and Bb). The median size of the minor axes of the uncertainty ellipses for the new measurements is 20 micro-arcseconds (mu as). Updated orbits for delta Equulei, kappa Pegasi, and V819 Herculis are also presented.
C1 [Muterspaugh, Matthew W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Lane, Benjamin F.] Charles Stark Draper Lab Inc, Cambridge, MA 02139 USA.
[Fekel, Francis C.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37203 USA.
[Konacki, Maciej] Polish Acad Sci, Nicholas Copernicus Astronom Ctr, PL-87100 Torun, Poland.
[Burke, Bernard F.] MIT, Dept Phys, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Kulkarni, S. R.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Colavita, M. M.; Shao, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wiktorowicz, Sloane J.] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Muterspaugh, MW (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM matthew1@ssl.berkeley.edu; blane@mit.edu; maciej@ncac.torun.pl
NR 34
TC 35
Z9 35
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD MAR
PY 2008
VL 135
IS 3
BP 766
EP 776
DI 10.1088/0004-6256/135/3/766
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 271WF
UT WOS:000253818700002
ER
PT J
AU Sahai, R
Morris, M
Contreras, CS
Claussen, M
AF Sahai, Raghvendra
Morris, Mark
Sanchez Contreras, Carmen
Claussen, Mark
TI Preplanetary nebulae: A Hubble space telescope imaging survey and a new
morphological classification system (vol 134, pg 2200, 2007)
SO ASTRONOMICAL JOURNAL
LA English
DT Correction
C1 [Sahai, Raghvendra] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morris, Mark] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Sanchez Contreras, Carmen] CSIC, Inst Estructura Mat, Dept Astrofis Mol & Infraroja, E-28006 Madrid, Spain.
[Claussen, Mark] Natl Radio Astron Observ, Socorro, NM 87801 USA.
RP Sahai, R (reprint author), CALTECH, Jet Prop Lab, MS 183-900, Pasadena, CA 91109 USA.
RI Sanchez-Contreras, Carmen/N-3718-2015
OI Sanchez-Contreras, Carmen/0000-0002-6341-592X
NR 1
TC 0
Z9 0
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD MAR
PY 2008
VL 135
IS 3
BP 1099
EP 1099
DI 10.1088/0004-6256/135/3/1099
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 271WF
UT WOS:000253818700031
ER
PT J
AU Mahabal, A
Djorgovski, SG
Turmon, M
Jewell, J
Williams, RR
Drake, AJ
Graham, MG
Donalek, C
Glikman, E
AF Mahabal, A.
Djorgovski, S. G.
Turmon, M.
Jewell, J.
Williams, R. R.
Drake, A. J.
Graham, M. G.
Donalek, C.
Glikman, E.
CA Palomar-Quest Team
TI Automated probabilistic classification of transients and variables
SO ASTRONOMISCHE NACHRICHTEN
LA English
DT Article; Proceedings Paper
CT Workshop on Hot-Wiring the Transient Universe
CY JUN 04-07, 2007
CL Tucson, AZ
SP VOEvent Working Grp, Heterogeneous Telescope Networks
DE astronomical databases : miscellaneous; methods : data analysis; methods
: statistical; surveys
AB There is an increasing number of large, digital, synoptic sky surveys, in which repeated observations are obtained over large areas of the sky in multiple epochs. Likewise, there is a growth in the number of (often automated or robotic) follow-up facilities with varied capabilities in terms of instruments, depth, cadence, wavelengths, etc., most of which are geared toward some specific astrophysical phenomenon. As the number of detected transient events grows, an automated, probabilistic classification of the detected variables and transients becomes increasingly important, so that an optimal use can be made of follow-up facilities, without unnecessary duplication of effort. We describe a methodology now under development for a prototype event classification system; it involves Bayesian and Machine Learning classifiers, automated incorporation of feedback from follow-up observations, and discriminated or directed follow-up requests. This type of methodology may be essential for the massive synoptic sky surveys in the future. (C) 2008 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.
C1 [Mahabal, A.; Djorgovski, S. G.; Williams, R. R.; Drake, A. J.; Graham, M. G.; Donalek, C.; Glikman, E.] CALTECH, Pasadena, CA 91125 USA.
[Turmon, M.; Jewell, J.] Jet Propuls Lab, Pasadena, CA USA.
RP Mahabal, A (reprint author), CALTECH, Pasadena, CA 91125 USA.
EM aam@astro.caltech.edu
NR 14
TC 28
Z9 28
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 MAR
PY 2008
VL 329
IS 3
BP 288
EP 291
DI 10.1002/asna.200710943
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 282CW
UT WOS:000254546200018
ER
PT J
AU Barthelmy, S
AF Barthelmy, S.
TI GCN and VOEvent: A status report
SO ASTRONOMISCHE NACHRICHTEN
LA English
DT Article; Proceedings Paper
CT Workshop on Hot-Wiring the Transient Universe
CY JUN 04-07, 2007
CL Tucson, AZ
SP VOEvent Working Grp, Heterogeneous Telescope Networks
DE astronomical databases : miscellaneous; gamma-rays : bursts
AB The GRB Coordinates Network (GCN) has filled an important niche in the conduct and progress of research on GRB for more than 14 years. The methods used to collect and distribute the positions, lightcurves, spectra, and images on GRB in real time (a few seconds) will be reviewed. For the research on GRBs to continue to move forward and for other fields of transient astronomy to move forward, enhancements are needed to the GCN. VOEvents is one of those changes, and that addition will be described here. The enhanced system will be called VO-GCN. (c) 2008 WILEY-VCH Verlag GmbH&Co. KGaA. Weinheim.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Barthelmy, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM scott@milkyway.gsfc.nasa.gov
RI Barthelmy, Scott/D-2943-2012
NR 2
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 MAR
PY 2008
VL 329
IS 3
BP 340
EP 342
DI 10.1002/asna.200710954
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 282CW
UT WOS:000254546200033
ER
PT J
AU van der Horst, AJ
Kamble, A
Resmi, L
Wijers, RAMJ
Bhattacharya, D
Scheers, B
Rol, E
Strom, R
Kouveliotou, C
Oosterloo, T
Ishwara-Chandra, CH
AF van der Horst, A. J.
Kamble, A.
Resmi, L.
Wijers, R. A. M. J.
Bhattacharya, D.
Scheers, B.
Rol, E.
Strom, R.
Kouveliotou, C.
Oosterloo, T.
Ishwara-Chandra, C. H.
TI Detailed study of the GRB 030329 radio afterglow deep into the
non-relativistic phase
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gamma rays : bursts; radio continuum : general; radiation mechanisms :
non-thermal
ID GAMMA-RAY BURST; LIGHT-CURVE; JET; CALORIMETRY; SUPERNOVA; MILLIMETER;
DYNAMICS; SIZE
AB Context. We explore the physics behind one of the brightest radio afterglows ever, GRB 030329, at late times when the jet is non-relativistic.
Aims. We determine the physical parameters of the blast wave and its surroundings, in particular the index of the electron energy distribution, the energy of the blast wave, and the density (structure) of the circumburst medium. We then compare our results with those from image size measurements.
Methods. We observed the GRB 030329 radio afterglow with the Westerbork Synthesis Radio Telescope and the Giant Metrewave Radio Telescope at frequencies from 325 MHz to 8.4 GHz, spanning a time range of 268-1128 days after the burst. We modeled all the available radio data and derived the physical parameters.
Results. The index of the electron energy distribution is p = 2.1, the circumburst medium is homogeneous, and the transition to the non-relativistic phase happens at t(NR) similar to 80 days. The energy of the blast wave and density of the surrounding medium are comparable to previous findings.
Conclusions. Our findings indicate that the blast wave is roughly spherical at t(NR), and they agree with the implications from the VLBI studies of image size evolution. It is not clear from the presented dataset whether we have seen emission from the counter jet or not. We predict that the Low Frequency Array will be able to observe the afterglow of GRB 030329 and many other radio afterglows, constraining the physics of the blast wave during its non-relativistic phase even further.
C1 [van der Horst, A. J.; Wijers, R. A. M. J.; Scheers, B.; Strom, R.] Univ Amsterdam, Astron Inst, NL-1098 SJ Amsterdam, Netherlands.
[Kamble, A.; Resmi, L.; Bhattacharya, D.] Raman Res Inst, Bangalore 560080, Karnataka, India.
[Resmi, L.] Indian Inst Sci, Joint Astron Programme, Bangalore 560012, Karnataka, India.
[Bhattacharya, D.] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Rol, E.] Univ Leicester, Dept Phys & Astron, Leicester LE2 7RH, Leics, England.
[Strom, R.; Oosterloo, T.] ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Kouveliotou, C.] NSSTC, MSFC, NASA, Huntsville, AL USA.
[Ishwara-Chandra, C. H.] Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India.
RP van der Horst, AJ (reprint author), Univ Amsterdam, Astron Inst, Kruislaan 403, NL-1098 SJ Amsterdam, Netherlands.
EM avdhorst@science.uva.nl
RI M, Manjunath/N-4000-2014; Bhattacharya, Dipankar/J-6927-2015;
OI M, Manjunath/0000-0001-8710-0730; Bhattacharya,
Dipankar/0000-0003-3352-3142; Wijers, Ralph/0000-0002-3101-1808
NR 31
TC 36
Z9 36
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 MAR
PY 2008
VL 480
IS 1
BP 35
EP 43
DI 10.1051/0004-6361:20078051
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 268JP
UT WOS:000253576400009
ER
PT J
AU Raiteri, CM
Villata, M
Larionov, VM
Aller, MF
Bach, U
Gurwell, M
Kurtanidze, OM
Lahteenmaki, A
Nilsson, K
Volvach, A
Aller, HD
Arkharov, AA
Bachev, R
Berdyugin, A
Bottcher, M
Buemi, CS
Calcidese, P
Cozzi, E
Di Paola, A
Dolci, M
Fan, JH
Forne, E
Foschini, L
Gupta, AC
Hagen-Thorn, VA
Hooks, L
Hovatta, T
Joshi, M
Kadler, M
Kimeridze, GN
Konstantinova, TS
Kostov, A
Krichbaum, TP
Lanteri, L
Larionova, LV
Lee, CU
Leto, P
Lindfors, E
Montagni, F
Nesci, R
Nieppola, E
Nikolashvili, MG
Ohlert, J
Oksanen, A
Ovcharov, E
Paakkonen, P
Pasanen, M
Pursimo, T
Ros, JA
Semkov, E
Sigua, LA
Smart, RL
Strigachev, A
Takalo, LO
Torii, K
Torniainen, I
Tornikoski, M
Trigilio, C
Tsunemi, H
Umana, G
Valcheva, A
AF Raiteri, C. M.
Villata, M.
Larionov, V. M.
Aller, M. F.
Bach, U.
Gurwell, M.
Kurtanidze, O. M.
Lahteenmaki, A.
Nilsson, K.
Volvach, A.
Aller, H. D.
Arkharov, A. A.
Bachev, R.
Berdyugin, A.
Boettcher, M.
Buemi, C. S.
Calcidese, P.
Cozzi, E.
Di Paola, A.
Dolci, M.
Fan, J. H.
Forne, E.
Foschini, L.
Gupta, A. C.
Hagen-Thorn, V. A.
Hooks, L.
Hovatta, T.
Joshi, M.
Kadler, M.
Kimeridze, G. N.
Konstantinova, T. S.
Kostov, A.
Krichbaum, T. P.
Lanteri, L.
Larionova, L. V.
Lee, C. -U.
Leto, P.
Lindfors, E.
Montagni, F.
Nesci, R.
Nieppola, E.
Nikolashvili, M. G.
Ohlert, J.
Oksanen, A.
Ovcharov, E.
Paakkonen, P.
Pasanen, M.
Pursimo, T.
Ros, J. A.
Semkov, E.
Sigua, L. A.
Smart, R. L.
Strigachev, A.
Takalo, L. O.
Torii, K.
Torniainen, I.
Tornikoski, M.
Trigilio, C.
Tsunemi, H.
Umana, G.
Valcheva, A.
TI Radio-to-UV monitoring of AO 0235+164 by the WEBT and Swift during the
2006-2007 outburst
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies : active; galaxies : BL Lacertae objects : general; galaxies :
BL Lacertae objects : individual : AO 0235+164; galaxies : jets;
galaxies : quasars : general
ID XMM-NEWTON OBSERVATIONS; BL-LACERTAE; AO 0235+164; LIGHT CURVES; HELICAL
JETS; VARIABILITY; CAMPAIGN; BLAZARS; STARS; FIELD
AB Context. The blazar AO 0235+164 was claimed to show a quasi-periodic behaviour in the radio and optical bands in the past, with the main outbursts repeating every 5-6 years. However, the predicted 2004 outburst did not occur, and further analysis suggested a longer time scale, according to which the next event would have occurred in the 2006-2007 observing season. Moreover, an extra emission component contributing to the UV and soft X-ray flux was detected, whose nature is not yet clear. An optical outburst was observed in late 2006-early 2007, which triggered a Whole Earth Blazar Telescope (WEBT) campaign as well as target of opportunity (ToO) observations by the Swift satellite.
Aims. In this paper, we present the radio-to-optical data taken by the WEBT together with the UV data acquired by the UltraViolet and Optical Telescope (UVOT) instrument onboard Swift to investigate both the outburst behaviour at different wavelengths and the nature of the extra emission component.
Methods. Multifrequency light curves have been assembled with data from 27 observatories; optical and UV fluxes have been cleaned from the contamination of the southern active galactic nucleus (AGN). We have analysed spectral energy distributions at different epochs, corresponding to different brightness states; extra absorption by the foreground galaxy has been taken into account.
Results. We found the optical outburst to be as strong as the big outbursts of the past: starting from late September 2006, a brightness increase of similar to 5 mag led to the outburst peak in February 19-21, 2007. We also observed an outburst at mm and then at cm wavelengths, with an increasing time delay going toward lower frequencies during the rising phase. Cross-correlation analysis indicates that the 1 mm and 37 GHz flux variations lagged behind the R-band ones by about 3 weeks and 2 months, respectively. These short time delays suggest that the corresponding jet emitting regions are only slightly separated and/or misaligned. In contrast, during the outburst decreasing phase the flux faded contemporaneously at all cm wavelengths. This abrupt change in the emission behaviour may suggest the presence of some "shutdown" mechanism of intrinsic or geometric nature. The behaviour of the UV flux closely follows the optical and near-IR one. By separating the synchrotron and extra component contributions to the UV flux, we found that they correlate, which suggests that the two emissions have a common origin.
C1 [Raiteri, C. M.; Villata, M.; Lanteri, L.; Smart, R. L.] Osserv Astron Torino, INAF, Turin, Italy.
[Larionov, V. M.; Hagen-Thorn, V. A.; Konstantinova, T. S.; Larionova, L. V.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia.
[Aller, M. F.; Aller, H. D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Larionov, V. M.] Pulkovo Observ, St Petersburg, Russia.
[Bach, U.] Max Planck Inst Radioastron, D-5300 Bonn, Germany.
[Gurwell, M.] Harvard Smithsonian Ctr Astroph, Cambridge, MA USA.
[Lahteenmaki, A.; Hovatta, T.; Nieppola, E.; Torniainen, I.; Tornikoski, M.] Helsinki Univ Technol, Metsahovi Radio Obs, FIN-02150 Espoo, Finland.
[Nilsson, K.; Berdyugin, A.; Lindfors, E.; Pasanen, M.; Takalo, L. O.] Univ Turku, Tuorla Observ, Piikkio, Finland.
[Bachev, R.; Semkov, E.; Strigachev, A.; Valcheva, A.] Bulgarian Acad Sci, Inst Astron, Sofia, Bulgaria.
[Boettcher, M.; Hooks, L.; Joshi, M.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA.
[Di Paola, A.] Osserv Astron Roma, INAF, Rome, Italy.
[Fan, J. H.] Guangzhou Univ, Ctr Astrophys, Guangzhou 510405, Guangdong, Peoples R China.
[Forne, E.] Agrupacio Astron Sabadell, Sabadell, Spain.
[Foschini, L.] IASF Bologna, INAF, Bologna, Italy.
[Gupta, A. C.] Chinese Acad Sci, YNAO, Kunming, Peoples R China.
[Kadler, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Krichbaum, T. P.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Lee, C. -U.] Korea Astron & Space Sci Inst, Taejon, South Korea.
[Nesci, R.] Univ Roma La Sapienza, Dept Phys, Rome, Italy.
[Ohlert, J.] Michael Adrian Observ, Trebur, Germany.
[Ovcharov, E.; Valcheva, A.] Univ Sofia, Sofia, Bulgaria.
[Paakkonen, P.] Univ Joensuu, Jakokoski Observ, FIN-80101 Joensuu, Finland.
[Pursimo, T.] Nord Opt Telescope, Santa Cruz de La Palma, Spain.
[Torii, K.] Osaka Univ, Suita, Osaka 565, Japan.
RP Raiteri, CM (reprint author), Osserv Astron Torino, INAF, Turin, Italy.
EM raiteri@oato.inaf.it; villata@oato.inaf.it
RI Foschini, Luigi/H-3833-2012; Larionov, Valeri/H-1349-2013; Lahteenmaki,
Anne/L-5987-2013; Kurtanidze, Omar/J-6237-2014; Grishina,
Tatiana/H-6873-2013; Hagen-Thorn, Vladimir/H-3983-2013;
OI Foschini, Luigi/0000-0001-8678-0324; Larionov,
Valeri/0000-0002-4640-4356; Grishina, Tatiana/0000-0002-3953-6676;
Hagen-Thorn, Vladimir/0000-0002-6431-8590; Larionova,
Liudmila/0000-0002-0274-1481; Buemi, Carla Simona/0000-0002-7288-4613;
Leto, Paolo/0000-0003-4864-2806; Di Paola, Andrea/0000-0002-2189-8644;
Villata, Massimo/0000-0003-1743-6946; Raiteri, Claudia
Maria/0000-0003-1784-2784
NR 34
TC 40
Z9 40
U1 0
U2 2
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2008
VL 480
IS 2
BP 339
EP 347
DI 10.1051/0004-6361:20079044
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 271RP
UT WOS:000253806700009
ER
PT J
AU Masetti, N
Mason, E
Landi, R
Giommi, P
Bassani, L
Malizia, A
Bird, AJ
Bazzano, A
Dean, AJ
Gehrels, N
Palazzi, E
Ubertini, P
AF Masetti, N.
Mason, E.
Landi, R.
Giommi, P.
Bassani, L.
Malizia, A.
Bird, A. J.
Bazzano, A.
Dean, A. J.
Gehrels, N.
Palazzi, E.
Ubertini, P.
TI High-redshift blazar identification for Swift j1656.3-3302
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE quasars : emission lines; quasars : individual : J1656.3-3302 galaxies :
high-redshift; galaxies : active; X-rays : galaxies; astrometry
ID RADIO-LOUD QUASARS; SOUTHERN SPECTROPHOTOMETRIC STANDARDS; RAY SURVEY
CATALOG; SPECTROSCOPY; TELESCOPE; EMISSION; SPECTRA; MISSION; OBJECTS;
IMAGER
AB We report on the high-redshift blazar identification of a new gamma-ray source, Swift J1656.3-3302, detected with the BAT imager onboard the Swift satellite and the IBIS instrument on the INTEGRAL satellite. Follow-up optical spectroscopy has allowed us to identify the counterpart as an R similar to 19 mag source that shows broad Lyman-alpha, Si IV, He II, C IV, and CIII] emission lines at redshift z = 2.40 +/- 0.01. Spectral evolution is observed in X-rays when the INTEGRAL/IBIS data are compared to the Swift/BAT results, with the spectrum steepening when the source gets fainter. The 0.7-200 keV X-ray continuum, observed with Swift/XRT and INTEGRAL/ IBIS, shows the power law shape typical of radio loud (broad emission line) active galactic nuclei (with a photon index Gamma similar to 1.6) and a hint of spectral curvature below similar to 2 keV, possibly due to intrinsic absorption (N-H similar to 7 x 10(22) cm(-2)) local to the source. Alternatively, a slope change (Delta Gamma similar to 1) around 2.7 keV can describe the X-ray spectrum equally well. At this redshift, the observed 20-100 keV luminosity of the source is similar to 10(48) erg s(-1) (assuming isotropic emission), making Swift J1656.3-3302 one of the most X-ray luminous blazars. This source is yet another example of a distant gamma-ray loud quasar discovered above 20 keV. It is also the farthest object, among the previously unidentified INTEGRAL sources, whose nature has been determined a posteriori through optical spectroscopy.
C1 [Masetti, N.; Landi, R.; Bassani, L.; Malizia, A.; Palazzi, E.] Inst Astrofis Spaziale & Fis Cosm Bologna, INAF, I-40129 Bologna, Italy.
[Mason, E.] European So Observ, Santiago 19, Chile.
[Giommi, P.] ASI Data Ctr, I-00044 Frascati, Italy.
[Dean, A. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Bazzano, A.] Inst Astrofis Spaziale & Fis Cosm Roma, INAF, I-00133 Rome, Italy.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Masetti, N (reprint author), Inst Astrofis Spaziale & Fis Cosm Bologna, INAF, Via Gobetti 101, I-40129 Bologna, Italy.
EM masetti@iasfbo.inaf.it
RI Gehrels, Neil/D-2971-2012; Palazzi, Eliana/N-4746-2015;
OI mason, elena/0000-0003-3877-0484; giommi, paolo/0000-0002-2265-5003;
Malizia, Angela/0000-0002-6558-1163; Palazzi,
Eliana/0000-0002-8691-7666; Bassani, Loredana/0000-0003-4858-6963;
Masetti, Nicola/0000-0001-9487-7740; Bazzano, Angela/0000-0002-2017-4396
NR 49
TC 14
Z9 14
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 MAR
PY 2008
VL 480
IS 3
BP 715
EP 721
DI 10.1051/0004-6361:20078901
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 274IB
UT WOS:000253993900015
ER
PT J
AU Caballero, I
Santangelo, A
Kretschmar, P
Staubert, R
Postnov, K
Klochkov, D
Camero-Arranz, A
Finger, MH
Kreykenbohm, I
Pottschmidt, K
Rothschild, RE
Suchy, S
Wilms, J
Wilson, CA
AF Caballero, I.
Santangelo, A.
Kretschmar, P.
Staubert, R.
Postnov, K.
Klochkov, D.
Camero-Arranz, A.
Finger, M. H.
Kreykenbohm, I.
Pottschmidt, K.
Rothschild, R. E.
Suchy, S.
Wilms, J.
Wilson, C. A.
TI The pre-outburst flare of the A 0535+26 August/September 2005 outburst
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays : binaries; stars : magnetic fields; stars : individual : A
0535+26
ID RAY TIMING EXPLORER; CYCLOTRON LINE; INTEGRAL OBSERVATION; A0535+262;
ENERGY; RXTE; PERFORMANCE; LUMINOSITY; BINARIES; ORBIT
AB We study the spectral and temporal behavior of the High Mass X-ray Binary A 0535+26 during a "pre-outburst flare" which took place similar to 5d before the peak of a normal (type I) outburst in August/September 2005. We compare the studied behavior with that observed during the outburst.
Methods. We analyse RXTE observations that monitored A 0535+26 during the outburst. We complete spectral and timing analyses of the data. We study the evolution of the pulse period, present energy-dependent pulse profiles both at the initial pre-outburst flare and close to outburst maximum, and measure how the cyclotron resonance-scattering feature (hereafter CRSF) evolves.
Results. We present three main results: a constant period P = 103.3960(5) s is measured until periastron passage, followed by a spin-up with a decreasing period derivative of. P = (-1.69 +/- 0.04) x 10(-8) s s(-1) at MJD 53 618, and P remains constant again at the end of the main outburst. The spin-up provides evidence for the existence of an accretion disk during the normal outburst. We measure a CRSF energy of E-cyc similar to 50 keV during the pre-outburst flare, and E-cyc similar to 46 keV during the main outburst. The pulse shape, which varies significantly during both pre-outburst flare and main outburst, evolves strongly with photon energy.
C1 [Caballero, I.; Santangelo, A.; Staubert, R.; Postnov, K.; Klochkov, D.; Kreykenbohm, I.] Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Kretschmar, P.] ESAC, ISOC, Madrid, Spain.
[Postnov, K.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Camero-Arranz, A.] Univ Valencia, Inst Ciencias Mat, GACE, Valencia 46071, Spain.
[Finger, M. H.; Wilson, C. A.] Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
[Kreykenbohm, I.] ISDC, CH-1290 Versoix, Switzerland.
[Pottschmidt, K.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA.
[Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Rothschild, R. E.; Suchy, S.] Univ Calif San Diego, CASS, La Jolla, CA 92093 USA.
[Wilms, J.] Univ Erlangen Nurnberg, Astron Inst, D-96049 Bamberg, Germany.
RP Caballero, I (reprint author), Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany.
EM isabel@astro.uni-tuebingen.de
RI Wilms, Joern/C-8116-2013; Kreykenbohm, Ingo/H-9659-2013;
OI Wilms, Joern/0000-0003-2065-5410; Kreykenbohm, Ingo/0000-0001-7335-1803;
Kretschmar, Peter/0000-0001-9840-2048
NR 35
TC 23
Z9 23
U1 0
U2 2
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2008
VL 480
IS 2
BP L17
EP U1
DI 10.1051/0004-6361:20079310
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 271RP
UT WOS:000253806700001
ER
PT J
AU Cordiner, MA
Cox, NLJ
Trundle, C
Evans, CJ
Hunter, I
Przybilla, N
Bresolin, F
Salama, F
AF Cordiner, M. A.
Cox, N. L. J.
Trundle, C.
Evans, C. J.
Hunter, I.
Przybilla, N.
Bresolin, F.
Salama, F.
TI Detection of diffuse interstellar bands in M 31
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE astrochemistry; galaxies : Local Group; galaxies : ISM; ISM : lines and
bands; ISM : clouds; ISM : dust; extinction
ID SMALL-MAGELLANIC-CLOUD; ULTRAVIOLET EXTINCTION; CA-II; M31;
SPECTROSCOPY; DUST; SUPERGIANTS; ABSORPTION; STARS; GAS
AB Aims. We investigate the diffuse interstellar band (DIB) spectrum in the interstellar medium of M31.
Methods. The DEIMOS spectrograph of the W. M. Keck observatory was used to make optical spectroscopic observations of two supergiant stars, MAG 63885 and MAG 70817, in the vicinity of the OB78 association in M 31 where the metallicity is approximately equal to solar.
Results. The lambda lambda 5780, 5797, 6203, 6283 and 6613 DIBs are detected in both sightlines at velocities matching the M31 interstellar Na I absorption. The spectra are classified and interstellar reddenings are derived for both stars. Diffuse interstellar band ( DIB) equivalent widths and radial velocities are presented.
Conclusions. The spectrum of DIBs observed in M31 towards MAG 63885 is found to be similar to that observed in the Milky Way. Towards MAG 70817 the DIB equivalent widths per unit reddening are about three times the Galactic average. Compared to observations elsewhere in the Universe, relative to reddening the M31 ISM in the vicinity of OB78 is apparently a highly favourable environment for the formation of DIB carriers.
C1 [Cordiner, M. A.; Trundle, C.; Hunter, I.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Cox, N. L. J.] ESA, Herschel Sci Ctr, European Space Astron Ctr, Madrid, Spain.
[Evans, C. J.] Royal Observ, UK ATC, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Przybilla, N.] Dr Remeis Sternwarte Bamberg, D-96049 Bamberg, Germany.
[Bresolin, F.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Salama, F.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Cordiner, MA (reprint author), Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
EM m.cordiner@qub.ac.uk
RI Salama, Farid/A-8787-2009
OI Salama, Farid/0000-0002-6064-4401
NR 45
TC 22
Z9 23
U1 0
U2 2
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2008
VL 480
IS 1
BP L13
EP L16
DI 10.1051/0004-6361:20079309
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 268JP
UT WOS:000253576400004
ER
PT J
AU Besson, DZ
Jenkins, J
Matsuno, S
Nam, J
Smith, M
Barwick, SW
Beatty, JJ
Binns, WR
Chen, C
Chen, P
Clem, JM
Connolly, A
Dowkontt, PF
DuVernois, MA
Field, RC
Goldstein, D
Gorham, PW
Goodhue, A
Hast, C
Hebert, CL
Hoover, S
Israel, MH
Kowalski, J
Learned, JG
Liewer, KM
Link, JT
Lusczek, E
Mercurio, B
Miki, C
Miocinovic, P
Naudet, CJ
Ng, J
Nichol, R
Palladino, K
Reil, K
Romero-Wolf, A
Rosen, M
Ruckman, L
Saltzberg, D
Seckel, D
Varner, GS
Walz, D
Wu, F
AF Besson, D. Z.
Jenkins, J.
Matsuno, S.
Nam, J.
Smith, M.
Barwick, S. W.
Beatty, J. J.
Binns, W. R.
Chen, C.
Chen, P.
Clem, J. M.
Connolly, A.
Dowkontt, P. F.
DuVernois, M. A.
Field, R. C.
Goldstein, D.
Gorham, P. W.
Goodhue, A.
Hast, C.
Hebert, C. L.
Hoover, S.
Israel, M. H.
Kowalski, J.
Learned, J. G.
Liewer, K. M.
Link, J. T.
Lusczek, E.
Mercurio, B.
Miki, C.
Miocinovic, P.
Naudet, C. J.
Ng, J.
Nichol, R.
Palladino, K.
Reil, K.
Romero-Wolf, A.
Rosen, M.
Ruckman, L.
Saltzberg, D.
Seckel, D.
Varner, G. S.
Walz, D.
Wu, F.
TI In situ radioglaciological measurements near Taylor Dome, Antarctica and
implications for ultra-high energy (UHE) neutrino astronomy
SO ASTROPARTICLE PHYSICS
LA English
DT Article
DE ultra-high energy neutrino detection; radioglaciology; askaryan effect
ID ICE SHEETS
AB Radiowave detection of the Cherenkov radiation produced by neutrino-ice collisions requires an understanding of the radiofrequency (RF) response of cold polar ice. We herein report on a series of radioglaciological measurements performed approximately 10 km north of Taylor Dome Station, Antarctica from December 6, 2006-December 16, 2006. Using RF signals broadcast from: (a) an englacial discone, submerged to a depth of 100 m and broadcasting to a surface dual-polarization horn receiver, and (b) a dual-polarization horn antenna on the surface transmitting signals which reflect off the underlying bed and back up to the surface receiver, we have made time-domain estimates of both the real (index-of-refraction "n") and imaginary (attenuation length "L-atten") components of the complex ice dielectric constant. We have also measured the uniformity of ice response along two orthogonal axes in the horizontal plane. We observe an apparent wavespeed asymmetry of order 0.1% between two orthogonal linear polarizations projected into the horizontal plane, consistent with some previous measurements, but somewhat lower than others. (C) 2008 Elsevier B.V. All rights reserved.
C1 [Besson, D. Z.; Link, J. T.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Matsuno, S.; Gorham, P. W.; Hebert, C. L.; Kowalski, J.; Learned, J. G.; Miki, C.; Miocinovic, P.; Romero-Wolf, A.; Rosen, M.; Ruckman, L.; Varner, G. S.] Univ Hawaii Manoa, Dept Phys & Astron, Honolulu, HI 96822 USA.
[Nam, J.; Barwick, S. W.; Goldstein, D.; Wu, F.] Univ Calif Irvine, Irvine, CA 92697 USA.
[Beatty, J. J.; Mercurio, B.; Nichol, R.; Palladino, K.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Binns, W. R.; Dowkontt, P. F.; Israel, M. H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Chen, C.; Chen, P.; Field, R. C.; Hast, C.; Ng, J.; Reil, K.; Walz, D.] Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA.
[Clem, J. M.; Seckel, D.] Univ Delaware, Newark, DE 19716 USA.
[Connolly, A.; Goodhue, A.; Hoover, S.; Saltzberg, D.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Lusczek, E.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[DuVernois, M. A.; Liewer, K. M.; Naudet, C. J.] Jet Propuls Lab, Pasadena, CA 91109 USA.
RP Besson, DZ (reprint author), Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
EM dbesson@ku.edu
RI Nichol, Ryan/C-1645-2008; Vieregg, Abigail/D-2287-2012; Connolly,
Amy/J-3958-2013; Beatty, James/D-9310-2011;
OI Beatty, James/0000-0003-0481-4952; Lusczek,
Elizabeth/0000-0003-4680-965X
NR 29
TC 12
Z9 12
U1 0
U2 4
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-6505
J9 ASTROPART PHYS
JI Astropart Phys.
PD MAR
PY 2008
VL 29
IS 2
BP 130
EP 157
DI 10.1016/j.astropartphys.2007.12.004
PG 28
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 280UO
UT WOS:000254452100006
ER
PT J
AU Bruhweiler, F
Verner, E
AF Bruhweiler, F.
Verner, E.
TI Modeling Fe II emission and revised Fe II (UV) empirical templates
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE line : formation; methods : numerical; quasars : emission lines; quasars
: individual (I Zw 1); ultraviolet : galaxies
ID ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT QUASARS; FLUORESCENCE LINES; BROAD
EMISSION; RR TELESCOPII; IRON EMISSION; O-VI; ZW 1; SPECTRUM; RATIOS
AB We use the narrow-lined broad-line region (BLR) of the Seyfert 1 galaxy, IZw 1, as a laboratory for modeling the ultraviolet (UV) Fe II 2100-3050 angstrom emission complex. We calculate a grid of Fe II emission spectra representative of BLR clouds and compare them with the observed I Zw 1 spectrum. Our predicted spectrum for log n(H)/(cm(-3)) = 11.0, log [Phi(H)/(cm(-2) s(-1)) = 20.5, and xi/( 1 km s(-1)) 20, using Cloudy and an 830 level model atom for Fe II with energies up to 14.06 eV, gives a better fit to the UV Fe II emission than models with fewer levels. Our analysis indicates ( 1) the observed UV Fe II emission must be corrected for an underlying Fe II pseudocontinuum; ( 2) Fe II emission peaks can be misidentified as that of other ions in active galactic nuclei ( AGNs) with narrow-lined BLRs possibly affecting deduced physical parameters; ( 3) the shape of 4200-4700 angstrom Fe II emission in I Zw 1 and other AGNs is a relative indicator of narrow-line region ( NLR) and BLR Fe II emission; ( 4) predicted ratios of Ly alpha, C III], and Fe II emission relative to Mg II lambda 2800 agree with extinction corrected observed I Zw1 fluxes, except for C IV lambda 1549; ( 5) the sensitivity of Fe II emission strength to microturbulence xi casts doubt on existing relative Fe/Mg abundances derived from Fe II ( UV)/Mg II flux ratios. Our calculated Fe II emission spectra, suitable for BLRs in AGNs, are available at http://iacs.cua.edu/people/verner/FeII.
C1 [Bruhweiler, F.; Verner, E.] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
[Bruhweiler, F.; Verner, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Bruhweiler, F (reprint author), Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, 200 Hannan Hall, Washington, DC 20064 USA.
EM bruhweiler@cua.edu; verner@milkyway.gsfc.nasa.gov
NR 44
TC 32
Z9 33
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2008
VL 675
IS 1
BP 83
EP 95
DI 10.1086/525557
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 268EP
UT WOS:000253562000008
ER
PT J
AU Sani, E
Risaliti, G
Salvati, M
Maiolino, R
Marconi, A
Berta, S
Braito, V
Della Ceca, R
Franceschini, A
AF Sani, E.
Risaliti, G.
Salvati, M.
Maiolino, R.
Marconi, A.
Berta, S.
Braito, V.
Della Ceca, R.
Franceschini, A.
TI 3-5 mu m spectroscopy of obscured AGNs in ULIRGs
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : active; galaxies : starburst; infrared : galaxies
ID ULTRALUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEUS; OPTICAL
SPECTROSCOPY; ENERGY-DISTRIBUTIONS; X-RAY; SAMPLE; SUPERANTENNAE;
MICRON; QUASAR; ICE
AB We present the results of infrared L-band (3-4 mu m) and M-band (4-5 mu m) Very Large Telescope (VLT) ISAAC spectroscopy of five bright ultraluminous infrared galaxies (ULIRGs) hosting an AGN. From our analysis we distinguish two types of sources: ULIRGs in which the AGN is unobscured ( with a flat continuum and no absorption features at 3.4 and 4.6 mu m), and those with highly obscured AGNs ( with a steep, reddened continuum and absorption features due to hydrocarbons and CO). Starburst activity is also present in all of the sources, as inferred from the 3.3 mu m PAH emission line. A strong correlation is found between continuum slope and CO optical depth, which suggests that deep carbon monoxide absorption is a common feature of highly obscured ULIRG AGNs. Finally, we show that the AGN dominates the 3-4 mu m emission, even if its contribution to the bolometric luminosity is small.
C1 [Sani, E.; Marconi, A.] Univ Florence, Dipartimento Astron, I-50125 Florence, Italy.
[Risaliti, G.; Salvati, M.] INAF Osservatorio Astron Roma, I-50125 Florence, Italy.
[Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Maiolino, R.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Berta, S.; Franceschini, A.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Braito, V.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Braito, V.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Della Ceca, R.] INAF Osservatorio Astron Brena, I-20121 Milan, Italy.
RP Sani, E (reprint author), Univ Florence, Dipartimento Astron, Largo E Fremi 2, I-50125 Florence, Italy.
RI Marconi, Alessandro/C-5880-2009;
OI Marconi, Alessandro/0000-0002-9889-4238; Della Ceca,
Roberto/0000-0001-7551-2252
NR 42
TC 24
Z9 24
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2008
VL 675
IS 1
BP 96
EP 105
DI 10.1086/523784
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 268EP
UT WOS:000253562000009
ER
PT J
AU Bonamente, M
Joy, M
LaRoque, SJ
Carlstrom, JE
Nagai, D
Marrone, DP
AF Bonamente, Massimiliano
Joy, Marshall
LaRoque, Samuel J.
Carlstrom, John E.
Nagai, Daisuke
Marrone, Daniel P.
TI Scaling relations from Sunyaev-Zel'dovich effect and Chandra X-ray
measurements of high-redshift galaxy clusters
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : clusters : general
ID COSMIC DISTANCE SCALE; MASS; GAS; CONSTRAINTS; COSMOLOGY; FRACTIONS;
TELESCOPE; EVOLUTION; CONSTANT; MODELS
AB We present Sunyaev-Zel'dovich Effect (SZE) scaling relations for 38 massive galaxy clusters at redshifts 0.14 <= z <= 0.89, observed with both the Chandra X-ray Observatory and the centimeter-wave SZE imaging system at the BIMA and OVRO interferometric arrays. An isothermal beta-model with the central 100 kpc excluded from the X-ray data is used to model the intracluster medium and to measure global cluster properties. For each cluster, we measure the X-ray spectroscopic temperature, SZE gas mass, total mass, and integrated Compton y-parameters within r(2500). Our measurements are in agreement with the expectations based on a simple self-similar model of cluster formation and evolution. We compare the cluster properties derived from our SZE observations with and without Chandra spatial and spectral information and find them to be in good agreement. We compare our results with cosmological numerical simulations and find that simulations that include radiative cooling, star formation, and feedback match well both the slope and normalization of our SZE scaling relations.
C1 [Bonamente, Massimiliano] Univ Alabama, Dept Phys, Huntsville, AL 35812 USA.
[Bonamente, Massimiliano; Joy, Marshall] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[LaRoque, Samuel J.; Carlstrom, John E.; Marrone, Daniel P.] Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Carlstrom, John E.] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA.
[Nagai, Daisuke] CALTECH, Pasadena, CA 91125 USA.
Univ Alabama, Ctr Space Plasma & Aeron Res, Space Plasma Interact Data Anal & Simulat Lab, Huntsville, AL 35812 USA.
RP Bonamente, M (reprint author), Univ Alabama, Dept Phys, Huntsville, AL 35812 USA.
NR 47
TC 80
Z9 80
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2008
VL 675
IS 1
BP 106
EP 114
DI 10.1086/525517
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 268EP
UT WOS:000253562000010
ER
PT J
AU Dessart, L
Blondin, S
Brown, PJ
Hicken, M
Hillier, DJ
Holland, ST
Immler, S
Kirshner, RP
Milne, P
Modjaz, M
Roming, PWA
AF Dessart, Luc
Blondin, Stephane
Brown, Peter J.
Hicken, Malcolm
Hillier, D. John
Holland, Stephen T.
Immler, Stefan
Kirshner, Robert P.
Milne, Peter
Modjaz, Maryam
Roming, Peter W. A.
TI Using quantitative spectroscopic analysis to determine the properties
and distances of type II plateau supernovae: SN 2005cs and SN 2006bp
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE radiative transfer; stars : atmospheres; stars : distances; stars :
evolution; supernovae : individual (2005cs, 2006bp)
ID EXPANDING PHOTOSPHERE METHOD; CORE-COLLAPSE SUPERNOVAE; X-RAY-EMISSION;
PRELIMINARY SPECTRAL-ANALYSIS; LARGE-MAGELLANIC-CLOUD; LIGHT-CURVE;
PLANETARY-NEBULAE; STANDARD CANDLES; CEPHEID DISTANCE; HUBBLE CONSTANT
AB We analyze the Type II plateau supernovae (SNe IIP) SN 2005cs and SN 2006bp with the non-LTE model atmosphere code CMFGEN. We fit 13 spectra in the first month for SN 2005cs and 18 for SN 2006bp. Swift ultraviolet photometry and ground-based optical photometry calibrate each spectrum. Our analysis shows that both objects were discovered less than 3 days after they exploded, making these the earliest SN IIP spectra ever studied. They reveal broad and very weak lines from highly ionized fast ejecta with an extremely steep density profile. We identify He II lambda 4686 emission in the SN 2006bp ejecta. Days later, the spectra resemble the prototypical Type IIP SN 1999em, which had a supergiant-like photospheric composition. Despite the association of SN 2005cs with possible X-ray emission, the emergent UV and optical light comes from the photosphere, not from circumstellar emission. We surmise that the very steep density falloff we infer at early times may be a fossil of the combined actions of the shock wave passage and radiation driving at shock breakout. Based on tailored CMFGEN models, the direct fitting technique and the expanding photosphere method both yield distances and explosion times that agree within a few percent. We derive a distance to NGC 5194, the host of SN 2005cs, of 8.9 +/- 0.5 Mpc and 17.5 +/- 0.8 Mpc for SN 2006bp in NGC 3953. The luminosity of SN 2006bp is 1.5 times that of SN 1999em and 6 times that of SN 2005cs. Reliable distances to SNe IIP that do not depend on a small range in luminosity provide an independent route to the Hubble constant and improved constraints on other cosmological parameters.
C1 [Dessart, Luc; Milne, Peter] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Dessart, Luc; Milne, Peter] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Blondin, Stephane; Hicken, Malcolm; Kirshner, Robert P.; Modjaz, Maryam] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA.
[Brown, Peter J.; Roming, Peter W. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Hillier, D. John] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Holland, Stephen T.; Immler, Stefan] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Xray Astrophys Branch, Greenbelt, MD 20771 USA.
[Hillier, D. John; Holland, Stephen T.] Univ Space Res Assoc, Columbia, MD 21044 USA.
RP Dessart, L (reprint author), Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
EM luc@as.arizona.edu
NR 102
TC 80
Z9 80
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2008
VL 675
IS 1
BP 644
EP 669
DI 10.1086/526451
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 268EP
UT WOS:000253562000049
ER
PT J
AU Tuthill, PG
Monnier, JD
Lawrance, N
Danchi, WC
Owocki, SP
Gayley, KG
AF Tuthill, Peter G.
Monnier, John D.
Lawrance, Nicholas
Danchi, William C.
Owocki, Stan P.
Gayley, Kenneth G.
TI The prototype colliding-wind pinwheel WR 104
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instrumentation : interferometers; stars : imaging; stars : individual
(WR 104); stars : mass loss; stars : winds, outflows
ID WOLF-RAYET STARS; SUDDEN RADIATIVE BRAKING; KECK APERTURE-MASKING;
MASSIVE STARS; DUST FORMATION; BINARY WR-140; X-RAY; INTERFEROMETRY;
EVOLUTION; BURST
AB Results from the most extensive study of the time-evolving dust structure around the prototype "pinwheel'' nebula WR 104 are presented. Encompassing 11 epochs in three near-infrared filter bandpasses, a homogeneous imaging data set spanning more than 6 yr (or 10 orbits) is presented. Data were obtained from the highly successful Keck Aperture Masking Experiment, which can recover high-fidelity images at extremely high angular resolutions, revealing the geometry of the plume with unprecedented precision. Inferred properties for the (unresolved) underlying binary and wind system are orbital period 241.5 +/- 0.5 days and angular outflow velocity 0.28 +/- 0.02 mas day(-1). An optically thin cavity of angular size 13.3 +/- 1.4 mas was found to lie between the central binary and the onset of the spiral dust plume. Rotational motion of the wind system induced by the binary orbit is found to have important ramifications: entanglement of the winds results in strong shock activity far downstream from the nose of the bow shock. The far greater fraction of the winds participating in the collision may play a key role in gas compression and the nucleation of dust at large radii from the central binary and shock stagnation point. Investigation of the effects of radiative braking points toward significant modifications of the simple hydrostatic colliding wind geometry, extending the relevance of this phenomenon to wider binary systems than previously considered. Limits placed on the maximum allowed orbital eccentricity of e less than or similar to 0.06 argue strongly for a prehistory of tidal circularization in this system. Finally, we discuss the implications of Earth's polar (i less than or similar to 16 degrees) vantage point onto a system likely to host supernova explosions at future epochs.
C1 [Tuthill, Peter G.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
[Monnier, John D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Lawrance, Nicholas] Univ Sydney, Sch Aerosp Mech & Mechatron Engn, Sydney, NSW 2006, Australia.
[Danchi, William C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Owocki, Stan P.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Gayley, Kenneth G.] Univ Iowa, Iowa City, IA 52245 USA.
RP Tuthill, PG (reprint author), Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
EM p.tuthill@physics.usyd.edu.au; monnier@umich.edu;
n.lawrance@acfr.usyd.edu.au; wcd@iri1.gsfc.nasa.gov;
owocki@bartol.udel.edu; ken.gayley@gmail.com
NR 75
TC 46
Z9 46
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2008
VL 675
IS 1
BP 698
EP 710
DI 10.1086/527286
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 268EP
UT WOS:000253562000053
ER
PT J
AU Rhee, JH
Song, I
Zuckerman, B
AF Rhee, Joseph H.
Song, Inseok
Zuckerman, B.
TI Warm dust in the terrestrial planet zone of a Sun-like pleiades star:
Collisions between planetary embryos?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared : stars; open clusters and associations :
individual (Pleiades) planetary systems : formation; stars : individual
(HD 23514)
ID DEBRIS DISKS; HIPPARCOS; ORIGIN; PLANETESIMALS; SPECTROGRAPH; MAGNITUDE;
EVOLUTION; ASTEROIDS; HD-69830; DIAGRAMS
AB Only a few solar-type main-sequence stars are known to be orbited by warm dust particles; the most extreme is the G0 field star BD + 20 307 that emits similar to 4% of its energy at mid-infrared wavelengths. We report the identification of a similarly dusty star HD 23514, an F6-type member of the Pleiades. A strong mid-IR silicate emission feature indicates the presence of small warm dust particles, but with the primary flux density peak at the nonstandard wavelength of similar to 9 mu m. The existence of so much dust within an AU or so of these stars is not easily accounted for given the very brief lifetime in orbit of small particles. The apparent absence of very hot (greater than or similar to 1000 K) dust at both stars suggests the possible presence of a planet closer to the stars than the dust. The observed frequency of the BD + 20 307/HD 23514 phenomenon indicates that the mass equivalent of Earth's Moon must be converted, via collisions of massive bodies, to tiny dust particles that find their way to the terrestrial planet zone during the first few hundred million years of the life of many (most?) Sun-like stars. Identification of these two dusty systems among youthful nearby solar-type stars suggests that terrestrial planet formation is common.
C1 [Rhee, Joseph H.; Zuckerman, B.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Song, Inseok] CALTECH, IPAC, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Zuckerman, B.] NASA, Astrobiol Inst, Washington, DC 20546 USA.
RP Rhee, JH (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
EM rhee@astro.ucla.edu; song@ipac.caltech.edu; ben@astro.ucla.edu
NR 48
TC 57
Z9 57
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2008
VL 675
IS 1
BP 777
EP 783
DI 10.1086/524935
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 268EP
UT WOS:000253562000058
ER
PT J
AU Sheeley, NR
Herbst, AD
Palatchi, CA
Wang, YM
Howard, RA
Moses, JD
Vourlidas, A
Newmark, JS
Socker, DG
Plunkett, SP
Korendyke, CM
Burlaga, LF
Davila, JM
Thompson, WT
St Cyr, OC
Harrison, RA
Davis, CJ
Eyles, CJ
Halain, JP
Wang, D
Rich, NB
Battams, K
Esfandiari, E
Stenborg, G
AF Sheeley, N. R.
Herbst, A. D.
Palatchi, C. A.
Wang, Y. -M.
Howard, R. A.
Moses, J. D.
Vourlidas, A.
Newmark, J. S.
Socker, D. G.
Plunkett, S. P.
Korendyke, C. M.
Burlaga, L. F.
Davila, J. M.
Thompson, W. T.
St Cyr, O. C.
Harrison, R. A.
Davis, C. J.
Eyles, C. J.
Halain, J. P.
Wang, D.
Rich, N. B.
Battams, K.
Esfandiari, E.
Stenborg, G.
TI Heliospheric images of the solar wind at Earth
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun : corona; Sun : coronal mass ejections (CMEs); Sun : magnetic fields
ID CORONAL MASS EJECTIONS
AB During relatively quiet solar conditions throughout the spring and summer of 2007, the SECCHI HI2 white-light telescope on the STEREO B solar-orbiting spacecraft observed a succession of wave fronts sweeping past Earth. We have compared these heliospheric images with in situ plasma and magnetic field measurements obtained by near-Earth spacecraft, and we have found a near perfect association between the occurrence of these waves and the arrival of density enhancements at the leading edges of high-speed solar wind streams. Virtually all of the strong corotating interaction regions are accompanied by large-scale waves, and the low-density regions between them lack such waves. Because the Sun was dominated by long-lived coronal holes and recurrent solar wind streams during this interval, there is little doubt that we have been observing the compression regions that are formed at low latitude as solar rotation causes the high-speed wind from coronal holes to run into lower speed wind ahead of it.
C1 [Sheeley, N. R.; Palatchi, C. A.; Wang, Y. -M.; Howard, R. A.; Moses, J. D.; Vourlidas, A.; Newmark, J. S.; Socker, D. G.; Plunkett, S. P.; Korendyke, C. M.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Burlaga, L. F.; Davila, J. M.; Thompson, W. T.; St Cyr, O. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20742 USA.
[Harrison, R. A.; Davis, C. J.] Rutherford Appleton Lab, Didcot OX11 OQX, Oxon, England.
[Eyles, C. J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Halain, J. P.] Univ Liege, Ctr Spatiale Liege, B-4031 Angleur, Belgium.
[Wang, D.; Rich, N. B.; Battams, K.; Esfandiari, E.] Interferometr Inc, Herndon, VA 20171 USA.
[Stenborg, G.] Catholic Univ Amer, Washington, DC 20064 USA.
RP Sheeley, NR (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
EM sheeley@spruce.nrl.navy.mil
RI Vourlidas, Angelos/C-8231-2009; Thompson, William/D-7376-2012; Scott,
Christopher/H-8664-2012
OI Vourlidas, Angelos/0000-0002-8164-5948; Scott,
Christopher/0000-0001-6411-5649
NR 12
TC 91
Z9 92
U1 1
U2 4
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2008
VL 675
IS 1
BP 853
EP 862
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 268EP
UT WOS:000253562000064
ER
PT J
AU Lis, DC
Bockelee-Morvan, D
Boissier, J
Crovisier, J
Biver, N
Charnley, SB
AF Lis, D. C.
Bockelee-Morvan, D.
Boissier, J.
Crovisier, J.
Biver, N.
Charnley, S. B.
TI Hydrogen isocyanide in comet 73P/Schwassmann-Wachmann (fragment B)
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets : individual (73P/Schwassmann-Wachmann); molecular processes;
radio lines : solar system
ID C1 IKEYA-ZHANG; SPECTROSCOPIC OBSERVATIONS; HNC; HCN; ABUNDANCES;
HYAKUTAKE; CHEMISTRY; SPECTRUM; U90.7; LEE
AB We present a sensitive 3 sigma upper limit of 1.1% for the HNC/HCN abundance ratio in comet 73P/SchwassmannWachmann (fragment B), obtained on 2006 May 10-11, using Caltech Submillimeter Observatory (CSO). This limit is a factor of similar to 7 lower than the values measured previously in moderately active comets at 1 AU from the Sun. Comet 73P/Schwassmann-Wachmann was depleted in most volatile species, except of HCN. The low HNC/HCN ratio thus argues against HNC production from polymers produced from HCN. However, thermal degradation of macromolecules, or polymers, produced from ammonia and carbon compounds, such as acetylene, methane, or ethane appears a plausible explanation for the observed variations of the HNC/HCN ratio in moderately active comets, including the very low ratio in comet 73P/Schwassmann-Wachmann reported here. Similar polymers have been invoked previously to explain anomalous N-14/N-15 ratios measured in cometary CN.
C1 [Lis, D. C.] CALTECH, Down Lab Phys 320 47, Pasadena, CA 91125 USA.
[Lis, D. C.] LESIA Observ, Paris, France.
[Boissier, J.; Crovisier, J.; Biver, N.] Observ Paris, CNRS, UMR 8109, F-92195 Meudon, France.
[Boissier, J.; Crovisier, J.; Biver, N.] LESIA, F-92195 Meudon, France.
[Charnley, S. B.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
RP Lis, DC (reprint author), CALTECH, Down Lab Phys 320 47, Pasadena, CA 91125 USA.
EM dcl@caltech.edu; Dominique.Bockelee@obspm.fr; Jeremie.Boissier@obspm.fr;
Jacques.Crovisier@obspm.fr; Nicolas.Biver@obspm.fr;
charnley@dusty.arc.nasa.gov
RI Charnley, Steven/C-9538-2012
NR 44
TC 24
Z9 24
U1 2
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2008
VL 675
IS 1
BP 931
EP 936
DI 10.1086/527345
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 268EP
UT WOS:000253562000072
ER
PT J
AU Dorodnitsyn, A
Kallman, T
Proga, D
AF Dorodnitsyn, A.
Kallman, T.
Proga, D.
TI An axisymmetric, hydrodynamical model for the torus wind in active
galactic nuclei
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE acceleration of particles; galaxies : active; hydrodynamics; methods :
numerical; quasars : absorption lines; X-rays : galaxies
ID X-RAY BINARIES; SEYFERT-GALAXIES; ANGULAR-MOMENTUM; IONIZED-GAS;
ENVIRONMENT; NGC-1068; NGC-3783
AB We report on time-dependent axisymmetric simulations of an X-ray-excited flow from a parsec-scale, rotating, cold torus around an active galactic nucleus. Our simulations account for radiative heating and cooling and radiation pressure force. The simulations follow the development of a broad biconical outflow induced mainly by X-ray heating. We compute synthetic spectra predicted by our simulations. The wind characteristics and the spectra support the hypothesis that a rotationally supported torus can serve as the source of a wind which is responsible for the warm absorber gas observed in the X-ray spectra of many Seyfert galaxies.
C1 [Dorodnitsyn, A.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA.
[Kallman, T.] Moscow Space Res Inst, Moscow 117997, Russia.
[Proga, D.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA.
RP Dorodnitsyn, A (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 662, Greenbelt, MD 20771 USA.
NR 20
TC 18
Z9 18
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 1
PY 2008
VL 675
IS 1
BP L5
EP L8
DI 10.1086/529374
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 291ZA
UT WOS:000255234900002
ER
PT J
AU Shioya, Y
Taniguchi, Y
Sasaki, SS
Nagao, T
Murayama, T
Takahashi, MI
Ajiki, M
Ideue, Y
Mihara, S
Nakajima, A
Scoville, NZ
Mobasher, B
Aussel, H
Giavalisco, M
Guzzo, L
Hasinger, G
Impey, C
Le Fevre, O
Lilly, S
Renzini, A
Rich, M
Sanders, DB
Schinnerer, E
Shopbell, P
Leauthaud, A
Kneib, JP
Rhodes, J
Massey, R
AF Shioya, Y.
Taniguchi, Y.
Sasaki, S. S.
Nagao, T.
Murayama, T.
Takahashi, M. I.
Ajiki, M.
Ideue, Y.
Mihara, S.
Nakajima, A.
Scoville, N. Z.
Mobasher, B.
Aussel, H.
Giavalisco, M.
Guzzo, L.
Hasinger, G.
Impey, C.
Le Fevre, O.
Lilly, S.
Renzini, A.
Rich, M.
Sanders, D. B.
Schinnerer, E.
Shopbell, P.
Leauthaud, A.
Kneib, J. -P.
Rhodes, J.
Massey, R.
TI The H alpha luminosity function and star formation rate at z approximate
to 0.24 in the COSMOS 2 square degree field
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE galaxies : distances and redshifts; galaxies : evolution; galaxies :
luminosity function, mass function
ID GALAXY REDSHIFT SURVEY; SUBARU DEEP FIELD; LYMAN BREAK GALAXIES;
NONTHERMAL RADIO-EMISSION; FORMATION RATE DENSITY; NEUTRAL GAS GALAXIES;
NORMAL DISK GALAXIES; DIGITAL SKY SURVEY; FORMATION HISTORY; FORMING
GALAXIES
AB To derive a new H alpha luminosity function and to understand the clustering properties of star-forming galaxies at z approximate to 0.24, we have made a narrowband imaging survey for H alpha-emitting galaxies in the Hubble Space Telescope (HST) COSMOS 2 square degree field. We used the narrowband filter NB816 (lambda(c) = 8150 angstrom, Delta lambda = 120 angstrom) and sampled H alpha emitters with EW(obs)(H alpha + [N II]) > 12 angstrom in a redshift range between z = 0.233 and 0.251 corresponding to a depth of 70 Mpc. We obtained 980 H alpha-emitting galaxies in a sky area of 5540 arcmin(2), corresponding to a survey volume of 3.1 x 10(4) Mpc(3). We derive a H alpha luminosity function with a best-fit Schechter function parameter set of alpha=-1.35(-0.13)(+0.11), log phi* = -2.65(-0.38)(+0.27), and L*(ergs s(-1)) = 41.94(-0.23)(+0.38). The H alpha luminosity density is 2.7(-0.6)(+0.7) x 10(39) ergs s(-1) Mpc(-3). After subtracting the AGN contribution ( 15%) to the H alpha luminosity density, the star formation rate density is evaluated as 1.8(-0.4)(+0.7) x 10(-2) M(circle dot) yr(-1) Mpc(-3). The angular two-point correlation function of H alpha-emitting galaxies of log L(H alpha) > 39.8 is well fit by a power-law form of w(theta) = 0.013(-0.001)(+0.002)theta(-0.88 +/- 0.03) , corresponding to the correlation function of xi(r) = (r/1.9 Mpc)(-1.88). We also find that the H alpha emitters with higher H alpha luminosity are more strongly clustered than those with lower luminosity.
C1 [Shioya, Y.; Taniguchi, Y.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan.
[Sasaki, S. S.; Ideue, Y.; Mihara, S.; Nakajima, A.] Ehime Univ, Grad Sch Sci & Engn, Matsuyama, Ehime 7908577, Japan.
[Sasaki, S. S.; Murayama, T.; Takahashi, M. I.; Ajiki, M.] Tohoku Univ, Astron Inst, Grad Sch Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan.
[Sasaki, S. S.; Scoville, N. Z.; Shopbell, P.; Kneib, J. -P.; Rhodes, J.; Massey, R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Nagao, T.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Scoville, N. Z.; Aussel, H.; Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Mobasher, B.; Giavalisco, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Aussel, H.] CEA Saclay, DSM DAPNIA SAp, F-91191 Gif Sur Yvette, France.
[Guzzo, L.] Osserv Astron Brera, Milan, Italy.
[Hasinger, G.] Max Planck Inst Extraterr Phys, D-85478 Garching, Germany.
[Impey, C.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Le Fevre, O.; Leauthaud, A.; Kneib, J. -P.] Lab Astrophys Marseille, F-13376 Marseille 12, France.
[Lilly, S.] ETH, Dept Phys, Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland.
[Renzini, A.] European So Observ, D-85748 Garching, Germany.
[Rich, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Massey, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Shioya, Y (reprint author), Ehime Univ, Res Ctr Space & Cosm Evolut, Bunkyo Cho, Matsuyama, Ehime 7908577, Japan.
RI Le Fevre, Olivier/G-7389-2011; Kneib, Jean-Paul/A-7919-2015
OI Kneib, Jean-Paul/0000-0002-4616-4989
NR 88
TC 52
Z9 53
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD MAR
PY 2008
VL 175
IS 1
BP 128
EP 137
DI 10.1086/523703
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 307CO
UT WOS:000256295600008
ER
PT J
AU Sakamoto, T
Barthelmy, SD
Barbier, L
Cummings, JR
Fenimore, EE
Gehrels, N
Hullinger, D
Krimm, HA
Markwardt, CB
Palmer, DM
Parsons, AM
Sato, G
Stamatikos, M
Tueller, J
Ukwatta, TN
Zhang, B
AF Sakamoto, T.
Barthelmy, S. D.
Barbier, L.
Cummings, J. R.
Fenimore, E. E.
Gehrels, N.
Hullinger, D.
Krimm, H. A.
Markwardt, C. B.
Palmer, D. M.
Parsons, A. M.
Sato, G.
Stamatikos, M.
Tueller, J.
Ukwatta, T. N.
Zhang, B.
TI The first Swift bat gamma-ray burst catalog
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE gamma rays : bursts
ID X-RAY; TELESCOPE; AFTERGLOW; SPECTRUM; FLASHES; MISSION; HARD
AB We present the first Swift Burst Alert Telescope (BAT) catalog of gamma-ray bursts (GRBs), which contains bursts detected by the BAT between 2004 December 19 and 2007 June 16. This catalog (hereafter the BAT1 catalog) contains burst trigger time, location, 90% error radius, duration, fluence, peak flux, and time-averaged spectral parameters for each of 237 GRBs, as measured by the BAT. The BAT-determined position reported here is within 1.75' of the Swift X-Ray Telescope (XRT)-determined position for 90% of these GRBs. The BAT T-90 and T-50 durations peak at 80 and 20 s, respectively. From the fluence-fluence correlation, we conclude that about 60% of the observed peak energies, E-peak(obs), of BAT GRBs could be less than 100 keV. We confirm that GRB fluence to hardness and GRB peak flux to hardness are correlated for BAT bursts in analogous ways to previous missions' results. The correlation between the photon index in a simple power-law model and E-peak(obs) is also confirmed. We also report the current status for the on-orbit BAT calibrations based on observations of the Crab Nebula.
C1 [Sakamoto, T.; Barthelmy, S. D.; Barbier, L.; Cummings, J. R.; Gehrels, N.; Krimm, H. A.; Markwardt, C. B.; Parsons, A. M.; Sato, G.; Stamatikos, M.; Tueller, J.; Ukwatta, T. N.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Sakamoto, T.; Stamatikos, M.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
[Cummings, J. R.] Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
[Fenimore, E. E.; Palmer, D. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Hullinger, D.] Moxtek Inc, Orem, UT 84057 USA.
[Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Markwardt, C. B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Sato, G.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Ukwatta, T. N.] George Washington Univ, Dept Phys, Ctr Nucl Studies, Washington, DC 20052 USA.
[Zhang, B.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA.
RP Sakamoto, T (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Tueller,
Jack/D-5334-2012; Parsons, Ann/I-6604-2012
NR 28
TC 117
Z9 119
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD MAR
PY 2008
VL 175
IS 1
BP 179
EP 190
DI 10.1086/523646
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 307CO
UT WOS:000256295600012
ER
PT J
AU Hains, JC
Taubman, BF
Thompson, AM
Stehr, JW
Marufu, LT
Doddridge, BG
Dickerson, RR
AF Hains, Jennifer C.
Taubman, Brett F.
Thompson, Anne M.
Stehr, Jeffrey W.
Marufu, Lackson T.
Doddridge, Bruce G.
Dickerson, Russell R.
TI Origins of chemical pollution derived from Mid-Atlantic aircraft
profiles using a clustering technique
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE ozone; SO2; clustering; emissions
ID SYNOPTIC METEOROLOGICAL CONTROLS; LIGHT-SCATTERING CHARACTERISTICS;
VERTICAL TRANSPORT PROCESSES; AIR-QUALITY MODELS; TROPOSPHERIC OZONE;
RELATIVE-HUMIDITY; PRECIPITATION CHEMISTRY; PARTICULATE MATTER; BACK
TRAJECTORIES; UNITED-STATES
AB Upwind sources of NOx and SO2 play a crucial role in the amount of O-3 and aerosols in the lower troposphere in the Mid-Atlantic US. This paper describes a novel method of clustering trace gas and aerosol profiles allowing for the quantification of the relationship between point sources and pollution levels. This improves our understanding of pollution origins and has the potential for prediction of episodes of poor air quality. A hierarchical clustering method was used to classify distinct chemical and meteorological events from over 200 aircraft vertical profiles in the lower troposphere. Profile measurements included O-3, SO2, CO and particle scattering from June to August 1997-2003, in the Mid-Atlantic US (mostly in Maryland, Pennsylvania and Virginia). The clustering technique could discriminate distinct profile shapes including measurements made during the 2002 Canadian forest fires. Forty-eight-hour back trajectories were run for each profile and the integrated NOx and SO2 point source emissions encountered by each trajectory were calculated using data from the EPA Clean Air Market Division's emissions database. There was a strong correlation between integrated NOx emissions and O-3 profiles, indicating that O-3 profiles are strongly influenced by and can be predicted with point source emissions. There is a prevalent concentration of SO2 over the eastern US with mixing ratios decreasing smoothly from about 3.5 ppb near the surface to 0.2 ppb at 2400 m. (C) 2007 Elsevier Ltd. All rights reserved.
C1 [Hains, Jennifer C.; Dickerson, Russell R.] Univ Maryland, Dept Chem, College Pk, MD 20742 USA.
[Taubman, Brett F.] Appalachian State Univ, Dept Chem, Boone, NC 28608 USA.
[Dickerson, Russell R.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Stehr, Jeffrey W.] Univ Maryland, Dept Atmospher Ocean & Space Sci, College Pk, MD 20742 USA.
[Marufu, Lackson T.; Doddridge, Bruce G.] NASA, Langley Res Ctr, Hampton, VA USA.
RP Hains, JC (reprint author), Univ Maryland, Dept Chem, College Pk, MD 20742 USA.
EM hains@knmi.nl
RI Stehr, Jeffrey/F-2638-2010; Dickerson, Russell/F-2857-2010; Thompson,
Anne /C-3649-2014
OI Stehr, Jeffrey/0000-0003-4840-6942; Dickerson,
Russell/0000-0003-0206-3083; Thompson, Anne /0000-0002-7829-0920
NR 45
TC 31
Z9 31
U1 1
U2 13
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 MAR
PY 2008
VL 42
IS 8
BP 1727
EP 1741
DI 10.1016/j.atmosenv.2007.11.052
PG 15
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 284SO
UT WOS:000254726300006
ER
PT J
AU Jordan, NS
Ichoku, C
Hoff, RM
AF Jordan, Nikisa S.
Ichoku, Charles
Hoff, Raymond M.
TI Estimating smoke emissions over the US Southern Great Plains using MODIS
fire radiative power and aerosol observations
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE fire radiative energy (FRE); smoke; MODIS; emissions
ID BIOMASS BURNING EMISSIONS; IMAGING SPECTRORADIOMETER MODIS;
OPTICAL-PROPERTIES; EOS-MODIS; SATELLITE; ENERGY; PARTICLES; PRODUCTS;
SYSTEM; LAND
AB A newly developed method, which involves the use of satellite measurements of energy released by fires, was used to estimate smoke emissions in the United States (US) Southern Great Plains (SGP). This SGP region was chosen because extensive agricultural and planned burning occurs there annually. Moderate resolution imaging spectroradiometer (MODIS) aerosol optical depth (AOD) and fire radiative energy (FRE) release rates (R-FRF), acquired in 2004 from the Terra and Aqua satellites, were used to derive a FRE-based smoke emission coefficient (C-e kgMJ(-1)), which when multiplied by R-FRE (MJs(-1)) gives the rate of smoke emission (kg s(-1)). Correlations between the smoke emission rates and the RFRE were significant for Terra-MODIS (R-2 = 0.645, n = 146, p < 0.0001) and Aqua-MODIS (R-2 = 0.752, n = 178, p < 0.0001). Furthermore, the C, values derived independently from Terra and Aqua were in close agreement, and the average C, for this area is 0.049 +/- 0.024 kg MJ(-1). A Monte Carlo (MC) probabilistic approach was used to approximate uncertainties from the smoke emission and resulting C,. For the first time, smoke emission estimates have been derived for the US SGP using observations of energy released by fires. Although more work is necessary, the present study demonstrates the feasibility of using RFRE for smoke emission estimation in that region. Burning peaked during the spring and fall seasons. Moreover, qualitative examination of smoke emission patterns side-by-side with local air-quality measurements indicated that the impact of smoke from local biomass burning activities was significant on the regional airquality. (c) 2008 Elsevier Ltd. All rights reserved.
C1 [Jordan, Nikisa S.; Hoff, Raymond M.] Univ Maryland, Joint Ctr Earth Syst Technol JCET, Cooperat Ctr Remote Sensing Sci & Technol CREST, Baltimore, MD 21250 USA.
[Ichoku, Charles] Univ Maryland, ESSIC, College Pk, MD 20742 USA.
[Ichoku, Charles] NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Greenbelt, MD 20771 USA.
RP Jordan, NS (reprint author), Univ Maryland, Joint Ctr Earth Syst Technol JCET, Cooperat Ctr Remote Sensing Sci & Technol CREST, Baltimore Cty 5523,Res Pk Dr,Suite 320, Baltimore, MD 21250 USA.
EM njordan1@umbc.edu
RI Hoff, Raymond/C-6747-2012; Ichoku, Charles/E-1857-2012
OI Ichoku, Charles/0000-0003-3244-4549
NR 61
TC 20
Z9 20
U1 3
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD MAR
PY 2008
VL 42
IS 9
BP 2007
EP 2022
DI 10.1016/j.atmosenv.2007.12.023
PG 16
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 297MM
UT WOS:000255620800005
ER
PT J
AU Civerolo, KL
Hogrefe, C
Lynn, B
Rosenzweig, C
Goldberg, R
Rosenthal, J
Knowlton, K
Kinney, PL
AF Civerolo, Kevin L.
Hogrefe, Christian
Lynn, Barry
Rosenzweig, Cynthia
Goldberg, Richard
Rosenthal, Joyce
Knowlton, Kim
Kinney, Patrick L.
TI Simulated effects of climate change on summertime nitrogen deposition in
the eastern US
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE atmospheric deposition; climate change; CMAQ; MM5; nitrogen
ID NORTHEASTERN UNITED-STATES; COMMUNITY MULTISCALE AIR; ATMOSPHERIC
DEPOSITION; ACIDIC DEPOSITION; DRY DEPOSITION; TRENDS NETWORK; MODEL;
QUALITY; INVENTORY; EMISSIONS
AB It is anticipated that climate change may impact regional-scale air quality and atmospheric deposition in the coming decades. To simulate the effects of climate change on nitrogen (N) deposition across numerous watersheds in the eastern US, we applied the NASA Goddard Institute for Space Studies General Circulation Model (GISS-GCM), Fifth Generation Pennsylvania State University/National Center for Atmospheric Research Mesoscale Model (MM5), Sparse Matrix Operator Kernel Emissions (SMOKE) modeling system, and the US Environmental Protection Agency Community Multiscale Air Quality (CMAQ) Model. Keeping chemical initial and boundary conditions, land use, and anthropogenic area and point source emissions fixed, this modeling system was applied over five summers (June-August) from 1993 to 1997 and five summers from 2053 to 2057. Over these eastern US watersheds, the modeling system estimated 3-14% increases in summertime N deposition as a result of climate change. This increase is primarily due to the direct effects of climate change on atmospheric conditions and chemistry. Wet N deposition is predicted to increase as a result of increased precipitation, while dry N deposition is predicted to increase as higher surface temperatures favor gas-phase nitric acid to particulate nitrate. The simulated increase suggests that additional reductions in N oxides and/or ammonia may be needed to fully realize the anticipated benefits of planned reduction strategies, including the Clean Air Interstate Rule (CAIR). (c) 2007 Elsevier Ltd. All rights reserved.
C1 [Civerolo, Kevin L.; Hogrefe, Christian] New York State Dept Environm Conservat, Div Air Resources, Albany, NY 12233 USA.
[Hogrefe, Christian] SUNY Albany, Atmospher Sci Res Ctr, Albany, NY 12222 USA.
[Lynn, Barry; Rosenzweig, Cynthia; Goldberg, Richard] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Rosenthal, Joyce] Columbia Univ, Grad Sch Architecture Planning & Preservat, New York, NY USA.
[Knowlton, Kim; Kinney, Patrick L.] Columbia Univ, Mailman Sch Publ Hlth, New York, NY USA.
RP Civerolo, KL (reprint author), New York State Dept Environm Conservat, Div Air Resources, 625 Broadway, Albany, NY 12233 USA.
EM kxcivero@gw.dec.state.ny.us
RI Kinney, Patrick/H-7914-2012;
OI Civerolo, Kevin/0000-0003-1536-2664
NR 40
TC 6
Z9 7
U1 0
U2 10
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 MAR
PY 2008
VL 42
IS 9
BP 2074
EP 2082
DI 10.1016/j.atmosenv.2007.11.049
PG 9
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 297MM
UT WOS:000255620800010
ER
PT J
AU Bhatia, AK
Landi, E
AF Bhatia, A. K.
Landi, E.
TI Atomic data and spectral line intensities for Ar XV
SO ATOMIC DATA AND NUCLEAR DATA TABLES
LA English
DT Article
ID BE-LIKE IONS; BERYLLIUM ISOELECTRONIC SEQUENCE; ELECTRON-IMPACT
EXCITATION; COLLISION STRENGTHS; EMISSION-LINES; OSCILLATOR-STRENGTHS;
RATE COEFFICIENTS; CROSS-SECTIONS; TRANSITIONS; NI
AB Electron impact collision strengths, energy levels, oscillator strengths, and spontaneous radiative decay rates are calculated for Ar XV. The configurations used are 2s(2), 2s2p, 2p(2), 2l3l', 2l4l' and 2s5l', with l = s, p and l' = s, p, d giving rise to 92 fine-structure levels in intermediate coupling, Collision strengths are calculated at eight incident energies (10, 20, 30, 60, 120, 180, 240, and 300 Ry) for transitions within the three lowest configurations, and five incident energies (60, 120, 180, 240, and 300 Ry) for transitions between the lowest five levels and the n = 3, 4, 5 configurations, using the distorted wave approximation. Excitation rate coefficients are calculated as a function of electron temperature by assuming a Maxwellian electron velocity distribution. Using the excitation rate coefficients and the radiative transition rates of the present work, and R-matrix results for the 2s(2), 2s2p, 2P(2) configurations available in the literature, statistical equilibrium equations for level populations are solved at electron densities covering the range of 10(8)-10(14) cm(-3) at an electron temperature of log T-e(K) = 6.6, corresponding to the maximum abundance of Ar XV. Spectral line intensities are calculated, and their diagnostic relevance is discussed. Observed line ratios indicate electron temperatures of the relevant emitting plasma close to log T-e(K) = 6.6. This dataset will be made available in the next version of the CHIANTI database. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Landi, E.] USN, Res Lab, Washington, DC 20375 USA.
[Bhatia, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Landi, E.] ARTEP Inc, Columbia, MD 21044 USA.
RP Landi, E (reprint author), USN, Res Lab, Washington, DC 20375 USA.
EM Landi@poppeo.nrl.navy.mil
RI Landi, Enrico/H-4493-2011
NR 31
TC 7
Z9 7
U1 0
U2 2
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0092-640X
J9 ATOM DATA NUCL DATA
JI Atom. Data Nucl. Data Tables
PD MAR
PY 2008
VL 94
IS 2
BP 223
EP 256
DI 10.1016/j.adt.2007.11.001
PG 34
WC Physics, Atomic, Molecular & Chemical; Physics, Nuclear
SC Physics
GA 274JW
UT WOS:000253998600002
ER
PT J
AU Le Marshall, J
Jung, J
Zapotocny, T
Redder, C
Dunn, M
Daniels, J
Riishojgaard, LP
AF Le Marshall, J.
Jung, J.
Zapotocny, T.
Redder, C.
Dunn, M.
Daniels, J.
Riishojgaard, Lars Peter
TI Impact of MODIS atmospheric motion vectors on a global NWP system
SO AUSTRALIAN METEOROLOGICAL MAGAZINE
LA English
DT Article
ID DATA ASSIMILATION SYSTEM; POLAR-REGIONS; CLOUD-DRIFT; WINDS
C1 [Le Marshall, J.; Jung, J.; Zapotocny, T.; Redder, C.; Dunn, M.; Daniels, J.; Riishojgaard, Lars Peter] Joint Ctr Satellite Data Assimilat, Camp Springs, MD USA.
[Jung, J.; Zapotocny, T.] CIMSS, Madison, WI USA.
[Redder, C.; Riishojgaard, Lars Peter] Global Modeling Assimilat Off, NASA GSFC, Greenbelt, MD USA.
[Dunn, M.] La Trobe Univ, Bundoora, Vic, Australia.
[Daniels, J.] NOAA NESDIS STAR, Camp Springs, MD USA.
RP Le Marshall, J (reprint author), Bur Meteorol, Ctr Australian Weather & Climate Res, GPO Box 1289, Melbourne, Vic 3001, Australia.
EM j.lemarshall@bom.gov.au
RI Daniels, Jaime/E-7933-2011
OI Daniels, Jaime/0000-0002-9438-6631
NR 19
TC 9
Z9 9
U1 0
U2 3
PU AUSTRALIAN BUREAU METEOROLOGY
PI MELBOURNE
PA GPO BOX 1289, MELBOURNE, VIC 3001, AUSTRALIA
SN 0004-9743
J9 AUST METEOROL MAG
JI Aust. Meteorol. Mag.
PD MAR
PY 2008
VL 57
IS 1
BP 45
EP 51
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 318IL
UT WOS:000257084700004
ER
PT J
AU Bornstein, BJ
Keating, SM
Jouraku, A
Hucka, M
AF Bornstein, Benjamin J.
Keating, Sarah M.
Jouraku, Akiya
Hucka, Michael
TI LibSBML: an API library for SBML
SO BIOINFORMATICS
LA English
DT Article
ID MODELS
AB LibSBML is an application programming interface library for reading, writing, manipulating and validating content expressed in the Systems Biology Markup Language (SBML) format. It is written in ISO C and C++, provides language bindings for Common Lisp, Java, Python, Perl, MATLAB and Octave, and includes many features that facilitate adoption and use of both SBML and the library. Developers can embed libSBML in their applications, saving themselves the work of implementing their own SBML parsing, manipulation and validation software.
C1 [Keating, Sarah M.; Hucka, Michael] CALTECH, Biol Network Modeling Ctr, Pasadena, CA 91125 USA.
[Bornstein, Benjamin J.] NASA, Jet Propuls Lab, Washington, DC 20546 USA.
[Jouraku, Akiya] Keio Univ, Sch Fundamental Sci & Technol, Yokohama, Kanagawa 223, Japan.
RP Keating, SM (reprint author), CALTECH, Biol Network Modeling Ctr, Pasadena, CA 91125 USA.
RI Hucka, Michael/B-1896-2012;
OI Keating, Sarah/0000-0002-3356-3542
FU Biotechnology and Biological Sciences Research Council; NIGMS NIH HHS
[R01 GM070923, R01 GM070923-04, R01 GM077671]
NR 8
TC 135
Z9 137
U1 1
U2 7
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 1367-4803
J9 BIOINFORMATICS
JI Bioinformatics
PD MAR
PY 2008
VL 24
IS 6
BP 880
EP 881
DI 10.1093/bioinformatics/btn051
PG 2
WC Biochemical Research Methods; Biotechnology & Applied Microbiology;
Computer Science, Interdisciplinary Applications; Mathematical &
Computational Biology; Statistics & Probability
SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology;
Computer Science; Mathematical & Computational Biology; Mathematics
GA 274OK
UT WOS:000254010400026
PM 18252737
ER
PT J
AU Gu, L
Hanson, PJ
Mac Post, W
Kaiser, DP
Yang, B
Nemani, R
Pallardy, SG
Meyers, T
AF Gu, Lianhong
Hanson, Paul J.
Mac Post, W.
Kaiser, Dale P.
Yang, Bai
Nemani, Ramakrishna
Pallardy, Stephen G.
Meyers, Tilden
TI The 2007 eastern US spring freezes: Increased cold damage in a warming
world?
SO BIOSCIENCE
LA English
DT Article
DE extreme temperature fluctuation; frost damage; plant phenology; climate
warming; carbon cycle
ID ELEVATED ATMOSPHERIC CO2; FROST HARDINESS; CLIMATE-CHANGE; WINTER THAW;
RED SPRUCE; SCOTS PINE; GROWTH; TOLERANCE; INJURY; TREES
AB Plant ecologists have long been concerned with a seemingly paradoxical scenario in the relationship between plant growth and climate change: warming may actually increase the risk of plant frost damage. The underlying hypothesis is that mild winters and warm, early springs, which are expected to occur as the climate warms, may induce premature plant development, resulting in exposure of vulnerable plant tissues and organs to subsequent late-season frosts. The 2007 spring freeze in the eastern United States provides an excellent opportunity to evaluate this hypothesis and assess its large-scale consequences. In this article, we contrast the rapid prefreeze phenological advancement caused by unusually warm conditions with the dramatic postfreeze setback, and report complicated patterns of freeze damage to plants. The widespread devastation of crops and natural vegetation occasioned by this event demonstrates the need to consider large fluctuations in spring temperatures a real threat to terrestrial ecosystem structure and functioning in a warming climate.
C1 [Gu, Lianhong; Hanson, Paul J.; Mac Post, W.; Kaiser, Dale P.; Yang, Bai] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA.
[Nemani, Ramakrishna] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Pallardy, Stephen G.] Univ Missouri, Dept Forestry, Columbia, MO USA.
[Meyers, Tilden] Natl Ocean Atmospher Adm, Air Resources Lab, Atmospher Turbulence & Diffus Div, Oak Ridge, TN USA.
RP Gu, L (reprint author), Oak Ridge Natl Lab, Div Environm Sci, POB 2008, Oak Ridge, TN 37831 USA.
EM lianhong-gu@ornl.gov
RI Hanson, Paul J./D-8069-2011; Post, Wilfred/B-8959-2012; Meyers,
Tilden/C-6633-2016; Gu, Lianhong/H-8241-2014
OI Hanson, Paul J./0000-0001-7293-3561; Gu, Lianhong/0000-0001-5756-8738
NR 38
TC 190
Z9 204
U1 8
U2 84
PU AMER INST BIOLOGICAL SCI
PI WASHINGTON
PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 USA
SN 0006-3568
J9 BIOSCIENCE
JI Bioscience
PD MAR
PY 2008
VL 58
IS 3
BP 253
EP 262
DI 10.1641/B580311
PG 10
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 275KQ
UT WOS:000254070700011
ER
PT J
AU Smith, SM
Zwart, SR
Heer, M
Lee, SMC
Baecker, N
Meuche, S
Macias, BR
Shackelford, LC
Schneider, S
Hargens, AR
AF Smith, Scott M.
Zwart, Sara R.
Heer, Martina
Lee, Stuart M. C.
Baecker, Natalie
Meuche, Sabine
Macias, Brandon R.
Shackelford, Linda C.
Schneider, Suzanne
Hargens, Alan R.
TI WISE-2005: Supine treadmill exercise within lower body negative pressure
and flywheel resistive exercise as a countermeasure to bed rest-induced
bone loss in women during 60-day simulated microgravity
SO BONE
LA English
DT Article
DE bone turnover markers; exercise; space flight; bed rest; simulated
weightlessness
ID MUSCLE-FIBER FUNCTION; RESISTANCE EXERCISE; SPACE-FLIGHT;
NUTRITIONAL-STATUS; UPRIGHT EXERCISE; CONCURRENT EXERCISE;
IDENTICAL-TWINS; FOLLOW-UP; PAMIDRONATE; RESORPTION
AB Bone loss associated with disuse during bed rest (BR), an analog of space flight, can be attenuated by exercise. In previous studies, the efficacy of either aerobic or resistive exercise countermeasures has been examined separately. We hypothesized that a regimen of combined resistive and aerobic exercise during BR would prevent bone resorption and promote bone formation. After a 20-day ambulatory adaptation to controlled confinement and diet, 16 women participated in a 60-day, 6 head-down-tilt BR and were assigned randomly to one of the two groups. Control subjects (CON, n=8) performed no countermeasure. Exercise subjects (EX, n=8) participated in an exercise program during BR, alternating between supine treadmill exercise within lower body negative pressure (3-4 d wk(-1)) and flywheel resistive exercise (2-3 d wk(-1)). By the last week of BR, excretion of helical peptide (CON, 79% +/- 44 increase; EX, 64% +/- 50, mean +/- SD) and N-terminal cross-linking telopeptide (CON, 51% +/- 34; EX, 43% +/- 56), markers of bone resorption, were greater than they were before BR in both groups (P<0.05). However, serum concentrations of the bone formation marker procollagen type I N propeptide were greater in EX than CON throughout and after bed rest (P<0.05), while concentrations of the bone formation marker bone alkaline phosphatase tended to be greater in EX than CON. Dual-energy X-ray absorptiometry results indicated that the exercise treatment significantly (P<0.05) attenuated loss of hip and leg bone mineral density in EX compared to CON. The combination of resistive and aerobic exercise did not prevent bone resorption but did promote bone formation, and helped mitigate the net bone loss associated with simulated microgravity. (c) 2007 Published by Elsevier Inc.
C1 [Smith, Scott M.; Shackelford, Linda C.] NASA, Lyndon B Johnson Space Ctr, Nutr Biochem Lab,Natl Aeronaut & Space Adm, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA.
[Zwart, Sara R.] Univ Space Res Assoc, Houston, TX 77058 USA.
[Heer, Martina; Baecker, Natalie] DLR, Inst Aerosp Med, Cologne, Germany.
[Lee, Stuart M. C.] Wyle, Houston, TX 77058 USA.
[Meuche, Sabine; Macias, Brandon R.; Hargens, Alan R.] Univ Calif San Diego, Med Ctr, Dept Orthopaed Surg, San Diego, CA 92103 USA.
[Meuche, Sabine] Charite Univ Med Berlin, Ctr Space Med, D-13353 Berlin, Germany.
[Schneider, Suzanne] Univ New Mexico, Dept Phys Performance & Dev, Albuquerque, NM 87131 USA.
RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Nutr Biochem Lab,Natl Aeronaut & Space Adm, Human Adaptat & Countermeasures Div, Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA.
EM scott.m.smith@nasa.gov
NR 41
TC 38
Z9 39
U1 1
U2 6
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 8756-3282
J9 BONE
JI Bone
PD MAR
PY 2008
VL 42
IS 3
BP 572
EP 581
DI 10.1016/j.bone.2007.11.015
PG 10
WC Endocrinology & Metabolism
SC Endocrinology & Metabolism
GA 271OW
UT WOS:000253799500014
PM 18249055
ER
PT J
AU Anthes, RA
Bernhardt, PA
Chen, Y
Cucurull, L
Dymond, KF
Ector, D
Healy, SB
Ho, SP
Hunt, DC
Kuo, YH
Liu, H
Manning, K
Mccormick, C
Meehan, TK
Randel, WJ
Rocken, C
Schreiner, WS
Sokolovskiy, SV
Syndergaard, S
Thompson, DC
Trenberth, KE
Wee, TK
Yen, NL
Zeng, Z
AF Anthes, R. A.
Bernhardt, P. A.
Chen, Y.
Cucurull, L.
Dymond, K. F.
Ector, D.
Healy, S. B.
Ho, S. -P.
Hunt, D. C.
Kuo, Y. -H.
Liu, H.
Manning, K.
Mccormick, C.
Meehan, T. K.
Randel, W. J.
Rocken, C.
Schreiner, W. S.
Sokolovskiy, S. V.
Syndergaard, S.
Thompson, D. C.
Trenberth, K. E.
Wee, T. -K.
Yen, N. L.
Zeng, Z.
TI The COSMOC/FORMOSAT-3 - Mission early results
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID RADIO OCCULTATION MEASUREMENTS; GLOBAL POSITIONING SYSTEM;
LOW-EARTH-ORBIT; COSMIC CONSTELLATION; TROPICAL TROPOPAUSE; LOWER
TROPOSPHERE; ATMOSPHERE; INSTRUMENT; CLIMATE; SIGNALS
AB The radio occultation (RO) technique, which makes use of radio signals transmitted by the global positioning system (GPS) satellites, has emerged as a powerful and relatively inexpensive approach for sounding the global atmosphere with high precision, accuracy, and vertical resolution in all weather and over both land and ocean. On 15 April 2006, the joint Taiwan-U.S. Constellation Observing System for Meteorology, Ionosphere, and Climate (COSMIC)/Formosa Satellite Mission 3 (COSMIC/FORMOSAT-3, hereafter COSMIC) mission, a constellation of six micro satellites, was launched into a 512-km orbit. After launch the satellites were gradually deployed to their final orbits at 800 km, a process that took about 17 months. During the early weeks of the deployment, the satellites were spaced closely, offering a unique opportunity to verify the high precision of RO measurements. As of September 2007, COSMIC is providing about 2000 RO soundings per day to support the research and operational communities. COSMIC RO data are of better quality than those from the previous missions and penetrate much farther down into the troposphere; 70%-90% of the soundings reach to within 1 km of the surface on a global basis. The data are having a positive impact oil operational global weather forecast models. With the ability to penetrate deep into the lower troposphere using an advanced open-loop tracking technique, the COSMIC RO instruments can observe the structure of the tropical atmospheric boundary layer. The value of RO for climate monitoring and research is demonstrated by the precise and consistent observations between different instruments, platforms, and missions. COSMIC observations are capable of intercalibrating microwave measurements from the Advanced Microwave Sounding Unit (AMSU) on different satellites. Finally, unique and useful observations of the ionosphere are being obtained using the RO receiver and two other instruments on the COSMIC satellites, the tiny ionosphere photometer (TIP) and the tri-band beacon.
C1 [Cucurull, L.; Ector, D.; Ho, S. -P.; Hunt, D. C.; Kuo, Y. -H.; Rocken, C.; Schreiner, W. S.; Sokolovskiy, S. V.; Syndergaard, S.; Wee, T. -K.; Zeng, Z.] Univ Corp Atmospher Res, Boulder, CO USA.
[Bernhardt, P. A.; Dymond, K. F.] Naval Res Lab, Washington, DC USA.
[Chen, Y.; Ho, S. -P.; Liu, H.; Manning, K.; Randel, W. J.; Trenberth, K. E.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Healy, S. B.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
[Meehan, T. K.] Jet Prop Lab, Pasadena, CA USA.
[Thompson, D. C.] Utah State Univ, Logan, UT 84322 USA.
[Yen, N. L.] Natl Space Org, Hsinchu, Taiwan.
RP Kuo, YH (reprint author), UCAR, POB 3000, Boulder, CO 80307 USA.
EM kuo@ucar.edu
RI Trenberth, Kevin/A-5683-2012; Zeng, Zhen/J-5183-2014; Cucurull,
Lidia/E-8900-2015; Randel, William/K-3267-2016; Syndergaard,
Stig/C-1103-2017
OI Trenberth, Kevin/0000-0002-1445-1000; Randel,
William/0000-0002-5999-7162; Syndergaard, Stig/0000-0003-3119-2618
NR 59
TC 375
Z9 392
U1 6
U2 44
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD MAR
PY 2008
VL 89
IS 3
BP 313
EP 333
DI 10.1175/BAMS-89-3-313
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 286MA
UT WOS:000254848800013
ER
PT J
AU Lau, KM
Ramanathan, V
Wu, GX
Li, Z
Tsay, SC
Hsu, C
Sikka, R
Holben, B
Lu, D
Tartari, G
Chin, M
Koudelova, R
Chen, H
Ma, Y
Huang, J
Taniguchi, K
Zhang, R
AF Lau, K. -M.
Ramanathan, V.
Wu, G. -X.
Li, Z.
Tsay, S. C.
Hsu, C.
Sikka, R.
Holben, B.
Lu, D.
Tartari, G.
Chin, M.
Koudelova, R.
Chen, H.
Ma, Y.
Huang, J.
Taniguchi, K.
Zhang, R.
TI The Joint Aerosol-Monsoon Experiment - A new challenge for monsoon
climate research
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID ATMOSPHERIC BROWN CLOUDS; TIBETAN PLATEAU; CLOUDINESS; REDUCTION;
POLLUTION; RAINFALL; IMPACTS; NETWORK; INDIA; CHINA
AB Aerosol- and moonsoon-related droughts and floods are two of the most serious environmental hazards confronting more than 60% of the population of the world living in the Asian monsoon countries. In recent years, thanks to improved satellite and in situ observations, and better models, great strides have been made in aerosol and monsoon research, respectively. There is now a growing body of evidence suggesting that interaction of aerosol forcing with monsoon dynamics may alter the redistribution of energy in the atmosphere and at the Earth's surface, thereby influencing monsoon water cycle and climate. In this article, the authors describe the scientific rationale and challenges for an integrated approach to study the interactions between aerosol and monsoon water cycle dynamics. A joint Aerosol-Monsoon Experiment (JAMEX) is proposed for 2007-11, with enhanced observations of the physical and chemical properties, sources and sinks, and long-range transport of aerosols, in conjunction with meteorological and oceanographic observations in the Indo-Pacific continental and oceanic regions. JAMEX will leverage on coordination among many ongoing and planned national research programs on aerosols and monsoons in China, India, Japan, Nepal, Italy, and the United States, as well as international research programs of the World Climate Research Program (WCRP) and the World Meteorological Organization (WMO).
C1 [Lau, K. -M.; Tsay, S. C.; Hsu, C.; Chin, M.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Ramanathan, V.] Univ Calif San Diego, Ctr Clouds Chem & Climate, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Wu, G. -X.] Chinese Acad Sci, Inst Atmospher Phys, State Key Lab Atmosphere Sci & Geophys Fluid Dyna, Beijing, Peoples R China.
[Li, Z.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Holben, B.] NASA, Goddard Space Flight Ctr, Lab Hydrosphere, Greenbelt, MD 20771 USA.
[Tartari, G.] CNR, Water Res Inst, Milan, Italy.
[Tartari, G.] EV K2 CNR Comm, Bergamo, Italy.
[Koudelova, R.] Univ Tokyo, CEOP Int Project Off, Tokyo, Japan.
[Ma, Y.] Chinese Acad Sci, Inst Tibetan Plateau Res, Beijing, Peoples R China.
[Huang, J.] Lanzhou Univ, Sch Atmospher Sci, Lanzhou 730000, Peoples R China.
[Taniguchi, K.] Univ Tokyo, Dept Civil Engn, Tokyo 113, Japan.
[Zhang, R.] Chinese Acad Sci, Inst Atmospher Phys, Beijing, Peoples R China.
RP Lau, KM (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
EM William.K.Lau@nasa.gov
RI Chin, Mian/J-8354-2012; Hsu, N. Christina/H-3420-2013; Li,
Zhanqing/F-4424-2010; Tsay, Si-Chee/J-1147-2014; Taniguchi,
Kenji/C-3429-2015; Lau, William /E-1510-2012
OI Li, Zhanqing/0000-0001-6737-382X; Lau, William /0000-0002-3587-3691
NR 36
TC 122
Z9 128
U1 2
U2 29
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD MAR
PY 2008
VL 89
IS 3
BP 369
EP +
DI 10.1175/BAMS-89-3-369
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 286MA
UT WOS:000254848800016
ER
PT J
AU Manderson, JP
AF Manderson, John P.
TI The spatial scale of phase synchrony in winter flounder
(Pseudopleuronectes americanus) production increased among southern New
England nurseries in the 1990s
SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES
LA English
DT Article
ID SHRIMP CRANGON-SEPTEMSPINOSA; NORTHEASTERN US ESTUARIES;
POPULATION-DYNAMICS; ENVIRONMENTAL NOISE; NARRAGANSETT BAY;
CLIMATE-CHANGE; PREDATION; HABITAT; GROWTH; LARVAE
AB The spatial scales at which the dynamics of subpopulations are synchronized affect regional population persistence and reflect the operational spatial scales of factors regulating populations. I examined phase synchrony in the fluctuations of age-0 winter flounder (Pseudopleuronectes americanus) production among 19 southern New England (SNE), USA, coastal nurseries. From 1990 to 2004, nursery production was synchronized at scales up to similar to 200 km based on spatial trends in cross-correlations of first-differenced age-0 abundance time series. However, sliding window analysis of 1975-2005 time series collected in six nurseries <= 55 km apart in northern SNE indicated that synchrony increased from low to high values in the early 1990s. Synchrony in production also increased among three nurseries <= 65 km apart in southern SNE from 1984 to 2004. Thus, interannual fluctuations in nursery production appeared to become synchronized at coarser spatial scales throughout SNE during the 1990s. This coarsening of the spatial scale of control of winter flounder nursery production was coincident with an increase in the frequency of springs with warm temperatures believed to negatively affect early life history processes. Spatial synchronization of winter flounder nursery ground production could destabilize the age-class structure and population dynamics in the region.
C1 NOAA, Natl Marine Fisheries Serv, Ecosyst Proc Div, Behav Ecol Branch,James J Howard Marine Sci Lab, Highlands, NJ 07732 USA.
RP Manderson, JP (reprint author), NOAA, Natl Marine Fisheries Serv, Ecosyst Proc Div, Behav Ecol Branch,James J Howard Marine Sci Lab, 74 Magruder Rd, Highlands, NJ 07732 USA.
EM john.manderson@noaa.gov
NR 54
TC 17
Z9 18
U1 2
U2 9
PU NATL RESEARCH COUNCIL CANADA-N R C RESEARCH PRESS
PI OTTAWA
PA BUILDING M 55, OTTAWA, ON K1A 0R6, CANADA
SN 0706-652X
J9 CAN J FISH AQUAT SCI
JI Can. J. Fish. Aquat. Sci.
PD MAR
PY 2008
VL 65
IS 3
BP 340
EP 351
DI 10.1139/F07-169
PG 12
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 271FT
UT WOS:000253775000002
ER
PT J
AU Vertrees, RA
Zwischenberger, JB
Boor, PJ
Popov, V
McCarthy, M
Solley, TN
Goodwin, TJ
AF Vertrees, Roger A.
Zwischenberger, Joseph B.
Boor, Paul J.
Popov, Vselovod
McCarthy, Maureen
Solley, Travis N.
Goodwin, Thomas J.
TI Cellular differentiation in three-dimensional lung cell cultures
SO CANCER BIOLOGY & THERAPY
LA English
DT Article
DE tissue engineering; lung cells; co-culture
ID EPITHELIAL MEMBRANE ANTIGEN; MUCIN GENE-EXPRESSION; III BETA-TUBULIN;
MONOCLONAL-ANTIBODIES; IN-VITRO; SQUAMOUS DIFFERENTIATION;
VONWILLEBRAND-FACTOR; MESENCHYMAL CELLS; BASEMENT-MEMBRANE; CARCINOMA
CELLS
AB Introduction: Aspects of human biology that are not sufficiently addressed by current cell culture models are cellular differentiation and three-dimensional ( 3-D) structural organization. A model that more closely associates the presence and biology of organelles to molecular expressions relevant to these organelles may provide evidence of cellular differentiation and the beginning steps in the construction of a 3-D architecture. The development of a new model-3-D cell cultures-may ultimately provide a better understanding of lung biology and pathobiology.
Purpose: The purpose of this study was to develop both traditional monolayer and 3-D cell cultures of a known and well documented normal lung cell line and then to determine similarities and differences between these cultures in terms of differentiation and molecular marker expression.
Results: Electron microscopy identified presence of lipid inclusion, microvilli, extra cellular matrix, and tight junctions in the 3-D cultures; differentiation not seen in ML cultures. The degree of differentiation determined by immunohistochemistry when the cell line was grown as ML or 3-D cultures shows that ultra-structure and marker expressions were more representative of control tissue than when cells were grown in 3-D than as MLs.
Methods: An immortalized cell line was grown as a traditional monolayer ( ML) in culture flasks and as 3-D cultures in rotating walled vessels and incubated under identical conditions. Comparison for presence of differentiation and marker expression between these cultures and control tissue collected from surgical patient specimens was studied. Electron microscopy for identification of ultra structures, and immunohistochemistry ( ZO-1, EMA, ICAM-1, villin, tubulin, CK 18, VWF, Collagen IV and human mucin) for phenotypic comparisons between cells in ML and 3-D cell cultures was conducted.
Summary: The development of 3-D cell cultures will provide for a new and more powerful tool in the study of lung biology and pathobiology.
C1 [Vertrees, Roger A.; Solley, Travis N.] Univ Texas Med Branch, Dept Surg, Galveston, TX 77555 USA.
[Boor, Paul J.; Popov, Vselovod] Univ Texas Med Branch, Dept Pathol, Galveston, TX 77555 USA.
[Zwischenberger, Joseph B.] Univ Kentucky, Dept Surg, Lexington, KY USA.
[McCarthy, Maureen] NASA, Lyndon B Johnson Space Ctr, Univ Space Res Assoc, Houston, TX 77058 USA.
[Goodwin, Thomas J.] NASA, Lyndon B Johnson Space Ctr, Dis Modelling Tissue Analogues Lab, Houston, TX 77058 USA.
RP Vertrees, RA (reprint author), Univ Texas Med Branch, Dept Surg, 301 Univ Blvd, Galveston, TX 77555 USA.
EM rvertree@utmb.edu
NR 69
TC 1
Z9 1
U1 0
U2 1
PU LANDES BIOSCIENCE
PI AUSTIN
PA 1806 RIO GRANDE ST, AUSTIN, TX 78702 USA
SN 1538-4047
J9 CANCER BIOL THER
JI Cancer Biol. Ther.
PD MAR
PY 2008
VL 7
IS 3
BP 405
EP U7
PG 8
WC Oncology
SC Oncology
GA 312HB
UT WOS:000256658700016
ER
PT J
AU Bishop, JL
Lane, MD
Dyar, MD
Brown, AJ
AF Bishop, J. L.
Lane, M. D.
Dyar, M. D.
Brown, A. J.
TI Reflectance and emission spectroscopy study of four groups of
phyllosilicates: smectites, kaolinite-serpentines, chlorites and micas
SO CLAY MINERALS
LA English
DT Article
DE spectroscopy; reflectance; emissivity; smectite; kaolinite; serpentine;
chlorite; mica
ID SOCIETY SOURCE CLAYS; BASE-LINE; INFRARED-SPECTROSCOPY; DIOCTAHEDRAL
SMECTITES; MINERALS; MARS; SPECTRA; DISSOLUTION; CELADONITE; CALIFORNIA
AB Coordinated visible/near-infrared reflectance/mid-infrared reflectance and emissivity spectra of four groups of phyllosilicates were undertaken to provide insights into the differences within and among groups of smectites, kaolinite-serpentines, chlorites and micas. Identification and characterization of phyllosilicates via remote sensing on Earth and Mars can be achieved using the OH combination bands in the 2.2-2.5 mu m region and the tetrahedral SiO4 vibrations from similar to 8.8-12 mu m (similar to 1140-830 cm(-1)) and similar to 20-25 mu m (500-400 cm(-1)). The sharp and well resolved OH combination bands in the 2.2-2.5 mu m region provide unique fingerprints for specific minerals. Al-rich phyllosilicates exhibit OH combination bands near 2.2 mu m, while these bands are observed near 2.29-2.31, 2.33-2.34 mu m and near 2.35-2.37 mu m for Fe3+-rich, Mg-rich and Fe2+-rich phyllosilicates, respectively. When a tetrahedral substitution of Al or Fe3+ for Si occurs, the position of the Si(Al,Fe)O-4 stretching mode absorption shifts. Depending on the size of the cation, the Si(Al,Fe)O-4 bending mode near 500 cm(-1) is split into multiple bands that may be distinguished via hyperspectral remote sensing techniques. The tetrahedral SiO4 vibrations are also influenced by the octahedral cations, such that Al-rich, Fe-rich and Mg-rich phyllosilicates can be discriminated in reflectance and emissivity spectra based on diagnostic positions of the stretching and bending bands. Differences among formation conditions for these four groups of phyllosilicates are also discussed. Hyperspectral remote sensing can be used to identify specific phyllosilicates using electronic and vibrational features and thus provide constraints on the chemistry and formation conditions of soils.
C1 [Bishop, J. L.; Brown, A. J.] NASA, Ames Res Ctr, SETI Inst, Mountain View, CA 94043 USA.
[Lane, M. D.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Dyar, M. D.] Mt Holyoke Coll, S Hadley, MA 01075 USA.
RP Bishop, JL (reprint author), NASA, Ames Res Ctr, SETI Inst, 515 N Whisman Rd, Mountain View, CA 94043 USA.
EM jbishop@mail.arc.nasa.gov
NR 60
TC 126
Z9 126
U1 10
U2 36
PU MINERALOGICAL SOC
PI TWICKENHAM
PA 12 BAYLIS MEWS, AMYAND PARK ROAD,, TWICKENHAM TW1 3HQ, MIDDLESEX,
ENGLAND
SN 0009-8558
EI 1471-8030
J9 CLAY MINER
JI Clay Min.
PD MAR
PY 2008
VL 43
IS 1
BP 35
EP 54
DI 10.1180/claymin.2008.043.1.03
PG 20
WC Chemistry, Physical; Geosciences, Multidisciplinary; Mineralogy
SC Chemistry; Geology; Mineralogy
GA 289GP
UT WOS:000255043300003
ER
PT J
AU Bishop, JL
Dyar, MD
Sklute, EC
Drief, A
AF Bishop, J. L.
Dyar, M. D.
Sklute, E. C.
Drief, A.
TI Physical alteration of antigorite: a Mossbauer spectroscopy, reflectance
spectroscopy and TEM study with applications to Mars
SO CLAY MINERALS
LA English
DT Article
DE antigorite; physical alteration; spectroscopy; Mossbauer; reflectance;
VNIR; HRTEM; SEM; Mars
ID MAGNETITE; MINERALS; SUBSTITUTION; SERPENTINES; KAOLINITE; LIZARDITE;
MAGHEMITE; HEMATITE; SPECTRA
AB Physical alteration of magnetite-bearing antigorite grains is investigated in this study using Mossbauer, visible/near-infrared (VNIR) and mid-IR spectroscopy coupled with scanning electron microscopy (SEM) and high-resolution transmission electron microscopy (HRTEM) analyses. An expected decrease in grain size with grinding is observed using SEM. The HRTEM images illustrate that the nanophase-sized grains which adhere to larger grains have 7 A antigorite patterns. Mossbauer spectroscopy shows the presence of antigorite, magnetite and an amorphous phase. Visible/near infrared spectra exhibit features common in serpentine. These spectra also show an increasing continuum slope with grinding, an effect which is characteristic of thin coatings or tiny grains on surfaces. Mid-IR spectra indicate the formation of fine-grained Si-OH and carbonate in these samples with grinding.
C1 [Bishop, J. L.] NASA, Ames Res Ctr, SETI Inst, Mountain View, CA 94043 USA.
[Dyar, M. D.; Sklute, E. C.] Mt Holyoke Coll, S Hadley, MA 01075 USA.
[Drief, A.] Clorox Serv Co, Pleasanton, CA 94588 USA.
RP Bishop, JL (reprint author), NASA, Ames Res Ctr, SETI Inst, 515 N Whisman Rd, Mountain View, CA 94043 USA.
EM Janice.L.Bishop@nasa.gov
NR 37
TC 7
Z9 7
U1 1
U2 15
PU MINERALOGICAL SOC
PI TWICKENHAM
PA 12 BAYLIS MEWS, AMYAND PARK ROAD,, TWICKENHAM TW1 3HQ, MIDDLESEX,
ENGLAND
SN 0009-8558
EI 1471-8030
J9 CLAY MINER
JI Clay Min.
PD MAR
PY 2008
VL 43
IS 1
BP 55
EP 67
DI 10.1180/claymin.2008.043.1.04
PG 13
WC Chemistry, Physical; Geosciences, Multidisciplinary; Mineralogy
SC Chemistry; Geology; Mineralogy
GA 289GP
UT WOS:000255043300004
ER
PT J
AU Barsi, S
Kassemi, M
AF Barsi, S.
Kassemi, M.
TI Numerical and experimental comparisons of the self-pressurization
behavior of an LH2 tank in normal gravity
SO CRYOGENICS
LA English
DT Article
DE space cryogenics; hydrogen; heat transfer
ID CRYOGENIC TANKS; STORAGE
AB In optimizing the design of cryogenic storage facilities for future in-orbit or on-surface applications the boil-off and the self-pressurization rates must be accurately predicted for different g-levels and for a variety of heat loads and distributions. In this paper, a two-phase CFD model is presented that describes the self-pressurization behavior of a flightweight partially full LH2 tank in normal gravity. Existing experimental data at different fill levels are used to assess the predictive capability of the model. The model's predictions indicate favorable agreement with the experimentally measured pressure histories. Small deviations are observed for the median fill level cases where it is suggested that a non-uniform heat load may be the source of this discrepancy. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Barsi, S.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
Natl Ctr Space Explorat Res, Cleveland, OH USA.
RP Barsi, S (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,Mail Stop 110-3, Cleveland, OH 44135 USA.
EM Stephen.J.Barsi@nasa.gov
NR 29
TC 12
Z9 16
U1 0
U2 9
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0011-2275
J9 CRYOGENICS
JI Cryogenics
PD MAR-APR
PY 2008
VL 48
IS 3-4
BP 122
EP 129
DI 10.1016/j.cryogenics.2008.01.003
PG 8
WC Thermodynamics; Physics, Applied
SC Thermodynamics; Physics
GA 317UY
UT WOS:000257046900005
ER
PT J
AU Welch, RB
Sampanes, AC
AF Welch, Robert. B.
Sampanes, Anthony. C.
TI Adapting to virtual environments: Visual-motor skill acquisition versus
perceptual recalibration
SO DISPLAYS
LA English
DT Article
DE virtual environments; adaptation; intersensory conflicts; sensory-motor
conflicts
ID PRISM ADAPTATION
AB Virtual environment (VE) technology exposes users to a variety of intersensory and sensory-motor discordances to which they must adapt for optimal performance. Our research has distinguished two types of adaptation: Visual-inotor skill acquisition and perceptual recalibration. The first involves learning a new way to coordinate hand and eye, while the second is an automatic, restricted process of perceptual learning. We conclude that an understanding of the controlling conditions and defining characteristics of these two adaptive mechanisms allows one to predict which is the more likely to occur with a given VE and how best to train its users. (c) 2007 Elsevier B.V. All rights reserved.
C1 [Welch, Robert. B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Sampanes, Anthony. C.] Univ Calif Santa Cruz, Dept Psychol, Santa Cruz, CA 95064 USA.
RP Welch, RB (reprint author), NASA, Ames Res Ctr, Mail Stop 262-2, Moffett Field, CA 94035 USA.
EM Robert.B.Welch@nasa.gov; acsampanes@yahoo.com
NR 21
TC 3
Z9 3
U1 1
U2 6
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0141-9382
J9 DISPLAYS
JI Displays
PD MAR
PY 2008
VL 29
IS 2
BP 152
EP 158
DI 10.1016/j.displa.2007.09.013
PG 7
WC Computer Science, Hardware & Architecture; Engineering, Electrical &
Electronic; Instruments & Instrumentation; Optics
SC Computer Science; Engineering; Instruments & Instrumentation; Optics
GA 259BB
UT WOS:000252913000013
ER
PT J
AU Cassady, RJ
Frisbee, RH
Gilland, JH
Houts, MG
LaPointe, MR
Maresse-Reading, CM
Oleson, SR
Polk, JE
Russell, D
Sengupta, A
AF Cassady, R. Joseph
Frisbee, Robert H.
Gilland, James H.
Houts, Michael G.
LaPointe, Michael R.
Maresse-Reading, Colleen M.
Oleson, Steven R.
Polk, James E.
Russell, Derrek
Sengupta, Anita
TI Recent advances in nuclear powered electric propulsion for space
exploration
SO ENERGY CONVERSION AND MANAGEMENT
LA English
DT Article
DE space propulsion; electric propulsion; electrostatic; electromagnetic;
plasma; nuclear
ID MAGNETOPLASMADYNAMIC THRUSTER
AB Nuclear and radioisotope powered electric thrusters are being developed as primary in space propulsion systems for potential future robotic and piloted space missions. Possible applications for high-power nuclear electric propulsion include orbit raising and maneuvering of large space platforms, lunar and Mars cargo transport, asteroid rendezvous and sample return, and robotic and piloted planetary missions, while lower power radioisotope electric propulsion could significantly enhance or enable some future robotic deep space science missions. This paper provides an overview of recent US high-power electric thruster research programs, describing the operating principles, challenges, and status of each technology. Mission analysis is presented that compares the benefits and performance of each thruster type for high priority NASA missions. The status of space nuclear power systems for high-power electric propulsion is presented. The paper concludes with a discussion of power and thruster development strategies for future radioisotope electric propulsion systems. (c) 2007 Elsevier Ltd. All rights reserved.
C1 [Houts, Michael G.; LaPointe, Michael R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Cassady, R. Joseph] Aerojet Corp, Redmond, WA USA.
[Frisbee, Robert H.; Maresse-Reading, Colleen M.; Polk, James E.; Sengupta, Anita] Jet Propuls Lab, Pasadena, CA USA.
[Gilland, James H.] Ohio Aerosp Inst, Cleveland, OH USA.
[Oleson, Steven R.] NASA, Glenn Res Ctr, Cleveland, OH USA.
[Russell, Derrek] Northrop Grumman Space Technol, Redondo Beach, CA USA.
RP LaPointe, MR (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM michael.r.lapointe@nasa.gov
NR 89
TC 6
Z9 8
U1 0
U2 12
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0196-8904
J9 ENERG CONVERS MANAGE
JI Energy Conv. Manag.
PD MAR
PY 2008
VL 49
IS 3
BP 412
EP 435
DI 10.1016/j.enconman.2007.10.015
PG 24
WC Thermodynamics; Energy & Fuels; Mechanics
SC Thermodynamics; Energy & Fuels; Mechanics
GA 269SP
UT WOS:000253670800005
ER
PT J
AU Silk, EA
Golliher, EL
Selvam, RP
AF Silk, Eric A.
Golliher, Eric L.
Selvam, R. Paneer
TI Spray cooling heat transfer: Technology overview and assessment of
future challenges for micro-gravity application
SO ENERGY CONVERSION AND MANAGEMENT
LA English
DT Article
DE spray cooling; heat transfer; micro-gravity; technology development
ID MULTIPLE-NOZZLE ARRAYS; DROPLET IMPACT; SINGLE-NOZZLE; FLUX CORRELATION;
SURFACE; FC-72; FREON-113; MODELS; WATER; FILM
AB Advanced on-board flight systems for future NASA space exploration programs consist of components such as laser-diode arrays (LDA's) and multi-chip modules (MCM's). Thermal management of these systems require high heat flux cooling capability (>= 100 W/ cm 2), tight temperature control (approx. +/- 2 degrees C), reliable start-up (on demand) and long term stability. Traditional multiphase thermal control technologies for space flight (e.g., loop heat pipes, capillary pumped loops, etc.) satisfy the temperature control, start-up and stability requirements, but their heat flux removal capabilities are limited. Spray cooling can provide high heat fluxes in excess of 100 W/cm(2) using fluorinerts and over 1000 W/cm(2) with water while allowing tight temperature control at low coolant fluid flow rates. Spray cooling has been flight proven in an open loop configuration through the Space shuttle's flash evaporator system (FES). However, several closed system issues require investigation to further advance the technology to a technology readiness level (TRL) appropriate for closed system space flight application. This paper provides a discussion of the current status of spray cooling technology as well as NASA's goals, current direction, and challenges associated with the implementation and practice of this technology in the micro-gravity environment. Published by Elsevier Ltd.
C1 [Silk, Eric A.] NASA, Goddard Space Flight Ctr, Thermal Engn Technol Dev Grp, Greenbelt, MD 20771 USA.
[Golliher, Eric L.] NASA, Glenn Res Ctr, Fluid Phys & Transport Branch, Cleveland, OH 44135 USA.
[Selvam, R. Paneer] Univ Arkansas, Power Elect Leveling Solut LLC, Fayetteville, AR 72701 USA.
[Selvam, R. Paneer] Univ Arkansas, Computat Mech Lab, Fayetteville, AR 72701 USA.
RP Silk, EA (reprint author), NASA, Goddard Space Flight Ctr, Thermal Engn Technol Dev Grp, Greenbelt, MD 20771 USA.
EM Eric.A.Silk@nasa.gov; rps@uark.edu
RI selvam, Rathinam/H-7849-2013
NR 57
TC 45
Z9 55
U1 6
U2 27
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0196-8904
J9 ENERG CONVERS MANAGE
JI Energy Conv. Manag.
PD MAR
PY 2008
VL 49
IS 3
BP 453
EP 468
DI 10.1016/j.enconman.2007.07.046
PG 16
WC Thermodynamics; Energy & Fuels; Mechanics
SC Thermodynamics; Energy & Fuels; Mechanics
GA 269SP
UT WOS:000253670800007
ER
PT J
AU Dyson, RW
Geng, SM
Tew, RC
Adelino, M
AF Dyson, Rodger W.
Geng, Steven M.
Tew, Roy C.
Adelino, Miguel
TI TOWARDS FULLY THREE-DIMENSIONAL VIRTUAL STIRLING CONVERTORS FOR
MULTI-PHYSICS ANALYSIS AND OPTIMIZATION
SO ENGINEERING APPLICATIONS OF COMPUTATIONAL FLUID MECHANICS
LA English
DT Article
DE computational simulation space power
AB The desire for fast, low-cost, and reliable Stirling convertor design decisions has motivated the development of a comprehensive in-house Stirling analysis capability. One of the predominant goals of this project is to enhance the Stirling industry's suite of design tools beyond the currently employed one-dimensional analysis to the level of a virtual three-dimensional full fidelity convertor including structural, mechanical, electromagnetic, and thermal dynamics. This virtual Stirling engine/linear alternator coupling can be used to pre-test prototype hardware, examine internal part performance, and investigate design modifications before expensive convertors are fabricated. An approach is presented for incorporating the complete three-dimensional geometry of modern Stirling convertors and coupling this with multi-physics capability to examine the effects of magnetic, pressure, gravity, spring, and inertial forces on startup behavior, material creep, and overall system performance/efficiency/reliability.
C1 [Dyson, Rodger W.; Geng, Steven M.; Tew, Roy C.; Adelino, Miguel] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Dyson, RW (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM rodger.w.dyson@nasa.gov
FU Science Mission Directorate (SMD); Radioisotope Power System (RPS)
Program
FX We would like to thank Dr. Kumud Ajmani, Dr. Jim Heldman, Dr. Vijay Garg
(late), and Dr. Isaac Lopez for their suggestions and guidance
concerning high performance computing and simulation. The work described
in this paper was performed for the Science Mission Directorate (SMD)
and the Radioisotope Power System (RPS) Program, which provided funding
for this project. Any opinions, findings, and conclusions or
recommendations expressed in this report are those of the authors and do
not necessarily reflect the views of the National Aeronautics and Space
Administration.
NR 53
TC 2
Z9 2
U1 1
U2 3
PU HONG KONG POLYTECHNIC UNIV, DEPT CIVIL & STRUCTURAL ENG
PI HONG KONG
PA HUNG HOM, KOWLOON, HONG KONG, 00000, PEOPLES R CHINA
SN 1994-2060
J9 ENG APPL COMP FLUID
JI Eng. Appl. Comp. Fluid Mech.
PD MAR
PY 2008
VL 2
IS 1
BP 95
EP 118
PG 24
WC Engineering, Multidisciplinary; Engineering, Mechanical; Mechanics
SC Engineering; Mechanics
GA V11JC
UT WOS:000207526900009
ER
PT J
AU Kandula, M
Nallasamy, R
Schallhorn, P
Duncil, L
AF Kandula, M.
Nallasamy, R.
Schallhorn, P.
Duncil, L.
TI AN APPLICATION OF OVERSET GRIDS TO PAYLOAD/FAIRING THREE-DIMENSIONAL
INTERNAL FLOW CFD ANALYSIS
SO ENGINEERING APPLICATIONS OF COMPUTATIONAL FLUID MECHANICS
LA English
DT Article
DE chimera overset grids; payload/fairing; turbulence models; Navier-Stokes
solutions; internal flow
AB The application of overset grids to the computational fluid dynamics analysis of three-dimensional internal flow in the payload/fairing of an expendable launch vehicle is described. In conjunction with the overset grid system, the flowfield in the payload/fairing configuration is obtained with the aid of OVERFLOW Navier-Stokes code. The solution exhibits a highly three-dimensional complex flowfield with swirl, separation, and vortices. Some of the computed flow features are compared with the measured Laser-Doppler Velocimetry (LDV) data on a 1/5th scale model of the payload/fairing configuration. The counter-rotating vortex structures and the location of the saddle point predicted by the CFD analysis are in general agreement with the LDV data. Comparisons of the computed (CFD) velocity profiles on horizontal and vertical lines in the LDV measurement plane in the faring nose region show reasonable agreement with the LDV data.
C1 [Kandula, M.; Nallasamy, R.] ASRC, Kennedy Space Ctr, FL 32899 USA.
[Schallhorn, P.; Duncil, L.] NASA, Kennedy Space Ctr, FL 32899 USA.
RP Kandula, M (reprint author), ASRC, Kennedy Space Ctr, FL 32899 USA.
EM Max.Kandula-1@nasa.gov
FU Kennedy Space Center
FX This work was supported by the Launch Services Program (LSP) at Kennedy
Space Center.
NR 18
TC 1
Z9 1
U1 0
U2 1
PU HONG KONG POLYTECHNIC UNIV, DEPT CIVIL & STRUCTURAL ENG
PI HONG KONG
PA HUNG HOM, KOWLOON, HONG KONG, 00000, PEOPLES R CHINA
SN 1994-2060
J9 ENG APPL COMP FLUID
JI Eng. Appl. Comp. Fluid Mech.
PD MAR
PY 2008
VL 2
IS 1
BP 119
EP 129
PG 11
WC Engineering, Multidisciplinary; Engineering, Mechanical; Mechanics
SC Engineering; Mechanics
GA V11JC
UT WOS:000207526900010
ER
PT J
AU Liao, K
Walker, MF
Joshi, A
Reschke, M
Leigh, RJ
AF Liao, Ke
Walker, Mark F.
Joshi, Anand
Reschke, Millard
Leigh, R. John
TI Vestibulo-ocular responses to vertical translation in normal human
subjects
SO EXPERIMENTAL BRAIN RESEARCH
LA English
DT Article
DE vestibulo-ocular reflex; locomotion; moving platform
ID EYE-MOVEMENTS; LISTINGS LAW; FIXATION DISTANCE; OCULAR RESPONSES;
VIEWING DISTANCE; PRIMARY POSITION; SQUIRREL-MONKEY; TARGET DISTANCE;
LINEAR MOTION; HEAD
AB Prior studies of the human translational vestibulo-ocular reflex (tVOR) report that eye rotations amount to less than 60% of those required to keep the eyes pointed at a stationary visual target, unlike the angular VOR (aVOR) which is optimized to maintain stable gaze. Our first goal was to determine if the performance of the tVOR improves when head translations are combined with head rotations in ambient lighting. A second goal was to measure tVOR during vertical head translations (bob), which has not received systematic study. We measured tVOR alone and in combination with the aVOR in 20 normal human subjects, aged 25-72 years, as they sat on a moving platform that bobbed at 2.0 Hz while rotating horizontally (yaw) at 1.0 Hz. When subjects viewed a visual target at 2 m, median "compensation gain" (eye rotational velocity/required eye rotational velocity to maintain foveal target fixation) was 0.52 during pure bob and 0.59 during combined bob-yaw; during viewing of a near target at similar to 17 cm, compensation gain was 0.58 for pure bob and 0.60 for combined bob-yaw. Mean phase lag of eye-in-head velocity for the tVOR was similar to 19 degrees with respect to the ideal compensatory response, irrespective of whether translation was accompanied by rotation. Thus, the tVOR changed only slightly during translation-rotation versus pure translation, and our subjects' ocular rotations remained at about 60% of those required to point the eyes at the target. Comparison of response during binocular or monocular viewing, and ambient or reduced illumination, indicated that relative image motion between the target and background was an important determinant of tVOR behavior. We postulate that tVOR evolved not to stabilize the image of the target on the fovea, but rather to minimize retinal image motion between objects lying in different planes, in order to optimize motion parallax information.
C1 [Walker, Mark F.; Leigh, R. John] Case Western Reserve Univ, Vet Affairs Med Ctr, Dept Neurol, Cleveland, OH 44106 USA.
[Liao, Ke; Walker, Mark F.; Joshi, Anand; Leigh, R. John] Case Western Reserve Univ, Univ Hosp, Cleveland, OH 44106 USA.
[Liao, Ke; Joshi, Anand; Leigh, R. John] Case Western Reserve Univ, Vet Affairs Med Ctr, Dept Biomed Engn, Cleveland, OH 44106 USA.
[Reschke, Millard] Johnson Space Ctr, Neurosci Labs, Houston, TX USA.
RP Leigh, RJ (reprint author), Case Western Reserve Univ, Vet Affairs Med Ctr, Dept Neurol, 11100 Euclid Ave, Cleveland, OH 44106 USA.
EM rjl4@case.edu
RI liao, ke/B-1453-2010
FU NEI NIH HHS [EY06717, R01 EY006717, R01 EY006717-23]
NR 38
TC 26
Z9 26
U1 0
U2 6
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013 USA
SN 0014-4819
J9 EXP BRAIN RES
JI Exp. Brain Res.
PD MAR
PY 2008
VL 185
IS 4
BP 553
EP 562
DI 10.1007/s00221-007-1181-z
PG 10
WC Neurosciences
SC Neurosciences & Neurology
GA 265LG
UT WOS:000253359800003
PM 17989972
ER
PT J
AU Encinas, JM
Vazquez, ME
Switzer, RC
Chamberland, DW
Nick, H
Levine, HG
Scarpa, PJ
Enikolopov, G
Steindler, DA
AF Encinas, Juan M.
Vazquez, Marcelo E.
Switzer, Robert C.
Chamberland, Dennis W.
Nick, Harry
Levine, Howard G.
Scarpa, Philip J.
Enikolopov, Grigori
Steindler, Dennis A.
TI Quiescent adult neural stem cells are exceptionally sensitive to cosmic
radiation
SO EXPERIMENTAL NEUROLOGY
LA English
DT Article
ID CENTRAL-NERVOUS-SYSTEM; HIPPOCAMPAL NEUROGENESIS; CONFOCAL MICROSCOPY;
IRRADIATION; BRAIN; STEREOLOGY; MARKERS; VITRO
AB Generation of new neurons in the adult brain, a process that is likely to be essential for learning, memory, and mood regulation, is impaired by radiation. Therefore, radiation exposure might have not only such previously expected consequences as increased probability of developing cancer, but might also impair cognitive function and emotional stability. Radiation exposure is encountered in settings ranging from cancer therapy to space travel; evaluating the neurogenic risks of radiation requires identifying the at-risk populations of stem and progenitor cells in the adult brain. Here we have used a novel reporter mouse line to find that early neural progenitors are selectively affected by conditions simulating the space radiation environment. This is reflected both in a decrease in the number of these progenitors in the neurogenic regions and in an increase in the number of dying cells in these regions. Unexpectedly, we found that quiescent neural stem cells, rather than their rapidly dividing progeny, are most sensitive to radiation. Since these stem cells are responsible for adult neurogenesis, their death would have a profound impact on the production of new neurons in the irradiated adult brain. Our finding raises an important concern about cognitive and emotional risks associated with radiation exposure. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Encinas, Juan M.; Enikolopov, Grigori] Cold Spring Harbor Lab, Cold Spring Harbor, NY 11724 USA.
[Vazquez, Marcelo E.] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Chamberland, Dennis W.; Levine, Howard G.; Scarpa, Philip J.] NASA, Kennedy Space Ctr, FL USA.
[Nick, Harry; Steindler, Dennis A.] Univ Florida, McKnight Brain Inst, Gainesville, FL 32611 USA.
RP Enikolopov, G (reprint author), Cold Spring Harbor Lab, 1 Bungtown Rd, Cold Spring Harbor, NY 11724 USA.
EM enik@cshl.edu
RI Enikolopov, Grigori/B-7771-2009; Encinas, Juan/E-3625-2010;
OI Enikolopov, Grigori/0000-0001-8178-8917; Encinas, Juan
Manuel/0000-0002-0402-972X
FU NHLBI NIH HHS [HL 70143]; NIMH NIH HHS [R21 MH081258, R21 MH081258-01];
NINDS NIH HHS [R01 NS037556, NS 37556]
NR 24
TC 20
Z9 21
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 0014-4886
J9 EXP NEUROL
JI Exp. Neurol.
PD MAR
PY 2008
VL 210
IS 1
BP 274
EP 279
DI 10.1016/j.expneurol.2007.10.021
PG 6
WC Neurosciences
SC Neurosciences & Neurology
GA 270WV
UT WOS:000253751800029
PM 18076878
ER
PT J
AU Grant, JA
Irwin, RP
Grotzinger, JP
Milliken, RE
Tornabene, LL
McEwen, AS
Weitz, CM
Squyres, SW
Glotch, TD
Thomson, BJ
AF Grant, John A.
Irwin, Rossman P., III
Grotzinger, John P.
Milliken, Ralph E.
Tornabene, Livio L.
McEwen, Alfred S.
Weitz, Catherine M.
Squyres, Steven W.
Glotch, Timothy D.
Thomson, Brad J.
TI HiRISE imaging of impact megabreccia and sub-meter aqueous strata in
Holden Crater, Mars
SO GEOLOGY
LA English
DT Article
DE Mars; stratigraphy; aqueous; megabreccia
ID EVOLUTION
AB High Resolution Imaging Science Experiment (HiRISE) images of Holden crater, Mars, resolve impact megabreccia unconformably overlain by sediments deposited during two Noachian-age phases of aqueous activity. A lighter-toned lower unit exhibiting phyllosilicates was deposited in a long-lived, quiescent distal alluvial or lacustrine setting. An overlying darker-toned and often blocky upper unit drapes the sequence and was emplaced during later high-magnitude flooding as an impounded Uzboi Vallis lake overtopped the crater rim. The stratigraphy provides the first geologic context for phyllosilicate deposition during persistent wet and perhaps habitable conditions on early Mars.
C1 [Grant, John A.; Irwin, Rossman P., III] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
[Grotzinger, John P.; Milliken, Ralph E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Tornabene, Livio L.; McEwen, Alfred S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Weitz, Catherine M.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Squyres, Steven W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Glotch, Timothy D.; Thomson, Brad J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Grant, JA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
RI Glotch, Timothy/B-6829-2008;
OI Thomson, Bradley/0000-0001-8635-8932
NR 21
TC 71
Z9 71
U1 0
U2 7
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0091-7613
EI 1943-2682
J9 GEOLOGY
JI Geology
PD MAR
PY 2008
VL 36
IS 3
BP 195
EP 198
DI 10.1130/G24340A.1
PG 4
WC Geology
SC Geology
GA 270WN
UT WOS:000253751000001
ER
PT J
AU Pumphrey, HC
Boone, C
Walker, KA
Bernath, P
Livesey, NJ
AF Pumphrey, H. C.
Boone, C.
Walker, K. A.
Bernath, P.
Livesey, N. J.
TI Tropical tape recorder observed in HCN
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ATMOSPHERIC CHEMISTRY; HYDROGEN-CYANIDE; MLS
AB The tropical tape recorder is an effect in which a seasonal cycle in the mixing ratio of a gas is imposed on air entering the stratosphere and is then transported upwards by the Brewer-Dobson circulation. We report the observation of this effect in the mixing ratio of HCN, as measured by two satellite instruments: MLS on Aura and ACE-FTS on SCISAT-1. The cycle does not repeat every year; the data so far suggest that the dominant period is about two years. The reason for this periodicity is not yet fully understood. Comparisons with MODIS fire-count data suggest that it may be connected to inter-annual variations in biomass burning in Indonesia and the surrounding region.
C1 [Pumphrey, H. C.] Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland.
[Boone, C.; Walker, K. A.; Bernath, P.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada.
[Livesey, N. J.] NASA, Jet Propuls Lab, Pasadena, CA USA.
RP Pumphrey, HC (reprint author), Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland.
EM pfb500@york.ac.uk
RI Bernath, Peter/B-6567-2012
OI Bernath, Peter/0000-0002-1255-396X
NR 18
TC 21
Z9 21
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 1
PY 2008
VL 35
IS 5
AR L05801
DI 10.1029/2007GL032137
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 270IW
UT WOS:000253715500002
ER
PT J
AU Xie, H
Gopalswamy, N
Cyr, OCS
Yashiro, S
AF Xie, H.
Gopalswamy, N.
Cyr, O. C. St.
Yashiro, S.
TI Effects of solar wind dynamic pressure and preconditioning on large
geomagnetic storms
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID TRANSPOLAR POTENTIAL SATURATION; ART. NO. 1341; RING CURRENT;
ENERGY-TRANSFER; RAM PRESSURE; DST; INJECTION; DECAY; MODEL
AB We investigate the effects of solar wind dynamic pressure, P(dyn), and preconditioning in 88 large magnetic storms (Dst < -100 nT) occurring during solar cycle 23. We have developed an improved model of the Dst profile, based on a modified Burton equation, where additional effects of Pdyn and diminished Dst pressure-correction have been taking into account. On the average, our model predicts the Dst peak values within 9% of observations and gives an overall RMS error of 11%, which is an improvement over those models whose injection functions only depend on the solar wind electric field. The results demonstrate that there is an increase in the Dst peak value when there is a large enhancement of Pdyn during the main phase of a storm. The average increase of the storm intensity is estimated to be 26% for 15 storms with the max (P(dyn)) > 15 nPa. We find that the preconditioning in multi-step Dst storms plays no significant role in strengthening the storm intensity, but increases the storm duration.
C1 [Xie, H.; Yashiro, S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Gopalswamy, N.; Cyr, O. C. St.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Xie, H (reprint author), Catholic Univ Amer, Dept Phys, 200 Hannan Hall, Washington, DC 20064 USA.
EM hong.xie@ssedmail.gsfc.nasa.gov
RI Gopalswamy, Nat/D-3659-2012;
OI Gopalswamy, Nat/0000-0001-5894-9954
NR 21
TC 12
Z9 13
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 1
PY 2008
VL 35
IS 6
AR L06S08
DI 10.1029/2007GL032298
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 270IX
UT WOS:000253715600001
ER
PT J
AU Chaloupka, M
Bjorndal, KA
Balazs, GH
Bolten, AB
Ehrhart, LM
Limpus, CJ
Suganuma, H
Troeeng, S
Yamaguchi, M
AF Chaloupka, Milani
Bjorndal, Karen A.
Balazs, George H.
Bolten, Alan B.
Ehrhart, Llewellyn M.
Limpus, Colin J.
Suganuma, Hiroyuki
Troeeng, Sebastian
Yamaguchi, Manami
TI Encouraging outlook for recovery of a once severely exploited marine
megaherbivore
SO GLOBAL ECOLOGY AND BIOGEOGRAPHY
LA English
DT Article
DE Chelonia mydas; conservation; green sea turtle; marine; stock recovery
ID TURTLES CHELONIA-MYDAS; SOMATIC GROWTH DYNAMICS; GREEN TURTLE;
SEA-TURTLES; COSTA-RICA; SURVIVAL PROBABILITY; POPULATION; DECLINE;
TRENDS; CONSERVATION
AB Aim To critically review the status of the green sea turtle (Chelonia mydas) using the best available scientific studies as there is a prevailing view that this species is globally endangered and its marine ecosystem functions compromised.
Location Ogasawara (Japan), Hawaii (USA), Great Barrier Reef (Australia), Florida (USA), Tortuguero (Costa Rica).
Methods We compiled seasonal nesting activity data from all reliable continuous long-term studies (> 25 years), which comprised data series for six of the world's major green turtle rookeries. We estimated the underlying time-specific trend in these six rookery-specific nester or nest abundance series using a generalized smoothing spline regression approach.
Results Estimated rates of nesting population increase ranged from c. 4-14% per annum over the past two to three decades. These rates varied considerably among the rookeries, reflecting the level of historical exploitation. Similar increases in nesting population were also evident for many other green turtle stocks that have been monitored for shorter durations than the long-term studies presented here.
Main conclusions We show that six of the major green turtle nesting populations in the world have been increasing over the past two to three decades following protection from human hazards such as exploitation of eggs and turtles. This population recovery or rebound capacity is encouraging and suggests that the green turtle is not on the brink of global extinction even though some stocks have been seriously depleted and are still below historical abundance levels. This demonstrates that relatively simple conservation strategies can have a profound effect on the recovery of once-depleted green turtle stocks and presumably the restoration of their ecological function as major marine consumers.
C1 [Chaloupka, Milani] Univ Queensland, Ecol Modelling Serv Pty Ltd, St Lucia, Qld 4067, Australia.
[Bjorndal, Karen A.; Bolten, Alan B.] Univ Florida, Ctr Sea Turtle Res, Dept Zool, Gainesville, FL 32611 USA.
[Balazs, George H.] Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96822 USA.
[Ehrhart, Llewellyn M.] Univ Cent Florida, Dept Biol, Orlando, FL 32816 USA.
[Ehrhart, Llewellyn M.] Hubbs Sea World Res Inst, Melbourne, FL 32951 USA.
[Limpus, Colin J.] Environm Protect Agcy, Queensland Pk & Wildlife Serv, City E, Qld 4002, Australia.
[Suganuma, Hiroyuki] Everlasting Nat Asia, Kanagawa Ku, Yokohama, Kanagawa 2210822, Japan.
[Troeeng, Sebastian] Carribbean Conservat Corp, San Pedro, Costa Rica.
[Troeeng, Sebastian] Lund Univ, Dept Anim Ecol, S-22362 Lund, Sweden.
[Yamaguchi, Manami] Ogasawara Marine Ctr, Ogasawara, Tokyo 1002101, Japan.
RP Chaloupka, M (reprint author), Univ Queensland, Ecol Modelling Serv Pty Ltd, PO Box 6150, St Lucia, Qld 4067, Australia.
EM m.chaloupka@uq.edu.au
OI Bjorndal, Karen/0000-0002-6286-1901
NR 61
TC 86
Z9 91
U1 5
U2 35
PU BLACKWELL PUBLISHING
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND
SN 1466-822X
J9 GLOBAL ECOL BIOGEOGR
JI Glob. Ecol. Biogeogr.
PD MAR
PY 2008
VL 17
IS 2
BP 297
EP 304
DI 10.1111/j.1466-8238.2007.00367.x
PG 8
WC Ecology; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA 259UI
UT WOS:000252966000015
ER
PT J
AU Hood, ED
Major, DW
Quinn, JW
Yoon, WS
Gavaskar, A
Edwards, EA
AF Hood, E. D.
Major, D. W.
Quinn, J. W.
Yoon, W. -S.
Gavaskar, A.
Edwards, E. A.
TI Demonstration of enhanced bioremediation in a TCE source area at Launch
Complex 34, Cape Canaveral Air Force Station
SO GROUND WATER MONITORING AND REMEDIATION
LA English
DT Article
ID DEHALOCOCCOIDES SP STRAIN; VINYL-CHLORIDE REDUCTASE; CHLOROETHENE
BIODEGRADATION; TETRACHLOROETHENE DNAPL; METHANOGENIC CONDITIONS; FIELD
DEMONSTRATION; CIS-DICHLOROETHENE; DECHLORINATION; ETHENE;
TRICHLOROETHENE
AB The ability of bioremediation to treat a source area containing trichloroethene (TCE) present as dense nonaqueous phase liquid (DNAPL) was assessed through a laboratory study and a pilot test at Launch Complex 34, Cape Canaveral Air Force Center. The results of microcosm testing indicate that the indigenous microbial community was capable of dechlorinating TCE to ethene if amended with electron donor; however, bioaugmentation with a dechlorinating culture (KB-1; SiREM, Guelph, Ontario, Canada) significantly increased the rate of ethene formation. In microcosms, the activity of the dechlorinating organisms in KB-1 was not inhibited at initial TCE concentrations as high as 2 mM. The initially high TCE concentration in ground water (1.2 mM or 155 mg/L) did not inhibit reductive dechlorination, and at the end of the study, the average concentration of ethene (2.4 mM or 67 mg/L) was in stoichiometric excess of this initial TCE concentration. The production of ethene in stoichiometric excess in comparison to the initial TCE concentration indicates that the bioremediation treatment enhanced the removal of TCE mass (either sorbed to soil or present as DNAPL). Detailed soil sampling indicated that the bioremediation treatment removed greater than 98.5% of the initial TCE mass. Confirmatory ground water samples collected 22 months after the bioremediation treatment indicated that chloroethene concentrations had continued to decline in the absence of further electron donor addition. The results of this study confirm that dechlorination to ethene can proceed at the high TCE concentrations often encountered in source areas and that bioremediation was capable of removing significant TCE mass from the test plot, suggesting that enhanced bioremediation is a potentially viable remediation technology for TCE source areas. Dehalococcoides abundance increased by 2 orders of magnitude following biostimulation and bioaugmentation.
C1 [Hood, E. D.; Major, D. W.] Geosyntec Consultants Inc, Guelph, ON N1G 5G3, Canada.
[Quinn, J. W.] NASA, Kennedy Space Ctr, FL 32899 USA.
[Yoon, W. -S.; Gavaskar, A.] Battelle Mem Inst, Environm Restorat Sect, Columbus, OH 43201 USA.
[Edwards, E. A.] Univ Toronto, Dept Chem Engn & Appl Chem, Toronto, ON M5S 3E5, Canada.
RP Hood, ED (reprint author), Geosyntec Consultants Inc, 130 Res Lane,Suite 2, Guelph, ON N1G 5G3, Canada.
EM ehood@geosyntec.com
OI Edwards, Elizabeth/0000-0002-8071-338X
NR 37
TC 22
Z9 27
U1 3
U2 20
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1069-3629
J9 GROUND WATER MONIT R
JI Ground Water Monit. Remediat.
PD SPR
PY 2008
VL 28
IS 2
BP 98
EP 107
DI 10.1111/j.1745-6592.2008.00197.x
PG 10
WC Water Resources
SC Water Resources
GA 304OO
UT WOS:000256119000008
ER
PT J
AU Lobascio, C
Briccarello, M
Destefanis, R
Faraud, M
Gialanella, G
Grossi, G
Guarnieri, V
Manti, L
Pugliese, M
Rusek, A
Scampoli, P
Durante, M
AF Lobascio, C.
Briccarello, M.
Destefanis, R.
Faraud, M.
Gialanella, G.
Grossi, G.
Guarnieri, V.
Manti, L.
Pugliese, M.
Rusek, A.
Scampoli, P.
Durante, M.
TI Accelerator-based tests of radiation shielding properties of materials
used in human space infrastructures
SO HEALTH PHYSICS
LA English
DT Article
DE accelerators; carcinogenesis; chromosomal aberration; shielding
ID GALACTIC COSMIC-RAYS; EXPOSURE; EXPLORATION; PROTECTION; METAPHASE;
MISSIONS; STATION; FE-56
AB Shielding is the only practical countermeasure for the exposure to cosmic radiation during space travel. It is well known that light, hydrogenated materials, such as water and polyethylene, provide the best shielding against space radiation. Kevlar and Nextel are two materials of great interest for spacecraft shielding because of their known ability to protect human space infrastructures from meteoroids and debris. We measured the response to simulated heavy-ion cosmic radiation of these shielding materials and compared it to polyethylene, Lucite (PMMA), and aluminum. As proxy to galactic nuclei we used 1 GeV n(-1) iron or titanium ions. Both physics and biology tests were performed. The results show that Kevlar, which is rich in carbon atoms (about 50% in number), is an excellent space radiation shielding material. Physics tests show that its effectiveness is close (80-90%) to that of polyethylene, and biology data suggest that it can reduce the chromosomal damage more efficiently than PMMA. Nextel is less efficient as a radiation shield, and the expected reduction on dose is roughly half that provided by the same mass of polyethylene. Both Kevlar and Nextel are more effective than aluminum in the attenuation of heavy-ion dose.
C1 [Gialanella, G.; Grossi, G.; Manti, L.; Pugliese, M.; Scampoli, P.; Durante, M.] Univ Federico II, Dept Phys & INFN, I-80126 Naples, Italy.
[Rusek, A.] Brookhaven Natl Lab, NASA, Space Radiat Lab, Upton, NY 11973 USA.
RP Durante, M (reprint author), Univ Federico II, Dipartimento Sci Fis, Via Cintia, I-80126 Naples, Italy.
EM Marco.Durante@na.infn.it
RI Durante, Marco/K-1315-2014;
OI Durante, Marco/0000-0002-4615-553X
NR 28
TC 18
Z9 18
U1 1
U2 11
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA
SN 0017-9078
EI 1538-5159
J9 HEALTH PHYS
JI Health Phys.
PD MAR
PY 2008
VL 94
IS 3
BP 242
EP 247
PG 6
WC Environmental Sciences; Public, Environmental & Occupational Health;
Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical
Imaging
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Nuclear Science & Technology; Radiology, Nuclear Medicine &
Medical Imaging
GA 263XN
UT WOS:000253249900003
PM 18301097
ER
PT J
AU Kraal, ER
Asphaug, E
Moore, JM
Howard, A
Bredt, A
AF Kraal, Erin R.
Asphaug, Erik
Moore, Jeffery M.
Howard, Alan
Bredt, Adam
TI Catalogue of large alluvial fans in martian impact craters
SO ICARUS
LA English
DT Article
DE Mars; surface; geological processes; Mars; climate
ID SEDIMENTARY PROCESSES; LASER ALTIMETER; MARS; LAKES; SYSTEM; FLOW
AB We conducted a systematic, global survey using Thermal Emission Imaging System Infrared (THEMIS IR) coverage (similar to 100 m/pixel) to search for large alluvial fans in impact craters on Mars. Our survey has focused on large fans (apron areas greater than similar to 40 km(2), usually located in craters greater than 20 km in diameter) due to the resolution of the THEMIS images and Mars Orbiter Laser Altimeter (MOLA) coverage. We find that the host craters are found to have a distinctive diameter range from 30-150 km. The fans generally cluster in three geographic areas - southern Margaritifer Terra, southwestern Terra Sabaea, and southwestern Tyrrhena Terra, however several outliers do exist. The alluvial fans do not form in a particular orientation along the crater rim nor are they associated with the location of current high rim topography. Fan area magnitude and variability increase with crater diameter while fan concavity magnitude and variability increase with decreasing crater diameter. Smaller fan aprons in general have higher, more variable concavity. The source of the water forming these fans is uncertain given the challenges of accommodating the global distribution pattern and formation patterns within the craters. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Kraal, Erin R.; Asphaug, Erik; Bredt, Adam] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
[Moore, Jeffery M.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Howard, Alan] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22903 USA.
[Kraal, Erin R.] Virginia Tech, Dept Geosci, Blacksburg, VA 24060 USA.
RP Kraal, ER (reprint author), Univ Calif Santa Cruz, Dept Earth & Planetary Sci, 1156 High St, Santa Cruz, CA 95064 USA.
EM ekraal@vt.edu
OI Howard, Alan/0000-0002-5423-1600
NR 29
TC 23
Z9 23
U1 2
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 MAR
PY 2008
VL 194
IS 1
BP 101
EP 110
DI 10.1016/j.icarus.2007.09.028
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 267JD
UT WOS:000253504400010
ER
PT J
AU Kitazato, K
Clark, BE
Abe, M
Abe, S
Takagi, Y
Hiroi, T
Arnouin-Jha, OSB
Abell, PA
Lederer, SM
Vilas, F
AF Kitazato, Kohei
Clark, Beth E.
Abe, Masanao
Abe, Shinsuke
Takagi, Yasuhiko
Hiroi, Takahiro
Arnouin-Jha, Olivier S. B.
Abell, Paul A.
Lederer, Susan M.
Vilas, Faith
TI Near-infrared spectrophotometry of Asteroid 25143 Itokawa from NIRS on
the Hayabusa spacecraft
SO ICARUS
LA English
DT Article
DE Asteroid Itokawa; photometry; spectrophotometry
ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; COHERENT BACKSCATTER; GALILEO
PHOTOMETRY; OPTICAL-CONSTANTS; SCATTERING; ROUGHNESS; PARTICLES;
433-EROS; LIGHT; MOON
AB A photometric analysis of the S-type Asteroid 25143 Itokawa is performed over multiple wavelengths ranging from 0.85 to 2.10 Pm based on disk-resolved reflectance spectra obtained with the Hayabusa near-infrared spectrometer (NIRS). We derive the global photometric properties of Itokawa in terms of Hapke's photometric model. We find that Itokawa has a single-scatter albedo that is 35-40% less than that of Asteroid 433 Eros. Itokawa also has a single-particle phase function that is more strongly back-scattering than that of Eros. Despite its hummocky surface strewn with large boulders, Itokawa exhibits an opposition effect. However, the total amplitude of the opposition surge for Itokawa was estimated to be less than unity while Eros and other S-type asteroids have been found to have model values exceeding unity. The wavelength dependence of the opposition surge width reveals that coherent backscatter contributes to the opposition effect on Itokawa's surface. The photometric roughness of Itokawa is well constrained to a value of 26 degrees +/- 1 degrees which is similar to Eros, suggesting that photometric roughness models the smallest surface roughness scale for which shadows exist. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Kitazato, Kohei; Abe, Masanao] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Kitazato, Kohei; Abe, Masanao] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan.
[Clark, Beth E.] Ithaca Coll, Dept Phys, Ithaca, NY 14850 USA.
[Abe, Shinsuke] Kobe Univ, Grad Sch Sci & Technol, Kobe, Hyogo 6518501, Japan.
[Takagi, Yasuhiko] Tohoku Gakuin Univ, Nagoya, Aichi 4658515, Japan.
[Hiroi, Takahiro] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Arnouin-Jha, Olivier S. B.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Abell, Paul A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Lederer, Susan M.] Calif State Univ San Bernardino, Dept Phys, San Bernardino, CA 92407 USA.
[Vilas, Faith] Univ Arizona, MMT Observ, Tucson, AZ 85721 USA.
RP Kitazato, K (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan.
EM kitazato@planeta.sci.isas.jaxa.jp
NR 35
TC 18
Z9 18
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 0019-1035
J9 ICARUS
JI Icarus
PD MAR
PY 2008
VL 194
IS 1
BP 137
EP 145
DI 10.1016/j.icarus.2007.08.029
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 267JD
UT WOS:000253504400013
ER
PT J
AU Gregg, TKP
Lopes, RM
AF Gregg, Tracy K. P.
Lopes, Rosaly M.
TI Lava lakes on Io: New perspectives from modeling
SO ICARUS
LA English
DT Article
DE Io; Jupiter; satellites; satellites; surfaces; volcanism; geological
processes
ID EAST PACIFIC RISE; SPREADING MIDOCEAN RIDGES; VOLCANIC-ERUPTIONS;
KILAUEA VOLCANO; FLOW-FIELD; HEAT-FLOW; GALILEO; MAGMA; HAWAII;
CONSTRAINTS
AB Loki Patera (310 degrees W, 12 degrees N) is Io's largest patera at similar to 180 kin in diameter. Its morphology and distinct thermal behavior have led researchers to hypothesize that Loki Patera may either be an active lava lake that experiences periodic overturn, or a shallow depression whose floor is episodically resurfaced with thin flows. Using results from mathematical models, we suggest that a better model for Loki's behavior is the terrestrial superfast spreading East Pacific Rise (EPR), near 17 degrees 30' south. We propose that, like at the southern EPR, Loki Patera is underlain by a thin, persistent magma "lens" that feeds thin, temporary lava lakes within the patera. Also like the southern EPR, overspilling of the volcanic depression is rare. with most of the lava volume being emplaced via a subsurface network of lava tubes. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Gregg, Tracy K. P.] SUNY Buffalo, Dept Geol, Buffalo, NY 14260 USA.
[Lopes, Rosaly M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gregg, TKP (reprint author), SUNY Buffalo, Dept Geol, 876 Nat Sci Complex, Buffalo, NY 14260 USA.
EM tgregg@geology.buffalo.edu
RI Lopes, Rosaly/D-1608-2016
OI Lopes, Rosaly/0000-0002-7928-3167
NR 55
TC 3
Z9 3
U1 1
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 MAR
PY 2008
VL 194
IS 1
BP 166
EP 172
DI 10.1016/j.icarus.2007.08.042
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 267JD
UT WOS:000253504400016
ER
PT J
AU Sekine, Y
Imanaka, H
Matsui, T
Khare, BN
Bakes, ELO
Mckay, CP
Sugita, S
AF Sekine, Yasuhito
Imanaka, Hiroshi
Matsui, Takafumi
Khare, Bishun N.
Bakes, Emma L. O.
Mckay, Christopher P.
Sugita, Seiji
TI The role of organic haze in Titan's atmospheric chemistry I. Laboratory
investigation on heterogeneous reaction of atomic hydrogen with Titan
tholin
SO ICARUS
LA English
DT Article
DE Titan; organic chemistry; satellites; atmospheres; atmospheres;
chemistry
ID CARBON-FILMS; METHYL RADICALS; AEROSOLS; ABSTRACTION; SURFACES; PLASMA;
GROWTH; MODEL; H-2
AB In Titan's atmosphere consisting of N-2 and CH4, large amounts of atomic hydrogen are produced by photochemical reactions during the formation of complex organics. This atomic hydrogen may undergo heterogeneous reactions with organic aerosol in the stratosphere and mesosphere of Titan. In order to investigate both the mechanisms and kinetics of the heterogeneous reactions, atomic deuterium is irradiated onto Titan tholin formed from N-2 and CH4 gas mixtures at various surface-temperatures of the tholin ranging from 160 to 3 10 K. The combined analyses of the as species and the exposed tholin indicate that the interaction mechanisms of atomic deuterium with the tholin are composed of three reactions; (a) abstraction of hydrogen from tholin resulting in gaseous HD formation (HD recombination), (b) addition of D atom into tholin (hydrogenation), and (c) removal of carbon and/or nitrogen (chemical erosion). The reaction probabilities of HD recombination and hydrogenation are obtained as eta(abst) = 1.9(+/- 0.6) x 10(-3) x exp(-300/T) and eta(hydro) = 2.08(+/- 0.64) x exp(- 1000/T), respectively. The chemical erosion process is very inefficient under the conditions of temperature range of Titan's stratosphere and mesosphere. Under Titan conditions, the rates of hydrogenation > HD recombination >> chemical erosion. Our measured HD recombination rate is about 10 times (with an uncertainty of a factor of 3-5) the prediction of previous theoretical model. These results imply that organic aerosol can remove atomic hydrogen efficiently from Titan's atmosphere through the heterogeneous reactions and that the presence of aerosol may affect the subsequent organic chemistry. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Sekine, Yasuhito] Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan.
[Imanaka, Hiroshi] Univ Arizona, Dept Chem, Tucson, AZ 85721 USA.
[Imanaka, Hiroshi; Khare, Bishun N.; Bakes, Emma L. O.] SETI Inst, Carl Sagan Ctr Study Life Univ, Mountain View, CA 94043 USA.
[Matsui, Takafumi; Sugita, Seiji] Univ Tokyo, Grad Sch Frontier Sci, Dept Complex Sci & Engn, Chiba 2278562, Japan.
[Khare, Bishun N.; Bakes, Emma L. O.; Mckay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Sekine, Y (reprint author), Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
EM sekine@impact.k.u-tokyo.acjp
RI Imanaka, Hiroshi/E-7816-2012
NR 34
TC 37
Z9 37
U1 0
U2 13
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 MAR
PY 2008
VL 194
IS 1
BP 186
EP 200
DI 10.1016/j.icarus.2007.08.031
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 267JD
UT WOS:000253504400018
ER
PT J
AU Sekine, Y
Lebonnois, S
Imanaka, H
Matsui, T
Bakes, ELO
Mckay, CP
Khare, BN
Sugita, S
AF Sekine, Yasuhito
Lebonnois, Sebastien
Imanaka, Hiroshi
Matsui, Takafumi
Bakes, Emma L. O.
Mckay, Christopher P.
Khare, Bishun N.
Sugita, Seiji
TI The role of organic haze in Titan's atmospheric chemistry II. Effect of
heterogeneous reaction to the hydrogen budget and chemical composition
of the atmosphere
SO ICARUS
LA English
DT Article
DE Titan; organic chemistry; satellites; atmospheres; atmospheres;
chemistry
ID POLYCYCLIC AROMATIC-HYDROCARBONS; AEROSOLS; MODEL; PHOTOCHEMISTRY;
CONSTITUENTS; SPECTROSCOPY; SENSITIVITY; DIACETYLENE; BENZENE; METHANE
AB One of the key components controlling the chemical composition and climatology of Titan's atmosphere is the removal of reactive atomic hydrogen from the atmosphere. A proposed process of the removal of atomic hydrogen is the heterogeneous reaction with organic aerosol. In this study, we investigate the effect of heterogeneous reactions in Titan's atmospheric chemistry using new measurements of the heterogeneous reaction rate [Sekine, Y., Imanaka, H., Matsui, T., Khare, B.N., Bakes, E.L.O., McKay, C.P., Sugita, S., 2008. Icarus 194, 186-200] in a one-dimensional photochemical model. Our results indicate that 60-75% of the atomic hydrogen in the stratosphere and mesosphere are consumed by the heterogeneous reactions. This result implies that the heterogeneous reactions on the aerosol surface may predominantly remove atomic hydrogen in Titan's stratosphere and mesosphere. The results of our calculation also indicate that a low concentration of atomic hydrogen enhances the concentrations of unsaturated complex organics, such as C4H2 and phenyl radical, by more than two orders in magnitude around 400 km in altitude. Such an increase in unsaturated species may induce efficient haze production in Titan's mesosphere and upper stratosphere. These results imply a positive feedback mechanism in haze production in Titan's atmosphere. The increase in haze production would affect the chemical composition of the atmosphere, which might induce further haze production. Such a positive feedback could tend to dampen the loss and supply cycles of CH4 due to an episodic CH4 release into Titan's atmosphere. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Sekine, Yasuhito] Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan.
UPMC, CNRS, Meteorol Dynam Lab, IPSL, F-75252 Paris, France.
[Imanaka, Hiroshi; Bakes, Emma L. O.] Univ Arizona, Dept Chem, Tucson, AZ 85721 USA.
[Imanaka, Hiroshi; Khare, Bishun N.] SETI Inst, Mountain View, CA 94043 USA.
[Matsui, Takafumi; Sugita, Seiji] Univ Tokyo, Grad Sch Frontier Sci, Dept Complex Sci & Engn, Chiba 2778562, Japan.
[Bakes, Emma L. O.; Mckay, Christopher P.; Khare, Bishun N.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Sekine, Y (reprint author), Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
EM sekine@impact.k.u-tokyo.ac.jp
RI Imanaka, Hiroshi/E-7816-2012
NR 47
TC 23
Z9 23
U1 0
U2 15
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR
PY 2008
VL 194
IS 1
BP 201
EP 211
DI 10.1016/j.icarus.2007.08.030
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 267JD
UT WOS:000253504400019
ER
PT J
AU McCord, TB
Hayne, P
Combe, JP
Hansen, GB
Barnes, JW
Rodriguez, S
Le Mouelic, S
Baines, EKH
Buratti, BJ
Sotin, C
Nicholson, P
Jaumann, R
Nelson, R
AF McCord, Thomas B.
Hayne, Paul
Combe, Jean-Philippe
Hansen, Gary B.
Barnes, Jason W.
Rodriguez, Sebastien
Le Mouelic, Stephane
Baines, E. Kevin H.
Buratti, Bonnie J.
Sotin, Christophe
Nicholson, Philip
Jaumann, Ralf
Nelson, Robert
CA Cassini VIMS Team
TI Titan's surface: Search for spectral diversity and composition using the
Cassini VIMS investigation
SO ICARUS
LA English
DT Article
DE Saturn; satellites; satellites; surfaces; spectroscopy
ID GALILEAN SATELLITES; WATER-ICE; REFLECTANCE; ABSORPTION; MIXTURES; WINDS
AB The surface composition of Titan is of great importance for understanding both the internal evolution of Titan and its atmosphere. The Visual and Infrared Mapping Spectrometer (VIMS) investigation on Cassini is observing Titan from 0.35 to 5.11 mu m with spatial resolution down to a few kilometers during each flyby of the spacecraft as it orbits Saturn. Our search for spectral diversity using seven methane transmission windows in the near infrared suggests that spectrally distinct units exist on the surface of Titan and that most of the surface can be modeled using only a few distinct spectral units: water frost, CO2 frost, atmospheric scattering, and an unknown material bright at 2 mu m. A dark, spectrally neutral material is also implied. Use of an atmospheric scattering component with spectral mixing analysis may provide a method for partially removing atmospheric effects. In some locations, atmospheric scattering accounts for the majority of the signal. There are also small regions with unusual spectra that may be due to low signal and high noise and/or may be exotic materials of interest. Further, we searched within the methane windows for spectral features associated with Titan's surface. Only the 5-mu m and, to a lesser extent, the 2-mu m window provide a reasonable opportunity for this as the shorter-wavelength windows are too narrow and the 2.8-mu m window is cluttered with an unknown atmospheric constituent. We find evidence for only one spectral feature: near 4.92 mu m for the 5-mu m bright Tui Regio region. CO2 frost with grains smaller than about 10 Pm is the best candidate we have found so far to explain this absorption as well as the feature's spectral contrast between the 2.7- and the 2.8-mu m atmosphere subwindows. This suggested CO2 identification is supported by the presence of an endmember in the spectral mixture analysis that is consistent with CO2 frost with large grain sizes. We find no other absorption features that are statistically significant, including those reported earlier by others. These results are consistent with but greatly extend our early analysis that treated only the T-a data set [McCord, T.B., et al., 2006a. Planet. Space Sci. 54, 1524-1539]. In the spectral feature search process, we explored in detail the noise characteristics of the VIMS data within the 5-mu m window. which has generally very low signal (4-20 DN), due to the measurement conditions and low illumination levels. We find noise of nearly Gaussian statistics except for some erratic darks and noise spikes, and the data set seems generally well behaved. We present examples of our attempt to improve on the standard VIMS pipeline data calibration. (C) 2007 Elsevier Inc. All rights reserved.
C1 [McCord, Thomas B.; Hayne, Paul; Combe, Jean-Philippe; Hansen, Gary B.] Bear Flight Ctr, Winthrop, WA 98862 USA.
[Hayne, Paul] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Hansen, Gary B.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.
[Barnes, Jason W.] Univ Arizona, Dept Planetary Sci & LPL, Tucson, AZ 85721 USA.
[Rodriguez, Sebastien] Ctr Etud Saclay, DAPNIA SAp, F-91191 Gif Sur Yvette, France.
[Le Mouelic, Stephane; Sotin, Christophe] Univ Nantes, LPG Nantes, F-44322 Nantes, France.
[Baines, E. Kevin H.; Buratti, Bonnie J.; Nelson, Robert] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Nicholson, Philip] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Jaumann, Ralf] DLR, Inst Planetary Res, D-12489 Berlin, Germany.
RP McCord, TB (reprint author), Bear Flight Ctr, POB 667,22 Fiddlers Rd, Winthrop, WA 98862 USA.
EM mccordtb@aol.com
RI Barnes, Jason/B-1284-2009; Rodriguez, Sebastien/H-5902-2016
OI Barnes, Jason/0000-0002-7755-3530; Rodriguez,
Sebastien/0000-0003-1219-0641
NR 55
TC 47
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 MAR
PY 2008
VL 194
IS 1
BP 212
EP 242
DI 10.1016/j.icarus.2007.08.039
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 267JD
UT WOS:000253504400020
ER
PT J
AU Achterberg, RK
Conrath, BJ
Gierasch, PJ
Flasar, EM
Nixon, CA
AF Achterberg, Richard K.
Conrath, Barney J.
Gierasch, Peter J.
Flasar, E. Michael
Nixon, Conor A.
TI Titan's middle-atmospheric temperatures and dynamics observed by the
Cassini Composite Infrared Spectrometer
SO ICARUS
LA English
DT Article
DE Titan; atmospheres; structure; atmospheres; dynamics; infrared
observations
ID LATITUDINAL VARIATIONS; GENERAL-CIRCULATION; STRATOSPHERE; VORTEX;
OCCULTATION; PROFILES; EMISSION; SPECTRA; DESCENT; MODEL
AB The Composite Infrared Radiometer-Spectrometer (CIRS) instrument, on the NASA Cassini Saturn orbiter, has been acquiring thermal emission spectra from the atmosphere of Titan since orbit insertion in 2004. Observation sequences for measuring stratospheric temperatures have been obtained using both a nadir mapping mode and a limb viewing mode. The limb observations give better vertical resolution, and give information from higher altitudes, while the nadir observations provide more complete longitude coverage. Because the scale height of Titan's atmosphere is large enough so that emission from a grazing ray is influenced by horizontal temperature variations in the atmosphere, we have developed a two-dimensional temperature retrieval algorithm for reducing the limb spectra, which solves simultaneously for meridional and vertical temperature variations. The analyzed nadir mapping data have sampled nearly all longitudes at latitudes from about 90 degrees S to 60 degrees N, providing temperatures between pressure levels of about 5 to 0.2 mbar. The limb data covers latitudes between about 75 degrees S and 85 degrees N, and yields temperatures between about 1 and 0.005 mbar, at a small number of longitudes. The retrieved temperatures are consistent with early results from nadir observations [Flasar, F.M., and 44 colleagues, 2005. Science 308, 975-978] between 0.5 and 5 mbar where both results are valid, with the warmest temperatures at the equator, and much stronger meridional temperature gradients in the northern (winter) hemisphere than in the southern. At higher altitudes not probed by nadir viewing, the limb data reveal that the stratopause is nearly 20 K warmer in the northern polar regions than at the equator and southern hemisphere, and that the altitude of the stratopause shifts from approximate to 0.1 mbar (300 km) near the equator to 0.01 mbar (400 km) poleward of about 40 degrees N. When the gradient wind equation is used to construct a zonal mean wind, the reversal in sign of the temperature leads to capping of the winter westerly flow. The core of the resulting jet is about 190 m s(-1) in magnitude, spans between 30 degrees N and 60 degrees N, and peaks near 0.1 mbar. Estimates of the radiative heating associated with the radiative disequilibrium lead to a meridional overturning timescale of about three Earth years. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Achterberg, Richard K.; Nixon, Conor A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Conrath, Barney J.; Gierasch, Peter J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Flasar, E. Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Achterberg, RK (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM richard.k.achterberg@nasa.gov
RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012
OI Nixon, Conor/0000-0001-9540-9121;
NR 39
TC 86
Z9 86
U1 0
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 MAR
PY 2008
VL 194
IS 1
BP 263
EP 277
DI 10.1016/j.icarus.2007.09.029
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 267JD
UT WOS:000253504400022
ER
PT J
AU Magee-Sauer, K
Mumma, MJ
DiSanti, MA
Dello Russo, N
Gibb, EL
Bonev, BP
Villanueva, GL
AF Magee-Sauer, Karen
Mumma, Michael J.
DiSanti, Michael A.
Dello Russo, Neil
Gibb, Erika L.
Bonev, Boncho P.
Villanueva, G. L.
TI The organic composition of Comet C/2001 A2 (LINEAR) I. Evidence for an
unusual organic chemistry
SO ICARUS
LA English
DT Article
DE comets; comets; composition; spectroscopy
ID O1 HALE-BOPP; C/1996 B2 HYAKUTAKE; OH PROMPT EMISSION; WATER PRODUCTION;
CARBON-MONOXIDE; SPECTROSCOPIC OBSERVATIONS; RADIO TELESCOPES; PARENT
VOLATILES; FRAGMENT-C; H1 LEE
AB We used the NIRSPEC instrument on the Keck-2 telescope atop Mauna Kea, HI to observe Comet C/2001 A2 (LINEAR) in a Target of Opportunity campaign on UT 2001 July 9.5, 10.5 August 4.4, 10.5. We measured seven organic parent volatiles (C2H6, C2H2, HCN, CH4, CO, CH3OH, H2CO) simultaneously with H2O. We obtained absolute production rates and relative abundances for parent volatiles, and also measured rotational temperatures for several of these species. The chemical composition of C/2001 A2 differs substantially from any comet we have observed to date. The abundances we measure (relative to H2O) for C2H6, C2H2, HCN, and CH3OH are enriched by a factor of similar to 2 to 3 in C/2001 A2 compared with most comets in our database. Other molecular species were detected within the typical range of measured abundances. C/2001 A2 presented a unique opportunity to study the chemistry of a fragmenting comet where pristine areas are exposed to the Sun. (c) 2007 Elsevier Inc. All rights reserved.
C1 [Magee-Sauer, Karen] Rowan Univ, Dept Phys & Astron, Glassboro, NJ 08028 USA.
[Mumma, Michael J.; DiSanti, Michael A.; Bonev, Boncho P.; Villanueva, G. L.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Dello Russo, Neil] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Gibb, Erika L.] Univ Missouri, Dept Phys & Astron, St Louis, MO 63121 USA.
[Bonev, Boncho P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Magee-Sauer, K (reprint author), Rowan Univ, Dept Phys & Astron, Glassboro, NJ 08028 USA.
EM sauer@rowan.edu
RI mumma, michael/I-2764-2013; Magee-Sauer, Karen/K-6061-2015; Dello Russo,
Neil/G-2727-2015
OI Magee-Sauer, Karen/0000-0002-4979-9875; Dello Russo,
Neil/0000-0002-8379-7304
NR 55
TC 35
Z9 35
U1 1
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 MAR
PY 2008
VL 194
IS 1
BP 347
EP 356
DI 10.1016/j.icarus.2007.10.006
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 267JD
UT WOS:000253504400027
ER
PT J
AU Cooper, PD
Moore, MH
Hudson, RL
AF Cooper, Paul D.
Moore, Marla H.
Hudson, Reggie L.
TI Radiation chemistry of H2O+O-2 ices
SO ICARUS
LA English
DT Article
DE ices; IR spectroscopy; satellites; composition; Europa; Ganymede;
enceladus
ID ELECTRON-STIMULATED PRODUCTION; CRYSTALLINE WATER ICE; AMORPHOUS SOLID
WATER; HYDROGEN-PEROXIDE; INFRARED-SPECTROSCOPY; ION IRRADIATION;
GALILEAN SATELLITES; MOLECULAR-OXYGEN; MATRIX-ISOLATION; FAR-IR
AB The chemistry and spectroscopy of proton-irradiated H2O + O-2 ices have been investigated in relation to the production of oxidants in icy satellite surfaces. Hydrogen peroxide (H2O2), ozone (O-3), and the hydroperoxy (HO2) and hydrogen trioxide (HO3) radicals have all been observed, and their temperature and dose dependent production trends have been measured. We find that O-2 aggregates form during the growth of H2O + O-2 ice films, and the presence of these aggregates greatly affects the HO2 and H2O2 yields. In addition, we have found that the position of the spectral maximum of the v(3) vibration of O-3 shifts with ice composition, giving an indication of the degree of dispersion of O-3 molecules within the ice. We discuss the relevance of these measurements to icy satellite surfaces. (c) 2007 Elsevier Inc. All rights reserved.
C1 [Cooper, Paul D.; Moore, Marla H.] NASA, Goddard Space Flight Ctr, Astrochem Branch, Greenbelt, MD 20771 USA.
[Hudson, Reggie L.] Eckerd Coll, Dept Chem, St Petersburg, FL 33711 USA.
RP Cooper, PD (reprint author), George Mason Univ, Dept Chem & Biochem, MS 3E2,4400 Univ Dr, Fairfax, VA 22030 USA.
EM pcooper6@gmu.edu
RI Hudson, Reggie/E-2335-2012
NR 44
TC 25
Z9 25
U1 4
U2 12
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD MAR
PY 2008
VL 194
IS 1
BP 379
EP 388
DI 10.1016/j.icarus.2007.10.002
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 267JD
UT WOS:000253504400030
ER
PT J
AU Zell, E
Engel-Cox, J
Eckman, R
Stackhouse, P
AF Zell, Erica
Engel-Cox, Jill
Eckman, Richard
Stackhouse, Paul, Jr.
TI Application of Satellite Sensor Data and Models for Energy Management
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
AB Effective, environmentally sound development, production, and delivery of energy depend on Earth monitoring information. Satellite remote sensing data and products provide unique, objective information that has the additional advantage of yielding global, homogeneous, and repetitive coverage. Satellite remote sensing data and products have been used extensively in parts of the energy sector for applications ranging from climatology to identification of solar and wind energy sources, vet there is significant potential to expand energy applications. This paper discusses the key energy sector organizations and decision-support tools with the greatest potential to benefit from new applications of satellite remote sensing data, identifies relevant remote sensing data and products with a focus on NASA Earth science resources, and provides examples that show the added value of the Earth observations. These examples come from the application of NASA data to solar energy information needs. Although continued work for support of solar energy is warranted, this paper focuses on areas identified with the greatest demonstrated potential for new or expanded applications: renewable energy (specifically wind, biomass, and hydroelectric resources), load forecasting, and long-term energy modeling. This study also addresses the evolving context of the Global Earth Observation System of Systems (GEOSS), and the broader framework of integrating satellite remote sensing into energy sector decision-support tools.
C1 [Zell, Erica; Engel-Cox, Jill] Battelle Mem Inst, Arlington, VA 22201 USA.
[Eckman, Richard] US Natl Aeronaut & Space Adm, Langley Res Ctr, Sci Directorate, Chem & Dynam Branch, Hampton, VA 23681 USA.
[Stackhouse, Paul, Jr.] US Natl Aeronaut & Space Adm, Langley Res Ctr, Sci Directorate, Climate Sci Branch, Hampton, VA 23681 USA.
RP Zell, E (reprint author), Battelle Mem Inst, Arlington, VA 22201 USA.
EM zelle@battelle.org
FU NASA Earth Science Applied Sciences
FX This work was Supported by the NASA Earth Science Applied Sciences
program under the Energy Management theme.
NR 36
TC 3
Z9 3
U1 1
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD MAR
PY 2008
VL 1
IS 1
BP 5
EP 17
DI 10.1109/JSTARS.2008.2001142
PG 13
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 436MM
UT WOS:000265418200003
ER
PT J
AU Lee, M
Wanke, MC
Lerttamrab, M
Young, EW
Grine, AD
Reno, JL
Siegel, PH
Dengler, RJ
AF Lee, Mark
Wanke, Michael C.
Lerttamrab, Maytee
Young, Erik W.
Grine, Albert D.
Reno, John L.
Siegel, Peter H.
Dengler, Robert J.
TI Heterodyne mixing of terahertz quantum cascade lasers using a planar
Schottky diode
SO IEEE JOURNAL OF SELECTED TOPICS IN QUANTUM ELECTRONICS
LA English
DT Article
DE heterodyne mixing; quantum cascade laser (QCL); Schottky diode;
terahertz (THz)
AB Terahertz quantum cascade lasers (QCLs) have been used together with a monolithic planar Schottky diode receiver to study the heterodyne mixing between dual internal modes of a QCL and between a single mode of a QCL and a known molecular line from a molecular gas laser. Dual-mode mixing shows that I e intrinsic linewidth of a free-running QCL is <= 30 kHz. Mixing against a molecular laser line gives a high precision measurement of a QCL's absolute frequency and can show transient turn-on behavior in a pulsed QCL.
C1 [Lee, Mark; Wanke, Michael C.; Lerttamrab, Maytee; Young, Erik W.; Grine, Albert D.; Reno, John L.] Sandia Natl Labs, Albuquerque, NM 87185 USA.
[Siegel, Peter H.; Dengler, Robert J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Lee, M (reprint author), Sandia Natl Labs, POB 5800, Albuquerque, NM 87185 USA.
EM mlee1@sandia.gov; mcwanke@sandia.gov; mlertta@sandia.gov;
ewyoung@sandia.gov; adgrine@sandia.gov; jlreno@sandia.gov;
phs@caltech.edu; no6b@no6b.nasa.gov
FU United States Department of Energy's National Nuclear Security
Administration [DE-AC04-94AL85000]
FX Sandia is a multiprogram laboratory operated by Sandia Corporation, a
Lockheed Martin Company, for the United States Department of Energy's
National Nuclear Security Administration under Contract
DE-AC04-94AL85000.
NR 11
TC 17
Z9 17
U1 0
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1077-260X
J9 IEEE J SEL TOP QUANT
JI IEEE J. Sel. Top. Quantum Electron.
PD MAR-APR
PY 2008
VL 14
IS 2
BP 370
EP 373
DI 10.1109/JSTQE.2007.910762
PG 4
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 342CY
UT WOS:000258763400014
ER
PT J
AU Maestrini, A
Ward, JS
Tripon-Canseliet, C
Gill, JJ
Lee, C
Javadi, H
Attopadhyay, GC
Mehdi, I
AF Maestrini, Alain
Ward, John S.
Tripon-Canseliet, Charlotte
Gill, John J.
Lee, Choonsup
Javadi, Hamid
Attopadhyay, Goutam Ch.
Mehdi, Imran
TI In-phase power-combined frequency triplers at 300 GHz
SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS
LA English
DT Article
DE frequency multiplier; frequency tripler; local oscillator; planar diode;
power-combining; Schottky diode; sub-millimeter wavelengths; varactor
AB We report on the design, fabrication and characterization of a 300 GHz Schottky-diode frequency tripler made of two mirror-image integrated circuits that are power-combined in-phase in a single waveguide block using compact Y-junctions at the input and output waveguides. Each chip features six anodes on a 5 mu m thick GaAs membrane. The tripler has 5-15% conversion efficiency measured across the 265-330 GHz band when driven with 50-250 mW of input power at room temperature. At 318 GHz it delivers a peak power of 26 mW with 11 % conversion efficiency. The power-combined frequency multiplier is compared with a single-chip tripler designed for the same band using the same integrated circuit.
C1 [Maestrini, Alain] Univ Paris 06, LISIF, Paris, France.
[Maestrini, Alain] Observ Paris, Lerma, France.
[Ward, John S.; Gill, John J.; Javadi, Hamid; Attopadhyay, Goutam Ch.; Mehdi, Imran] CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA.
[Tripon-Canseliet, Charlotte] Univ Paris 06, LISIF, F-75005 Paris, France.
RP Maestrini, A (reprint author), Univ Paris 06, LISIF, Paris, France.
EM alain.maestrini@obspm.fr; john.ward@jpl.nasa.gov;
Charlotte.Canseliet@lisif.jussieu.fr
NR 6
TC 31
Z9 33
U1 0
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1531-1309
J9 IEEE MICROW WIREL CO
JI IEEE Microw. Wirel. Compon. Lett.
PD MAR
PY 2008
VL 18
IS 3
BP 218
EP 220
DI 10.1109/LMWC.2008.916820
PG 3
WC Engineering, Electrical & Electronic
SC Engineering
GA 273FZ
UT WOS:000253917100024
ER
PT J
AU Feather, MS
Cornford, SL
Hicks, KA
Kiper, JD
Menzies, T
AF Feather, Martin S.
Cornford, Steven L.
Hicks, Kenneth A.
Kiper, James D.
Menzies, Tim
TI A broad, quantitative model for making early requirements decisions
SO IEEE SOFTWARE
LA English
DT Article
C1 [Feather, Martin S.; Cornford, Steven L.] CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA.
[Hicks, Kenneth A.] CALTECH, Jet Propuls Lab, Syst Modeling & Analysis Program Off, Pasadena, CA 91125 USA.
[Kiper, James D.] Miami Univ, Sch Engn & Appl Sci, Oxford, OH 45056 USA.
[Menzies, Tim] W Virginia Univ, Morgantown, WV 26506 USA.
RP Feather, MS (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA.
EM Martin.S.Feather@ipl.nasa.gov; Steven.L.Cornford@ipl.nasa.gov;
Kenneth.A.Hicks@ipl.nasa.gov; kiperjd@muohio.edu; tim@menzies.us
NR 14
TC 8
Z9 8
U1 0
U2 1
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 0740-7459
EI 1937-4194
J9 IEEE SOFTWARE
JI IEEE Softw.
PD MAR-APR
PY 2008
VL 25
IS 2
BP 49
EP 56
DI 10.1109/MS.2008.29
PG 8
WC Computer Science, Software Engineering
SC Computer Science
GA 265QN
UT WOS:000253376100019
ER
PT J
AU Weisbin, CR
Smith, JH
Van Houten, T
Moeller, R
Zimmerman, W
Smythe, W
Lincoln, W
Elfes, A
Adumitroaie, V
Silberg, R
AF Weisbin, Charles R.
Smith, Jeffrey H.
Van Houten, Tracy
Moeller, Robert
Zimmerman, Wayne
Smythe, William
Lincoln, William
Elfes, Alberto
Adumitroaie, Virgil
Silberg, Robert
TI Technical Feasibility and Relative Productivity of Alternate NASA
Robotic Missions to a Lunar Dark Crater
SO IEEE SYSTEMS JOURNAL
LA English
DT Article
DE Analysis software; decision making; exploration; fuel cell; NASA lunar
missions; optimization; power sources; productivity; return on
investment; radioisotope thermoelectric generator (RTG); technology
development; value
AB Two concepts for large-scale, complex, robotic missions to search for frozen water at the lunar South Pole are systematically analyzed to determine their relative productivity and investment requirements. A concurrent design team, a technology-assessment tool, and a sensitivity model are integrated to search a large, complex trade space. Performance goals for a broad portfolio of missions comprising NASA's lunar exploration program are optimized subject to budget, workforce, and other nontechnical constraints. Explicit distinction is made between enabling and enhancing technologies. Uncertainties and dependencies are included within the optimization framework. Given the constraints used in this analysis, the study determines that the longer mission [using a radioisotope thermoelectric generator (RTG)] would return 14 times the value of the shorter mission (using a methanol-oxygen fuel cell) for roughly a 17% increase in cost, and would be enabled with the recommended temporal technology portfolio. To assess the robustness of the investment recommendations, other potential fuel-cell chemistries are evaluated along with potential improvements in rover speed and autonomy, and a reduced activity profile. Results indicate that a lithium-oxygen fuel cell would enable the highest level of productivity among the three fuel cells studied, though not as high as that permitted by an RTG. For the shorter duration mission concepts, it was found that productivity could be enhanced by reducing the number of activities from the baseline 15 to 4, thereby permitting time for each activity to be more fully accomplished.
C1 [Weisbin, Charles R.; Silberg, Robert] CALTECH, Jet Prop Lab, Web Solut Grp, Raytheon, Pasadena, CA 91109 USA.
RP Weisbin, CR (reprint author), CALTECH, Jet Prop Lab, Web Solut Grp, Raytheon, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM charles.r.weisbin@jpl.nasa.gov
RI Elfes, Alberto/E-2463-2011
OI Elfes, Alberto/0000-0003-2433-995X
FU LaRC; Exploration Technology Development Program (ETDP)
FX The authors would like to thank J. Falker (currently at the NASA Johnson
Space Center); J. Derleth and B. Claybaugh of NASA Program Analysis and
Evaluation (PA & E); D. Craig of the Exploration Systems Mission
Directorate Integration Office (DIO); P. Troutman of LaRC supporting the
DIO; C. Moore of the ESMD Advanced Capabilities Division (ACD); F. Peri
and D. Beals of the Exploration Technology Development Program (ETDP)
who support ACD; R. Wheeler and M. Adler leading the Team X Concurrent
Design Effort; and S. Prusha who manages the System Modeling and
Analysis Program Office for graciously contributing resources,
analytical review and critique, and advocacy for this effort. They would
also like to thank A. Loverro, who helped guide the Team X design
session; S. Sherrit, who provided invaluable information about drilling
and sample acquisition; K. Shelton, who helped formulate and manipulate
the resulting START database; and H. Hua and J. Mrozinski who
implemented the START optimization algorithms and associated output
display. Finally, the authors would like to thank R. Orozco who
converted the substance of this paper into the format required by the
publication.
NR 14
TC 1
Z9 1
U1 1
U2 8
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1932-8184
EI 1937-9234
J9 IEEE SYST J
JI IEEE Syst. J.
PD MAR
PY 2008
VL 2
IS 1
BP 120
EP 128
DI 10.1109/JSYST.2007.908171
PG 9
WC Computer Science, Information Systems; Engineering, Electrical &
Electronic; Operations Research & Management Science; Telecommunications
SC Computer Science; Engineering; Operations Research & Management Science;
Telecommunications
GA V10NC
UT WOS:000207469700013
ER
PT J
AU Morabito, DD
Imbriale, W
Keihm, S
AF Morabito, David D.
Imbriale, William
Keihm, Stephen
TI Observing the Moon at microwave frequencies using a large-diameter deep
space network antenna
SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION
LA English
DT Article
DE antenna radiation patterns; microwave antennas; Moon; temperature
measurement
AB The Moon radiates energy at infrared and microwave wavelengths, in addition to reflecting sunlight at optical wavelengths. As a result, an antenna pointed at or near the Moon will result in an increase in system operating noise temperature, which needs to be accounted for in RF telecommunications, radio science or radiometric link calculations. The NASA Deep Space Network (DSN) may use its large-diameter antennas in future lunar robotic or human missions, and thus it is important to understand the nature of this temperature increase as a function of observing frequency, lunar phase, and angular position of the antenna beam on the lunar disk. This paper reports on a comprehensive lunar noise temperature measurement campaign and associated theoretical treatment for a 34-m diameter Deep Space Network antenna observing an extended source such as the Moon. A set of measurements over a wide range of lunar phase angles was acquired at DSS-13, a 34-m diameter beam waveguide antenna (BWG) located at Goldstone, California at 2.3 GHz (S-band), 8.4 GHz (X-band) and 32 GHz (Ka-band). For validation purposes, independent predictions of noise temperature increase were derived using a physical optics characterization of the 34-m diameter antenna gain patterns and Apollo model-based brightness temperature maps of the Moon as input. The model-based predictions of noise temperature increase were compared with the measurements at all three frequencies. In addition, a methodology is presented that relates noise temperature increase due to the Moon to disk-centered or disk-averaged brightness temperature of the Moon at the microwave frequencies of interest. Comparisons were made between the measurements and models in the domain of lunar disk-centered and disk-averaged brightness temperatures. It is anticipated that the measurements and associated theoretical development will be useful in developing telecommunications strategies for future high-rate Ka-band communications where large diameter DSN antennas will be required.
C1 [Morabito, David D.; Imbriale, William; Keihm, Stephen] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Morabito, DD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM ddm@godzilla.jpl.nasa.gov
NR 19
TC 9
Z9 12
U1 0
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 0018-926X
J9 IEEE T ANTENN PROPAG
JI IEEE Trans. Antennas Propag.
PD MAR
PY 2008
VL 56
IS 3
BP 650
EP 660
DI 10.1109/TAP.2007.915471
PG 11
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA 274VB
UT WOS:000254029300005
ER
PT J
AU Cheng, MK
Nakashima, MA
Moision, BE
Harrikins, J
AF Cheng, Michael K.
Nakashima, Michael A.
Moision, Bruce E.
Harrikins, Jon
TI Optimizations of a hardware decoder for deep-space optical
communications
SO IEEE TRANSACTIONS ON CIRCUITS AND SYSTEMS I-REGULAR PAPERS
LA English
DT Article
DE cyclic redundancy check (CRC); field-programmable gate array (FPGA)
implementation; optical communications; quadratic polynomial
interleaver; turbo decoding
ID PERMUTATION POLYNOMIALS; INTEGER RINGS; CODES; INTERLEAVERS
AB The National Aeronautics and Space Administration has developed a capacity approaching modulation and coding scheme that comprises a serial concatenation of an inner accumulate pulse-position modulation (PPM) and an outer convolutional code [or serially concatenated PPM (SCPPM)] for deep-space optical communications. Decoding of this code uses the turbo principle. However, due to the nonbinary property of SCPPM, a straightforward application of classical turbo decoding is very inefficient. Here, we present various optimizations applicable in hardware implementation of the SCPPM decoder. More specifically, we feature a Super Gamma computation to efficiently handle parallel trellis edges, a pipeline-friendly "maxstar top-2" circuit that reduces the max-only approximation penalty, a low-latency cyclic redundancy check circuit for window-based decoders, and a high-speed algorithmic polynomial interleaver that leads to memory savings. Using the featured optimizations, we implement a 6.72 megabits-per-second (Mbps) SCPPM decoder on a single field-programmable gate array (FPGA). Compared to the current data rate of 256 kilobits per second from Mars, the SCPPM coded scheme represents a throughput increase of more than twenty-six fold. Extension to a 50-Mbps decoder on a board with multiple FPGAs follows naturally. We show through hardware simulations that the SCPPM coded system can operate within 1 dB of the Shannon capacity at nominal operating conditions.
C1 [Cheng, Michael K.; Nakashima, Michael A.; Moision, Bruce E.; Harrikins, Jon] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Cheng, MK (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM mkcheng@jpl.nasa.gov
NR 23
TC 11
Z9 12
U1 0
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1549-8328
J9 IEEE T CIRCUITS-I
JI IEEE Trans. Circuits Syst. I-Regul. Pap.
PD MAR
PY 2008
VL 55
IS 2
BP 644
EP 658
DI 10.1109/TCSI.2007.913733
PG 15
WC Engineering, Electrical & Electronic
SC Engineering
GA 275KJ
UT WOS:000254070000014
ER
PT J
AU Narasimham, B
Shuler, RL
Black, JD
Bhuva, BL
Schrimpf, RD
Witulski, AF
Holman, WT
Massengill, LW
AF Narasimham, Balaji
Shuler, Robert L.
Black, Jeffrey D.
Bhuva, Bharat L.
Schrimpf, Ronald D.
Witulski, Arthur F.
Holman, William Timothy
Massengill, Lloyd W.
TI Quantifying the reduction in collected charge and soft errors in the
presence of guard rings
SO IEEE TRANSACTIONS ON DEVICE AND MATERIALS RELIABILITY
LA English
DT Article
DE collected charge; guard rings (GRs); pulse-width; radiation hardening by
design (RHBD); single event (SE); SE transient (SET); soft error;
soft-error rate (SER)
ID MITIGATION
AB Soft errors pose a major reliability threat to advanced electronic components and systems. Novel techniques are needed to mitigate the soft-error rate (SER) of integrated circuits (ICs), and in some cases, a combination of different mitigation techniques may be required for significant performance improvements. In this paper, an autonomous single-event-transient (SET) pulse-width characterization technique is used to quantify the effect of hardened-by-design structures, such as guard rings (GRs), in reducing the collected charge and SER of ICs. Experimental results obtained for a 0.35-mu m technology show a reduced SET pulse-width for devices with GRs; the corresponding reduction in SER was estimated to be greater than 55% for technologies ranging from 0.35 mu m to 70 nm.
C1 [Narasimham, Balaji; Black, Jeffrey D.; Bhuva, Bharat L.; Schrimpf, Ronald D.; Witulski, Arthur F.; Holman, William Timothy; Massengill, Lloyd W.] Vanderbilt Univ, Nashville, TN 37235 USA.
[Shuler, Robert L.] NASA, Lyndon B Johnson Space Ctr, Avion Syst Div, Houston, TX 77058 USA.
RP Narasimham, B (reprint author), Vanderbilt Univ, 221 Kirkland Hall, Nashville, TN 37235 USA.
EM balaji.narasimham@vanderbilt.edu
RI Schrimpf, Ronald/L-5549-2013
OI Schrimpf, Ronald/0000-0001-7419-2701
NR 11
TC 7
Z9 8
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1530-4388
EI 1558-2574
J9 IEEE T DEVICE MAT RE
JI IEEE Trans. Device Mater. Reliab.
PD MAR
PY 2008
VL 8
IS 1
BP 203
EP 209
DI 10.1109/TDMR.2007.912778
PG 7
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA 275KF
UT WOS:000254069600022
ER
PT J
AU Kerr, YH
Le Vine, DM
AF Kerr, Yann H.
Le Vine, David M.
TI Foreword to the special issue on the Soil Moisture and Ocean Salinity
(SMOS) mission
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Editorial Material
ID APERTURE MICROWAVE RADIOMETER; RETRIEVAL; SPACE; ESTAR
C1 [Kerr, Yann H.] CESBIO, F-31401 Toulouse, France.
[Le Vine, David M.] NASA, Goddard Space Flight Ctr, Instrumentat Sci Branch, Greenbelt, MD 20771 USA.
RP Kerr, YH (reprint author), CESBIO, F-31401 Toulouse, France.
NR 19
TC 8
Z9 9
U1 0
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2008
VL 46
IS 3
BP 583
EP 585
DI 10.1109/TGRS.2008.917807
PG 3
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 270QB
UT WOS:000253734200001
ER
PT J
AU Panciera, R
Walker, JP
Kalma, JD
Kim, EJ
Hacker, JM
Merlin, O
Berger, M
Skou, N
AF Panciera, Rocco
Walker, Jeffrey P.
Kalma, Jetse D.
Kim, Edward J.
Hacker, Joerg M.
Merlin, Olivier
Berger, Michael
Skou, Niels
TI The NAFE'05/CoSMOS data set: Toward SMOS soil moisture retrieval,
downscaling, and assimilation
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE microwave radiometry; National Airborne Field Experiment (NAFE); passive
microwave; soil moisture; Soil Moisture and Ocean Salinity (SMOS)
ID MODEL; BAND
AB The National Airborne Field Experiment 2005 (NAFE'05) and the Campaign for validating the Operation of Soil Moisture and Ocean Salinity (COSMOS) were undertaken in November 2005 in the Goulburn River catchment, which is located in southeastern Australia. The objective of the joint campaign was to provide simulated Soil Moisture and Ocean Salinity (SMOS) observations using airborne L-band radiometers supported by soil moisture and other relevant ground data for the following: 1) the development of SMOS soil moisture retrieval algorithms; 2) developing approaches for downscaling the low-resolution data from SMOS; and 3) testing its assimilation into land surface models for root zone soil moisture retrieval. This paper describes the NAFE'05 and COSMOS airborne data sets together with the ground data collected in support of both aircraft campaigns. The airborne L-band acquisitions included 40 km x 40 km coverage flights at 500-m and 1-km resolution for the simulation of a SMOS pixel, multiresolution flights with ground resolution ranging from 1 km to 62.5 m, multiangle observations, and specific flights that targeted the vegetation dew and sun glint effect on L-band soil moisture retrieval. The L-band data were accompanied by airborne thermal infrared and optical measurements. The ground data consisted of continuous soil moisture profile measurements at 18 monitoring sites throughout the 40 km x 40 km study area and extensive spatial near-surface soil moisture measurements concurrent with airborne monitoring. Additionally, data were collected on rock coverage and temperature, surface roughness, skin and soil temperatures, dew amount, and vegetation water content and biomass. These data are available at www.nafe.unimelb. edu.au.
C1 [Panciera, Rocco; Walker, Jeffrey P.; Merlin, Olivier] Univ Melbourne, Dept Civil & Environm Engn, Melbourne, Vic 3010, Australia.
[Kalma, Jetse D.] Univ Newcastle, Sch Engn, Callaghan, NSW 2308, Australia.
[Kim, Edward J.] NASA, Hydrospher & Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hacker, Joerg M.] Airborne Res Australia, Salisbury, SA 5106, Australia.
[Berger, Michael] European Space Agcy, Earth Observat Ctr, ESRIN, Sci Strategy Coordinat & Planning Off EOP SA, I-00044 Frascati, Italy.
[Skou, Niels] Tech Univ Denmark, DK-2800 Lyngby, Denmark.
[Skou, Niels] Danish Natl Space Ctr, DK-2100 Copenhagen, Denmark.
[Hacker, Joerg M.] Flinders Univ S Australia, Adelaide, SA 5001, Australia.
RP Panciera, R (reprint author), Univ Melbourne, Dept Civil & Environm Engn, Melbourne, Vic 3010, Australia.
EM rocco@civenv.unimelb.edu.au
RI Walker, Jeffrey/D-2624-2009
NR 18
TC 64
Z9 66
U1 0
U2 11
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2008
VL 46
IS 3
BP 736
EP 745
DI 10.1109/TGRS.2007.915403
PG 10
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 270QB
UT WOS:000253734200015
ER
PT J
AU Marquette, ML
Byerly, D
Sognier, M
AF Marquette, Michele L.
Byerly, Diane
Sognier, Marguerite
TI The effects of three-dimensional cell culture on single myoblasts
SO IN VITRO CELLULAR & DEVELOPMENTAL BIOLOGY-ANIMAL
LA English
DT Article
DE myoblast; 3D; three dimensional; skeletal muscle; F-actin; podia
ID PROSTATE-CANCER CELLS; ELECTRON-MICROSCOPY; DEPENDENT CONTROL;
GENE-EXPRESSION; LATRUNCULIN-A; APOPTOSIS; GROWTH; DIFFERENTIATION;
FIBROBLASTS; ADHESION
AB Identification of cellular and morphological changes in myoblasts during three-dimensional (3D) culture may provide novel insight into skeletal muscle morphogenesis. One particular morphological change that occurs during the transition from monolayer culture to the 3D environment is the appearance of cytoplasmic projections (podia). The purpose of these studies was to determine if: (1) 3D culture increased podia formation in single cells, and (2) podia were F-actin dependent. C2C12 cells were grown in 3D conditions using a rotary cell culture system (RCCS) for 3, 6, and 9 h, fixed, and stained. Analysis of confocal images revealed that podia were significantly more numerous on RCCS cultured cells than those on suspension controls. Further, the podia of RCCS cultured cells decreased in number and increased in length during the time intervals examined. RCCS cultured cells showed no significant changes in viability, Annexin V staining, and activated Caspase 3 expression over time. In contrast, significant decreases in viability of suspension controls occurred. The application of 2 mu M Latrunculin A (Lat A), an actin depolymerizing agent, significantly reduced the number of cells with podia. The number of cells with podia recovered with Lat A removal. Changes in viability and apoptosis markers were not significant during Lat A application or washout experiments. These observations reveal that: (1) culture conditions in the RCCS increase the quantity of podia formation; (2) these podia increase in length with time; and (3) F-actin plays a role in podia formation.
C1 [Marquette, Michele L.; Byerly, Diane] NASA, Lyndon B Johnson Space Ctr, ORAU, Houston, TX 77058 USA.
[Sognier, Marguerite] USRA, Houston, TX 77058 USA.
RP Marquette, ML (reprint author), NASA, Lyndon B Johnson Space Ctr, ORAU, 2101 NASA Rd 1, Houston, TX 77058 USA.
EM michele.marquette-1@nasa.gov
NR 38
TC 3
Z9 3
U1 0
U2 1
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013 USA
SN 1071-2690
J9 IN VITRO CELL DEV-AN
JI In Vitro Cell. Dev. Biol.-Anim.
PD MAR-APR
PY 2008
VL 44
IS 3-4
BP 105
EP 114
DI 10.1007/s11626-007-9078-5
PG 10
WC Cell Biology; Developmental Biology
SC Cell Biology; Developmental Biology
GA 283GE
UT WOS:000254623900009
PM 18246406
ER
PT J
AU Jordan, JA
Verhoff, AM
Fischer, DG
AF Jordan, J. A.
Verhoff, A. M.
Fischer, D. G.
TI Assessing the in vitro respiratory toxicity of fine particles of Al2O3
and SiO2: A precursor study for lunar dust toxicity
SO IN VITRO CELLULAR & DEVELOPMENTAL BIOLOGY-ANIMAL
LA English
DT Meeting Abstract
C1 NASA, Glenn Res Ctr, Biosci & Technol Branch, Cleveland, OH 44135 USA.
Clayton State Univ, Dept Nat Sci, Morrow, GA 30260 USA.
EM dgfisher@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 3
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1071-2690
J9 IN VITRO CELL DEV-AN
JI In Vitro Cell. Dev. Biol.-Anim.
PD SPR
PY 2008
VL 44
SU S
BP S48
EP S48
PG 1
WC Cell Biology; Developmental Biology
SC Cell Biology; Developmental Biology
GA 338XL
UT WOS:000258542600123
ER
PT J
AU O'Sullivan, C
Cahill, G
Murphy, JA
Gear, WK
Harris, J
Ade, PAR
Church, SE
Thompson, KL
Pryke, C
Bock, J
Bowden, M
Brown, ML
Carlstrom, JE
Castro, PG
Culverhouse, T
Friedman, RB
Ganga, KM
Haynes, V
Hinderks, JR
Kovak, J
Lange, AE
Leitch, EM
Mallie, OE
Melhuish, SJ
Orlando, A
Piccirillo, L
Pisano, G
Rajguru, N
Rusholme, BA
Schwarz, R
Taylor, AN
Wu, EYS
Zemcov, M
AF O'Sullivan, C.
Cahill, G.
Murphy, J. A.
Gear, W. K.
Harris, J.
Ade, P. A. R.
Church, S. E.
Thompson, K. L.
Pryke, C.
Bock, J.
Bowden, M.
Brown, M. L.
Carlstrom, J. E.
Castro, P. G.
Culverhouse, T.
Friedman, R. B.
Ganga, K. M.
Haynes, V.
Hinderks, J. R.
Kovak, J.
Lange, A. E.
Leitch, E. M.
Mallie, O. E.
Melhuish, S. J.
Orlando, A.
Piccirillo, L.
Pisano, G.
Rajguru, N.
Rusholme, B. A.
Schwarz, R.
Taylor, A. N.
Wu, E. Y. S.
Zemcov, M.
TI The quasi-optical design of the QUaD telescope
SO INFRARED PHYSICS & TECHNOLOGY
LA English
DT Article
DE quasioptics; gaussian beam modes; optical design; feedhorn design;
cosmic microwave background
ID CMB POLARIZATION EXPERIMENT; CORRUGATED HORNS; MILLIMETER-WAVE; DASI
AB We describe the optical design and performance of 'QUEST and DASI' or 'QUaD', a ground-based high-resolution experiment designed to measure the polarisation properties of the cosmic microwave background radiation. QUaD uses bolometric detectors at 100 and 150 GHz on a 2.6 m Cassegrain telescope. The QUaD optics are designed to minimise systematic effects as well as to maximise sensitivity, and we report here on the comprehensive quasi-optical analysis used to achieve this design. We also present initial optical performance measurements achieved in operation, and discuss changes made to the optics to overcome some errors in the mechanical construction of the primary mirror. The QUaD experiment is now fully operational and taking world-leading data at the South Pole. (C) 2007 Elsevier B.V. All rights reserved.
C1 [O'Sullivan, C.; Cahill, G.; Murphy, J. A.] Natl Univ Ireland Maynooth, Dept Expt Phys, Kildare, Ireland.
[Gear, W. K.; Harris, J.; Ade, P. A. R.; Bowden, M.; Haynes, V.; Mallie, O. E.; Melhuish, S. J.; Orlando, A.; Piccirillo, L.; Pisano, G.; Rajguru, N.; Zemcov, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Church, S. E.; Thompson, K. L.; Bowden, M.; Hinderks, J. R.; Rusholme, B. A.; Wu, E. Y. S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Church, S. E.; Thompson, K. L.; Bowden, M.; Hinderks, J. R.; Rusholme, B. A.; Wu, E. Y. S.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Pryke, C.; Carlstrom, J. E.; Culverhouse, T.; Friedman, R. B.; Schwarz, R.] Univ Chicago, Kavli Inst Cosmol Phys, Dept Astron & Astrophys, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Bock, J.; Leitch, E. M.; Zemcov, M.] Jet Prop Lab, Pasadena, CA 91109 USA.
[Bock, J.; Kovak, J.; Lange, A. E.; Leitch, E. M.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA.
[Brown, M. L.; Castro, P. G.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ganga, K. M.] CNRS, Lab APC, F-75205 Paris 13, France.
RP O'Sullivan, C (reprint author), Natl Univ Ireland Maynooth, Dept Expt Phys, Kildare, Ireland.
EM creidhe.osullivan@nuim.ie
RI Melhuish, Simon/B-1299-2016;
OI Melhuish, Simon/0000-0001-8725-4991; Orlando,
Angiola/0000-0001-8004-5054
NR 21
TC 12
Z9 12
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1350-4495
J9 INFRARED PHYS TECHN
JI Infrared Phys. Technol.
PD MAR
PY 2008
VL 51
IS 4
BP 277
EP 286
DI 10.1016/j.infrared.2007.10.001
PG 10
WC Instruments & Instrumentation; Optics; Physics, Applied
SC Instruments & Instrumentation; Optics; Physics
GA 288KA
UT WOS:000254984100001
ER
PT J
AU Biswas, R
Oliker, L
AF Biswas, Rupak
Oliker, Leonid
TI Special issue on performance characterization of the world's most
powerful supercomputers - Part 1 - Preface
SO INTERNATIONAL JOURNAL OF HIGH PERFORMANCE COMPUTING APPLICATIONS
LA English
DT Editorial Material
C1 [Biswas, Rupak] NASA, Ames Res Ctr, NAS Div, Moffett Field, CA 94035 USA.
[Oliker, Leonid] Lawrence Berkeley Natl Lab, NERSC, CRD, Berkeley, CA 94720 USA.
RP Biswas, R (reprint author), NASA, Ames Res Ctr, NAS Div, Moffett Field, CA 94035 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 1094-3420
J9 INT J HIGH PERFORM C
JI Int. J. High Perform. Comput. Appl.
PD SPR
PY 2008
VL 22
IS 1
BP 3
EP 4
DI 10.1177/10943420070085013
PG 2
WC Computer Science, Hardware & Architecture; Computer Science,
Interdisciplinary Applications; Computer Science, Theory & Methods
SC Computer Science
GA 270LZ
UT WOS:000253723600001
ER
PT J
AU Hood, R
Biswas, R
Chang, J
Djornehri, MJ
Jin, H
AF Hood, Robert
Biswas, Rupak
Chang, Johnny
Djornehri, M. Jahed
Jin, Haoqiang
TI Benchmarking the Columbia supercluster
SO INTERNATIONAL JOURNAL OF HIGH PERFORMANCE COMPUTING APPLICATIONS
LA English
DT Article
DE SGI altix; HPC challenge benchmarks; NAS parallel benchmarks;
computational fluid dynamics
AB Columbia, NASA's 10,240-processor supercluster, has been ranked as one of the fastest computers in the world since November 2004. In this paper we examine the performance characteristics of its production subclusters, which are typically configurations ranging in size from 512 to 2048 processors. We evaluate floating-point performance, memory bandwidth, and message passing communication speeds using a subset of the HPC Challenge benchmarks, the NAS Parallel Benchmarks, and a computational fluid dynamics application. Our experimental results quantify the performance improvement resulting from changes in interconnect bandwidth, processor speed, and cache size across the different types of SGI Altix 3700s that constitute Columbia. We also report on our experiments that investigate the performance impact of processors sharing a path to memory. Finally, our tests of the different interconnect fabrics available indicate substantial promise for scaling applications to run on configurations of more than 512 CPUs.
C1 [Hood, Robert; Biswas, Rupak; Chang, Johnny; Djornehri, M. Jahed; Jin, Haoqiang] NASA, Ames Res Ctr, NASA Adv Supercomp NAS Div, Moffett Field, CA 94035 USA.
RP Hood, R (reprint author), NASA, Ames Res Ctr, NASA Adv Supercomp NAS Div, Moffett Field, CA 94035 USA.
EM RHOOD@MAIL.ARC.NASA.GOV
NR 15
TC 0
Z9 0
U1 0
U2 0
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 1094-3420
J9 INT J HIGH PERFORM C
JI Int. J. High Perform. Comput. Appl.
PD SPR
PY 2008
VL 22
IS 1
BP 97
EP 112
DI 10.1177/1094342006085021
PG 16
WC Computer Science, Hardware & Architecture; Computer Science,
Interdisciplinary Applications; Computer Science, Theory & Methods
SC Computer Science
GA 270LZ
UT WOS:000253723600007
ER
PT J
AU Nakano, A
Kalia, RK
Nomura, KI
Sharma, A
Vashishta, P
Shimojo, F
Van Duin, ACT
Goddard, WA
Biswas, R
Srivastava, D
Yang, LH
AF Nakano, Aiichiro
Kalia, Rajiv K.
Nomura, Ken-Ichi
Sharma, Ashish
Vashishta, Priya
Shimojo, Fuyuki
Van Duin, Adri C. T.
Goddard, William A., III
Biswas, Rupak
Srivastava, Deepak
Yang, Lin H.
TI De novo ultrascale atomistic simulations on high-end parallel
supercomputers
SO INTERNATIONAL JOURNAL OF HIGH PERFORMANCE COMPUTING APPLICATIONS
LA English
DT Article
DE hierarchical simulation; molecular dynamics; reactive force field;
quantum mechanics; density functional theory; parallel computing; grid
computing
ID MOLECULAR-DYNAMICS SIMULATIONS; DENSITY-FUNCTIONAL THEORY;
ELECTRONIC-STRUCTURE METHODS; COMPUTATIONAL CHEMISTRY; SPACE; COMPUTERS;
ALGORITHM; IMPLEMENTATION; OXIDATION; CERAMICS
AB We present a de novo, hierarchical simulation framework for first-principles based predictive simulations of materials and their validation on high-end parallel supercomputers and geographically distributed clusters. In this framework, high-end chemically reactive and non-reactive molecular dynamics (MID) simulations explore a wide solution space to discover microscopic mechanisms that govern macroscopic material properties, into which highly accurate quantum mechanical (QM) simulations are embedded to validate the discovered mechanisms and quantify the uncertainty of the solution. The framework includes an embedded divide-and conquer (EDC) algorithmic framework for the design of linear-scaling simulation algorithms with minimal bandwidth complexity and tight error control. The EDC framework also enables adaptive hierarchical simulation with automated model transitioning assisted by graph-based event tracking. A tunable hierarchical cellular decomposition parallelization framework then maps the O(N) EDC algorithms onto petaflops computers, while achieving performance tunability through a hierarchy of parameterized cell data/ computation structures, as well as its implementation using hybrid grid remote procedure call + message passing + threads programming. High-end computing platforms such as IBM BlueGene/L, SGI Altix 3000 and the NSF TeraGrid provide an excellent test grounds for the framework. On these platforms, we have achieved unprecedented scales of quantum-mechanically accurate and well validated, chemically reactive atomistic simulations-1.06 billion-atom fast reactive force-field MID and 11.8 million-atom (1.04 trillion grid points) quantum-mechanical MID in the framework of the EDC density functional theory on adaptive multigrids-in addition to 134 billion-atom non-reactive space-time multiresolution MD, with the parallel efficiency as high as 0.998 on 65,536 dual-processor BlueGene/L nodes. We have also achieved an automated execution of hierarchical QM/MD simulation on a grid consisting of 6 supercomputer centers in the US and Japan (in total of 150,000 processor hours), in which the number of processors change dynamically on demand and resources are allocated and migrated dynamically in response to faults. Furthermore, performance portability has been demonstrated on a wide range of platforms such as BlueGene/L, Altix 3000, and AMD Opteron-based Linux clusters.
C1 [Nakano, Aiichiro; Kalia, Rajiv K.; Nomura, Ken-Ichi; Sharma, Ashish; Vashishta, Priya; Shimojo, Fuyuki] Univ So Calif, Collaborat Adv Comp & Simulat, Los Angeles, CA 90089 USA.
[Sharma, Ashish] Ohio State Univ, Dept Biomed Informat, Columbus, OH 43210 USA.
[Van Duin, Adri C. T.] Kumamoto Univ, Fac Gen Educ, Dept Phys, Kumamoto 8608555, Japan.
[Van Duin, Adri C. T.; Goddard, William A., III] CALTECH, Mat & Proc Simulat Ctr, Pasadena, CA 91125 USA.
[Biswas, Rupak; Srivastava, Deepak] NASA, Ames Res Ctr, NASA Adv Supercomp NAS Div, Moffett Field, CA 94035 USA.
[Yang, Lin H.] Lawrence Livermore Natl Lab, Phys H Div, Livermore, CA 94551 USA.
RP Nakano, A (reprint author), Univ So Calif, Collaborat Adv Comp & Simulat, Los Angeles, CA 90089 USA.
EM ANAKANO@USC.EDU
NR 58
TC 30
Z9 30
U1 2
U2 13
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 1094-3420
EI 1741-2846
J9 INT J HIGH PERFORM C
JI Int. J. High Perform. Comput. Appl.
PD SPR
PY 2008
VL 22
IS 1
BP 113
EP 128
DI 10.1177/1094342007085015
PG 16
WC Computer Science, Hardware & Architecture; Computer Science,
Interdisciplinary Applications; Computer Science, Theory & Methods
SC Computer Science
GA 270LZ
UT WOS:000253723600008
ER
PT J
AU Hull, DH
Harries, KA
AF Hull, Daniel H.
Harries, Kent A.
TI On the applicability of fixed point theory to the behavior of coupled
core walls
SO INTERNATIONAL JOURNAL OF STRUCTURAL STABILITY AND DYNAMICS
LA English
DT Article
DE coupled walls; dynamic behavior; fixed point theory; structural
optimization
ID DESIGN
AB The performance-based design of coupled core wall systems offers a number of advantages over conventional strength-based methods in terms of constructability and structural performance. Under large seismic loads, the expected degradation of the coupling beams in coupled wall structures results in an evolution of the lateral force resisting system from a coupled wall system to a system of linked cantilever wall piers. The present study focuses on the performance of the eventually obtained linked wall pier systems and defines their performance in a novel way: as the minimization of transmissibility of horizontal ground motion. In this paper, fixed point theory (FPT) is used to establish initial design values for the coupling beams required to optimize the dynamic response of the linked wall pier system. An initial parametric study of the application of FPT to optimizing the behavior of linked wall piers is presented. The resulting optimized wall systems are compared with practically obtainable, rigid and uncoupled systems subject to a linear time history analysis to assess the extent and practicality of optimization obtained.
C1 [Hull, Daniel H.] NASA, Kennedy Space Ctr, FL 32899 USA.
[Harries, Kent A.] Univ Pittsburgh, Dept Civil & Environm Engn, Pittsburgh, PA 15261 USA.
RP Hull, DH (reprint author), NASA, Kennedy Space Ctr, FL 32899 USA.
EM kharries@pitt.edu
OI Harries, Kent/0000-0002-8421-2523
NR 17
TC 4
Z9 4
U1 0
U2 2
PU WORLD SCIENTIFIC PUBL CO PTE LTD
PI SINGAPORE
PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE
SN 0219-4554
J9 INT J STRUCT STAB DY
JI Int. J. Struct. Stab. Dyn.
PD MAR
PY 2008
VL 8
IS 1
BP 161
EP 186
DI 10.1142/S0219455408002594
PG 26
WC Engineering, Civil; Engineering, Mechanical; Mechanics
SC Engineering; Mechanics
GA 278NF
UT WOS:000254292900009
ER
PT J
AU McKay, TL
Gedeon, DJ
Vickerman, MB
Hylton, AG
Ribita, D
Olar, HH
Kaiser, PK
Parsons-Wingerter, P
AF McKay, Terri L.
Gedeon, Dan J.
Vickerman, Mary B.
Hylton, Alan G.
Ribita, Daniela
Olar, Harry H.
Kaiser, Peter K.
Parsons-Wingerter, Patricia
TI Selective inhibition of angiogenesis in small blood vessels and decrease
in vessel diameter throughout the vascular tree by triamcinolone
acetonide
SO INVESTIGATIVE OPHTHALMOLOGY & VISUAL SCIENCE
LA English
DT Article
ID ENDOTHELIAL GROWTH-FACTOR; INTRAVITREAL TRIAMCINOLONE; MORPHOMETRY;
EXPRESSION; VEGF
AB PURPOSE. To quantify the effects of the steroid triamcinolone acetonide (TA) on branching morphology within the angiogenic microvascular tree of the chorioallantoic membrane (CAM) of quail embryos.
METHODS. Increasing concentrations of TA (0-16 ng/mL) were applied topically on embryonic day (E) 7 to the chorioallantoic membrane (CAM) of quail embryos cultured in petri dishes and incubated for an additional 24 or 48 hours until fixation. Binary (black/white) microscopic images of arterial end points were quantified by generational analysis of vessel branching (VESGEN) software to obtain major vascular parameters that include vessel diameter (D-v), fractal dimension (D-f), tortuosity (T-v), and densities of vessel area, length, number, and branch point (A(v), L-v, N-v, and Br-v). For assessment of specific changes in vascular morphology induced by TA, the VESGEN software automatically segmented the vascular tree into branching generations (G(1)... G(10)) according to changes in vessel diameter and branching.
RESULTS. Vessel density decreased significantly up to 34% as the function of increasing concentration of TA according to A(v), L-v, Br-v, N-v, and D-f. TA selectively inhibited the growth of new, small vessels because L v decreased from 13.14 +/- 0.61 cm/cm(2) for controls to 8.012 +/- 0.82 cm/cm(2) at 16 ng TA/mL in smaller branching generations (G(7)-G(10)) and for N v from 473.83 +/- 29.85 cm(-2) to 302.32 +/- 33.09 cm(-2). In contrast, vessel diameter (D v) decreased throughout the vascular tree (G(1)-G(10)).
CONCLUSIONS. By VESGEN analysis, TA selectively inhibited the angiogenesis of smaller blood vessels, but decreased the vessel diameter of all vessels within the vascular tree.
C1 [McKay, Terri L.; Gedeon, Dan J.; Vickerman, Mary B.; Hylton, Alan G.; Ribita, Daniela; Olar, Harry H.; Parsons-Wingerter, Patricia] NASA, Glenn Res Ctr, Res Technol & Directorate, Cleveland, OH 44135 USA.
[McKay, Terri L.; Gedeon, Dan J.; Vickerman, Mary B.; Hylton, Alan G.; Ribita, Daniela; Olar, Harry H.; Parsons-Wingerter, Patricia] NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA.
[Kaiser, Peter K.] Cole Eye Inst, Cleveland Clin Fdn, Cleveland, OH 44195 USA.
RP Parsons-Wingerter, P (reprint author), NASA, Glenn Res Ctr, Res Technol & Directorate, MS 110-3, Cleveland, OH 44135 USA.
EM patricia.parsons@grc.nasa.gov
FU NEI NIH HHS [R01EY17529, R01EY17528]
NR 26
TC 19
Z9 20
U1 0
U2 0
PU ASSOC RESEARCH VISION OPHTHALMOLOGY INC
PI ROCKVILLE
PA 12300 TWINBROOK PARKWAY, ROCKVILLE, MD 20852-1606 USA
SN 0146-0404
J9 INVEST OPHTH VIS SCI
JI Invest. Ophthalmol. Vis. Sci.
PD MAR
PY 2008
VL 49
IS 3
BP 1184
EP 1190
DI 10.1167/iovs.07-1329
PG 7
WC Ophthalmology
SC Ophthalmology
GA 271TZ
UT WOS:000253812900050
PM 18326748
ER
PT J
AU Di, KC
Xu, FL
Wang, J
Agarwal, S
Brodyagina, E
Li, RX
Matthies, L
AF Di, Kaichang
Xu, Fengliang
Wang, Jue
Agarwal, Sanchit
Brodyagina, Evgenia
Li, Rongxing
Matthies, Larry
TI Photogrammetric processing of rover imagery of the 2003 Mars Exploration
Rover mission
SO ISPRS JOURNAL OF PHOTOGRAMMETRY AND REMOTE SENSING
LA English
DT Article
DE Mars rover; topographic mapping; rover localization; incremental bundle
adjustment; tie point selection
ID LANDING-SITE; LOCALIZATION; CAMERAS; SYSTEM
AB In the 2003 Mars Exploration Rover (MER) mission, the twin rovers, Spirit and Opportunity, carry identical Athena instrument payloads and engineering cameras for exploration of the Gusev Crater and Meridiani Planum landing sites. This paper presents the photogrammetric processing techniques for high accuracy topographic mapping and rover localization at the two landing sites. Detailed discussions about camera models, reference frames, interest point matching, automatic tie point selection, image network construction, incremental bundle adjustment, and topographic product generation are given. The developed rover localization method demonstrated the capability of correcting position errors caused by wheel slippages, azimuthal angle drift and other navigation errors. A comparison was also made between the bundle-adjusted rover traverse and the rover track imaged from the orbit. Mapping products including digital terrain models, orthophotos, and rover traverse maps have been generated for over two years of operations, and disseminated to scientists and engineers of the mission through a web-based GIS. The maps and localization information have been extensively used to support tactical operations and strategic planning of the mission. (C) 2007 International Society for Photogrammetry and Remote Sensing, Inc. (ISPRS). Published by Elsevier B.V. All rights reserved.
C1 [Di, Kaichang; Xu, Fengliang; Wang, Jue; Agarwal, Sanchit; Brodyagina, Evgenia; Li, Rongxing] Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Mapping & GIS Lab, Columbus, OH 43210 USA.
[Matthies, Larry] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Li, RX (reprint author), Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Mapping & GIS Lab, 470 Hitchcock Hall,2070 Neil Ave, Columbus, OH 43210 USA.
EM li.282@osu.edu
RI Wang, Jue/C-9215-2009;
OI Wang, Jue/0000-0002-9901-9996; di, kai chang/0000-0001-6581-6615
NR 47
TC 16
Z9 26
U1 1
U2 13
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0924-2716
EI 1872-8235
J9 ISPRS J PHOTOGRAMM
JI ISPRS-J. Photogramm. Remote Sens.
PD MAR
PY 2008
VL 63
IS 2
BP 181
EP 201
DI 10.1016/j.isprsjprs.2007.07.007
PG 21
WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing;
Imaging Science & Photographic Technology
SC Physical Geography; Geology; Remote Sensing; Imaging Science &
Photographic Technology
GA 283TY
UT WOS:000254660600003
ER
PT J
AU Consiglio, MC
Carreno, V
Williams, DM
Munoz, C
AF Consiglio, Maria C.
Carreno, Victor
Williams, Daniel M.
Munoz, Cesar
TI Conflict prevention and separation assurance in Small Aircraft
Transportation Systems
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT AIAA 5th Aviation, Technology, Integration, and Operations Conference
(ATIO)
CY SEP 26-28, 2005
CL Arlington, VA
SP AIAA
AB A multilayer approach to the prevention of conflicts due to the loss of aircraft-to-aircraft separation that relies on procedures and onboard automation was implemented as part of the Small Aircraft Transportation Systems Higher-Volume-Operations concept. The multilayer system gives pilots support and guidance during the execution of normal operations and advance warning for procedure deviations or off-nominal operations. This paper describes the major concept elements of this multilayer approach to separation assurance and conflict prevention and provides the rationale for its design. All the algorithms and functionality described in this paper were implemented in an aircraft simulation in the Air Traffic Operations Laboratory at NASA Langley Research Center and on the NASA Cirrus SR22 research aircraft.
C1 [Consiglio, Maria C.] NASA, Langley Res Ctr, Crew Syst Branch, Hampton, VA 23681 USA.
[Carreno, Victor] NASA, Langley Res Ctr, Safety Crit Avionics Syst Branch, Hampton, VA 23681 USA.
[Williams, Daniel M.] NASA, Langley Res Ctr, Aviat Operat & Evaluat Branch, Hampton, VA 23681 USA.
[Munoz, Cesar] Natl Inst Aerosp, Format Methods Team, Hampton, VA 23666 USA.
RP Consiglio, MC (reprint author), NASA, Langley Res Ctr, Crew Syst Branch, 24 W Taylor St,Mail Stop 152, Hampton, VA 23681 USA.
NR 17
TC 8
Z9 8
U1 0
U2 1
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2008
VL 45
IS 2
BP 353
EP 358
DI 10.2514/1.20586
PG 6
WC Engineering, Aerospace
SC Engineering
GA 285FB
UT WOS:000254761600001
ER
PT J
AU Consiglio, MC
Williams, DM
Murdoch, JL
Adams, CA
AF Consiglio, Maria C.
Williams, Daniel M.
Murdoch, Jennifer L.
Adams, Catherine A.
TI Concept validation experiment for small aircraft transportation system
higher-volume operations
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT AIAA 5th Aviation, Technology, Integration, and Operations Conference
(ATIO)
CY SEP 26-28, 2005
CL Arlington, VA
SP AIAA
AB A human-in-the-loop simulation experiment was conducted at the NASA Langley Research Center's Air Traffic Operations Laboratory in an effort to comprehensively validate tools and procedures intended to enable the small aircraft transportation system higher-volume-operations concept of operations. These procedures were developed with the goal of increasing the rate of operations at nontowered, nonradar airports in near all-weather conditions. A key element of the new design is the establishment of a volume of airspace around designated airports at which pilots accept responsibility for self-separation. Flights operating at these airports are given approach-sequencing information computed by a ground-based automated system. The validation experiment was conducted to determine if a pilot could safety and proficiently fly an airplane while performing the newly developed procedures. Comparative measures of flight path error, perceived workload, and situation awareness were obtained for two types of simulated scenarios. Baseline scenarios were representative of today's system using procedure separation, in which air traffic control grants one approach or departure clearance at a time. Test scenarios represented the newly developed approach and departure procedures. Results from the experiment indicate that low-time pilots were able to fly the test procedures in a simulation environment and maintain self-separation as safely and proficiently as flying today's procedures.
C1 [Consiglio, Maria C.; Adams, Catherine A.] NASA, Langley Res Ctr, Crew Syst Branch, Hampton, VA 23681 USA.
[Williams, Daniel M.; Murdoch, Jennifer L.] NASA, Langley Res Ctr, Aviat Operat & Evaluat Branch, Hampton, VA 23681 USA.
RP Consiglio, MC (reprint author), NASA, Langley Res Ctr, Crew Syst Branch, 24 W Taylor St,Mail Stop 152, Hampton, VA 23681 USA.
NR 15
TC 2
Z9 2
U1 0
U2 2
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2008
VL 45
IS 2
BP 359
EP 365
DI 10.2514/1.20588
PG 7
WC Engineering, Aerospace
SC Engineering
GA 285FB
UT WOS:000254761600002
ER
PT J
AU Davila, CG
Camanho, PP
Turon, A
AF Davila, Carlos G.
Camanho, Pedro P.
Turon, Albert
TI Effective simulation of delamination in aeronautical structures using
shells and cohesive elements
SO JOURNAL OF AIRCRAFT
LA English
DT Article
ID ENERGY-RELEASE RATE; PLATE ELEMENTS; ZONE MODEL; FRACTURE; COMPUTATION;
COMPOSITES; TOUGHNESS; STRESSES; GROWTH; CRACK
AB A cohesive element for shell analysis is presented. The element can be used to simulate the initiation and growth of delaminations between stacked noncoincident layers of shell elements. The procedure to construct the element accounts for the thickness offset by applying the kinematic relations of shell deformation to transform the stiffness and internal force of a zero-thickness cohesive element such that interfacial continuity between the layers is enforced. The procedure is demonstrated by simulating the response and failure of the mixed-mode bending test and a skin-stiffener debond specimen. In addition, it is shown that stacks of shell elements can be used to create effective models to predict the in-plane and delamination failure modes of thick components. The results indicate that simple shell models can retain many of the necessary predictive attributes of much more complex three-dimensional models while providing the computational efficiency that is necessary for design.
C1 [Davila, Carlos G.] NASA, Langley Res Ctr, Durabil Damage Tolerance & Reliabil Branch, Hampton, VA 23602 USA.
[Camanho, Pedro P.] Univ Porto, Fac Engn, Dept Engn Mecan & Gestao Ind, P-4200465 Oporto, Portugal.
[Turon, Albert] Univ Girona, Dept Engn Mecan & Construccio Ind, Girona, Spain.
RP Davila, CG (reprint author), NASA, Langley Res Ctr, Durabil Damage Tolerance & Reliabil Branch, Mail Stop 188E, Hampton, VA 23602 USA.
RI Davila, Carlos/D-8559-2011; AMADE Research Group, AMADE/B-6537-2014;
Balanzat, Josep Costa/C-1017-2014; Turon, Albert/C-6875-2008;
OI AMADE Research Group, AMADE/0000-0002-5778-3291; Turon,
Albert/0000-0002-2554-2653; Camanho, Pedro/0000-0003-0363-5207
NR 35
TC 31
Z9 32
U1 4
U2 21
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2008
VL 45
IS 2
BP 663
EP 672
DI 10.2514/1.32832
PG 10
WC Engineering, Aerospace
SC Engineering
GA 285FB
UT WOS:000254761600034
ER
PT J
AU Soller, BR
Yang, Y
Lee, SMC
Wilson, C
Hagan, RD
AF Soller, Babs R.
Yang, Ye
Lee, Stuart M. C.
Wilson, Cassie
Hagan, R. Donald
TI Noninvasive determination of exercise-induced hydrodgen ion threshold
through direct optical measurement
SO JOURNAL OF APPLIED PHYSIOLOGY
LA English
DT Article
DE pH; anaerobic threshold; near-infrared spectroscopy; cycling; lactate;
carbon dioxide
ID NEAR-INFRARED SPECTROSCOPY; SURFACE HISTIDYL RESIDUES; NORMAL ADULT
HEMOGLOBIN; VENOUS-BLOOD PH; ANAEROBIC THRESHOLD; GAS-EXCHANGE;
REFLECTANCE SPECTROSCOPY; IN-VIVO; SUBMAXIMAL EXERCISE;
OXYGEN-SATURATION
AB The intensity of exercise above which oxygen uptake (Vo(2)) does not account for all of the required energy to perform work has been associated with lactate accumulation in the blood ( lactate threshold, LT) and elevated carbon dioxide output ( gas exchange threshold). An increase in hydrogen ion concentration ([H+]) is approximately concurrent with elevation of blood lactate and CO2 output during exercise. Near-infrared spectra (NIRS) and invasive interstitial fluid pH (pHm) were measured in the flexor digitorum profundus during handgrip exercise to produce a mathematical model relating the two measures with an estimated error of 0.035 pH units. This NIRS pHm model was subsequently applied to spectra collected from the vastus lateralis of 10 subjects performing an incremental-intensity cycle protocol. Muscle oxygen saturation (SmO2) was also calculated from spectra. We hypothesized that a H (+) threshold could be identified for these subjects and that it would be different from but correlated with the LT. Lactate, gas exchange, SmO2, and H (+) thresholds were determined as a function of Vo(2) using bilinear regression. LT was significantly different from both the gas exchange threshold (Delta = 0.27 +/- 0.29 l/ min) and H+ threshold (Delta = 0.29 +/- 0.23 l/ min), but the gas exchange threshold was not significantly different from the H+ threshold (Delta = 0.00 +/- 0.38 l/min). The H+ threshold was strongly correlated with LT (R-2 = 0.95) and the gas exchange threshold (R-2 = 0.85). This initial study demonstrates the feasibility of noninvasive pHm estimations, the determination of H+ threshold, and the relationship between H+ and classical metabolic thresholds during incremental exercise.
C1 [Soller, Babs R.; Yang, Ye] Univ Massachusetts, Sch Med, Dept Anesthesiol, Worcester, MA 01655 USA.
[Lee, Stuart M. C.] Wyle Labs, Houston, TX USA.
[Wilson, Cassie] JES Tech, Houston, TX USA.
[Hagan, R. Donald] NASA, Johnson Space Ctr, Houston, TX USA.
RP Soller, BR (reprint author), Univ Massachusetts, Sch Med, Dept Anesthesiol, 55 Lake Ave N, Worcester, MA 01655 USA.
EM babs.soller@umassmed.edu
NR 43
TC 14
Z9 14
U1 1
U2 10
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 MAR
PY 2008
VL 104
IS 3
BP 837
EP 844
DI 10.1152/japplphysiol.00849.2007
PG 8
WC Physiology; Sport Sciences
SC Physiology; Sport Sciences
GA 271XV
UT WOS:000253822900035
PM 18096753
ER
PT J
AU Collins, MW
Morris, SB
AF Collins, Michael W.
Morris, Scott B.
TI Testing for adverse impact when sample size is small
SO JOURNAL OF APPLIED PSYCHOLOGY
LA English
DT Article
DE selection; adverse impact; significance testing
ID 2X2 CONTINGENCY-TABLES; PERSONAL OPINIONS; CONTROVERSY; HOMOGENEITY
AB Adverse impact evaluations often call for evidence that the disparity between groups in selection rates is statistically significant, and practitioners must choose which test statistic to apply in this situation. To identify the most effective testing procedure, the authors compared several alternate test statistics in terms of Type I error rates and power, focusing on situations with small samples. Significance testing was found to be of limited value because of low power for all tests. Among the alternate test statistics, the widely-used Z-test on the difference between two proportions performed reasonably well, except when sample size was extremely small. A test suggested by G. J. G. Upton (1982) provided slightly better control of Type I error under some conditions but generally produced results similar to the Z-test. Use of the Fisher Exact Test and Yates's continuity-corrected chi-square test are not recommended because of overly conservative Type I error rates and substantially lower power than the Z-test.
C1 [Collins, Michael W.; Morris, Scott B.] IIT, Inst Psychol, Chicago, IL 60616 USA.
RP Collins, MW (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy,Mail Code AH, Houston, TX 77058 USA.
EM michael.w.collins@nasa.gov
NR 20
TC 18
Z9 19
U1 0
U2 15
PU AMER PSYCHOLOGICAL ASSOC
PI WASHINGTON
PA 750 FIRST ST NE, WASHINGTON, DC 20002-4242 USA
SN 0021-9010
J9 J APPL PSYCHOL
JI J. Appl. Psychol.
PD MAR
PY 2008
VL 93
IS 2
BP 463
EP 471
DI 10.1037/0021-9010.93.2.463
PG 9
WC Psychology, Applied; Management
SC Psychology; Business & Economics
GA 275FJ
UT WOS:000254057000018
PM 18361646
ER
PT J
AU Minnis, P
Doelling, DR
Nguyen, L
Miller, WF
Chakrapani, V
AF Minnis, Patrick
Doelling, David R.
Nguyen, Louis
Miller, Walter F.
Chakrapani, Venkatesan
TI Assessment of the visible channel calibrations of the VIRS on TRMM and
MODIS on Aqua and Terra
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID RADIANT ENERGY SYSTEM; IN-FLIGHT CALIBRATION; RADIOMETRIC VALIDATION;
PART I; CLOUDS; CERES; INSTRUMENT; SATELLITE; ORBIT; METHODOLOGY
AB Several recent research satellites carry self-calibrating multispectral imagers that can be used for calibrating operational imagers lacking complete self-calibrating capabilities. In particular, the visible (VIS, 0.65 mu m) channels on operational meteorological satellites are generally calibrated before launch, but require vicarious calibration techniques to monitor the gains and offsets once they are in orbit. To ensure that the self-calibrating instruments are performing as expected, this paper examines the consistencies between the VIS channel (channel 1) reflectances of the Moderate Resolution Imaging Spectroradiometer (MODIS) instruments on the Terra and Aqua satellites and the version 5a and 6 reflectances of the Visible Infrared Scanner (VIRS) on the Tropical Rainfall Measuring Mission using a variety of techniques. These include comparisons of Terra and Aqua VIS radiances with coincident broadband shortwave radiances from the well-calibrated Clouds and the Earth's Radiant Energy System (CERES), time series of deep convective cloud (DCC) albedos, and ray-matching intercalibrations between each of the three satellites. Time series of matched Terra and VIRS data, Aqua and VIRS data, and DCC reflected fluxes reveal that an older version (version 5a, ending in early 2004) of the VIRS calibration produced a highly stable record, while the latest version (version 6) appears to overestimate the sensor gain change by similar to 1% yr(-1) as the result of a manually induced gain adjustment. Comparisons with the CERES shortwave radiances unearthed a sudden change in the Terra MODIS calibration that caused a 1.17% decrease in the gain on 19 November 2003 that can be easily reversed. After correction for these manual adjustments, the trends in the VIRS and Terra channels are no greater than 0.1% yr(-1). Although the results were more ambiguous, no statistically significant trends were found in the Aqua MODIS channel 1 gain. The Aqua radiances are 1% greater, on average, than their Terra counterparts, and after normalization are 4.6% greater than VIRS radiances, in agreement with theoretical calculations. The discrepancy between the two MODIS instruments should be taken into account to ensure consistency between parameters derived from them. With the adjustments, any of the three instruments can serve as references for calibrating other satellites. Monitoring of the calibrations continues in near-real time and the results are available via the World Wide Web.
C1 [Minnis, Patrick; Doelling, David R.; Nguyen, Louis] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
[Miller, Walter F.] Sci Syst & Applicat Inc, Hampton, VA USA.
[Chakrapani, Venkatesan] Hampton Univ, Hampton, VA 23668 USA.
RP Minnis, P (reprint author), NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
EM patrick.minnis-l@nasa.gov
RI Minnis, Patrick/G-1902-2010
OI Minnis, Patrick/0000-0002-4733-6148
NR 27
TC 35
Z9 35
U1 0
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD MAR
PY 2008
VL 25
IS 3
BP 385
EP 400
DI 10.1175/2007JTECHA1021.1
PG 16
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 284XL
UT WOS:000254741100003
ER
PT J
AU Lee, JN
Hameed, S
Shindell, DT
AF Lee, Jae N.
Hameed, Sultan
Shindell, Drew T.
TI The northern annular mode in summer and its relation to solar activity
variations in the GISS ModelE
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE stratosphere; troposphere; summer northern annular mode; solar activity
ID GREENHOUSE-GAS; SIMULATIONS
AB The northern annular mode (NAM) has been successfully used in several studies to understand the variability of the winter atmosphere and its modulation by solar activity. The variability of summer circulation can also be described by the leading empirical orthogonal function (EOF) of geopotential heights. We compare the annular modes of the summer geopotential heights in the northern hemisphere stratosphere and troposphere in the Goddard Institute for Space Studies (GISS) ModelE with those in the National Centers for Environmental Prediction/National Center for Atmospheric Research (NCEP/NCAR) reanalysis. In the stratosphere, the summer NAM obtained from NCEP/NCAR reanalysis as well as from the ModelE simulations has the same sign throughout the northern hemisphere, but shows greater variability at low latitudes. The patterns in both analyses are consistent with the interpretation that low NAM conditions represent an enhancement of the seasonal difference between the summer and the annual averages of geopotential height, temperature and velocity distributions, while the reverse holds for high NAM conditions. Composite analysis of high and low NAM cases in both model and observation suggests that the summer stratosphere is more "summer-like" when the solar activity is near a maximum. This means that the zonal easterly wind flow is stronger and the temperature is higher than normal. Thus increased irradiance favors a low summer NAM. A quantitative comparison of the anti-correlation between the NAM and the solar forcing is presented in the model and in the observation, both of which show lower/higher NAM index in solar maximum/minimum conditions. The temperature fluctuations in simulated solar minimum conditions are greater than in solar maximum throughout the summer stratosphere.
The summer NAM in the troposphere obtained from NCEP/NCAR reanalysis has a dipolar zonal structure with maximum variability over the Asian monsoon region. The corresponding EOF in ModelE has a qualitatively similar structure but with less variability in the Asian monsoon region which is displaced eastward of its observed position. In both the NCEP/NCAR reanalysis and the GCM the negative anomalies associated with the NAM in the Euro-Atlantic and Aleutian island regions are enhanced in the solar minimum conditions, though the results are not statistically significant. (C) 2007 Elsevier Ltd. All rights reserved.
C1 [Lee, Jae N.; Hameed, Sultan] SUNY Stony Brook, Inst Terr & Planetary Atmospheres, Stony Brook, NY 11794 USA.
[Shindell, Drew T.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Shindell, Drew T.] Columbia Univ, New York, NY USA.
RP Lee, JN (reprint author), SUNY Stony Brook, Inst Terr & Planetary Atmospheres, Stony Brook, NY 11794 USA.
EM jaelee@atmsci.msrc.sunysb.edu
RI Shindell, Drew/D-4636-2012
NR 16
TC 4
Z9 6
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD MAR
PY 2008
VL 70
IS 5
BP 730
EP 741
DI 10.1016/j.jastp.2007.10.012
PG 12
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 285ZP
UT WOS:000254815000003
ER
PT J
AU Iraci, LT
Riffel, BG
Robinson, CB
Michelsen, RR
Stephenson, RM
AF Iraci, Laura T.
Riffel, Brent G.
Robinson, Carly B.
Michelsen, Rebecca R.
Stephenson, Rachel M.
TI The acid catalyzed nitration of methanol: formation of methyl nitrate
via aerosol chemistry (vol 58, pg 253, 2007)
SO JOURNAL OF ATMOSPHERIC CHEMISTRY
LA English
DT Correction
C1 [Iraci, Laura T.; Riffel, Brent G.; Robinson, Carly B.; Michelsen, Rebecca R.; Stephenson, Rachel M.] NASA, Ames Res Ctr, Atmospher Sci Branch, Moffett Field, CA 94035 USA.
[Riffel, Brent G.] Univ Calif Davis, Inst Transport Studies, Davis, CA 95616 USA.
[Robinson, Carly B.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA.
[Michelsen, Rebecca R.] Randolph Macon Coll, Dept Chem, Ashland, VA 23005 USA.
[Stephenson, Rachel M.] Univ Calif Los Angeles, Dept Chem & Biochem, Los Angeles, CA 90095 USA.
RP Iraci, LT (reprint author), NASA, Ames Res Ctr, Atmospher Sci Branch, Mail Stop 245-5, Moffett Field, CA 94035 USA.
EM Laura.T.Iraci@NASA.gov
NR 1
TC 0
Z9 0
U1 0
U2 2
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0167-7764
J9 J ATMOS CHEM
JI J. Atmos. Chem.
PD MAR
PY 2008
VL 59
IS 3
BP 237
EP 238
DI 10.1007/s10874-008-9098-x
PG 2
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 332MS
UT WOS:000258087700006
ER
PT J
AU Lin, JL
Lee, MI
Kim, D
Kang, IS
Frierson, DMW
AF Lin, Jia-Lin
Lee, Myong-In
Kim, Daehyun
Kang, In-Sik
Frierson, Dargan M. W.
TI The impacts of convective parameterization and moisture triggering on
AGCM-simulated convectively coupled equatorial waves
SO JOURNAL OF CLIMATE
LA English
DT Article
ID MADDEN-JULIAN OSCILLATION; GENERAL-CIRCULATION MODEL; TROPICAL
INTRASEASONAL OSCILLATIONS; SIMPLE MULTICLOUD PARAMETERIZATION; AIR-SEA
INTERACTION; PART I; LOW-FREQUENCY; KELVIN WAVES; STRATIFORM
INSTABILITY; CUMULUS CONVECTION
AB This study examines the impacts of convective parameterization and moisture convective trigger on convectively coupled equatorial waves simulated by the Seoul National University (SNU) atmospheric general circulation model (AGCM). Three different convection schemes are used, including the simplified Arakawa-Schubert (SAS) scheme, the Kuo (1974) scheme, and the moist convective adjustment (MCA) scheme, and a moisture convective trigger with variable strength is added to each scheme. The authors also conduct a "no convection" experiment with deep convection schemes turned off. Space-time spectral analysis is used to obtain the variance and phase speed of dominant convectively coupled equatorial waves, including the Madden-Julian oscillation (MJO), Kelvin, equatorial Rossby (ER), mixed Rossby-gravity (MRG), and eastward inertio-gravity (EIG) and westward inertio-gravity (WIG) waves.
The results show that both convective parameterization and the moisture convective trigger have significant impacts on AGCM-simulated, convectively coupled equatorial waves. The MCA scheme generally produces larger variances of convectively coupled equatorial waves including the MJO, more coherent eastward propagation of the MJO, and a more prominent MJO spectral peak than the Kuo and SAS schemes. Increasing the strength of the moisture trigger significantly enhances the variances and slows down the phase speeds of all wave modes except the MJO, and usually improves the eastward propagation of the MJO for the Kuo and SAS schemes, but the effect for the MCA scheme is small. The no convection experiment always produces one of the best signals of convectively coupled equatorial waves and the MJO.
C1 [Lin, Jia-Lin] CIRES Climate Diagnost Ctr, Boulder, CO USA.
[Lin, Jia-Lin] NOAA, Earth Syst Res Lab, Boulder, CO USA.
[Lee, Myong-In] NASA, GSFC, Global Modeling & Assimilat Off, Greenbelt, MD USA.
[Kim, Daehyun; Kang, In-Sik] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea.
[Frierson, Dargan M. W.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
RP Lin, JL (reprint author), Ohio State Univ, Dept Geog, Columbus, OH 43210 USA.
EM lin789@osu.edu
RI Frierson, Dargan/F-1763-2010; 안, 민섭/D-9972-2015;
OI Frierson, Dargan/0000-0001-8952-5644; Lee, Myong-In/0000-0001-8983-8624
NR 94
TC 69
Z9 69
U1 0
U2 6
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 MAR
PY 2008
VL 21
IS 5
BP 883
EP 909
DI 10.1175/2007JCLI1790.1
PG 27
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 278DK
UT WOS:000254263700003
ER
PT J
AU Schoeberl, MR
Douglass, AR
Newman, PA
Lait, LR
Lary, D
Waters, J
Livesey, N
Froidevaux, L
Lambert, A
Read, W
Filipiak, MJ
Pumphrey, HC
AF Schoeberl, M. R.
Douglass, A. R.
Newman, P. A.
Lait, L. R.
Lary, D.
Waters, J.
Livesey, N.
Froidevaux, L.
Lambert, A.
Read, W.
Filipiak, M. J.
Pumphrey, H. C.
TI QBO and annual cycle variations in tropical lower stratosphere trace
gases from HALOE and Aura MLS observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID QUASI-BIENNIAL OSCILLATION; WATER-VAPOR; OCCULTATION EXPERIMENT; EOS
MLS; OZONE; SATELLITE; CIRCULATION; TROPOSPHERE; ATMOSPHERE; TRANSPORT
AB We have analyzed thirteen years ( 1993 to 2005) of HALOE and over two years of EOS MLS observations ( September 2004 to December 2006) for QBO and annual cycle trace variations in tropical H2O, HCl, ozone, N2O, CO, HF, and CH4. We use these results to develop the theory explaining both Brewer-Dobson circulation (BDC) and QBO driven fluctuations in tropical trace gases. For H2O, BDC variations drive part of the tropopause annual forcing through annual variations in the temperature as has been shown previously. For CO, the annual variations in the BDC amplify the annual fluctuations in CO at the tropopause as has recently been shown by Randel et al (2007). In both cases, the tropopause signal is carried upward by the mean BDC. For ozone, N2O, HCl and other gases, photochemical processes force fluctuations in the trace gases to be synchronized with annual and QBO variations in the zonal mean residual vertical velocity as is shown using lag correlations.
C1 [Schoeberl, M. R.; Douglass, A. R.; Newman, P. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lait, L. R.; Lary, D.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
[Waters, J.; Livesey, N.; Froidevaux, L.; Lambert, A.; Read, W.] NASA, Jet Propuls Lab, Pasadena, CA USA.
[Filipiak, M. J.; Pumphrey, H. C.] Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland.
RP Schoeberl, MR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM schom@zephyr.gsfc.nasa.gov
RI Lary, David/A-6163-2010; Newman, Paul/D-6208-2012; Douglass,
Anne/D-4655-2012
OI Newman, Paul/0000-0003-1139-2508;
NR 39
TC 46
Z9 46
U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 1
PY 2008
VL 113
IS D5
AR D05301
DI 10.1029/2007JD008678
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 270JB
UT WOS:000253716000001
ER
PT J
AU Wang, PKC
Hadaegh, FY
AF Wang, P. K. C.
Hadaegh, F. Y.
TI Stability analysis of switched dynamical systems with state-space
dilation and contraction
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article; Proceedings Paper
CT AIAA Guidance, Navigation, and Control Conference
CY AUG 21-24, 2006
CL Keystone, CO
ID MULTIPLE LYAPUNOV FUNCTIONS
AB This paper considers switched dynamical systems with state-space dilation and contraction formed by concatenating the states of a set of local dynamical systems or semiflows on state spaces with different dimensions at specified time instants. These systems arise naturally in many aerospace applications, such as multibody dynamic systems involving changes in the degrees of freedom and systems composed of multiple spacecraft with docking and undocking capabilities flying information. The notions of stability of invariant sets in the sense of Lyapunov for usual dynamical systems are extended to this class of switched dynamical systems. Also, the notion of finite-time stability with specified bounds is introduced. Sufficient stability conditions are established for a special class of switched dynamical systems with state-space dilation and contraction. Their application to spacecraft formation stability analysis is discussed.
C1 [Wang, P. K. C.] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA.
[Hadaegh, F. Y.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Wang, PKC (reprint author), Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA.
NR 14
TC 10
Z9 11
U1 0
U2 0
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD MAR-APR
PY 2008
VL 31
IS 2
BP 395
EP 401
DI 10.2514/1.28407
PG 7
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 272RF
UT WOS:000253876600012
ER
PT J
AU Hughes, SP
AF Hughes, Steven P.
TI General method for optimal guidance of spacecraft formations
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
ID RELATIVE MOTION; ELLIPTIC ORBITS; DESIGN; LISA
AB One of the most interesting and challenging aspects of formation guidance algorithm design is the coupling of the orbit design and the science return. The effectiveness of the formation as a science instrument is intimately coupled with the relative geometry and evolution of the collection of spacecraft. Therefore, the science return can be maximized by optimizing the orbit design according to a performance metric relevant to the science mission goals. In this work, we present a general method for optimal formation guidance that is applicable to missions whose performance metric, requirements, and constraints can be cast as functions that are explicitly dependent upon the orbit states and spacecraft relative positions and velocities. The approach is fully nonlinear, accommodates orbital perturbations, and is applicable to multiple flight regimes including highly eccentric, hyperbolic, interplanetary, or libration point orbits. Furthermore, the method is applicable to small formations, as well as large formations and constellations. We present a general form for the cost and constraint functions, and derive their semi-analytic gradients with respect to the formation initial conditions. The gradients are broken down into two types. The first type are gradients of the mission-specific performance metric with respect to formation geometry. The second type are derivatives of the formation geometry with respect to the orbit initial conditions. The fact that these two types of derivatives appear separately allows us to derive and implement a general framework that requires minimal modification to be applied to different missions or mission phases. To illustrate the applicability of the approach, we conclude with applications to two missions: the Magnetospheric Multiscale Mission, and the Laser Interferometer Space Antenna.
C1 NASA, Goddard Space Flight Ctr, Flight Dynam Anal Branch, Greenbelt, MD 20771 USA.
RP Hughes, SP (reprint author), NASA, Goddard Space Flight Ctr, Flight Dynam Anal Branch, Greenbelt, MD 20771 USA.
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
NR 32
TC 10
Z9 11
U1 0
U2 8
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD MAR-APR
PY 2008
VL 31
IS 2
BP 414
EP 423
DI 10.2514/1.23731
PG 10
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 272RF
UT WOS:000253876600014
ER
PT J
AU Markley, FL
AF Markley, F. Landis
TI Unit quaternion from rotation matrix
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
ID DIRECTION-COSINE MATRIX; SINGULARITY-FREE EXTRACTION; VECTOR
OBSERVATIONS
C1 NASA, Goddard Space Flight Ctr, Guidance Navigat & Control Syst Engn Branch, Greenbelt, MD 20771 USA.
RP Markley, FL (reprint author), NASA, Goddard Space Flight Ctr, Guidance Navigat & Control Syst Engn Branch, Code 591, Greenbelt, MD 20771 USA.
NR 17
TC 5
Z9 6
U1 0
U2 4
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD MAR-APR
PY 2008
VL 31
IS 2
BP 440
EP 442
DI 10.2514/1.31730
PG 3
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 272RF
UT WOS:000253876600019
ER
PT J
AU Mehta, SK
Tyring, SK
Gilden, DH
Cohrs, RJ
Leal, MJ
Castro, VA
Feiveson, AH
Ott, CM
Pierson, DL
AF Mehta, Satish K.
Tyring, Stephen K.
Gilden, Donald H.
Cohrs, Randall J.
Leal, Melanie J.
Castro, Victoria A.
Feiveson, Alan H.
Ott, C. Mark
Pierson, Duane L.
TI Varicella-zoster virus in the saliva of patients with herpes zoster
SO JOURNAL OF INFECTIOUS DISEASES
LA English
DT Article; Proceedings Paper
CT 32nd International Herpesvirus Workshop
CY JUL 07-12, 2007
CL Asheville, NC
ID SINE HERPETE; REACTIVATION; INFECTION
AB Fifty-four patients with herpes zoster were treated with valacyclovir. On treatment days 1, 8, and 15, pain was scored and saliva examined for varicella-zoster virus (VZV) DNA. VZV DNA was found in every patient the day treatment was started and later disappeared in 82%. There was a positive correlation between the presence of VZV DNA and pain and between VZV DNA copy number and pain (P<.0005). VZV DNA was present in 1 patient before rash and in 4 after pain resolved and was not present in any of 6 subjects with chronic pain or in 14 healthy subjects. Analysis of human saliva has potential usefulness in the diagnosis of neurological disease produced by VZV without rash.
C1 [Gilden, Donald H.; Cohrs, Randall J.] Univ Colorado, Hlth Sci Ctr, Dept Neurol, Denver, CO 80262 USA.
[Gilden, Donald H.] Univ Colorado, Hlth Sci Ctr, Dept Microbiol, Denver, CO 80262 USA.
[Tyring, Stephen K.] Univ Texas Houston, Hlth Sci Ctr, Houston, TX USA.
[Feiveson, Alan H.; Ott, C. Mark; Pierson, Duane L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Mehta, Satish K.; Leal, Melanie J.; Castro, Victoria A.] Enterprise Advisory Serv Inc, Houston, TX USA.
RP Gilden, DH (reprint author), Univ Colorado, Hlth Sci Ctr, Dept Neurol, Mail Stop B-182,4200 E 9th Ave, Denver, CO 80262 USA.
EM don.gilden@uchsc.edu
FU NIA NIH HHS [AG06127, R01 AG006127, R01 AG006127-20, R37 AG006127];
NINDS NIH HHS [NS32623, P01 NS032623, P01 NS032623-20]
NR 15
TC 41
Z9 43
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0022-1899
J9 J INFECT DIS
JI J. Infect. Dis.
PD MAR 1
PY 2008
VL 197
IS 5
BP 654
EP 657
DI 10.1086/527420
PG 4
WC Immunology; Infectious Diseases; Microbiology
SC Immunology; Infectious Diseases; Microbiology
GA 271FD
UT WOS:000253773400006
PM 18260763
ER
PT J
AU Tahmasebi, F
AF Tahmasebi, Farhad
TI Closure to "Discussion of 'Kinematics of a new high-precision
three-degree-of-freedom parallel manipulator" (2008, ASME J. Mech. Des.,
130, p. 035501)
SO JOURNAL OF MECHANICAL DESIGN
LA English
DT Editorial Material
ID MINIMANIPULATOR
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Tahmasebi, F (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM farhad.tahmasebi@nasa.gov
NR 14
TC 0
Z9 0
U1 0
U2 0
PU ASME-AMER SOC MECHANICAL ENG
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 1050-0472
J9 J MECH DESIGN
JI J. Mech. Des.
PD MAR
PY 2008
VL 130
IS 3
AR 035502
PG 2
WC Engineering, Mechanical
SC Engineering
GA 276MA
UT WOS:000254144900017
ER
PT J
AU Robichaud, DJ
Hodges, JT
Brown, LR
Lisak, D
Maslowski, P
Yeung, LY
Okumura, M
Miller, CE
AF Robichaud, David J.
Hodges, Joseph T.
Brown, Linda R.
Lisak, Daniel
Maslowski, Piotr
Yeung, Laurence Y.
Okumura, Mitchio
Miller, Charles E.
TI Experimental intensity and lineshape parameters of the oxygen A-band
using frequency-stabilized cavity ring-down spectroscopy
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE oxygen; A-band; intensities; cavity ring-down spectroscopy
ID FOURIER-TRANSFORM SPECTROSCOPY; MOLECULAR LINE ABSORPTION; SCATTERING
ATMOSPHERE; QUANTITATIVE MEASUREMENTS; LASER SPECTROSCOPY;
PRESSURE-SHIFT; HIGH-PRECISION; BROADENED HF; O-2; TRANSITIONS
AB Line intensities, self- and air-broadened linewidths, pressure-induced shifts, and collisional narrowing coefficients were measured from 2 <= J'<= 32 in the P branch of the O-2 A-band (12975-13110 cm(-1)) utilizing Galatry line profiles. Spectra were recorded using the frequency-stabilized cavity ring-down spectrometer located at NIST, Gaithersburg, MD with a spectral resolution <0.0001 cm(-1) and noise-equivalent absorption coefficient of 6 x 10(-8) m(-1) Hz(-1/2). Line intensities, obtained from calibrated gas samples for 2 <= X <= 32, are similar to 1% lower than the values in current spectroscopic databases. At higher J(18 <= J' <= 32), the measured air- and self- broadened half widths are up to 20% lower than the extrapolated values given in HITRAN 2004, while corresponding half-widths for 2 <= J' <= 15 are in better agreement. Available self-broadened half widths are fitted to empirical expressions with an rms of 0.8%. We discuss the implications of our results for accurate remote sensing of surface pressure and photon path length distributions. (C) 2008 Published by Elsevier Inc.
C1 [Hodges, Joseph T.; Lisak, Daniel; Maslowski, Piotr] NIST, Proc Measurments Div, Gaithersburg, MD 20899 USA.
[Robichaud, David J.; Yeung, Laurence Y.; Okumura, Mitchio] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
[Brown, Linda R.; Miller, Charles E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lisak, Daniel; Maslowski, Piotr] Uniwersytet Mikolaja Kopernika, Inst Fizyki, PL-87100 Torun, Poland.
RP Hodges, JT (reprint author), NIST, Proc Measurments Div, 100 Bureau Dr, Gaithersburg, MD 20899 USA.
EM joseph.bodges@nist.gov; Linda.R.Brown@jpl.nasa.gov; mo@caltech.edu;
charles.e.miller@jpl.nasa.gov
RI Hodges, Joseph/B-4578-2009; Yeung, Laurence/D-4574-2009; Lisak,
Daniel/E-1470-2014; Maslowski, Piotr/H-4476-2014; Okumura,
Mitchio/I-3326-2013
OI Yeung, Laurence/0000-0001-9901-2607; Maslowski,
Piotr/0000-0001-8882-7106; Okumura, Mitchio/0000-0001-6874-1137
NR 61
TC 49
Z9 48
U1 1
U2 17
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
EI 1096-083X
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD MAR
PY 2008
VL 248
IS 1
BP 1
EP 13
DI 10.1016/j.jms.2007.10.010
PG 13
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 264BI
UT WOS:000253259800001
ER
PT J
AU Thadathil, P
Thoppil, P
Rao, RR
Muraleedharan, PM
Somayajulu, YK
Gopalakrishna, VV
Murtugudde, R
Reddy, GV
Revichandran, C
AF Thadathil, Pankajakshan
Thoppil, Prasad
Rao, R. R.
Muraleedharan, P. M.
Somayajulu, Y. K.
Gopalakrishna, V. V.
Murtugudde, Raghu
Reddy, G. V.
Revichandran, C.
TI Seasonal variability of the observed barrier layer in the Arabian sea
SO JOURNAL OF PHYSICAL OCEANOGRAPHY
LA English
DT Article
ID NORTH INDIAN-OCEAN; EQUATORIAL PACIFIC-OCEAN; SURFACE-LAYER;
MIXED-LAYER; TOGA DECADE; DYNAMICS; MONSOON; SALINITY; MODEL;
THERMODYNAMICS
AB The formation mechanisms of the barrier layer ( BL) and its seasonal variability in the Arabian Sea ( AS) are studied using a comprehensive dataset of temperature and salinity profiles from Argo and other archives for the AS. Relatively thick BL of 20-60 m with large spatial extent is found in the central-southwestern AS ( CSWAS), the convergence zone of the monsoon wind, during the peak summer monsoon ( July-August) and in the southeastern AS ( SEAS) and northeastern AS ( NEAS) during the winter ( January-February). Although the BL in the SEAS has been reported before, the observed thick BL in the central-southwestern AS during the peak summer monsoon and in the northeastern AS during late winter are the new findings of this study. The seasonal variability of BL thickness ( BLT) is closely related to the processes that occur during summer and winter monsoons. During both seasons, the Ekman processes and the distribution of low-salinity waters in the surface layer show a dominant influence on the observed BLT distributions. In addition, Kelvin and Rossby waves also modulate the observed BL thickness in the AS. The relatively low salinity surface water overlying the Arabian Sea high-salinity water ( ASHSW) provides an ideal ground for strong haline stratification in the CSWAS ( during summer monsoon) and in NEAS ( during winter monsoon). During summer, northward advection of equatorial low-salinity water by the Somali Current and the offshore advection of low-salinity water from the upwelling region facilitate the salinity stratification that is necessary to develop the observed BL in the CSWAS. In the SEAS, during winter, the winter monsoon current ( WMC) carries less saline water over relatively high salinity ambient water to form the observed BL there. The winter West India Coastal Current ( WICC) transports the low-salinity water from the SEAS to the NEAS, where it lies over the subducted ASHSW leading to strong haline stratification. Ekman pumping together with the downwelling Kelvin wave in the NEAS deepen the thermocline to cause the observed thick BL in the NEAS.
C1 [Thadathil, Pankajakshan; Muraleedharan, P. M.; Somayajulu, Y. K.; Gopalakrishna, V. V.; Reddy, G. V.] Natl Inst Oceanog, Panaji, Goa, India.
[Thoppil, Prasad] Univ So Mississippi, Dept Marine Sci, Hattiesburg, MS 39406 USA.
[Thoppil, Prasad] NASA, Stenis Space Ctr, Mississippi State, MS USA.
[Rao, R. R.] Naval Phys Oceanog Lab, Kochi, India.
[Murtugudde, Raghu] Univ Maryland, Earth Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Revichandran, C.] Natl Inst Oceanog, Reg Ctr, Kochi, India.
RP Thadathil, P (reprint author), Natl Inst Oceanog, Panaji, Goa, India.
EM pankaj@nio.org
NR 53
TC 15
Z9 15
U1 0
U2 3
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-3670
J9 J PHYS OCEANOGR
JI J. Phys. Oceanogr.
PD MAR
PY 2008
VL 38
IS 3
BP 624
EP 638
DI 10.1175/2007JPO3798.1
PG 15
WC Oceanography
SC Oceanography
GA 276EQ
UT WOS:000254124500005
ER
PT J
AU Walsh, EJ
Banner, ML
Wright, CW
Vandemark, DC
Chapron, B
Jensen, J
Lee, S
AF Walsh, E. J.
Banner, M. L.
Wright, C. W.
Vandemark, D. C.
Chapron, B.
Jensen, J.
Lee, S.
TI The southern ocean waves experiment. Part III: Sea surface slope
statistics and near-nadir remote sensing
SO JOURNAL OF PHYSICAL OCEANOGRAPHY
LA English
DT Article
ID PROBABILITY DENSITY-FUNCTIONS; SPECTRUM SPATIAL VARIATION;
WIND-GENERATED WAVES; ATMOSPHERIC STABILITY; RADAR BACKSCATTER; MODEL;
DEPENDENCE; SCATTERING
AB During the Southern Ocean Waves Experiment (SOWEX), registered ocean wave topography and backscattered power data at Ka band ( 36 GHz) were collected with the NASA Scanning Radar Altimeter ( SRA) off the coast of Tasmania under a wide range of wind and sea conditions, from quiescent to gale-force winds with 9-m significant wave height. Collection altitude varied from 35 m to over 1 km, allowing determination of the sea surface mean square slope ( mss), the directional wave spectrum, and the detailed variation of backscattered power with incidence angle, which deviated from a simple Gaussian scattering model. The non-Gaussian characteristics of the backscatter increased systematically with the mss, suggesting that a global model to characterize Ka-band radar backscatter from the sea surface within 25 of nadir might be possible.
C1 [Walsh, E. J.; Wright, C. W.] NASA, Goddard Space Flight Ctr, Wallops Isl, VA USA.
[Banner, M. L.] Univ New S Wales, Sch Math, Sydney, NSW, Australia.
[Vandemark, D. C.] Univ New Hampshire, Ocean Proc Anal Lab, Durham, NH 03824 USA.
[Chapron, B.] IFREMER, Ctr Brest, Dept Oceanog Spatiale, F-29280 Plouzane, France.
[Jensen, J.] Natl Ctr Atmospher Res, Res Aircraft Facil, Broomfield, CO USA.
[Lee, S.] CSIRO Marine & Atmospher Res, Aspendale, Vic, Australia.
RP Walsh, EJ (reprint author), NOAA, Earth Syst Res Lab, PSD3 325 Broadway, Boulder, CO 80305 USA.
EM edward.walsh@nasa.gov
RI Jensen, Jorgen/C-9211-2009; Chapron, Bertrand/O-6527-2015;
OI Banner, Michael/0000-0002-0799-5341
NR 31
TC 11
Z9 11
U1 1
U2 7
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-3670
EI 1520-0485
J9 J PHYS OCEANOGR
JI J. Phys. Oceanogr.
PD MAR
PY 2008
VL 38
IS 3
BP 670
EP 685
DI 10.1175/2007JPO3771.1
PG 16
WC Oceanography
SC Oceanography
GA 276EQ
UT WOS:000254124500008
ER
PT J
AU Whitacre, JF
Zaghib, K
West, WC
Ratnakumar, BV
AF Whitacre, J. F.
Zaghib, K.
West, W. C.
Ratnakumar, B. V.
TI Dual active material composite cathode structures for Li-ion batteries
SO JOURNAL OF POWER SOURCES
LA English
DT Article
DE mixed active material cathodes; Li battery; LiFePO4; LiNiMnO2; LiCoO2;
hybrid
ID X-RAY-DIFFRACTION; ELECTROCHEMICAL-BEHAVIOR; LAYERED CATHODE;
PERFORMANCE; ELECTRODES; CAPACITY; HYBRID; SPINEL; CELLS; LIMN2O4
AB The efficacy of composite Li-ion battery cathodes made by mixing active materials that possessed either high-rate capability or high specific energy was examined. The cathode structures studied contained carbon-coated LiFePO4 and either Li[Li0.17Mn0.58Ni0.25]O-2 or LiCoO2. These active materials were arranged using three different electrode geometries: fully intermixed, fully separated, or layered. Discharge rate studies, cycle-life evaluation, and electrochemical impedance spectroscopy studies were conducted using coin cell test structures containing Li-metal anodes. Results indicated that electrode configuration was correlated to rate capability and degree of polarization if there was a large differential between the rate capabilities of the two active material species. (C) 2007 Elsevier B.V. All rights reserved.
C1 [Whitacre, J. F.] Carnegie Mellon Univ, Dept Mat Sci & Engn, Pittsburgh, PA 15213 USA.
[Whitacre, J. F.] Carnegie Mellon Univ, Dept Engn & Publ Policy, Pittsburgh, PA 15213 USA.
[Zaghib, K.] Inst Rech Hydro Quebec, Varennes, PQ J3X 1S1, Canada.
[West, W. C.; Ratnakumar, B. V.] CALTECH, Jet Prop Lab, Electrochem Technol Grp, Pasadena, CA 91109 USA.
RP Whitacre, JF (reprint author), Carnegie Mellon Univ, Dept Mat Sci & Engn, Pittsburgh, PA 15213 USA.
EM whitacre@andrew.cmu.edu
NR 31
TC 34
Z9 37
U1 2
U2 54
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-7753
J9 J POWER SOURCES
JI J. Power Sources
PD MAR 1
PY 2008
VL 177
IS 2
BP 528
EP 536
DI 10.1016/j.jpowsour.2007.11.076
PG 9
WC Chemistry, Physical; Electrochemistry; Energy & Fuels; Materials
Science, Multidisciplinary
SC Chemistry; Electrochemistry; Energy & Fuels; Materials Science
GA 272QE
UT WOS:000253873700035
ER
PT J
AU Alahmad, M
Hess, H
Mojarradi, M
West, W
Whitacre, J
AF Alahmad, Mahmoud
Hess, Herb
Mojarradi, Mohammad
West, William
Whitacre, Jay
TI Battery switch array system with application for JPL's rechargeable
micro-scale batteries
SO JOURNAL OF POWER SOURCES
LA English
DT Article
DE battery; battery scheduling; battery system; microbattery; power
management; reconfigurable architecture
AB A battery switch array system is developed for solid-state rechargeable micro-scale lithium batteries, designed and developed by Jet Propulsion Laboratory (JPL), California Institute of Technology, for aerospace applications. The heart of the system is a topology unique in its dynamic reconfiguration ability by providing selective connection and isolation and versatile in its core design by incorporating passive, active or energy storage elements. It allows up to N-batteries to be connected in any desired configuration; providing maximum voltage, maximum capacity and a voltage/capacity ratio. This battery switch array system is part of a power management system that is developed to utilize these features and provide for multiple charging algorithms, real time status information and fault tolerant capabilities. A two microbattery prototype circuit is built using a microprocessor-based controller for verification of the system design and its features. The topology and its features will be explored in this paper to provide methods for modular and scalable energy storage system design. (C) 2007 Elsevier B.V. All rights reserved.
C1 [Alahmad, Mahmoud; Hess, Herb] Univ Idaho, Moscow, ID 83843 USA.
[Mojarradi, Mohammad; West, William; Whitacre, Jay] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Alahmad, M (reprint author), Univ Idaho, Moscow, ID 83843 USA.
EM malahmad2@unl.edu; hhess@ece.uidaho.edu;
Mohammad.M.Mojarradi@JPL.NASA.GOV; W.C.West@JPL.NASA.GOV;
J.F.Whitacre@JPL.NASA.GOV
NR 19
TC 12
Z9 12
U1 0
U2 7
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-7753
J9 J POWER SOURCES
JI J. Power Sources
PD MAR 1
PY 2008
VL 177
IS 2
BP 566
EP 578
DI 10.1016/j.jpowsour.2007.11.053
PG 13
WC Chemistry, Physical; Electrochemistry; Energy & Fuels; Materials
Science, Multidisciplinary
SC Chemistry; Electrochemistry; Energy & Fuels; Materials Science
GA 272QE
UT WOS:000253873700040
ER
PT J
AU Mulenburg, G
AF Mulenburg, Gerald
TI Rainbows & ratholes: Best practices for managing successful projects
SO JOURNAL OF PRODUCT INNOVATION MANAGEMENT
LA English
DT Book Review
C1 [Mulenburg, Gerald] NASA, Washington, DC 20546 USA.
NR 2
TC 0
Z9 0
U1 0
U2 0
PU BLACKWELL PUBLISHING
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND
SN 0737-6782
J9 J PROD INNOVAT MANAG
JI J. Prod. Innov. Manage.
PD MAR
PY 2008
VL 25
IS 2
BP 207
EP 209
DI 10.1111/j.1540-5885.2008.00294_3.x
PG 3
WC Business; Engineering, Industrial; Management
SC Business & Economics; Engineering
GA 268LZ
UT WOS:000253582600010
ER
PT J
AU Titov, E
Gallagher-Rogers, A
Levin, D
Reed, B
AF Titov, E.
Gallagher-Rogers, A.
Levin, D.
Reed, Brian
TI Examination of a collision-limiter direct simulation Monte Carlo method
for micropropulsion applications
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article
ID FLOW; NOZZLES
AB A wide range of flow regimes occur in micronozzles, from the transitional to the continuum regime, which prevents the use of a single computational method such as direct simulation Monte Carlo or computational fluid dynamics and Navier-Stokes. A collision-limiter approach is proposed that extends the applicability of direct simulation Monte Carlo to the continuum regime and can be used to solve a wide range of microelectromechanical system flows when it is coupled with the baseline direct simulation Monte Carlo. A comparison of the results obtained with this computational technique with new experimental data and Navier-Stokes results suggests consistency between experimental and computational methods for three-dimensional microelectromechanical system micronozzles with stagnation pressures on the order of 5 atm. However, the level of agreement was found to vary with the nozzle geometry, suggesting that additional research is needed for both computations and experiments in this flow regime.
C1 [Titov, E.; Gallagher-Rogers, A.; Levin, D.] Penn State Univ, Dept Aerosp Engn, University Pk, PA 16802 USA.
[Reed, Brian] NASA, John H Glenn Res Ctr Lewis Field, Elect Propuls Branch, Cleveland, OH 44135 USA.
RP Titov, E (reprint author), Penn State Univ, Dept Aerosp Engn, University Pk, PA 16802 USA.
NR 27
TC 8
Z9 8
U1 0
U2 3
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0748-4658
J9 J PROPUL POWER
JI J. Propul. Power
PD MAR-APR
PY 2008
VL 24
IS 2
BP 311
EP 321
DI 10.2514/1.28793
PG 11
WC Engineering, Aerospace
SC Engineering
GA 274QW
UT WOS:000254016900018
ER
PT J
AU Leonard, C
Diehr, M
Rosmus, P
Maguire, WC
AF Leonard, C.
Diehr, M.
Rosmus, P.
Maguire, W. C.
TI Radiative transition probabilities in the X-2 Pi(g) state of CO2+
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE carbon dioxide; carbon dioxide cation; dipole moment function;
Renner-Teller effect; rovibronic intensities; radiative; transition
probabilities; thermal emission spectrum; Mars' atmosphere
ID ULTRAVIOLET SPECTROMETER EXPERIMENT; THERMAL EMISSION SPECTROMETER;
TRIATOMIC-MOLECULES; VARIATIONAL METHOD; VIBRONIC STRUCTURE; UPPER
ATMOSPHERE; ENERGY-LEVELS; MARS; BANDS; ION
AB Using ab initio calculated potential energy and electric dipole moment functions, absolute radiative transition probabilities between the rovibronic Renner-Teller states of the electronic ground state X-2 Pi(g) of CO2+ have been evaluated. The rovibronic eigenstates were obtained (up to 6500 cm(-1) and J <= 13/2) from variational calculations including the Renner-Teller and spin-orbit angular momentum couplings. The absolute intensities for the rovibrational states of the neutral CO2 electronic ground state, calculated by a similar approach, are found to be in excellent agreement with experimental data. For CO2+ the presented results are expected to have similar accuracy. It is found that the overtone intensities of the antisymmetric stretching mode of CO2+ are of similar magnitude as the fundamental transitions, in contrast with CO2. The theoretically generated IR-emission spectrum is compared with the limb spectrum of the Mars atmosphere, measured by the Thermal Emission Spectrometer on Mars Global Surveyor. (C) 2007 Elsevier Ltd. All rights reserved.
C1 [Leonard, C.; Diehr, M.; Rosmus, P.] Univ Marne la Vallee, Chim Theor Lab, Marne La Vallee 2, France.
[Maguire, W. C.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
RP Leonard, C (reprint author), Univ Marne la Vallee, Chim Theor Lab, EA 2180,5 Blvd Descartes,Champs Marne 77454, Marne La Vallee 2, France.
EM celine.leonard@univ-mlv.fr
OI LEONARD, Celine/0000-0003-0303-3505
NR 55
TC 8
Z9 8
U1 0
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD MAR
PY 2008
VL 109
IS 4
BP 535
EP 548
DI 10.1016/j.jqsrt.2007.07.011
PG 14
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 242JD
UT WOS:000251720500001
ER
PT J
AU Lattanzi, V
Walters, A
Pearson, JC
Drouin, BJ
AF Lattanzi, Valerio
Walters, Adam
Pearson, John C.
Drouin, Brian J.
TI THz spectrum of monodeuterated methane
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE methane; line positions; deuterated methane; interstellar spectra
ID ELECTRIC DIPOLE MOMENT; OUTER SOLAR-SYSTEM; D/H ISOTOPIC RATIO;
GROUND-STATE; ROTATIONAL SPECTRUM; CH3D; ABUNDANCE; SPECTROSCOPY;
DEUTERIUM; TITAN
AB We report new measurements of the rotational spectrum of monodeuterated methane (CH3D) in the range of 690-1200 GHz which allow for an accurate prediction of all lines in the range of the high-resolution spectrometer of the Herschel Space Observatory. Comparison is also made with the previous analysis based on infrared combination differences. Three lines of (CH3D)-C-13 were measured in natural abundance. (C) 2007 Elsevier Ltd. All rights reserved.
C1 [Pearson, John C.; Drouin, Brian J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lattanzi, Valerio; Walters, Adam] Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France.
[Lattanzi, Valerio] Univ Roma La Sapienza, Dept Phys, Rome, Italy.
RP Drouin, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM brian.j.drouin@jpl.nasa.gov
NR 38
TC 11
Z9 11
U1 0
U2 10
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD MAR
PY 2008
VL 109
IS 4
BP 580
EP 586
DI 10.1016/j.jqsrt.2007.09.002
PG 7
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 242JD
UT WOS:000251720500005
ER
PT J
AU Reda, DC
Wilder, MC
Bogdanoff, DW
Prabhu, DK
AF Reda, D. C.
Wilder, M. C.
Bogdanoff, D. W.
Prabhu, D. K.
TI Transition experiments on blunt bodies with distributed roughness in
hypersonic free flight
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA 45th Aerospace Sciences Meeting and Exhibit
CY JAN 08-11, 2007
CL Reno, NV
SP Amer Inst Aeronaut & Astronaut
ID BOUNDARY-LAYER-TRANSITION
AB Models of hemispherical and blunt large-angle conical geometries were flown in the NASA Ames hypersonic ballistic range to investigate the influence of distributed surface roughness on transition to turbulence. Transition-zone fronts were defined from optically measured global surface temperature distributions. Measurements of preconditioned surface roughness, surface temperature, average transition-front location, and freestream environment were combined with real-gas Navier-Stokes calculations of model flowfields, including laminar boundary-layer development in these flowfields, to transform all data into dimensionless parameters used to correlate transition onset/location on rough blunt bodies in hypersonic flow. A combination of present and previously published results led to the formulation of a transition correlation applicable over all three regimes potentially encountered by an ablating blunt-body heat shield undergoing atmospheric entry: the smooth-wall asymptote, the critical-roughness Reynolds number regime, and the large-roughness/low-Reynolds-number asymptote.
C1 [Reda, D. C.] NASA, Ames Res Ctr, Space Technol Div, Moffett Field, CA 94035 USA.
[Bogdanoff, D. W.; Prabhu, D. K.] ELORET Corp, Sunnyvale, CA 94086 USA.
[Wilder, M. C.] NASA, Ames Res Ctr, Reacting Flow Environm Branch, Moffett Field, CA 94035 USA.
RP Reda, DC (reprint author), NASA, Ames Res Ctr, Space Technol Div, Mail Stop 229-3, Moffett Field, CA 94035 USA.
NR 12
TC 5
Z9 5
U1 2
U2 6
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2008
VL 45
IS 2
BP 210
EP 215
DI 10.2514/1.30288
PG 6
WC Engineering, Aerospace
SC Engineering
GA 285FE
UT WOS:000254761900006
ER
PT J
AU Berry, SA
Horvath, TJ
AF Berry, Scott A.
Horvath, Thomas J.
TI Discrete-roughness transition for hypersonic flight vehicles
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA 45th Aerospace Sciences Meeting and Exhibit
CY JAN 08-11, 2007
CL Reno, NV
SP Amer Inst Aeronaut & Astronaut
ID SHUTTLE ORBITER; TUNNEL
AB The importance of discrete roughness and the correlations developed to predict the onset of boundary-layer transition on hypersonic flight vehicles are discussed. The paper is organized by hypersonic vehicle applications characterized in a general sense by the boundary layer: slender with hypersonic conditions at the edge of the boundary layer, moderately blunt with supersonic, and blunt with subsonic. This paper is intended to be a review of recent discrete-roughness-transition work completed at NASA Langley Research Center in support of agency flight test programs. First, a review is provided of discrete-roughness wind-tunnel data and the resulting correlations that were developed. Then results obtained from flight vehicles (in particular, the recently flown Hyper-X and shuttle missions) are discussed and compared with the ground-based correlations. Based on these comparisons, wind-tunnel-derived roughness criteria are shown to provide a reliable means for predicting transition behavior for flight vehicles.
C1 [Berry, Scott A.; Horvath, Thomas J.] NASA, Langley Res Ctr, Aerothermodynam Branch, Res & Technol Directorate, Hampton, VA 23681 USA.
RP Berry, SA (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, Res & Technol Directorate, Mail Stop 408A, Hampton, VA 23681 USA.
NR 49
TC 15
Z9 16
U1 2
U2 6
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2008
VL 45
IS 2
BP 216
EP 227
DI 10.2514/1.30970
PG 12
WC Engineering, Aerospace
SC Engineering
GA 285FE
UT WOS:000254761900007
ER
PT J
AU Covington, MA
Heinemann, JM
Goldstein, HE
Chen, YK
Terrazas-Salinas, I
Balboni, JA
Olejniczak, J
Martinez, ER
AF Covington, M. A.
Heinemann, J. M.
Goldstein, H. E.
Chen, Y. -K.
Terrazas-Salinas, I.
Balboni, J. A.
Olejniczak, J.
Martinez, E. R.
TI Performance of a low density ablative heat shield material
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA 37th Thermophysics Conference
CY JUN 28-JUL 01, 2004
CL Portland, OR
SP AIAA
AB An evaluation of the Stardust spacecraft forebody heat shield design was conducted to address uncertainties in original development and qualification efforts. Results are reported for additional arc jet tests and analyses done on the ablative and thermal performance of the low density ablative material used in the Stardust design for conditions simulating nominal peak convective heating conditions expected for Stardust sample return capsule Earth entry. Test data were used to adjust iteratively the thermophysical properties in an ablative response computer code to match experimental in-depth temperatures. Ablative recession rates and maximum internal temperatures were satisfactorily predicted by the computer code using derived properties for nominal peak entry heating rates and for rates 37% greater than nominal. Experimental and computer model maximum internal material temperatures were in agreement over a range of conditions and are considered to validate the Stardust heat shield design although measured in-depth temperature data show consistent temperature rise deviations that are not accurately modeled by the computer code. Predicted Stardust heat shield performance based on these results indicates that maximum attachment bond line temperatures will be considerably less than the maximum allowable of 250 degrees C, and total recession will be a small fraction of the as-designed thickness.
C1 [Goldstein, H. E.] NASA, Ames Res Ctr, Adv Comp Sci Res Inst, Moffett Field, CA 94035 USA.
[Covington, M. A.; Heinemann, J. M.] Eloret Corp, Sunnyvale, CA 94086 USA.
NR 14
TC 9
Z9 12
U1 1
U2 9
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2008
VL 45
IS 2
BP 237
EP 247
DI 10.2514/1.12403
PG 11
WC Engineering, Aerospace
SC Engineering
GA 285FE
UT WOS:000254761900009
ER
PT J
AU Grebow, DJ
Ozimek, MT
Howell, KC
Folta, DC
AF Grebow, Daniel J.
Ozimek, Martin T.
Howell, Kathleen C.
Folta, David C.
TI Multibody orbit architectures for lunar south pole coverage
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AAS/AIAA 16th Space Flight Mechanics Meeting
CY JAN 22-26, 2006
CL Tampa, FL
SP Amer Astronaut Soc, Amer Inst Aeronaut & Astronaut
ID 3-DIMENSIONAL PERIODIC-ORBITS; TRAJECTORY DESIGN; HALO ORBITS; POINT;
CONSTELLATIONS
AB A potential ground station at the lunar south pole has prompted studies of orbit architectures that ensure adequate coverage. The creation of multibody orbit constellations begins with an investigation of periodic orbits in the circular restricted three-body problem. A detailed analysis of halo and vertical families, as well as other orbits near the libration points in the vicinity of the moon, suggests that constant communications can be achieved with two spacecraft in combinations of Earth-moon libration-point orbits. In particular, the investigation focuses on nine different orbits from these families with periods ranging from 7 to 16 days. Natural solutions are generated in a full-ephemeris model including solar perturbations. Possible ground stations on the moon and the Earth are established for coverage results and verification of communications capabilities. Preliminary station-keeping costs are also computed for long-term communications with the ground stations.
C1 [Grebow, Daniel J.; Ozimek, Martin T.; Howell, Kathleen C.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA.
[Folta, David C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Grebow, DJ (reprint author), Purdue Univ, Sch Aeronaut & Astronaut, Armstrong Hall,701 W Stadium Ave, W Lafayette, IN 47907 USA.
NR 32
TC 16
Z9 16
U1 0
U2 3
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2008
VL 45
IS 2
BP 344
EP 358
DI 10.2514/1.28738
PG 15
WC Engineering, Aerospace
SC Engineering
GA 285FE
UT WOS:000254761900020
ER
PT J
AU Wilson, JL
Mazzoleni, AP
DeJarnette, FR
Antol, J
Hajos, GA
Strickland, CV
AF Wilson, Jamie L.
Mazzoleni, Andre P.
DeJarnette, Fred R.
Antol, Jeffrey
Hajos, Gregory A.
Strickland, Christopher V.
TI Design, analysis, and testing of Mars Tumbleweed rover concepts
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID DYNAMICS; PLANE; BALL; MOTION; BODY
AB A Mars Tumbleweed rover is a spherical, wind-driven, planetary rover. Compared with conventional rovers, a tumbleweed rover can travel farther faster and gain access to areas such as valleys and chasms that previously were inaccessible. This paper presents design, mathematical modeling, computer simulation, and testing of various tumbleweed rover concepts. In particular, we present wind-tunnel data indicating that a box-kite configuration represents a promising tumbleweed rover design, we show that a working box-kite-type tumbleweed can be constructed, and we show that center of mass variation shows promise as the basis of a tumbleweed rover navigation system.
C1 [Wilson, Jamie L.] N Carolina State Univ, Raleigh, NC 27695 USA.
[Antol, Jeffrey; Hajos, Gregory A.] NASA, Langley Res Ctr, Architectures Missions & Sci Branch, Hampton, VA 23681 USA.
[Strickland, Christopher V.] NASA, Wallops Flight Facil, Mech Syst Branch, Wallops Isl, VA 23337 USA.
NR 46
TC 12
Z9 15
U1 0
U2 9
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2008
VL 45
IS 2
BP 370
EP 382
DI 10.2514/1.31288
PG 13
WC Engineering, Aerospace
SC Engineering
GA 285FE
UT WOS:000254761900022
ER
PT J
AU Britch, SC
Linthicum, KJ
Anyamba, A
Tucker, CJ
Pak, EW
AF Britch, Seth C.
Linthicum, Kenneth J.
Anyamba, Assaf
Tucker, Compton J.
Pak, Edwin W.
CA Mosquito Surveillance Team
TI Long-term surveillance data and patterns of invasion by Aedes albopictus
in Florida
SO JOURNAL OF THE AMERICAN MOSQUITO CONTROL ASSOCIATION
LA English
DT Article
DE Aedes albopictus; Florida; geographic information system (GIS);
mosquito-borne virus; normalized difference vegetation index (NDVI)
ID UNITED-STATES; AEGYPTI; AFRICA; SPREAD; VECTOR; COUNTY; FIELD
AB We used geographic information system (GIS) and long-term mosquito surveillance data from Lake, Pasco, Manatee, and Sarasota Counties, FL, to look at patterns of invasion by Aedes albopictus and concurrent changes in resident Ae. aegypti. We investigated environmental factors associated with population changes in these species with the use of satellite climate data. Aedes aegypti densities attenuated rapidly following the arrival of Ae. albopictus in most counties, yet both species persisted in equilibrium in Manatee County. We discuss the relative importance of rainfall, habitat, and proximity to urban areas in the population dynamics of these species in sympatry.
C1 [Britch, Seth C.; Linthicum, Kenneth J.] USDA ARS, Ctr Med Agr & Vet Entomol, Gainesville, FL 32608 USA.
[Anyamba, Assaf; Tucker, Compton J.; Pak, Edwin W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mosquito Surveillance Team] Manatee Cty Mosquito Control Dist, Palmetto, FL 34220 USA.
[Mosquito Surveillance Team] Lake Cty Mosquito & Aquat Plant Management, Tavares, FL 32778 USA.
[Mosquito Surveillance Team] Pasco Cty Mosquito Control Dist, Odessa, FL 33556 USA.
[Mosquito Surveillance Team] Sarasota Cty Mosquito Control Dist, Sarasota, FL 34233 USA.
RP Britch, SC (reprint author), USDA ARS, Ctr Med Agr & Vet Entomol, 1600-1700 SW 23rd Dr, Gainesville, FL 32608 USA.
RI Valle, Ruben/A-7512-2013
NR 17
TC 15
Z9 16
U1 2
U2 11
PU AMER MOSQUITO CONTROL ASSOC
PI EATONTOWN
PA P O BOX 234, EATONTOWN, NJ 07724-0234 USA
SN 8756-971X
J9 J AM MOSQUITO CONTR
JI J. Am. Mosq. Control Assoc.
PD MAR
PY 2008
VL 24
IS 1
BP 115
EP 120
DI 10.2987/5594.1
PG 6
WC Entomology
SC Entomology
GA 280FH
UT WOS:000254410300020
PM 18437824
ER
PT J
AU Tesfaye, S
Rowan, MG
Mueller, K
Trudgill, BD
Harding, DJ
AF Tesfaye, S.
Rowan, M. G.
Mueller, K.
Trudgill, B. D.
Harding, D. J.
TI Relay and accommodation zones in the Dobe and Hanle grabens, central
Afar, Ethiopia and Djibouti
SO JOURNAL OF THE GEOLOGICAL SOCIETY
LA English
DT Article
ID NORMAL-FAULT SYSTEMS; AFRICAN RIFT SYSTEM; HYDROCARBON EXPLORATION;
SEGMENT LINKAGE; BLOCK ROTATION; EAST-AFRICA; RAMPS; DISPLACEMENT;
EXTENSION; GEOMETRY
AB The right-stepping Dobe and Hanle grabens display a variety of structures that serve to transfer extensional displacement. These structures range from relay zones between overlapping fault segments to accommodation zones between interacting rift segments. The study reveals the presence of three examples of displacement transfer structures: a breached relay zone, a large-scale accommodation zone that is partially breached, and a composite zone that combines elements of both. All three examples exhibit common structural elements. First, dipping ramps develop between horizontal horst blocks and graben floors. Second, these ramps are cut by numerous faults, most of which are antithetic to the ramps and the graben boundary faults. The antithetic faults bound elongate blocks that are rotated into the grabens. Third, crosscutting faults partially or completely link the en echelon or overlapping graben boundary faults. The identification of precursory structures (mode I fractures) at the leading edge of the Dobe-Hanle accommodation zone breaching faults suggest that the breaching process may be continuing. The spatial alignment from north to south of the crosscutting faults, open fractures and lineaments indicates that the breaching process is progressing from the Dobe graben towards the Hanle graben.
C1 [Tesfaye, S.] Lincoln Univ, Cooperat Res Program, Jefferson City, MO 65102 USA.
[Rowan, M. G.] Rowan Consulting Inc, Boulder, CO 80302 USA.
[Mueller, K.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA.
[Trudgill, B. D.] Colorado Sch Mines, Dept Geol & Geol Engn, Golden, CO 80401 USA.
[Harding, D. J.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
RP Tesfaye, S (reprint author), Lincoln Univ, Cooperat Res Program, 104 Foster Hall,820 Chestnut St, Jefferson City, MO 65102 USA.
EM tesfayes@lincolnu.edu
NR 49
TC 7
Z9 7
U1 2
U2 9
PU GEOLOGICAL SOC PUBL HOUSE
PI BATH
PA UNIT 7, BRASSMILL ENTERPRISE CENTRE, BRASSMILL LANE, BATH BA1 3JN, AVON,
ENGLAND
SN 0016-7649
J9 J GEOL SOC LONDON
JI J. Geol. Soc.
PD MAR
PY 2008
VL 165
BP 535
EP 547
DI 10.1144/0016-76492007-093
PN 2
PG 13
WC Geosciences, Multidisciplinary
SC Geology
GA 272RC
UT WOS:000253876200008
ER
PT J
AU Ramon, ML
Nelson, PA
De Martini, E
Walsh, WJ
Bernardi, G
AF Ramon, Marina L.
Nelson, Peter A.
De Martini, Edward
Walsh, William J.
Bernardi, Giacomo
TI Phylogeography, historical demography, and the role of post-settlement
ecology in two Hawaiian damselfish species
SO MARINE BIOLOGY
LA English
DT Article
ID PELAGIC LARVAL DURATION; CORAL-REEF FISH; GREAT-BARRIER-REEF;
DASCYLLUS-ALBISELLA; MARINE POPULATIONS; GENETIC-STRUCTURE;
SPATIAL-PATTERNS; DISPERSAL; MITOCHONDRIAL; CONNECTIVITY
AB Coral reef fish generally have relatively sedentary juvenile and adult phases and a presumed highly dispersive pelagic larval phase, yet previous studies that have tried to relate pelagic larval duration (PLD) to population structure have given inconsistent results. In the present study, the population structures of two damselfishes, Stegastes fasciolatus and Dascyllus albisella, were examined using mitochondrial control region sequences. The two species have similar PLDs (similar to 25 and 27 days respectively), but consistently differ in their settlement preferences, habitat, and densities in populations throughout the Hawaiian Archipelago, from Hawaii north to Kure Atoll, and south to Johnston Atoll. Information on habitat preferences and population densities were collected between September 2000 and October 2002, and tissue samples for the genetic studies were collected between January and April 2004. Based on the differences in habitat and abundance of the two species, the expectation was that S. fasciolatus would have high genetic variability but little population structure compared to D. albisella, and this was largely confirmed. Stegastes fasciolatus had little population structure in most of the Hawaiian Islands, and D. albisella showed evidence of strong population structure throughout its range. An exception to this pattern was the large difference between the Kure Atoll population of S. fasciolatus and all others. These results suggest that the interaction of several biological factors (e.g. species-specific spawning habitat and season) with environmental factors (e.g. seasonal wind and current patterns) may have more influence on population structure than single life history characteristics, such as the PLD.
C1 [Ramon, Marina L.; Nelson, Peter A.] Univ Calif Santa Cruz, Dept Ecol & Evolut Biol, Santa Cruz, CA 95060 USA.
[Nelson, Peter A.] HT Harvey & Associates, Los Gatos, CA 95032 USA.
[De Martini, Edward] SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Ntal Ocean & Atmospher Adm, Honolulu, HI 96822 USA.
[Walsh, William J.] Div Aquat Resources, Kailua, HI 96740 USA.
RP Bernardi, G (reprint author), Univ Calif Santa Cruz, Dept Ecol & Evolut Biol, 100 Shaffer Rd, Santa Cruz, CA 95060 USA.
EM bernardi@biology.ucsc.edu
RI Bernardi, Giacomo/F-6346-2011
OI Bernardi, Giacomo/0000-0002-8249-4678
NR 61
TC 20
Z9 20
U1 1
U2 11
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 0025-3162
EI 1432-1793
J9 MAR BIOL
JI Mar. Biol.
PD MAR
PY 2008
VL 153
IS 6
BP 1207
EP 1217
DI 10.1007/s00227-007-0894-7
PG 11
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 265HZ
UT WOS:000253351000019
ER
PT J
AU Roth, DJ
Seebo, JP
Winfree, WP
AF Roth, Don J.
Seebo, Jeffrey P.
Winfree, William P.
TI Simultaneous Noncontact Precision Imaging of Microstructural and
Thickness Variation in Dielectric Materials Using Terahertz Energy
SO MATERIALS EVALUATION
LA English
DT Article
DE space shuttle; external tank; thermal protection system; sprayon foam
insulation; terahertz; velocity; thickness; density
ID ULTRASONIC VELOCITY
AB This paper describes a noncontact, single-sided terahertz electromagnetic measurement and imaging technique that simultaneously characterizes microstructural (for example, spatially lateral density) and thickness variation in dielectric (insulating) materials. The technique was demonstrated for two materials - space shuttle external tank spray-on foam insulation and a silicon nitride ceramic. It is believed that this technique can be used for current and future NASA thermal protection systems and other dielectric material testing applications, where microstructural and thickness variation require precision mapping. Scaling up to more complex shapes, such as cylindrical structures and structures with beveled regions, would appear to be feasible.
C1 [Roth, Don J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Seebo, Jeffrey P.] NASA, Langley Res Ctr, Lockheed Martin Space Syst Co, Hampton, VA 23681 USA.
RP Roth, DJ (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM donald.j.roth@nasa.gov
NR 26
TC 4
Z9 4
U1 0
U2 1
PU AMER SOC NONDESTRUCTIVE TEST
PI COLUMBUS
PA 1711 ARLINGATE LANE PO BOX 28518, COLUMBUS, OH 43228-0518 USA
SN 0025-5327
J9 MATER EVAL
JI Mater. Eval.
PD MAR
PY 2008
VL 66
IS 3
BP 325
EP 331
PG 7
WC Materials Science, Characterization & Testing
SC Materials Science
GA 373NJ
UT WOS:000260978400004
ER
PT J
AU Connolly, HC
Smith, C
Benedix, G
Folco, L
Righter, K
Zipfel, J
Yamaguchi, A
Aoudjehane, HC
AF Connolly, Harold C., Jr.
Smith, Caroline
Benedix, Gretchen
Folco, Luigi
Righter, Kevin
Zipfel, Jutta
Yamaguchi, Akira
Aoudjehane, Hasnaa Chennaoui
TI The Meteoritical Bulletin, No. 93, 2008 March
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
AB In this edition of the Meteoritical Bulletin, 1443 approved meteorite names with their relevant data are reported, one from a specific location within Africa, 2 11 from Northwest Africa, 5 from KOR-EAMET, 598 from the Chinese Antarctic Expedition, 23 from the Americas, 151 from Asia, three from Australia, two from Europe, two from NOVA, and 447 from ANSMET that were not reported in the Meteoritical Bulletin no. 87. Also reported are 4 falls frorn the Americas. Sonic highlights of approved meteorites are 10 lunar (including NWA 5000, an 11.528 kg sample), 3 Martian, 4 irons (one from Indonesia), 2 ureilites, 5 mesosiderites, I pallasite, 6 brachinites, 3 CV3s, 4 CO3s, 8 CMs, 12 CK3s, and many more. Finally, the Committee on Nomenclature of the Meteoritical Society announces two new names series in North America.
C1 [Connolly, Harold C., Jr.] CUNY, Dept Phys Sci, Kingsborough Community Coll, Brooklyn, NY 11235 USA.
[Connolly, Harold C., Jr.] CUNY, Grad Sch, Brooklyn, NY 11235 USA.
[Connolly, Harold C., Jr.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA.
[Connolly, Harold C., Jr.] Univ Arizona, Lunar & Planetary Lab, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Smith, Caroline; Benedix, Gretchen] Nat Hist Museum, Dept Mineral, London SW7 5BD, England.
[Folco, Luigi] Museo Nazl Antartide, I-53100 Siena, Italy.
[Righter, Kevin] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Zipfel, Jutta] Forsch Inst, Sekt Meteoritenforsch, D-60325 Frankfurt, Germany.
[Zipfel, Jutta] Nat Museum Senckenberg, D-60325 Frankfurt, Germany.
[Yamaguchi, Akira] Natl Inst Polar Res, Antarctic Meteorite Res Ctr, Tokyo 1738515, Japan.
[Aoudjehane, Hasnaa Chennaoui] Univ Hassan II Casablanca, Fac Sci, Dept Geol, Casablanca, Morocco.
RP Connolly, HC (reprint author), CUNY, Dept Phys Sci, Kingsborough Community Coll, 2001 Oriental Blvd, Brooklyn, NY 11235 USA.
EM meteorite@kingsborough.edu
OI Benedix, Gretchen/0000-0003-0990-8878
NR 3
TC 23
Z9 23
U1 3
U2 5
PU METEORITICAL SOC
PI FAYETTEVILLE
PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD MAR
PY 2008
VL 43
IS 3
BP 571
EP 632
PG 62
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 339GQ
UT WOS:000258566500010
ER
PT J
AU Leeuw, TK
Tsyboulski, DA
Nikolaev, PN
Bachilo, SM
Arepalli, S
Weisman, RB
AF Leeuw, Tonya K.
Tsyboulski, Dmitri A.
Nikolaev, Pavel N.
Bachilo, Sergei M.
Arepalli, Sivaram
Weisman, R. Bruce
TI Strain measurements on individual single-walled carbon nanotubes in a
polymer host: Structure-dependent spectral shifts and load transfer
SO NANO LETTERS
LA English
DT Article
ID COMPOSITES; PHOTOLUMINESCENCE; FLUORESCENCE; STRENGTH
AB The fluorescence spectra of individual semiconducting single-walled carbon nanotubes embedded in polymer films were measured during the application of controlled stretching and compressive strains. Nanotube band gaps were found to shift in systematic patterns that depend on the (n,m) structural type and are in excellent agreement with the predictions of theoretical models. Loss of nanotube - host adhesion was revealed by abrupt irregularities in plots of spectral shift vs strain.
C1 [Leeuw, Tonya K.; Tsyboulski, Dmitri A.; Bachilo, Sergei M.; Weisman, R. Bruce] Rice Univ, Dept Chem, Richard E Smalley Inst Nanoscale Sci & Technol, Houston, TX 77005 USA.
[Leeuw, Tonya K.; Tsyboulski, Dmitri A.; Bachilo, Sergei M.; Weisman, R. Bruce] Rice Univ, Ctr Biol Environm Nanotechnol, Houston, TX 77005 USA.
[Nikolaev, Pavel N.; Arepalli, Sivaram] NASA, Lyndon B Johnson Space Ctr, ERC Inc, Houston, TX 77058 USA.
RP Weisman, RB (reprint author), Rice Univ, Dept Chem, Richard E Smalley Inst Nanoscale Sci & Technol, 6100 Main St, Houston, TX 77005 USA.
EM weisman@rice.edu
RI Arepalli, Sivaram/A-5372-2010;
OI Weisman, R. Bruce/0000-0001-8546-9980
NR 28
TC 39
Z9 39
U1 8
U2 23
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1530-6984
J9 NANO LETT
JI Nano Lett.
PD MAR
PY 2008
VL 8
IS 3
BP 826
EP 831
DI 10.1021/nl072861c
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 273QS
UT WOS:000253947400011
PM 18298093
ER
PT J
AU Wolff, JA
Ramos, FC
Hart, GL
Patterson, JD
Brandon, AD
AF Wolff, J. A.
Ramos, F. C.
Hart, G. L.
Patterson, J. D.
Brandon, A. D.
TI Columbia River flood basalts from a centralized crustal magmatic system
SO NATURE GEOSCIENCE
LA English
DT Article
ID LARGE IGNEOUS PROVINCES; OS ISOTOPE SYSTEMATICS; YELLOWSTONE HOTSPOT;
PACIFIC-NORTHWEST; PLUME HEAD; MANTLE; ORIGIN; CONTAMINATION; VOLCANISM;
PLATEAU
AB The Columbia River Basalt Group in the northwestern United States(1), comprising about 230,000 cubic kilometres of rock, exhibits unusual patterns in lava distribution, geochemistry and its apparent relationship to regional tectonics. Consequently, there is little consensus on the origin of its magmas(2-12). Here, we examine the isotopic ratios of Sr, Nd, Pb and Os and trace-element abundances in Columbia River basalts. The results suggest that most of the lava was produced when magma derived from a mantle plume assimilated continental crust in a central magma chamber system located at the boundary between the North American craton and the accreted terranes of Idaho and Oregon. Other, related basalts are the product of mixing between the mantle plume and different types of regional upper mantle. Magma was then transported over a wide region by an extensive network of dykes, a process that has been identified in other flood basalt provinces as well(13). Interactions of the plume with surrounding upper mantle, and of mantle-derived magmas with regional crust, provide a relatively simple(6,7,9,14,15) model to explain the more unusual features of the main-phase Columbia River Basalts.
C1 [Wolff, J. A.; Hart, G. L.] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA.
[Ramos, F. C.; Patterson, J. D.] Cent Washington Univ, Dept Geol Sci, Ellensburg, WA 98926 USA.
[Brandon, A. D.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Wolff, JA (reprint author), Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA.
EM jawolff@mail.wsu.edu
NR 30
TC 41
Z9 41
U1 2
U2 23
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 MAR
PY 2008
VL 1
IS 3
BP 177
EP 180
DI 10.1038/ngeo124
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 309AZ
UT WOS:000256433400016
ER
PT J
AU Sullivan, BM
Davies, P
Hodgdon, KK
Salamone, JA
Pilon, A
AF Sullivan, Brenda M.
Davies, Patricia
Hodgdon, Kathleen K.
Salamone, Joseph A.
Pilon, Anthony
TI Realism assessment of sonic boom simulators
SO NOISE CONTROL ENGINEERING JOURNAL
LA English
DT Article
ID LOUDNESS; NOISE
AB Developments in small supersonic aircraft design are predicted to result in low-intensity sonic booms. Booms generated by current aircraft are similar to those that led to the ban on commercial supersonic flight over the US, so are unsuitable for parametric studies of psychoacoustic response to low-intensity booms. Therefore, simulators have been used to study the impact of predicted low-intensity sonic booms. However, simulators have been criticized because, when simulating conventional-level booms, the sounds were observed to be unrealistic by people experienced in listening to sonic booms. Thus, two studies were conducted to measure the perceived realism of three sonic boom simulators. Experienced listeners rated the realism of conventional sonic boom signatures when played in these simulators. The effects on perceived realism of factors such as duration of post-boom noise, exclusion of very low frequency components, inclusion of ground reflections, and type of simulator were examined. Duration of post-boom noise was found to have a strong effect on perceived realism, while type of simulator had a weak effect. It was determined that post-boom noise had to be at least 1.5 seconds long for the sound to be rated very realistic. Loudness level did not affect realism for the range of sounds played in the tests (80-93 dB ASEL). (C) 2008 Institute of Noise Control Engineering.
C1 [Sullivan, Brenda M.] NASA, Langley Res Ctr, Struct Acoust Branch, Hampton, VA 23681 USA.
[Davies, Patricia] Purdue Univ, Sch Mech Engn, Ray W Herrick Labs, W Lafayette, IN 47907 USA.
[Hodgdon, Kathleen K.] Penn State Univ, Appl Res Lab, State Coll, PA 16801 USA.
[Salamone, Joseph A.] Gulfstream Aerosp Corp, Savannah, GA 31407 USA.
[Pilon, Anthony] Lockheed Martin Aeronaut Co, Adv Dev Programs, Palmdale, CA 93599 USA.
RP Sullivan, BM (reprint author), NASA, Langley Res Ctr, Struct Acoust Branch, Mail Stop 463, Hampton, VA 23681 USA.
EM brenda.m.suillivan@nasa.gov; daviesp@ecn.purdue.edu; kkh2@psu.edu;
joe.salamone@gulfstream.com; tony.pilon@lmco.com
NR 25
TC 2
Z9 2
U1 0
U2 0
PU INST NOISE CONTROL ENGINEERING
PI AMES
PA IOWA STATE UNIV, COLLEGE ENGINEERING, 212 MARSTON HALL, AMES, IA
50011-2152 USA
SN 0736-2501
J9 NOISE CONTROL ENG J
JI Noise Control Eng. J.
PD MAR-APR
PY 2008
VL 56
IS 2
BP 141
EP 157
DI 10.3397/1.2919547
PG 17
WC Acoustics; Engineering, Multidisciplinary
SC Acoustics; Engineering
GA 309KT
UT WOS:000256460000005
ER
PT J
AU Mariani, F
Orsini, S
Candidi, M
Marcucci, MF
Acuna, M
Musmann, G
Ness, NF
AF Mariani, F.
Orsini, S.
Candidi, M.
Marcucci, M. F.
Acuna, M.
Musmann, G.
Ness, N. F.
TI On the current circulation about a high-voltage s/c: Two more
case-studies by the TSS-1R tethered satellite mission
SO NUOVO CIMENTO DELLA SOCIETA ITALIANA DI FISICA C-GEOPHYSICS AND SPACE
PHYSICS
LA English
DT Article
ID FIELD
AB Magnetic field observations by the TEMAG experiment on the TSS-1R satellite for two events of constant stimulated current along the tether are discussed. Previous evidence of a complex, unexpected, electric azimuthal current circulation in close proximity of the high-voltage spacecraft is further supported and complemented. While previous events cover time intervals shorter than a spill cycle, the two new ones allow a complete coverage for a full spin cycle. The reed of deeper theoretical approach as well as of more experimental observations is stressed.
C1 [Mariani, F.] Univ Roma Tor Vergata, Dipartimento Fis, Rome, Italy.
[Orsini, S.; Candidi, M.; Marcucci, M. F.] INAF CNR, Ist Fis Spazio Interplanetario, Rome, Italy.
[Acuna, M.] NASA, GSFC, Greenbelt, MD 20771 USA.
[Musmann, G.] Tech Univ Carolo Wilhelmina Braunschweig, Braunschweig, Germany.
[Ness, N. F.] Univ Delaware, Newark, DE USA.
RP Mariani, F (reprint author), Univ Roma Tor Vergata, Dipartimento Fis, Rome, Italy.
EM franco.mariani@roma2.infn.it
NR 5
TC 1
Z9 1
U1 0
U2 0
PU SOC ITALIANA FISICA
PI BOLOGNA
PA VIA SARAGOZZA, 12, I-40123 BOLOGNA, ITALY
SN 1124-1896
J9 NUOVO CIMENTO C
JI Nuovo Cimento Soc. Ital. Fis. C-Geophys. Space Phys.
PD MAR-APR
PY 2008
VL 31
IS 2
BP 135
EP 141
DI 10.1393/ncc/i2008-10287-3
PG 7
GA 393PZ
UT WOS:000262386500002
ER
PT J
AU Lagerloef, G
Colomb, FR
Le Vine, D
Wentz, F
Yueh, S
Ruf, C
Lilly, J
Gunn, J
Chao, Y
deCharon, A
Feldman, G
Swift, C
AF Lagerloef, Gary
Colomb, F. Raul
Le Vine, David
Wentz, Frank
Yueh, Simon
Ruf, Christopher
Lilly, Jonathan
Gunn, John
Chao, Yi
deCharon, Annette
Feldman, Gene
Swift, Calvin
TI THE AQUARIUS/SAC-D MISSION: DESIGNED TO MEET THE SALINITY REMOTE-SENSING
CHALLENGE
SO OCEANOGRAPHY
LA English
DT Article
ID SEA-SURFACE SALINITY; L-BAND; OCEAN SALINITY; SMOS MISSION; SPACE;
RETRIEVAL; MODEL
C1 [Lagerloef, Gary] NASA, Aquarius Miss Earth & Space Res, Seattle, WA USA.
[Colomb, F. Raul] CONAE, Argentine Space Agcy, Buenos Aires, DF, Argentina.
[Le Vine, David] NASA, Goddard Space Flight Ctr, Instrument Sci Branch, NASA Aquarius Miss, Greenbelt, MD 20771 USA.
[Wentz, Frank] Remote Sensing Syst, Santa Rosa, CA USA.
[Yueh, Simon; Chao, Yi] NASA, Jet Prop Lab, Pasadena, CA USA.
[Ruf, Christopher] Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA.
[Lilly, Jonathan; Gunn, John] Earth & Space Res, Seattle, WA USA.
[deCharon, Annette] Bigelow Lab Ocean Sci, West Boothbay Harbor, ME USA.
[Feldman, Gene] NASA, Goddard Space Flight Ctr, SeaWiFS, Greenbelt, MD 20771 USA.
[Swift, Calvin] Univ Massachusetts, Amherst, MA 01003 USA.
RP Lagerloef, G (reprint author), NASA, Aquarius Miss Earth & Space Res, Seattle, WA USA.
EM lager@esr.org
RI Ruf, Christopher/I-9463-2012
NR 23
TC 197
Z9 205
U1 0
U2 12
PU OCEANOGRAPHY SOC
PI ROCKVILLE
PA P.O. BOX 1931, ROCKVILLE, MD USA
SN 1042-8275
J9 OCEANOGRAPHY
JI Oceanography
PD MAR
PY 2008
VL 21
IS 1
BP 68
EP 81
PG 14
WC Oceanography
SC Oceanography
GA 382XJ
UT WOS:000261638400012
ER
PT J
AU Boyer, T
Carton, J
Chao, Y
Gordon, A
Johnson, G
Lagerloef, G
Large, B
Riser, S
Schmitt, R
AF Boyer, Tim
Carton, Jim
Chao, Yi
Gordon, Arnold
Johnson, Greg
Lagerloef, Gary
Large, Bill
Riser, Steve
Schmitt, Ray
CA CLIVAR Salinity Working Grp
TI What's Next for Salinity?
SO OCEANOGRAPHY
LA English
DT Article
C1 [Carton, Jim] Univ Maryland, College Pk, MD 20742 USA.
[Chao, Yi] NASA, Jet Prop Lab, Washington, DC USA.
[Gordon, Arnold] Columbia Univ, Lamont Doherty Earth Observ, New York, NY 10027 USA.
[Riser, Steve] Univ Washington, Seattle, WA 98195 USA.
[Schmitt, Ray] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
EM rschmitt@whoi.edu
RI carton, james/C-4807-2009
OI carton, james/0000-0003-0598-5198
FU NASA
FX The Salinity Working Group recognizes Cathy Stephens and David Legler of
the US CLIVAR Office as well as Eric Lindstrom of NASA for their Support
activities.
NR 0
TC 0
Z9 1
U1 0
U2 2
PU OCEANOGRAPHY SOC
PI ROCKVILLE
PA P.O. BOX 1931, ROCKVILLE, MD USA
SN 1042-8275
J9 OCEANOGRAPHY
JI Oceanography
PD MAR
PY 2008
VL 21
IS 1
BP 82
EP 85
PG 4
WC Oceanography
SC Oceanography
GA 382XJ
UT WOS:000261638400013
ER
PT J
AU Hofmann, E
Druon, JN
Fennel, K
Friedrichs, M
Haidvogel, D
Lee, C
Mannino, A
McClain, C
Najjar, R
O'Reilly, J
Pollard, D
Previdi, M
Seitzinger, S
Siewert, J
Signorini, S
Wilkin, J
AF Hofmann, Eileen
Druon, Jean-Noel
Fennel, Katja
Friedrichs, Marjorie
Haidvogel, Dale
Lee, Cindy
Mannino, Antonio
McClain, Charles
Najjar, Raymond
O'Reilly, John
Pollard, David
Previdi, Michael
Seitzinger, Sybil
Siewert, John
Signorini, Sergio
Wilkin, John
CA USECoS Team
TI EASTERN US CONTINENTAL SHELF CARBON BUDGET Integrating Models, Data
Assimilation, and Analysis
SO OCEANOGRAPHY
LA English
DT Article
ID DISSOLVED ORGANIC-CARBON; CZCS-CHLOROPHYLL IMAGERY; WARM-CORE RING;
ATLANTIC BIGHT; OCEAN COLOR; ECOSYSTEM MODEL; DEEP-OCEAN; MATTER;
PHYTOPLANKTON; PARTICULATE
C1 [Hofmann, Eileen] Old Dominion Univ, Dept Ocean Earth & Atmospher Sci, Norfolk, VA USA.
[Druon, Jean-Noel; Mannino, Antonio; McClain, Charles] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fennel, Katja] Dalhousie Univ, Dept Oceanog, Halifax, NS, Canada.
[Friedrichs, Marjorie] Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA.
[Haidvogel, Dale; Previdi, Michael; Seitzinger, Sybil; Wilkin, John] Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08903 USA.
[Lee, Cindy] SUNY Stony Brook, Marine Sci Res Ctr, Stony Brook, NY 11794 USA.
[Najjar, Raymond; Siewert, John] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[O'Reilly, John] NOAA, Natl Marine Fisheries Serv, Narragansett Lab, Narragansett, RI 02882 USA.
[Pollard, David] Penn State Univ, Earth & Environm Syst Inst, State Coll, PA USA.
[Signorini, Sergio] Sci Applicat Int Corp, Beltsville, MD USA.
RP Hofmann, E (reprint author), Old Dominion Univ, Dept Ocean Earth & Atmospher Sci, Norfolk, VA USA.
EM hofmann@ccpo.odu.edu
RI Fennel, Katja/A-7470-2009; Lee, Cindy/B-1456-2009; Wilkin,
John/E-5343-2011; Mannino, Antonio/I-3633-2014;
OI Fennel, Katja/0000-0003-3170-2331; Lee, Cindy/0000-0002-7608-6213;
Wilkin, John/0000-0002-5444-9466; Friedrichs,
Marjorie/0000-0003-2828-7595
FU National Aeronautics and Space Administration Interdisciplinary Science
Program
FX The USECoS project is Supported by the National Aeronautics and Space
Administration Interdisciplinary Science Program.
NR 65
TC 19
Z9 19
U1 0
U2 12
PU OCEANOGRAPHY SOC
PI ROCKVILLE
PA P.O. BOX 1931, ROCKVILLE, MD USA
SN 1042-8275
J9 OCEANOGRAPHY
JI Oceanography
PD MAR
PY 2008
VL 21
IS 1
BP 86
EP 104
PG 19
WC Oceanography
SC Oceanography
GA 382XJ
UT WOS:000261638400014
ER
PT J
AU Trigwell, S
Biris, AS
Sims, RA
Mazumder, MK
AF Trigwell, Steve
Biris, A. S.
Sims, Robert A.
Mazumder, Malay K.
TI Effects of powder velocity and contact materials on tribocharging of
polymer powders for powder coating applications
SO PARTICULATE SCIENCE AND TECHNOLOGY
LA English
DT Article
DE back corona; charge-to-mass; Faraday penetration; powders; tribocharging
ID ELECTRIFICATION
AB Electrostatic powder deposition using corona charging is widely used in a plethora of industrial applications. Disadvantages of this technique are back corona onset and the Faraday penetration limitation. Another method to charge powders is to use tribochargers. Tribocharging depends upon the work function difference between the contacting materials and generates bipolarly charged particles. In this study, acrylic and epoxy powders were fluidized and charged by passing through stainless steel, copper, aluminum, and polycarbonate static mixers, respectively. The particle velocity and powder flow rate were varied to determine their effect on the net charge-to-mass ratio (Q/M) acquired by the powders. The Q/M increased rapidly with velocities between 1.5 to 2.5 m/s and stabilized for higher velocities but decreased with increasing powder flow rate at a constant velocity. The net positive or negative charge on each powder was determined to be dependant on the charger material. The use of an aluminum charger (net negative charge) in combination with a PTFE finger nozzle (net positive charge) resulted in a net powder Q/M of -0.05 mu C/g. The generation of an ion-free powder cloud with high bipolar charge but overall charge density of almost zero is anticipated to provide a better coverage of recessed areas.
C1 [Trigwell, Steve] NASA, Kennedy Space Ctr, Electrostat & Surface Phys Lab, ASRC Aerosp 24, Kennedy Space Ctr, FL 32899 USA.
[Biris, A. S.; Sims, Robert A.; Mazumder, Malay K.] Univ Arkansas, Dept Appl Sci, Little Rock, AR 72204 USA.
RP Trigwell, S (reprint author), NASA, Kennedy Space Ctr, Electrostat & Surface Phys Lab, ASRC Aerosp 24, Mail Stop ASRC-20, Kennedy Space Ctr, FL 32899 USA.
EM steven.trigwell-l@nasa.gov
RI Biris, Alexandru/A-8507-2010
NR 16
TC 4
Z9 4
U1 1
U2 3
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA
SN 0272-6351
J9 PARTICUL SCI TECHNOL
JI Part. Sci. Technol.
PD MAR-APR
PY 2008
VL 26
IS 2
BP 145
EP 157
DI 10.1080/02726350801890946
PG 13
WC Engineering, Chemical
SC Engineering
GA 286HL
UT WOS:000254836900005
ER
PT J
AU Huang, SL
Rich, PM
Crabtree, RL
Potter, CS
Fu, PD
AF Huang, Shengli
Rich, Paul M.
Crabtree, Robert L.
Potter, Christopher S.
Fu, Pinde
TI Modeling monthly near-surface air temperature from solar radiation and
lapse rate: Application over complex terrain in Yellowstone National
Park
SO PHYSICAL GEOGRAPHY
LA English
DT Article
DE montane ecosystem; solar radiation; surface temperature; Yellowstone
National Park
ID INTERPOLATION; PRECIPITATION; SIMULATION; VEGETATION; ECOSYSTEM;
REGIONS; SITES
AB Spatially distributed surface temperature over complex topography is important to many ecological processes, but it varies spatially and temporally in complex ways and is difficult to measure at landscape scales at tens of meters resolution. Our goal is to develop a methodology that accurately predicts Surface temperature in mountain ecosystems. First, we modeled monthly incoming solar radiation (insolation) based on topography and observed variation in atmospheric conditions, and accounting for site latitude, elevation, and Surface orientation (slope and aspect), daily and seasonal shifts in sun angle, and effects of shadows cast by surrounding topography. Then we investigated the ability to predict monthly average temperature from lapse rates together with energy input from insolation. Monthly lapse rates are not constant and have a seasonal variation. Monthly temperature is not highly correlated with the corresponding monthly insolation; however, it is highly correlated with a one-month-lag insolation, enabling calculation of a lag-corrected linear regression. We used this regression to calculate 30 m resolution surface temperature maps for mountain areas at Yellowstone National Park. The comparison between our modeled temperature and observed temperature shows the mean average errors range from 0.90 degrees C to 1.49 degrees C. Our approach, with consideration of influences of topography and variable atmospheric conditions on energy from insolation, and with appropriate time lags, greatly improves the ability to calculate spatially distributed temperature regimes in complex terrain.
C1 [Huang, Shengli; Potter, Christopher S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Huang, Shengli; Crabtree, Robert L.] Yellowstone Ecol Res Ctr, Bozeman, MT 59718 USA.
[Rich, Paul M.] Creekside Ctr Earth Observat, Menlo Pk, CA 94025 USA.
[Fu, Pinde] ESRI Inc, Redlands, CA 92373 USA.
RP Huang, SL (reprint author), NASA, Ames Res Ctr, Mail Stop 242-4, Moffett Field, CA 94035 USA.
FU NASA [NNS06AA23G]
FX We thank NASA for providing the financial support (contract No.
NNS06AA23G). This research was also supported by an appointment to the
NASA Postdoctoral Program at the Ames Research Center, administered by
Oak Ridge Associated Universities through a contract with NASA. We also
thank Mrs. Met Peng for collecting and pre-processing weather data and
Mrs. Diane Ehernberger for carefully improving the English.
NR 38
TC 18
Z9 20
U1 2
U2 13
PU BELLWETHER PUBL LTD
PI COLUMBIA
PA 8640 GUILFORD RD, STE 200, COLUMBIA, MD 21046 USA
SN 0272-3646
J9 PHYS GEOGR
JI Phys. Geogr.
PD MAR-APR
PY 2008
VL 29
IS 2
BP 158
EP 178
DI 10.2747/0272-3646.29.2.158
PG 21
WC Environmental Sciences; Geography, Physical; Geosciences,
Multidisciplinary; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Physical Geography; Geology;
Meteorology & Atmospheric Sciences
GA 352PE
UT WOS:000259508500004
ER
PT J
AU Abbott, B
Abbott, R
Adhikari, R
Agresti, J
Ajith, P
Allen, B
Amin, R
Anderson, SB
Anderson, WG
Arain, M
Araya, M
Armandula, H
Ashley, M
Aston, S
Aufmuth, P
Aulbert, C
Babak, S
Ballmer, S
Bantilan, H
Barish, BC
Barker, C
Barker, D
Barr, B
Barriga, P
Barton, MA
Bayer, K
Belczynski, K
Berukoff, SJ
Betzwieser, J
Beyersdorf, PT
Bhawal, B
Bilenko, IA
Billingsley, G
Biswas, R
Black, E
Blackburn, K
Blackburn, L
Blair, D
Bland, B
Bogenstahl, J
Bogue, L
Bork, R
Boschi, V
Bose, S
Brady, PR
Braginsky, VB
Brau, JE
Brinkmann, M
Brooks, A
Brown, DA
Bullington, A
Bunkowski, A
Buonanno, A
Burmeister, O
Busby, D
Butler, WE
Byer, RL
Cadonati, L
Cagnoli, G
Camp, JB
Cannizzo, J
Cannon, K
Cantley, CA
Cao, J
Cardenas, L
Carter, K
Casey, MM
Castaldi, G
Cepeda, C
Chalkley, E
Charlton, P
Chatterji, S
Chelkowski, S
Chen, Y
Chiadini, F
Chin, D
Chin, E
Chow, J
Christensen, N
Clark, J
Cochrane, P
Cokelaer, T
Colacino, CN
Coldwell, R
Coles, M
Conte, R
Cook, D
Corbitt, T
Coward, D
Coyne, D
Creighton, JDE
Creighton, TD
Croce, RP
Crooks, DRM
Cruise, AM
Csatorday, P
Cumming, A
Dalrymple, J
D'Ambrosio, E
Danzmann, K
Davies, G
Daw, E
Debra, D
Degallaix, J
Degree, M
Delker, T
Demma, T
Dergachev, V
Desai, S
DeSalvo, R
Dhurandhar, S
Daiz, M
Dickson, J
Di Credico, A
Diederichs, G
Dietz, A
Ding, H
Doomes, EE
Drever, RWP
Dumas, JC
Dupuis, RJ
Dwyer, JG
Ehrens, P
Espinoza, E
Etzel, T
Evans, M
Evans, T
Fairhurst, S
Fan, Y
Fazi, D
Fejer, MM
Finn, LS
Fiumara, V
Fotopoulos, N
Franzen, A
Franzen, KY
Freise, A
Frey, R
Fricke, T
Fritschel, P
Frolov, VV
Fyffe, M
Galdi, V
Ganezer, KS
Garofoli, J
Gholami, I
Giaime, JA
Giampanis, S
Giardina, KD
Goda, K
Goetz, E
Goggin, L
Gonzalez, G
Gossler, S
Grant, A
Gras, S
Gray, C
Gray, M
Greenhalgh, J
Gretarsson, AM
Grosso, R
Grote, H
Grunewald, S
Guenther, M
Gustafson, R
Hage, B
Hammer, D
Hanna, C
Hanson, J
Harms, J
Harry, G
Harstad, E
Hayler, T
Heefner, J
Heinzel, G
Heng, IS
Heptonstall, A
Heurs, M
Hewitson, M
Hirose, E
Hoak, D
Hosken, D
Hough, J
Howell, E
Hoyland, D
Huttner, SH
Ingram, D
Innerhofer, E
Ito, M
Itoh, Y
Ivanov, A
Jackrel, D
Jennrich, O
Johnson, B
Johnson, WW
Johnston, WR
Jones, DI
Jones, G
Jones, R
Ju, L
Kalmus, P
Kalogera, V
Kasprzyk, D
Katsavounidis, E
Kawabe, K
Kawamura, S
Kawazoe, F
Kells, W
Keppel, DG
Khalili, FY
Killow, CJ
Kim, C
King, P
Kissel, JS
Klimenko, S
Kokeyama, K
Kondrashov, V
Kopparapu, RK
Kozak, D
Krishnan, B
Kwee, P
Lam, PK
Landry, M
Lantz, B
Lazzarini, A
Lee, B
Lei, M
Leiner, J
Leonhardt, V
Leonor, I
Libbrecht, K
Libson, A
Lindquist, P
Lockerbie, NA
Logan, J
Longo, M
Lormand, M
Lubinski, M
Luck, H
Machenschalk, B
MacInnis, M
Mageswaran, M
Mailand, K
Malec, M
Mandic, V
Marano, S
Marka, S
Markowitz, J
Maros, E
Martin, I
Marx, JN
Mason, K
Matone, L
Matta, V
Mavalvala, N
McCarthy, R
McClelland, DE
McGuire, SC
McHugh, M
McKenzie, K
McNabb, JWC
McWilliams, S
Meier, T
Melissinos, A
Mendell, G
Mercer, RA
Meshkov, S
Messaritaki, E
Messenger, CJ
Meyers, D
Mikhailov, E
Mitra, S
Mitrofanov, VP
Mitselmakher, G
Mittleman, R
Miyakawa, O
Mohanty, S
Moreno, G
Mossavi, K
MowLowry, C
Moylan, A
Mudge, D
Mueller, G
Mukherjee, S
Muller-Ebhardt, H
Munch, J
Murray, P
Myers, E
Myers, J
Nagano, S
Nash, T
Newton, G
Nishizawa, A
Nocera, F
Numata, K
Nutzman, P
O'Reilly, B
O'Shaughnessy, R
Ottaway, DJ
Overmier, H
Owen, BJ
Pan, Y
Papa, MA
Parameshwaraiah, V
Parameswariah, C
Patel, P
Pedraza, M
Penn, S
Pierro, V
Pinto, IM
Pitkin, M
Pletsch, H
Plissi, MV
Postiglione, F
Prix, R
Quetschke, V
Raab, F
Rabeling, D
Radkins, H
Rahkola, R
Rainer, N
Rakhmanov, M
Ramsunder, M
Rawlins, K
Ray-Majumder, S
Re, V
Regimbau, T
Rehbein, H
Reid, S
Reitze, DH
Ribichini, L
Richman, S
Riesen, R
Riles, K
Rivera, B
Robertson, NA
Robinson, C
Robinson, EL
Roddy, S
Rodriguez, A
Rogan, AM
Rollins, J
Romano, JD
Romie, J
Rong, H
Route, R
Rowan, S
Rudieger, A
Ruet, L
Russell, P
Ryan, K
Sakata, S
Samidi, M
de la Jordana, LS
Sandberg, V
Sanders, GH
Sannibale, V
Saraf, S
Sarin, P
Sathyaprakash, BS
Sato, S
Saulson, PR
Savage, R
Savov, P
Sazonov, A
Schediwy, S
Schilling, R
Schnabel, R
Schofield, R
Schutz, BF
Schwinberg, P
Scott, SM
Searle, AC
Sears, B
Seifert, F
Sellers, D
Sengupta, AS
Shawhan, P
Shoemaker, DH
Sibley, A
Sidles, JA
Siemens, X
Sigg, D
Sinha, S
Sintes, AM
Slagmolen, BJJ
Slutsky, J
Smith, JR
Smith, MR
Somiya, K
Strain, KA
Strand, NE
Strom, DM
Stuver, A
Summerscales, TZ
Sun, KX
Sung, M
Sutton, PJ
Sylvestre, J
Takahashi, H
Takamori, A
Tanner, DB
Tarallo, M
Taylor, R
Taylor, R
Thacker, J
Thorne, KA
Thorne, KS
Thuring, A
Tinto, M
Tokmakov, KV
Torres, C
Torrie, C
Traylor, G
Trias, M
Tyler, W
Ugolini, D
Ungarelli, C
Urbanek, K
Vahlbruch, H
Vallisneri, M
Van Den Broeck, C
van Putten, M
Varvella, M
Vass, S
Vecchio, A
Veitch, J
Veitch, P
Villar, A
Vorvick, C
Vyachanin, SP
Waldman, SJ
Wallace, L
Ward, H
Ward, R
Watts, K
Webber, D
Weidner, A
Weinert, M
Weinstein, A
Weiss, R
Wen, L
Wen, S
Wette, K
Whelan, JT
Whitbeck, DM
Whitcomb, SE
Whiting, BF
Wiley, S
Wilkinson, C
Willems, PA
Williams, L
Willke, B
Wilmut, I
Winkler, W
Wipf, CC
Wise, S
Wiseman, AG
Woan, G
Woods, D
Wooley, R
Worden, J
Wu, W
Yakushin, I
Yamamoto, H
Yan, Z
Yoshida, S
Yunes, N
Zaleski, KD
Zanolin, M
Zhang, J
Zhang, L
Zhao, C
Zotov, N
Zucker, M
Muhlen, HZ
Zweizig, J
Hild, S
AF Abbott, B.
Abbott, R.
Adhikari, R.
Agresti, J.
Ajith, P.
Allen, B.
Amin, R.
Anderson, S. B.
Anderson, W. G.
Arain, M.
Araya, M.
Armandula, H.
Ashley, M.
Aston, S.
Aufmuth, P.
Aulbert, C.
Babak, S.
Ballmer, S.
Bantilan, H.
Barish, B. C.
Barker, C.
Barker, D.
Barr, B.
Barriga, P.
Barton, M. A.
Bayer, K.
Belczynski, K.
Berukoff, S. J.
Betzwieser, J.
Beyersdorf, P. T.
Bhawal, B.
Bilenko, I. A.
Billingsley, G.
Biswas, R.
Black, E.
Blackburn, K.
Blackburn, L.
Blair, D.
Bland, B.
Bogenstahl, J.
Bogue, L.
Bork, R.
Boschi, V.
Bose, S.
Brady, P. R.
Braginsky, V. B.
Brau, J. E.
Brinkmann, M.
Brooks, A.
Brown, D. A.
Bullington, A.
Bunkowski, A.
Buonanno, A.
Burmeister, O.
Busby, D.
Butler, W. E.
Byer, R. L.
Cadonati, L.
Cagnoli, G.
Camp, J. B.
Cannizzo, J.
Cannon, K.
Cantley, C. A.
Cao, J.
Cardenas, L.
Carter, K.
Casey, M. M.
Castaldi, G.
Cepeda, C.
Chalkley, E.
Charlton, P.
Chatterji, S.
Chelkowski, S.
Chen, Y.
Chiadini, F.
Chin, D.
Chin, E.
Chow, J.
Christensen, N.
Clark, J.
Cochrane, P.
Cokelaer, T.
Colacino, C. N.
Coldwell, R.
Coles, M.
Conte, R.
Cook, D.
Corbitt, T.
Coward, D.
Coyne, D.
Creighton, J. D. E.
Creighton, T. D.
Croce, R. P.
Crooks, D. R. M.
Cruise, A. M.
Csatorday, P.
Cumming, A.
Dalrymple, J.
D'Ambrosio, E.
Danzmann, K.
Davies, G.
Daw, E.
DeBra, D.
Degallaix, J.
Degree, M.
Delker, T.
Demma, T.
Dergachev, V.
Desai, S.
DeSalvo, R.
Dhurandhar, S.
Daiz, M.
Dickson, J.
Di Credico, A.
Diederichs, G.
Dietz, A.
Ding, H.
Doomes, E. E.
Drever, R. W. P.
Dumas, J. -C.
Dupuis, R. J.
Dwyer, J. G.
Ehrens, P.
Espinoza, E.
Etzel, T.
Evans, M.
Evans, T.
Fairhurst, S.
Fan, Y.
Fazi, D.
Fejer, M. M.
Finn, L. S.
Fiumara, V.
Fotopoulos, N.
Franzen, A.
Franzen, K. Y.
Freise, A.
Frey, R.
Fricke, T.
Fritschel, P.
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de la Jordana, L. Sancho
Sandberg, V.
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Wiley, S.
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Willems, P. A.
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Willke, B.
Wilmut, I.
Winkler, W.
Wipf, C. C.
Wise, S.
Wiseman, A. G.
Woan, G.
Woods, D.
Wooley, R.
Worden, J.
Wu, W.
Yakushin, I.
Yamamoto, H.
Yan, Z.
Yoshida, S.
Yunes, N.
Zaleski, K. D.
Zanolin, M.
Zhang, J.
Zhang, L.
Zhao, C.
Zotov, N.
Zucker, M.
Muehlen, H. zur
Zweizig, J.
Hild, S.
TI Search for gravitational waves associated with 39 gamma-ray bursts using
data from the second, third, and fourth LIGO runs
SO PHYSICAL REVIEW D
LA English
DT Article
ID 25 APRIL 1998; SHORT-DURATION GRBS; SIGNAL-TO-NOISE; CORE-COLLAPSE;
REDSHIFT DISTRIBUTIONS; UNUSUAL SUPERNOVA; FORMATION RATES;
STAR-FORMATION; NEUTRON-STARS; ERROR BOX
AB We present the results of a search for short-duration gravitational-wave bursts associated with 39 gamma-ray bursts (GRBs) detected by gamma-ray satellite experiments during LIGO's S2, S3, and S4 science runs. The search involves calculating the crosscorrelation between two interferometer data streams surrounding the GRB trigger time. We search for associated gravitational radiation from single GRBs, and also apply statistical tests to search for a gravitational-wave signature associated with the whole sample. For the sample examined, we find no evidence for the association of gravitational radiation with GRBs, either on a single-GRB basis or on a statistical basis. Simulating gravitational-wave bursts with sine-Gaussian waveforms, we set upper limits on the root-sum-square of the gravitational-wave strain amplitude of such waveforms at the times of the GRB triggers. We also demonstrate how a sample of several GRBs can be used collectively to set constraints on population models. The small number of GRBs and the significant change in sensitivity of the detectors over the three runs, however, limits the usefulness of a population study for the S2, S3, and S4 runs. Finally, we discuss prospects for the search sensitivity for the ongoing S5 run, and beyond for the next generation of detectors.
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Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Ottaway,
David/J-5908-2015; Postiglione, Fabio/O-4744-2015; Messaritaki,
Eirini/D-7393-2016; Sigg, Daniel/I-4308-2015; Pinto,
Innocenzo/L-3520-2016; Kawazoe, Fumiko/F-7700-2011; Freise,
Andreas/F-8892-2011; Kawabe, Keita/G-9840-2011; Tarallo,
Marco/B-2096-2012; Finn, Lee Samuel/A-3452-2009; Agresti,
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Li/C-2623-2013
OI Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636;
Howell, Eric/0000-0001-7891-2817; LONGO, Maurizio/0000-0001-8325-4003;
Pierro, Vincenzo/0000-0002-6020-5521; Ward, Robert/0000-0001-5503-5241;
Whelan, John/0000-0001-5710-6576; Fairhurst,
Stephen/0000-0001-8480-1961; Lueck, Harald/0000-0001-9350-4846; Lam,
Ping Koy/0000-0002-4421-601X; Galdi, Vincenzo/0000-0002-4796-3600;
Sylvestre, Julien/0000-0001-8136-4348; McClelland,
David/0000-0001-6210-5842; Strain, Kenneth/0000-0002-2066-5355; Aulbert,
Carsten/0000-0002-1481-8319; Messaritaki, Eirini/0000-0002-9917-4160;
Freise, Andreas/0000-0001-6586-9901; MATTA,
VINCENZO/0000-0002-2046-4027; MARANO, Stefano/0000-0002-5307-0980;
Whiting, Bernard F/0000-0002-8501-8669; Veitch,
John/0000-0002-6508-0713; Papa, M.Alessandra/0000-0002-1007-5298;
Boschi, Valerio/0000-0001-8665-2293; Biswas, Rahul/0000-0002-0774-8906;
Pinto, Innocenzo M./0000-0002-2679-4457; Stuver,
Amber/0000-0003-0324-5735; Nishizawa, Atsushi/0000-0003-3562-0990;
Zweizig, John/0000-0002-1521-3397; O'Shaughnessy,
Richard/0000-0001-5832-8517; Pitkin, Matthew/0000-0003-4548-526X;
Chiadini, Francesco/0000-0002-9339-8622; Vecchio,
Alberto/0000-0002-6254-1617; Postiglione, Fabio/0000-0003-0628-3796;
Sigg, Daniel/0000-0003-4606-6526; Tarallo, Marco/0000-0001-5169-4987;
Finn, Lee Samuel/0000-0002-3937-0688; Agresti, Juri/0000-0001-6119-2470;
Allen, Bruce/0000-0003-4285-6256; Zhao, Chunnong/0000-0001-5825-2401;
NR 76
TC 50
Z9 50
U1 2
U2 13
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 MAR
PY 2008
VL 77
IS 6
AR 062004
DI 10.1103/PhysRevD.77.062004
PG 22
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 282CF
UT WOS:000254544500008
ER
PT J
AU Abbott, B
Abbott, R
Adhikari, R
Agresti, J
Ajith, P
Allen, B
Amin, R
Anderson, SB
Anderson, WG
Arain, M
Araya, M
Armandula, H
Ashley, M
Aston, S
Aufmuth, P
Aulbert, C
Babak, S
Ballmer, S
Bantilan, H
Barish, BC
Barker, C
Barker, D
Barr, B
Barriga, P
Barton, MA
Bayer, K
Belczynski, K
Betzwieser, J
Beyersdorf, PT
Bhawal, B
Bilenko, IA
Billingsley, G
Biswas, R
Black, E
Blackburn, K
Blackburn, L
Blair, D
Bland, B
Bogenstahl, J
Bogue, L
Bork, R
Boschi, V
Bose, S
Brady, PR
Braginsky, VB
Brau, JE
Brinkmann, M
Brooks, A
Brown, DA
Bullington, A
Bunkowski, A
Buonanno, A
Burmeister, O
Busby, D
Butler, WE
Byer, RL
Cadonati, L
Cagnoli, G
Camp, JB
Cannizzo, J
Cannon, K
Cantley, CA
Cao, J
Cardenas, L
Carter, K
Casey, MM
Castaldi, G
Cepeda, C
Chalkey, E
Charlton, P
Chatterji, S
Chelkowski, S
Chen, Y
Chiadini, F
Chin, D
Chin, E
Chow, J
Christensen, N
Clark, J
Cochrane, P
Cokelaer, T
Colacino, CN
Coldwell, R
Conte, R
Cook, D
Corbitt, T
Coward, D
Coyne, D
Creighton, JDE
Creighton, TD
Croce, RP
Crooks, DRM
Cruise, AM
Cumming, A
Dalrymple, J
D'Ambrosio, E
Danzmann, K
Davies, G
Debra, D
Degallaix, J
Degree, M
Demma, T
Dergachev, V
Desai, S
DeSalvo, R
Dhurandhar, S
Diaz, M
Dickson, J
Di Credico, A
Diederichs, G
Dietz, A
Doomes, EE
Drever, RWP
Dumas, JC
Dupuis, RJ
Dwyer, JG
Ehrens, P
Espinoza, E
Etzel, T
Evans, M
Evans, T
Fairhurst, S
Fan, Y
Fazi, D
Fejer, MM
Finn, LS
Fiumara, V
Fotopoulos, N
Franzen, A
Franzen, KY
Freise, A
Frey, R
Fricke, T
Fritschel, P
Frolov, VV
Fyffe, M
Galdi, V
Ganezer, KS
Garofoli, J
Gholami, I
Giaime, JA
Giampanis, S
Giardina, KD
Goda, K
Goetz, E
Goggin, L
Gonzalez, G
Gossler, S
Grant, A
Gras, S
Gray, C
Gray, M
Greenhalgh, J
Gretarsson, AM
Grosso, R
Grote, H
Grunewald, S
Guenther, M
Gustafson, R
Hage, B
Hammer, D
Hanna, C
Hanson, J
Harms, J
Harry, G
Harstad, E
Hayler, T
Heefner, J
Heng, IS
Heptonstall, A
Heurs, M
Hewitson, M
Hild, S
Hirose, E
Hoak, D
Hosken, D
Hough, J
Howell, E
Hoyland, D
Huttner, SH
Ingram, D
Innerhofer, E
Ito, M
Itoh, Y
Ivanov, A
Jackrel, D
Johnson, B
Johnson, WW
Jones, DI
Jones, G
Jones, R
Ju, L
Kalmus, P
Kalogera, V
Kasprzyk, D
Katsavounidis, E
Kawabe, K
Kawamura, S
Kawazoe, F
Kells, W
Keppel, DG
Khalili, FY
Kim, C
King, P
Kissel, JS
Klimenko, S
Kokeyama, K
Kondrashov, V
Kopparapu, RK
Kozak, D
Krishnan, B
Kwee, P
Lam, PK
Landry, M
Lantz, B
Lazzarini, A
Lee, B
Lei, M
Leiner, J
Leonhardt, V
Leonor, I
Libbrecht, K
Lindquist, P
Lockerbie, NA
Longo, M
Lormand, M
Lubinski, M
Luck, H
Machenschalk, B
MacInnis, M
Mageswaran, M
Mailand, K
Malec, M
Mandic, V
Marano, S
Marka, S
Markowitz, J
Maros, E
Martin, I
Marx, JN
Mason, K
Matone, L
Matta, V
Mavalvala, N
McCarthy, R
McClelland, DE
McGuire, SC
McHugh, M
McKenzie, K
McNabb, JWC
McWilliams, S
Meier, T
Melissinos, A
Mendell, G
Mercer, RA
Meshkov, S
Messaritaki, E
Messenger, CJ
Meyers, D
Mikhailov, E
Mitra, S
Mitrofanov, VP
Mitselmakher, G
Mittleman, R
Miyakawa, O
Mohanty, S
Moreno, G
Mossavi, K
MowLowry, C
Moylan, A
Mudge, D
Mueller, G
Mukherjee, S
Muller-Ebhardt, H
Munch, J
Murray, P
Myers, E
Myers, J
Nash, T
Newton, G
Nishizawa, A
Nocera, F
Numata, K
O'Reilly, B
O'Shaughnessy, R
Ottaway, DJ
Overmier, H
Owen, BJ
Pan, Y
Papa, MA
Parameshwaraiah, V
Parameswariah, C
Patel, P
Pedraza, M
Penn, S
Pierro, V
Pinto, IM
Pitkin, M
Pletsch, H
Plissi, MV
Postiglione, F
Prix, R
Quetschke, V
Raab, F
Rabeling, D
Radkins, H
Rahkola, R
Rainer, N
Rakhmanov, M
Rawlins, K
Ray-Majumder, S
Re, V
Regimbau, T
Rehbein, H
Reid, S
Reitze, DH
Ribichini, L
Riesen, R
Riles, K
Rivera, B
Robertson, NA
Robinson, C
Robinson, EL
Roddy, S
Rodriguez, A
Rogan, AM
Rollins, J
Romano, JD
Romie, J
Route, R
Rowan, S
Rudiger, A
Ruet, L
Russell, P
Ryan, K
Sakata, S
Samidi, M
De la Jordana, LS
Sandberg, V
Sanders, GH
Sannibale, V
Saraf, S
Sarin, P
Sathyaprakash, BS
Sato, S
Saulson, PR
Savage, R
Savov, P
Sazonov, A
Schediwy, S
Schilling, R
Schnabel, R
Schofield, R
Schutz, BF
Schwinberg, P
Scott, SM
Searle, AC
Sears, B
Seifert, F
Sellers, D
Sengupta, AS
Shawhan, P
Shoemaker, DH
Sibley, A
Sidles, JA
Siemens, X
Sigg, D
Sinha, S
Sintes, AM
Slagmolen, BJJ
Slutsky, J
Smith, JR
Smith, MR
Somiya, K
Strain, KA
Strom, DM
Stuver, A
Summerscales, TZ
Sun, KX
Sung, M
Sutton, PJ
Takahashi, H
Tanner, DB
Tarallo, M
Taylor, R
Taylor, R
Thacker, J
Thorne, KA
Thorne, KS
Thuring, A
Tokmakov, KV
Torres, C
Torrie, C
Traylor, G
Trias, M
Tyler, W
Ugolini, D
Ungarelli, C
Urbanek, K
Vahlbruch, H
Vallisneri, M
Van Den Broeck, C
van Putten, M
Varvella, M
Vass, S
Vecchio, A
Veitch, J
Veitch, P
Villar, A
Vorvick, C
Vyachanin, SP
Waldman, SJ
Wallace, L
Ward, H
Ward, R
Watts, K
Webber, D
Weidner, A
Weinert, M
Weinstein, A
Weiss, R
Wen, S
Wette, K
Whelan, JT
Whitbeck, DM
Whitcomb, SE
Whiting, BF
Wiley, S
Wilkinson, C
Willems, PA
Williams, L
Willke, B
Wilmut, I
Winkler, W
Wipf, CC
Wise, S
Wiseman, AG
Woan, G
Woods, D
Wooley, R
Worden, J
Wu, W
Yakushin, I
Yamamoto, H
Yan, Z
Yoshida, S
Yunes, N
Zanolin, M
Zhang, J
Zhang, L
Zhao, C
Zotov, N
Zucker, M
Muhlen, HZ
Zweizig, J
AF Abbott, B.
Abbott, R.
Adhikari, R.
Agresti, J.
Ajith, P.
Allen, B.
Amin, R.
Anderson, S. B.
Anderson, W. G.
Arain, M.
Araya, M.
Armandula, H.
Ashley, M.
Aston, S.
Aufmuth, P.
Aulbert, C.
Babak, S.
Ballmer, S.
Bantilan, H.
Barish, B. C.
Barker, C.
Barker, D.
Barr, B.
Barriga, P.
Barton, M. A.
Bayer, K.
Belczynski, K.
Betzwieser, J.
Beyersdorf, P. T.
Bhawal, B.
Bilenko, I. A.
Billingsley, G.
Biswas, R.
Black, E.
Blackburn, K.
Blackburn, L.
Blair, D.
Bland, B.
Bogenstahl, J.
Bogue, L.
Bork, R.
Boschi, V.
Bose, S.
Brady, P. R.
Braginsky, V. B.
Brau, J. E.
Brinkmann, M.
Brooks, A.
Brown, D. A.
Bullington, A.
Bunkowski, A.
Buonanno, A.
Burmeister, O.
Busby, D.
Butler, W. E.
Byer, R. L.
Cadonati, L.
Cagnoli, G.
Camp, J. B.
Cannizzo, J.
Cannon, K.
Cantley, C. A.
Cao, J.
Cardenas, L.
Carter, K.
Casey, M. M.
Castaldi, G.
Cepeda, C.
Chalkey, E.
Charlton, P.
Chatterji, S.
Chelkowski, S.
Chen, Y.
Chiadini, F.
Chin, D.
Chin, E.
Chow, J.
Christensen, N.
Clark, J.
Cochrane, P.
Cokelaer, T.
Colacino, C. N.
Coldwell, R.
Conte, R.
Cook, D.
Corbitt, T.
Coward, D.
Coyne, D.
Creighton, J. D. E.
Creighton, T. D.
Croce, R. P.
Crooks, D. R. M.
Cruise, A. M.
Cumming, A.
Dalrymple, J.
D'Ambrosio, E.
Danzmann, K.
Davies, G.
DeBra, D.
Degallaix, J.
Degree, M.
Demma, T.
Dergachev, V.
Desai, S.
DeSalvo, R.
Dhurandhar, S.
Diaz, M.
Dickson, J.
Di Credico, A.
Diederichs, G.
Dietz, A.
Doomes, E. E.
Drever, R. W. P.
Dumas, J. -C.
Dupuis, R. J.
Dwyer, J. G.
Ehrens, P.
Espinoza, E.
Etzel, T.
Evans, M.
Evans, T.
Fairhurst, S.
Fan, Y.
Fazi, D.
Fejer, M. M.
Finn, L. S.
Fiumara, V.
Fotopoulos, N.
Franzen, A.
Franzen, K. Y.
Freise, A.
Frey, R.
Fricke, T.
Fritschel, P.
Frolov, V. V.
Fyffe, M.
Galdi, V.
Ganezer, K. S.
Garofoli, J.
Gholami, I.
Giaime, J. A.
Giampanis, S.
Giardina, K. D.
Goda, K.
Goetz, E.
Goggin, L.
Gonzalez, G.
Gossler, S.
Grant, A.
Gras, S.
Gray, C.
Gray, M.
Greenhalgh, J.
Gretarsson, A. M.
Grosso, R.
Grote, H.
Grunewald, S.
Guenther, M.
Gustafson, R.
Hage, B.
Hammer, D.
Hanna, C.
Hanson, J.
Harms, J.
Harry, G.
Harstad, E.
Hayler, T.
Heefner, J.
Heng, I. S.
Heptonstall, A.
Heurs, M.
Hewitson, M.
Hild, S.
Hirose, E.
Hoak, D.
Hosken, D.
Hough, J.
Howell, E.
Hoyland, D.
Huttner, S. H.
Ingram, D.
Innerhofer, E.
Ito, M.
Itoh, Y.
Ivanov, A.
Jackrel, D.
Johnson, B.
Johnson, W. W.
Jones, D. I.
Jones, G.
Jones, R.
Ju, L.
Kalmus, P.
Kalogera, V.
Kasprzyk, D.
Katsavounidis, E.
Kawabe, K.
Kawamura, S.
Kawazoe, F.
Kells, W.
Keppel, D. G.
Khalili, F. Ya.
Kim, C.
King, P.
Kissel, J. S.
Klimenko, S.
Kokeyama, K.
Kondrashov, V.
Kopparapu, R. K.
Kozak, D.
Krishnan, B.
Kwee, P.
Lam, P. K.
Landry, M.
Lantz, B.
Lazzarini, A.
Lee, B.
Lei, M.
Leiner, J.
Leonhardt, V.
Leonor, I.
Libbrecht, K.
Lindquist, P.
Lockerbie, N. A.
Longo, M.
Lormand, M.
Lubinski, M.
Lueck, H.
Machenschalk, B.
MacInnis, M.
Mageswaran, M.
Mailand, K.
Malec, M.
Mandic, V.
Marano, S.
Marka, S.
Markowitz, J.
Maros, E.
Martin, I.
Marx, J. N.
Mason, K.
Matone, L.
Matta, V.
Mavalvala, N.
McCarthy, R.
McClelland, D. E.
McGuire, S. C.
McHugh, M.
McKenzie, K.
McNabb, J. W. C.
McWilliams, S.
Meier, T.
Melissinos, A.
Mendell, G.
Mercer, R. A.
Meshkov, S.
Messaritaki, E.
Messenger, C. J.
Meyers, D.
Mikhailov, E.
Mitra, S.
Mitrofanov, V. P.
Mitselmakher, G.
Mittleman, R.
Miyakawa, O.
Mohanty, S.
Moreno, G.
Mossavi, K.
MowLowry, C.
Moylan, A.
Mudge, D.
Mueller, G.
Mukherjee, S.
Muller-Ebhardt, H.
Munch, J.
Murray, P.
Myers, E.
Myers, J.
Nash, T.
Newton, G.
Nishizawa, A.
Nocera, F.
Numata, K.
O'Reilly, B.
O'Shaughnessy, R.
Ottaway, D. J.
Overmier, H.
Owen, B. J.
Pan, Y.
Papa, M. A.
Parameshwaraiah, V.
Parameswariah, C.
Patel, P.
Pedraza, M.
Penn, S.
Pierro, V.
Pinto, I. M.
Pitkin, M.
Pletsch, H.
Plissi, M. V.
Postiglione, F.
Prix, R.
Quetschke, V.
Raab, F.
Rabeling, D.
Radkins, H.
Rahkola, R.
Rainer, N.
Rakhmanov, M.
Rawlins, K.
Ray-Majumder, S.
Re, V.
Regimbau, T.
Rehbein, H.
Reid, S.
Reitze, D. H.
Ribichini, L.
Riesen, R.
Riles, K.
Rivera, B.
Robertson, N. A.
Robinson, C.
Robinson, E. L.
Roddy, S.
Rodriguez, A.
Rogan, A. M.
Rollins, J.
Romano, J. D.
Romie, J.
Route, R.
Rowan, S.
Ruediger, A.
Ruet, L.
Russell, P.
Ryan, K.
Sakata, S.
Samidi, M.
De la Jordana, L. Sancho
Sandberg, V.
Sanders, G. H.
Sannibale, V.
Saraf, S.
Sarin, P.
Sathyaprakash, B. S.
Sato, S.
Saulson, P. R.
Savage, R.
Savov, P.
Sazonov, A.
Schediwy, S.
Schilling, R.
Schnabel, R.
Schofield, R.
Schutz, B. F.
Schwinberg, P.
Scott, S. M.
Searle, A. C.
Sears, B.
Seifert, F.
Sellers, D.
Sengupta, A. S.
Shawhan, P.
Shoemaker, D. H.
Sibley, A.
Sidles, J. A.
Siemens, X.
Sigg, D.
Sinha, S.
Sintes, A. M.
Slagmolen, B. J. J.
Slutsky, J.
Smith, J. R.
Smith, M. R.
Somiya, K.
Strain, K. A.
Strom, D. M.
Stuver, A.
Summerscales, T. Z.
Sun, K. -X.
Sung, M.
Sutton, P. J.
Takahashi, H.
Tanner, D. B.
Tarallo, M.
Taylor, R.
Taylor, R.
Thacker, J.
Thorne, K. A.
Thorne, K. S.
Thuering, A.
Tokmakov, K. V.
Torres, C.
Torrie, C.
Traylor, G.
Trias, M.
Tyler, W.
Ugolini, D.
Ungarelli, C.
Urbanek, K.
Vahlbruch, H.
Vallisneri, M.
Van Den Broeck, C.
van Putten, M.
Varvella, M.
Vass, S.
Vecchio, A.
Veitch, J.
Veitch, P.
Villar, A.
Vorvick, C.
Vyachanin, S. P.
Waldman, S. J.
Wallace, L.
Ward, H.
Ward, R.
Watts, K.
Webber, D.
Weidner, A.
Weinert, M.
Weinstein, A.
Weiss, R.
Wen, S.
Wette, K.
Whelan, J. T.
Whitbeck, D. M.
Whitcomb, S. E.
Whiting, B. F.
Wiley, S.
Wilkinson, C.
Willems, P. A.
Williams, L.
Willke, B.
Wilmut, I.
Winkler, W.
Wipf, C. C.
Wise, S.
Wiseman, A. G.
Woan, G.
Woods, D.
Wooley, R.
Worden, J.
Wu, W.
Yakushin, I.
Yamamoto, H.
Yan, Z.
Yoshida, S.
Yunes, N.
Zanolin, M.
Zhang, J.
Zhang, L.
Zhao, C.
Zotov, N.
Zucker, M.
Muehlen, H. zur
Zweizig, J.
TI Search for gravitational waves from binary inspirals in S3 and S4 LIGO
data
SO PHYSICAL REVIEW D
LA English
DT Article
ID BLACK-HOLE BINARIES; GAMMA-RAY BURSTS; NEUTRON-STAR; COMPACT BINARIES;
2ND-POST-NEWTONIAN ORDER; CONSTRAINING POPULATION; SYNTHESIS MODELS;
RATES; RADIATION; MERGERS
AB We report on a search for gravitational waves from the coalescence of compact binaries during the third and fourth LIGO science runs. The search focused on gravitational waves generated during the inspiral phase of the binary evolution. In our analysis, we considered three categories of compact binary systems, ordered by mass: (i) primordial black hole binaries with masses in the range 0.35M center dot m(1), m(2) 1.0M center dot, (ii) binary neutron stars with masses in the range 1.0M center dot m(1), m(2) 3.0M center dot, and (iii) binary black holes with masses in the range 3.0M center dot m(1), m(2) m(max) with the additional constraint m(1) + m(2) m(max), where m(max) was set to 40.0M center dot and 80.0M center dot in the third and fourth science runs, respectively. Although the detectors could probe to distances as far as tens of Mpc, no gravitational-wave signals were identified in the 1364 hours of data we analyzed. Assuming a binary population with a Gaussian distribution around 0.75 - 0.75M center dot, 1.4 - 1.4M center dot, and 5.0 - 5.0M center dot, we derived 90%- confidence upper limit rates of 4.9 yr(-1)L(10)(-1) for primordial black hole binaries, 1.2 yr(-1)L(10)(-1) for binary neutron stars, and 0: 5 yr(-1)L(10)(-1) for stellar mass binary black holes, where L-10 is 10(10) times the blue-light luminosity of the Sun.
C1 [Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Anderson, S. B.; Araya, M.; Armandula, H.; Ballmer, S.; Barish, B. C.; Bhawal, B.; Billingsley, G.; Black, E.; Blackburn, K.; Bork, R.; Boschi, V.; Brown, D. A.; Busby, D.; Cardenas, L.; Cepeda, C.; Chatterji, S.; Creighton, T. D.; D'Ambrosio, E.; DeSalvo, R.; Drever, R. W. P.; Dupuis, R. J.; Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.; Fairhurst, S.; Fazi, D.; Goggin, L.; Heefner, J.; Ivanov, A.; Kells, W.; Keppel, D. G.; King, P.; Kondrashov, V.; Kozak, D.; Lazzarini, A.; Lei, M.; Libbrecht, K.; Lindquist, P.; Mageswaran, M.; Mailand, K.; Mandic, V.; Maros, E.; Marx, J. N.; Meshkov, S.; Messaritaki, E.; Meyers, D.; Miyakawa, O.; Muller-Ebhardt, H.; Nash, T.; Nocera, F.; Robertson, N. A.; Russell, P.; Samidi, M.; Sanders, G. H.; Sannibale, V.; Sears, B.; Siemens, X.; Smith, M. R.; Sutton, P. J.; Tarallo, M.; Traylor, G.; Tyler, W.; Varvella, M.; Vass, S.; Villar, A.; Waldman, S. J.; Wallace, L.; Ward, R.; Webber, D.; Weinstein, A.; Whitcomb, S. E.; Willems, P. A.; Yamamoto, H.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA.
[Aulbert, C.; Babak, S.; Chen, Y.; Gholami, I.; Grunewald, S.; Krishnan, B.; Machenschalk, B.; Papa, M. A.; Prix, R.; Schutz, B. F.; Sintes, A. M.; Somiya, K.; Takahashi, H.; Whelan, J. T.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany.
[Ajith, P.; Allen, B.; Brinkmann, M.; Bunkowski, A.; Burmeister, O.; Chelkowski, S.; Cochrane, P.; Danzmann, K.; Grote, H.; Harms, J.; Heurs, M.; Hewitson, M.; Lueck, H.; Mossavi, K.; Pletsch, H.; Rainer, N.; Rehbein, H.; Ribichini, L.; Ruediger, A.; Schilling, R.; Schnabel, R.; Seifert, F.; Smith, J. R.; Somiya, K.; Weidner, A.; Weinert, M.; Willke, B.; Winkler, W.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
[Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Ashley, M.; Chow, J.; Dickson, J.; Gossler, S.; Gray, M.; Lam, P. K.; McClelland, D. E.; McKenzie, K.; MowLowry, C.; Moylan, A.; Rabeling, D.; Scott, S. M.; Searle, A. C.; Slagmolen, B. J. J.; Wette, K.] Australian Natl Univ, Canberra, ACT 0200, Australia.
[Garofoli, J.; Wiley, S.] Calif State Univ Dominguez Hills, Carson, CA 90747 USA.
[Brown, D. A.; Savov, P.; Siemens, X.; Thorne, K. S.; Vallisneri, M.] CALTECH, CaRT, Pasadena, CA 91125 USA.
[Cokelaer, T.; Davies, G.; Dietz, A.; Fairhurst, S.; Jones, G.; Regimbau, T.; Robinson, C.; Romano, J. D.; Sathyaprakash, B. S.; Schutz, B. F.; Sengupta, A. S.; Van Den Broeck, C.] Cardiff Univ, Cardiff CF2 3YB, Wales.
[Bantilan, H.; Christensen, N.] Carleton Coll, Northfield, MN 55057 USA.
[Charlton, P.; Matone, L.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia.
[Dwyer, J. G.; Kalmus, P.; Marka, S.; Rollins, J.] Columbia Univ, New York, NY 10027 USA.
[Gretarsson, A. M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA.
[Dhurandhar, S.; Mitra, S.] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Barker, C.; Barker, D.; Bland, B.; Cook, D.; Garofoli, J.; Gray, C.; Guenther, M.; Ingram, D.; Johnson, B.; Kawabe, K.; Landry, M.; Lubinski, M.; McCarthy, R.; Mendell, G.; Moreno, G.; Myers, E.; Myers, J.; Parameshwaraiah, V.; Raab, F.; Radkins, H.; Rivera, B.; Ryan, K.; Sandberg, V.; Savage, R.; Schwinberg, P.; Sigg, D.; Vorvick, C.; Wilkinson, C.; Worden, J.] LIGO Hanford Observ, Richland, WA 99352 USA.
[Bogue, L.; Carter, K.; Evans, T.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Hanson, J.; Hoak, D.; Lormand, M.; O'Reilly, B.; Overmier, H.; Parameswariah, C.; Patel, P.; Pedraza, M.; Riesen, R.; Roddy, S.; Romie, J.; Sellers, D.; Sibley, A.; Thacker, J.; Traylor, G.; Watts, K.; Wooley, R.; Yakushin, I.] LIGO Livingston Observ, Livingston, LA 70754 USA.
[Bayer, K.; Blackburn, L.; Cadonati, L.; Cao, J.; Corbitt, T.; Fritschel, P.; Goda, K.; Harry, G.; Innerhofer, E.; Katsavounidis, E.; MacInnis, M.; Markowitz, J.; Mason, K.; Mavalvala, N.; Mikhailov, E.; Mittleman, R.; Ottaway, D. J.; Rawlins, K.; Ruet, L.; Sarin, P.; Shoemaker, D. H.; van Putten, M.; Wen, S.; Wipf, C. C.; Zanolin, M.; Zucker, M.] MIT, LIGO, Cambridge, MA 02139 USA.
[Amin, R.; Betzwieser, J.; Giaime, J. A.; Gonzalez, G.; Hanna, C.; Johnson, W. W.; Kopparapu, R. K.; Rodriguez, A.; Slutsky, J.; Sung, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA.
[Amin, R.; Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA.
[McHugh, M.] Loyola Univ, New Orleans, LA 70118 USA.
[Bilenko, I. A.; Braginsky, V. B.; Khalili, F. Ya.; Mitrofanov, V. P.; Vyachanin, S. P.] Moscow MV Lomonosov State Univ, Moscow 119992, Russia.
[Camp, J. B.; Cannizzo, J.; McWilliams, S.; Numata, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kawamura, S.; Kawazoe, F.; Kokeyama, K.; Leonhardt, V.; Nishizawa, A.; Sakata, S.; Sato, S.] Natl Astron Observ, Tokyo 1818588, Japan.
[Belczynski, K.; Kalogera, V.; Kim, C.; O'Shaughnessy, R.] Northwestern Univ, Evanston, IL 60208 USA.
[Saraf, S.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Greenhalgh, J.; Hayler, T.; Wilmut, I.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[Beyersdorf, P. T.] San Jose State Univ, San Jose, CA 95192 USA.
[Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA.
[Doomes, E. E.; McGuire, S. C.] So Univ & A&M Coll, Baton Rouge, LA 70813 USA.
[Bullington, A.; Byer, R. L.; DeBra, D.; Di Credico, A.; Fejer, M. M.; Jackrel, D.; Lantz, B.; Route, R.; Sinha, S.; Sun, K. -X.; Urbanek, K.] Stanford Univ, Stanford, CA 94305 USA.
[Dalrymple, J.; Di Credico, A.; Hirose, E.; Saulson, P. R.] Syracuse Univ, Syracuse, NY 13244 USA.
[Desai, S.; Finn, L. S.; McNabb, J. W. C.; Owen, B. J.; Rakhmanov, M.; Stuver, A.; Thorne, K. A.; Whitbeck, D. M.; Yunes, N.] Penn State Univ, University Pk, PA 16802 USA.
[Diaz, M.; Grosso, R.; Mohanty, S.; Mukherjee, S.; Torres, C.] Univ Texas Brownsville & Texas Southmost Coll, Brownsville, TX 78520 USA.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[De la Jordana, L. Sancho; Sintes, A. M.; Trias, M.] Univ Illes Balears, E-07122 Palma de Mallorca, Spain.
[Aufmuth, P.; Danzmann, K.; Diederichs, G.; Franzen, A.; Hage, B.; Hild, S.; Kwee, P.; Lueck, H.; Malec, M.; Meier, T.; Thuering, A.; Vahlbruch, H.; Willke, B.; Muehlen, H. zur] Leibniz Univ Hannover, D-30167 Hannover, Germany.
[Brooks, A.; Hosken, D.; Mudge, D.; Munch, J.; Veitch, P.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Aston, S.; Colacino, C. N.; Cruise, A. M.; Freise, A.; Hoyland, D.; Kasprzyk, D.; Re, V.; Robinson, E. L.; Ungarelli, C.; Vecchio, A.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England.
[Arain, M.; Coldwell, R.; Franzen, K. Y.; Klimenko, S.; Mercer, R. A.; Mitselmakher, G.; Mueller, G.; Quetschke, V.; Reitze, D. H.; Sazonov, A.; Tanner, D. B.; Whiting, B. F.; Williams, L.; Wise, S.; Wu, W.] Univ Florida, Gainesville, FL 32611 USA.
[Barriga, P.; Barton, M. A.; Bogenstahl, J.; Cagnoli, G.; Cantley, C. A.; Casey, M. M.; Chalkey, E.; Clark, J.; Crooks, D. R. M.; Cumming, A.; Grant, A.; Heng, I. S.; Heptonstall, A.; Hough, J.; Huttner, S. H.; Jones, R.; Martin, I.; Messenger, C. J.; Murray, P.; Newton, G.; Reid, S.; Robertson, N. A.; Rowan, S.; Strain, K. A.; Taylor, R.; Tokmakov, K. V.; Torrie, C.; Veitch, J.; Ward, H.; Woan, G.] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland.
[Buonanno, A.; Pan, Y.; Pitkin, M.; Plissi, M. V.; Shawhan, P.] Univ Maryland, College Pk, MD 20742 USA.
[Chin, D.; Dergachev, V.; Goetz, E.; Gustafson, R.; Riles, K.; Zhang, J.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Brau, J. E.; Frey, R.; Fricke, T.; Harstad, E.; Ito, M.; Leonor, I.; Rahkola, R.; Schofield, R.; Strom, D. M.] Univ Oregon, Eugene, OR 97403 USA.
[Butler, W. E.; Giampanis, S.; Melissinos, A.] Univ Rochester, Rochester, NY 14627 USA.
[Chiadini, F.; Conte, R.; Fiumara, V.; Longo, M.; Marano, S.; Matta, V.; Postiglione, F.] Univ Salerno, I-84084 Salerno, Italy.
[Castaldi, G.; Croce, R. P.; Demma, T.; Galdi, V.; Pierro, V.; Pinto, I. M.] Univ Sannio, I-82100 Benevento, Italy.
[Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Lockerbie, N. A.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland.
[Siemens, X.] Univ Washington, Seattle, WA 98195 USA.
[Barton, M. A.; Blair, D.; Chin, E.; Degallaix, J.; Dumas, J. -C.; Fan, Y.; Gras, S.; Howell, E.; Ju, L.; Lee, B.; Schediwy, S.; Yan, Z.; Zhao, C.] Univ Western Australia, Crawley, WA 6009, Australia.
[Anderson, W. G.; Biswas, R.; Brady, P. R.; Cannon, K.; Creighton, J. D. E.; Fotopoulos, N.; Hammer, D.; Itoh, Y.; Papa, M. A.; Ray-Majumder, S.; Wiseman, A. G.; Woods, D.] Univ Wisconsin, Milwaukee, WI 53201 USA.
Vassar Coll, New York, NY 12604 USA.
[Bose, S.; Leiner, J.; Rogan, A. M.] Washington State Univ, Pullman, WA 99164 USA.
RP Abbott, B (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
RI Khalili, Farit/D-8113-2012; Chiadini, Francesco/E-1812-2015; Vecchio,
Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Ottaway,
David/J-5908-2015; Postiglione, Fabio/O-4744-2015; Messaritaki,
Eirini/D-7393-2016; Tarallo, Marco/B-2096-2012; Sigg,
Daniel/I-4308-2015; Pinto, Innocenzo/L-3520-2016; Harms,
Jan/J-4359-2012; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016;
Chen, Yanbei/A-2604-2013; Allen, Bruce/K-2327-2012; Bilenko,
Igor/D-5172-2012; Strain, Kenneth/D-5236-2011; Raab,
Frederick/E-2222-2011; Casey, Morag/C-9703-2010; Mitrofanov,
Valery/D-8501-2012; Martin, Iain/A-2445-2010; Hild, Stefan/A-3864-2010;
McClelland, David/E-6765-2010; Pitkin, Matthew/I-3802-2013; Schutz,
Bernard/B-1504-2010; Rowan, Sheila/E-3032-2010; Agresti,
Juri/G-8168-2012; Zhao, Chunnong/C-2403-2013; Ju, Li/C-2623-2013; Re,
Virginia /F-6403-2013; Barker, David/A-5671-2013; Lueck,
Harald/F-7100-2011; Kawabe, Keita/G-9840-2011; Kawazoe,
Fumiko/F-7700-2011; Freise, Andreas/F-8892-2011; Galdi,
Vincenzo/B-1670-2008; Lam, Ping Koy/A-5276-2008; Finn, Lee
Samuel/A-3452-2009; Vyatchanin, Sergey/J-2238-2012; Howell,
Eric/H-5072-2014; Ward, Robert/I-8032-2014;
OI Chiadini, Francesco/0000-0002-9339-8622; Vecchio,
Alberto/0000-0002-6254-1617; Postiglione, Fabio/0000-0003-0628-3796;
Tarallo, Marco/0000-0001-5169-4987; Sigg, Daniel/0000-0003-4606-6526;
Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636;
Allen, Bruce/0000-0003-4285-6256; Strain, Kenneth/0000-0002-2066-5355;
McClelland, David/0000-0001-6210-5842; Pitkin,
Matthew/0000-0003-4548-526X; Agresti, Juri/0000-0001-6119-2470; Zhao,
Chunnong/0000-0001-5825-2401; Lueck, Harald/0000-0001-9350-4846; Galdi,
Vincenzo/0000-0002-4796-3600; Lam, Ping Koy/0000-0002-4421-601X; Finn,
Lee Samuel/0000-0002-3937-0688; Freise, Andreas/0000-0001-6586-9901;
MATTA, VINCENZO/0000-0002-2046-4027; MARANO,
Stefano/0000-0002-5307-0980; Whiting, Bernard F/0000-0002-8501-8669;
Veitch, John/0000-0002-6508-0713; Papa,
M.Alessandra/0000-0002-1007-5298; Stuver, Amber/0000-0003-0324-5735;
Nishizawa, Atsushi/0000-0003-3562-0990; Zweizig,
John/0000-0002-1521-3397; O'Shaughnessy, Richard/0000-0001-5832-8517;
Aulbert, Carsten/0000-0002-1481-8319; Howell, Eric/0000-0001-7891-2817;
LONGO, Maurizio/0000-0001-8325-4003; Pierro,
Vincenzo/0000-0002-6020-5521; Ward, Robert/0000-0001-5503-5241; Whelan,
John/0000-0001-5710-6576; Fairhurst, Stephen/0000-0001-8480-1961;
Boschi, Valerio/0000-0001-8665-2293; Pinto, Innocenzo
M./0000-0002-2679-4457
NR 56
TC 100
Z9 100
U1 3
U2 18
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 MAR
PY 2008
VL 77
IS 6
AR 062002
DI 10.1103/PhysRevD.77.062002
PG 13
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 282CF
UT WOS:000254544500006
ER
PT J
AU Rubinstein, R
Luo, LS
AF Rubinstein, Robert
Luo, Li-Shi
TI Theory of the lattice Boltzmann equation: Symmetry properties of
discrete velocity sets
SO PHYSICAL REVIEW E
LA English
DT Article
ID NONIDEAL GASES; MODELS; DIMENSIONS
AB The lattice Boltzmann equation replaces continuous particle velocity space by a finite set; the velocity distribution function then varies over a finite-dimensional vector space instead of over an infinite-dimensional function space. The number of linearly independent moments of the distribution function in a lattice Boltzmann model cannot exceed the number of velocities; finite dimensionality therefore necessarily induces linear dependences among the moments that do not exist in a continuous theory. Given a finite velocity set, it is important to know which moments are free of these dependences. Elementary group theory is applied to the solution of this problem. It is found that decomposing the velocity set into subsets that transform among themselves under an appropriate symmetry group makes it straightforward to uncover linear dependences among the moments. The construction of some standard two- and three-dimensional models is reviewed from this viewpoint, and procedures for constructing higher-dimensional models are suggested.
C1 [Rubinstein, Robert] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Luo, Li-Shi] Old Dominion Univ, Dept Math & Stat, Ctr Computat Sci, Norfolk, VA 23529 USA.
RP Rubinstein, R (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM r.rubinstein@nasa.gov; lluo@odu.edu
RI Luo, Li-Shi/A-4561-2011
OI Luo, Li-Shi/0000-0003-1215-7892
NR 35
TC 24
Z9 24
U1 0
U2 7
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1539-3755
J9 PHYS REV E
JI Phys. Rev. E
PD MAR
PY 2008
VL 77
IS 3
AR 036709
DI 10.1103/PhysRevE.77.036709
PN 2
PG 11
WC Physics, Fluids & Plasmas; Physics, Mathematical
SC Physics
GA 282AL
UT WOS:000254539900113
PM 18517559
ER
PT J
AU Gamero-Castano, M
AF Gamero-Castano, Manuel
TI Characterization of the electrosprays of 1-ethyl-3-methylimidazolium
bis(trifluoromethylsulfonyl) imide in vacuum
SO PHYSICS OF FLUIDS
LA English
DT Article
ID UNIVERSAL SCALING LAWS; TAYLOR CONES; IONIC LIQUIDS; JETS; SURFACES;
BREAKUP; MODEL
AB The electrosprays of 1-ethyl-3-methylimidazolium bis(trifluoromethylsulfonyl) imide are composed of a complex mixture of ions and charged droplets, which can be analyzed to determine the structure of the beam and infer significant features of the electrohydrodynamic atomization. In particular, we use a combination of retarding potential and time of flight techniques to study these beams and are able to quantify the voltage drop along the cone jet, together with the velocity and diameter of the jet at the breakup location, confirm the strong influence of viscosity and electrification in the breakup, show that the electric field in and near the Taylor cone tip is insensitive to external electrostatic parameters, and study the spatial distribution of ions and droplets, whereby the paradoxical absence of ions in the outmost region of the beam is established. The research described in this article can be exploited in the modeling of capillary instability of charged jets: testing the results of these models is difficult, especially when nanojets are involved, and our findings and techniques provide the experimental support required by the theoretical activity. The present research is also applicable to the modeling of colloid thruster beams. (C) 2008 American Institute of Physics.
C1 Univ Calif Irvine, Dept Mech & Aerosp Engn, Irvine, CA 92717 USA.
Jet Propuls Lab, Pasadena, CA 91108 USA.
RP Gamero-Castano, M (reprint author), Univ Calif Irvine, Dept Mech & Aerosp Engn, Irvine, CA 92717 USA.
NR 29
TC 11
Z9 11
U1 2
U2 5
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 1070-6631
J9 PHYS FLUIDS
JI Phys. Fluids
PD MAR
PY 2008
VL 20
IS 3
AR 032103
DI 10.1063/1.2899658
PG 11
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA 281ZO
UT WOS:000254537600009
ER
PT J
AU Birn, J
Borovsky, JE
Hesse, M
AF Birn, J.
Borovsky, J. E.
Hesse, M.
TI Properties of asymmetric magnetic reconnection
SO PHYSICS OF PLASMAS
LA English
DT Article
ID CHALLENGE; MAGNETOTAIL; MHD
AB Properties of magnetic reconnection are investigated in two-dimensional, resistive magnetohydrodynamic (MHD) simulations of current sheets separating plasmas with different magnetic field strengths and densities. Specific emphasis is on the influence of the external parameters on the reconnection rate. The effect of the dissipation in the resistive MHD model is separated from this influence by evaluating resistivity dependence together with the dependence on the background parameters. Two scenarios are considered, which may be distinguished as driven and nondriven reconnection. In either scenario, the maximum reconnection rate (electric field) is found to depend on appropriate hybrid expressions based on a magnetic field strength and an Alfven speed derived from the characteristic values in the two inflow regions. The scaling compares favorably with an analytic formula derived recently by Cassak and Shay [Phys. Plasmas 14, 102114 (2007)] applied to the regime of fast reconnection. An investigation of the energy flow and conversion in the vicinity of the reconnection site revealed a significant role of enthalpy flux generation, in addition to the expected conversion of Poynting flux to kinetic energy flux. This enthalpy flux generation results from Ohmic heating as well as adiabatic, that is, compressional heating. The latter is found more important when the magnetic field strengths in the two inflow regions are comparable in magnitude. (C) 2008 American Institute of Physics.
C1 [Birn, J.; Borovsky, J. E.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Birn, J (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA.
EM jbirn@lanl.gov
RI Hesse, Michael/D-2031-2012; NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
NR 15
TC 43
Z9 43
U1 0
U2 1
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 1070-664X
J9 PHYS PLASMAS
JI Phys. Plasmas
PD MAR
PY 2008
VL 15
IS 3
AR 032101
DI 10.1063/1.2888491
PG 13
WC Physics, Fluids & Plasmas
SC Physics
GA 281ZR
UT WOS:000254537900005
ER
PT J
AU Peters, GH
Smith, JA
Mungas, GS
Bearman, GH
Shiraishi, L
Beegle, LW
AF Peters, Gregory H.
Smith, J. Anthony
Mungas, Gregory S.
Bearman, Gregory H.
Shiraishi, Lori
Beegle, Luther W.
TI RASP-based sample acquisition of analogue Martian permafrost samples:
Implications for NASA's Phoenix scout mission
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mars geological processes; Mars sampling technology : Mars in situ
investigations
ID GROUND ICE; MARS; BEHAVIOR
AB Sample acquisition studies of ice-dirt mixtures under simulated Martian conditions approximating the 2007/8 Phoenix Scout mission are reported. The experiments were performed using a prototype rapid acquisition sampling package (RASP) that is similar to the one mounted on the 2007/8 Phoenix scout robotic arm. This mission will acquire a sample from permafrost-like regolith that is estimated at strengths near 45 MPa to measure the volatile composition including H(2)O. Sublimation loss during sample acquisition and transfer will have a significant effect on the determination of water content, a major Phoenix mission goal. Laboratory sample acquisition was performed under Martian ambient pressures (5 Torr) in which water is unstable and ice quickly sublimates. Basalt samples consisting of various size, and shapes subjected to various temperature ranges were used as the aggregate material of the water saturated permafrost analogues expected to be found at the Phoenix landing site. In our laboratory experiments roughly 5-6% of the initial water-ice was sublimed due to energy imparted by the tool to the sample during sample acquisition. This loss is in addition to any others from passive sublimation as the samples are transferred to the instruments for analysis. We determined that the energy necessary to excavate the permafrost samples with the RASP to be on the order of 0.05 W h/cm(3). Finally, we discuss the potential to use a RASP on future in situ Martian missions. (c) 2007 Elsevier Ltd. All rights reserved.
C1 [Beegle, Luther W.] CALTECH, Jet Prop Lab, Planetary Sci Sect, Pasadena, CA 91109 USA.
[Shiraishi, Lori] CALTECH, Jet Prop Lab, Instrument Mech Engn Sect, Pasadena, CA 91109 USA.
[Peters, Gregory H.; Smith, J. Anthony; Mungas, Gregory S.; Bearman, Gregory H.] CALTECH, Jet Prop Lab, In Situ Instrument Syst Sect, Pasadena, CA 91109 USA.
RP Beegle, LW (reprint author), CALTECH, Jet Prop Lab, Planetary Sci Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Gregory.H.Peters@jpl.nasa.gov; J.Anthony.Smith@jpl.nasa.gov;
Greg.S.Mungas@jpl.nasa.gov; Gregory.H.Bearman@jpl.nasa.gov;
Lori.R.Shiraishi@jpl.nasa.gov; Luther.Beegle@jpl.nasa.gov
RI Beegle, Luther/A-6354-2010
NR 12
TC 4
Z9 4
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 MAR
PY 2008
VL 56
IS 3-4
BP 303
EP 309
DI 10.1016/j.pss.2007.10.001
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 279QZ
UT WOS:000254371000001
ER
PT J
AU Graves, SDB
Mckay, CP
Griffith, CA
Ferri, F
Fulchignoni, M
AF Graves, S. D. B.
McKay, C. P.
Griffith, C. A.
Ferri, F.
Fulchignoni, M.
TI Rain and hail can reach the surface of Titan
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Titan; methane; Huygens; rain; hail
ID HUYGENS PROBE; ATMOSPHERE; METHANE; CLOUDS; CONDENSATION; EVAPORATION;
DESCENT; ETHANE; VAPOR; LAKES
AB We have calculated the condensation and evaporation of ternary CH4-N-2-C2H6 liquid drops and solid CH4 hail as they fall through Titan's lower atmosphere to determine the likelihood that precipitation reaches the ground. Assuming the humidity profile determined by the Huygens probe, binary liquid CH4/N-2 condensate grows in the region from similar to 8 to 15 km in Titan's atmosphere because the combined humidity of CH4 and N-2 exceeds saturation. These drops evaporate below similar to 8 km. We determine the fate of 10 mu m seeds composed of ethane, which is expected to provide condensation sites. In addition, we study the fate of already formed raindrops with radii of 1-4.75 mm falling out of the growth region. High (50%) and low (0%) ethane relative humidities (RH) are considered in the calculation. We find that drops with radii similar to 3 mm and smaller dropping from 8 km reach the ground in compositional equilibrium with the atmosphere in the high ethane RH case as a result of the stabilizing influence of the ethane, and evaporate in the atmosphere in the low ethane RH case. Large drops (> similar to 3 mm) reach the surface large and cold because the latent heat loss due to the evaporation of methane cools the drop and slows the evaporation rate. Pure methane hail hits the ground if its radius is initially more than 4 mm at 16 km above the surface and sublimates in the atmosphere if its radius is smaller. (c) 2007 Elsevier Ltd. All rights reserved.
C1 [Graves, S. D. B.; McKay, C. P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Griffith, C. A.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Fulchignoni, M.] Observ Paris, Lab Etud Spatiales & Instrumentat Astrophys, F-92195 Meudon, France.
[Ferri, F.] Univ Padua, I-35131 Padua, Italy.
RP Graves, SDB (reprint author), CALTECH, Dept Planetary Sci, MS 150-21, Pasadena, CA 91125 USA.
EM sdgraves@gps.caltech.edu
NR 31
TC 53
Z9 54
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 MAR
PY 2008
VL 56
IS 3-4
BP 346
EP 357
DI 10.1016/j.pss.2007.11.001
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 279QZ
UT WOS:000254371000005
ER
PT J
AU Furfaro, R
Dohm, JM
Fink, W
Kargel, J
Schulze-Makuch, D
Fairen, AG
Palmero-Rodriguez, A
Baker, VR
Ferre, PT
Hare, TM
Tarbell, MA
Miyamoto, H
Komatsu, G
AF Furfaro, R.
Dohm, J. M.
Fink, W.
Kargel, J.
Schulze-Makuch, D.
Fairen, A. G.
Palmero-Rodriguez, A.
Baker, V. R.
Ferre, P. T.
Hare, T. M.
Tarbell, M. A.
Miyamoto, H.
Komatsu, G.
TI The search for life beyond Earth through fuzzy expert systems
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE fuzzy logic; tier-scalable mission autonomy; astrobiology; search for
life; bobotic planetary exploration; autonomous planetary reconnaissance
ID PLANETARY RECONNAISSANCE MISSIONS; LINGUISTIC-SYNTHESIS; GLOBAL
DISTRIBUTION; PARADIGM SHIFT; THARSIS REGION; MARS ODYSSEY;
ENVIRONMENTS; EXPLORATION; ENCELADUS; DEPOSITS
AB Autonomy will play a key role in future science-driven, tier-scalable robotic planetary reconnaissance to extremely challenging (by existing means), locales on Mars and elsewhere that have the potential to yield significant geological and possibly exobiologic information. The full-scale and optimal deployment of the agents employed by tier-scalable architectures requires the design, implementation, and integration of an intelligent reconnaissance system. Such a system should be designed to enable fully automated and comprehensive characterization of an operational area, as well as to integrate existing information with acquired, "in transit" spatial and temporal sensor data, to identify and home in on prime candidate locales. These may include locales with the greatest potential of containing life.
Founded on the premise that water and energy are key to life, we have designed a fuzzy system that can (1) acquire the appropriate past/present water/energy indicators while the tier-scalable mission architecture is deployed (first layer), and (2) evaluate habitability through a specialized fuzzy knowledge-base of the water and energy information (second layer) acquired in (1). The system has been tested through hypothetical deployments at two hypothesized regions on Mars. The fuzzy-based expert's simulation results corroborate the same conclusions provided by the human expert, and thus highlight the system's potential capability to effectively and autonomously reason as an interdisciplinary scientist in the quest for life. While the approach is demonstrated for Mars, the methodology is general enough to be extended to other planetary bodies. It can be readily modified and updated as our interdisciplinary understanding of planetary environments improves. We believe this work represents a foundational step toward implementing higher-level intelligence in robotic. tier-scalable planetary reconnaissance within and beyond the solar system. (c) 2007 Elsevier Ltd. All rights reserved.
C1 [Furfaro, R.] Univ Arizona, Dept Aerosp & Mech Engn, Tucson, AZ 85721 USA.
[Dohm, J. M.; Kargel, J.; Baker, V. R.; Ferre, P. T.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
[Dohm, J. M.; Baker, V. R.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Fink, W.; Tarbell, M. A.] CALTECH, Visual & Autonomous Explorat Syst Res Lab, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Schulze-Makuch, D.] Washington State Univ, Dept Geol, Pullman, WA 99164 USA.
[Fairen, A. G.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Hare, T. M.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Palmero-Rodriguez, A.] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan.
[Miyamoto, H.] Univ Tokyo, Dept Geosyst Engn, Tokyo, Japan.
[Komatsu, G.] Univ Annunzio, Int Res Sch Planetary Sci, Pescara, Italy.
RP Furfaro, R (reprint author), Univ Arizona, Dept Aerosp & Mech Engn, Tucson, AZ 85721 USA.
EM robertof@email.arizona.edu
RI Miyamoto, Hideaki/B-9666-2008; Miyamoto, Hideaki/E-3381-2012; Dohm,
James/A-3831-2014; Komatsu, Goro/I-7822-2012;
OI Komatsu, Goro/0000-0003-4155-108X; Hare, Trent/0000-0001-8842-389X;
Schulze-Makuch, Dirk/0000-0002-1923-9746
NR 64
TC 14
Z9 14
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 MAR
PY 2008
VL 56
IS 3-4
BP 448
EP 472
DI 10.1016/j.pss.2007.09.006
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 279QZ
UT WOS:000254371000015
ER
PT J
AU Oberst, J
Schwarz, G
Behnke, T
Hoffmann, H
Matz, KD
Flohrer, J
Hirsch, H
Roatsch, T
Scholten, F
Hauber, E
Brinkmann, B
Jaumann, R
Williams, D
Kirk, R
Duxbury, T
Leu, C
Neukum, G
AF Oberst, J.
Schwarz, G.
Behnke, T.
Hoffmann, H.
Matz, K. -D.
Flohrer, J.
Hirsch, H.
Roatsch, T.
Scholten, F.
Hauber, E.
Brinkmann, B.
Jaumann, R.
Williams, D.
Kirk, R.
Duxbury, T.
Leu, C.
Neukum, G.
TI The imaging performance of the SRC on Mars Express
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mars; Mars express; instruments; cameras
ID RESOLUTION STEREO CAMERA; MARTIAN ATMOSPHERE; VERTICAL STRUCTURE;
CHRONOLOGY; HRSC
AB The Mars Express spacecraft carries the pushbroom scanner high-resolution stereo camera (HRSC) and its added imaging subsystem super resolution channel (SRC). The SRC is equipped with its own optical system and a 1024 x 1024 framing sensor. SRC produces snapshots with 2.3 in ground pixel size from the nominal spacecraft pericenter height of 250 km, which are typically embedded in the central part of the large HRSC scenes. The salient features of the SRC are its light-weight optics, a reliable CCD detector, and high-speed read-out electronics. The quality and effective visibility of details in the SRC images unfortunately falls short of what has been expected. in cases where thermal balance cannot be reached, artifacts, Such as blurring and "ghost features" are observed in the images. In addition, images show large numbers of blemish pixels and are plagued by electronic noise. As a consequence, we have developed various image improving algorithms, which are discussed in this paper. While results are encouraging, further studies of image restoration by dedicated processing appear worthwhile. The SRC has obtained more than 6940 images at the time of writing (1 September 2007), which often show fascinating details in surface morphology. SRC images are highly useful for a variety of applications in planetary geology, for studies of the Mars atmosphere, and for astrometric observations of the Martian satellites. This paper will give a full account of the design philosophy, technical concept, calibration, operation, integration with HRSC, and performance, as well as science accomplishments of the SRC. (c) 2007 Elsevier Ltd. All rights reserved.
C1 [Oberst, J.; Behnke, T.; Hoffmann, H.; Matz, K. -D.; Flohrer, J.; Hirsch, H.; Roatsch, T.; Scholten, F.; Hauber, E.; Brinkmann, B.; Jaumann, R.] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany.
[Schwarz, G.] German Aerosp Ctr, Remote Sensing Technol Inst, Oberpfaffenhofen, Germany.
[Williams, D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Kirk, R.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Duxbury, T.] Jet Propuls Lab, Pasadena, CA USA.
[Leu, C.; Neukum, G.] Free Univ Berlin, Inst Geosci, D-1000 Berlin, Germany.
RP Oberst, J (reprint author), German Aerosp Ctr, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany.
EM Juergen.Oberst@dlr.de
NR 29
TC 20
Z9 21
U1 1
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 MAR
PY 2008
VL 56
IS 3-4
BP 473
EP 491
DI 10.1016/j.pss.2007.09.009
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 279QZ
UT WOS:000254371000016
ER
PT J
AU Hawes, WM
Duffey, MR
AF Hawes, W. Michael
Duffey, Michael R.
TI Formulation of Financial Valuation Methodologies for NASA's Human
Spaceflight Projects
SO PROJECT MANAGEMENT JOURNAL
LA English
DT Article
DE NASA; real options; project valuation
AB The National Aeronautics and Space Administration (NASA) must continually evaluate proposals to upgrade its human spaceflight systems. These proposals may be initiated to enhance safety, improve performance, or provide improved cost value. In the current restrictive budget environment, the cost valuation should be strengthened to ensure the best use of limited funding. NASA has not frequently utilized financial analysis in project consideration, and business case analysis is often lacking during annual budgetary assessments. Some of the reasons inhibiting financial analysis are uncertainty in the projections of long life-cycle costs, gains that may seem intangible and difficult to monetize, and the political environment. This paper explores ways in which some financial valuation methods, coupled with reformulation of project cash flows, might enhance NASA's analysis process. Among these methods is real option analysis (ROA), which is discussed in the context of several NASA upgrade projects.
C1 [Hawes, W. Michael] NASA Headquarters, Space Operat Mission Directorate, Washington, DC USA.
[Duffey, Michael R.] George Washington Univ, Dept Engn Management & Syst Engn, Washington, DC USA.
RP Hawes, WM (reprint author), NASA Headquarters, Space Operat Mission Directorate, Washington, DC USA.
NR 17
TC 5
Z9 5
U1 0
U2 2
PU WILEY PERIODICALS, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN STREET, MALDEN, MA 02148-529 USA
SN 8756-9728
J9 PROJ MANAG J
JI Proj. Manag. J.
PD MAR
PY 2008
VL 39
IS 1
BP 85
EP 94
DI 10.1002/pmj.20032
PG 10
WC Management
SC Business & Economics
GA V18OM
UT WOS:000208014100008
ER
PT J
AU Almimi, AA
Kulahci, M
Montgomery, DC
AF Almimi, Ashraf A.
Kulahci, Murat
Montgomery, Douglas C.
TI Estimation of missing observations in two-level split-plot designs
SO QUALITY AND RELIABILITY ENGINEERING INTERNATIONAL
LA English
DT Article
DE missing observations; half-normal plot; unreplicated two-level factorial
and fractional factorial split-plot designs; alias chains of effects
AB Inserting estimates for the missing observations from split-plot designs restores their balanced or orthogonal structure and alleviates the difficulties in the statistical analysis. In this article, we extend a method due to Draper and Stoneman to estimate the missing observations from unreplicated two-level factorial and fractional factorial split-plot (FSP and FFSP) designs. The missing observations, which can either be from the same whole plot, from different whole plots, or comprise entire whole plots, are estimated by equating to zero a number of specific contrast columns equal to the number of the missing observations. These estimates are inserted into the design table and the estimates for the remaining effects (or alias chains of effects as the case with FFSP designs) are plotted on two half-normal plots: one for the whole-plot effects and the other for the subplot effects. If the smaller effects do not point at the origin, then different contrast columns to some or all of the initial ones should be discarded and the plots re-examined for bias. Using examples, we show how the method provides estimates for the missing observations that are very close to their actual values. Copyright (C) 2007 John Wiley & Sons, Ltd.
C1 [Almimi, Ashraf A.; Kulahci, Murat; Montgomery, Douglas C.] Arizona State Univ, Dept Ind Engn, Tempe, AZ 85287 USA.
[Kulahci, Murat] Tech Univ Denmark, DK-2800 Lyngby, Denmark.
[Almimi, Ashraf A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Montgomery, DC (reprint author), Arizona State Univ, Dept Ind Engn, Tempe, AZ 85287 USA.
EM doug.montgomery@asu.edu
OI kulahci, murat/0000-0003-4222-9631
NR 11
TC 0
Z9 0
U1 1
U2 3
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND
SN 0748-8017
J9 QUAL RELIAB ENG INT
JI Qual. Reliab. Eng. Int.
PD MAR
PY 2008
VL 24
IS 2
BP 127
EP 152
DI 10.1002/qre.871
PG 26
WC Engineering, Multidisciplinary; Engineering, Industrial; Operations
Research & Management Science
SC Engineering; Operations Research & Management Science
GA 280GP
UT WOS:000254414100002
ER
PT J
AU Muller, J
Kylander, M
Wust, RAJ
Weiss, D
Martinez-Cortizas, A
LeGrande, AN
Jennerjahn, T
Behling, H
Anderson, WT
Jacobson, G
AF Muller, Joanne
Kylander, Malin
Wuest, Raphael A. J.
Weiss, Dominik
Martinez-Cortizas, Antonio
LeGrande, Allegra N.
Jennerjahn, Tim
Behling, Herman
Anderson, William T.
Jacobson, Geraldine
TI Possible evidence for wet Heinrich phases in tropical NE Australia: the
Lynch's Crater deposit
SO QUATERNARY SCIENCE REVIEWS
LA English
DT Article
ID ABRUPT CLIMATE-CHANGE; INTERDECADAL PACIFIC OSCILLATION; NORTHEASTERN
BRAZIL; CONVERGENCE ZONE; ICE; EVENTS; CYCLES; RECORD; OCEAN;
CONSEQUENCES
AB Unarguably, one of the most significant paleoclimatological discoveries of the last two decades has been that of abrupt climate events (Dansgaard-Oeschger cycles and Heinrich events). Most evidence for these events has originated from the high-latitude Northern Hemisphere.. with few records documenting the response of the low latitude Southern Hemisphere. Here we present new data from Lynch's Crater, a unique terrestrial record from NE-Australia that may show evidence for southward propagations of the Intertropical Convergence Zone (ITCZ) during abrupt climate perturbations as a result of alteration of the low latitude air masses. Proxies for precipitation/wetness indicate enhanced rainfall in the region during Heinrich events (H events 1-3) and the 8.2 ka Northern Hemisphere cold event. A fully coupled atmosphere/ocean climate model simulating a 1 Sv freshwater influx to the North Atlantic Ocean produces a scenario which agrees with the climate changes shown by the Lynch's Crater record. The model shows precipitation anomalies that include a southward migration of the ITCZ and a zonal shift in mid-latitude storm tracks over the Southern Hemisphere equatorial region. These data indicate large-scale shifts of the austral summer ITCZ position that is known to control monsoonal precipitation in NE Australia. This terrestrial record from Australia may demonstrate the involvement of the tropical western Pacific Ocean in ITCZ migrations during abrupt climate events of the last glacial period. Defining such past migrations offers insight into the importance and role of the equatorial region in global climate dynamics. (C) 2007 Elsevier Ltd. All rights reserved.
C1 [Muller, Joanne] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
[Kylander, Malin; Weiss, Dominik] James Cook Univ N Queensland, Sch Earth Sci, Townsville, Qld 4811, Australia.
[Kylander, Malin; Weiss, Dominik] Nat Hist Museum London, London SW7 2AZ, England.
[Martinez-Cortizas, Antonio] Fac Biol, Dept Edafol & Quim Agricola, E-15782 Santiago, Spain.
[LeGrande, Allegra N.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[LeGrande, Allegra N.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
[Jennerjahn, Tim] Zentrum Marine Tropenokol, D-28359 Bremen, Germany.
[Behling, Herman] Univ Gottingen, Albrecht Von Haller Inst Plant Sci, Dept Palynol & Climate Dynam, D-37073 Gottingen, Germany.
[Anderson, William T.] Florida Int Univ, SE Environm Res Ctr, Dept Earth Sci, Miami, FL 33199 USA.
[Jacobson, Geraldine] Australian Nucl Sci & Technol Org, Sydney, NSW, Australia.
RP Muller, J (reprint author), Woods Hole Oceanog Inst, Mail Stop 21, Woods Hole, MA 02543 USA.
EM jmuller@whoi.edu
RI LeGrande, Allegra/D-8920-2012; Martinez Cortizas, Antonio/M-6196-2015;
OI LeGrande, Allegra/0000-0002-5295-0062; Martinez Cortizas,
Antonio/0000-0003-0430-5760; Weiss, Dominik/0000-0001-8074-9430
NR 42
TC 49
Z9 51
U1 0
U2 12
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0277-3791
J9 QUATERNARY SCI REV
JI Quat. Sci. Rev.
PD MAR
PY 2008
VL 27
IS 5-6
BP 468
EP 475
DI 10.1016/j.quascirev.2007.11.006
PG 8
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA 293RH
UT WOS:000255351900004
ER
PT J
AU Adams, DO
Yarger, CB
Webb, NJ
Hunter, A
Oborn, KD
Saether, E
Wilson, JW
Badavi, FF
AF Adams, D. O.
Yarger, C. B.
Webb, N. J.
Hunter, A.
Oborn, K. D.
Saether, E.
Wilson, J. W.
Badavi, F. F.
TI Multi-functional sandwich composite for spacecraft applications
SO SAMPE JOURNAL
LA English
DT Article
AB Multi-functional sandwich composites are proposed to integrate the previously separate objectives of radiation shielding, structural integrity, damage tolerance, thermal insulation, and debris/micrometeoroid shielding into a viable structural design. Effective radiation shielding is provided through the selection of hydrogen-rich polymeric materials for the primary sandwich composite structure. Using facesheet and core materials selected based on radiation shielding simulations, prototype sandwich configurations were manufactured that featured transverse reinforcements for damage tolerance and an internal Surlyn(R) self-healing membrane layer. Flatwise tensile and core shear testing were performed to assess material compatibility between the facesheet and core layers and to identify any manufacturing-related problems. Acceptable interlaminar strengths were obtained for all configurations investigated. The results from this initial assessment suggest that multi-functional sandwich composite configurations may be used to maximize the efficiency of advanced material usage in future structural spacecraft applications.
C1 [Adams, D. O.; Yarger, C. B.; Webb, N. J.; Hunter, A.; Oborn, K. D.] Univ Utah, Dept Mech Engn, Salt Lake City, UT 84112 USA.
[Saether, E.; Wilson, J. W.] NASA Langley Res Ctr, Hampton, VA USA.
[Badavi, F. F.] Christopher Newport Univ, Dept Phys, Newport News, VA 23606 USA.
RP Adams, DO (reprint author), Univ Utah, Dept Mech Engn, Salt Lake City, UT 84112 USA.
NR 11
TC 1
Z9 1
U1 1
U2 7
PU SAMPE PUBLISHERS
PI COVINA
PA 1161 PARKVIEW DRIVE, COVINA, CA 91722 USA
SN 0091-1062
J9 SAMPE J
JI Sampe J.
PD MAR-APR
PY 2008
VL 44
IS 2
BP 38
EP 49
PG 12
WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 266UT
UT WOS:000253463300005
ER
PT J
AU Zander, R
Mahieu, E
Demoulin, P
Duchatelet, P
Roland, G
Servais, C
De Maziere, M
Reimann, S
Rinsland, CP
AF Zander, R.
Mahieu, E.
Demoulin, P.
Duchatelet, P.
Roland, G.
Servais, C.
De Maziere, M.
Reimann, S.
Rinsland, C. P.
TI Our changing atmosphere: Evidence based on long-term infrared solar
observations at the Jungfraujoch since 1950
SO SCIENCE OF THE TOTAL ENVIRONMENT
LA English
DT Article; Proceedings Paper
CT International Conference Celebrating the 75th Anniversary of the High
Altitude Research Station Jungfraujoch
CY SEP 11-13, 2006
CL Interlaken, SWITZERLAND
DE atmospheric composition changes; infrared remote sensing; infrared
spectroscopy; climate change; Montreal and Kyoto Protocols
ID GROUND-BASED FTIR; SPECTROSCOPIC MEASUREMENTS; STRATOSPHERIC CHLORINE;
COLUMN ABUNDANCES; STATION; NORTHERN; TREND; HEMISPHERE; SPECTRA; CLONO2
AB The Institute of Astrophysics of the University of Liege has been present at the High Altitude Research Station Jungfraujoch, Switzerland, since the late 1940s, to perform spectrometric solar observations under dry and weakly polluted high-mountain conditions. Several solar atlases of photometric quality, extending altogether from the near-ultra-violet to the middle-infrared, were produced between 1956 and 1994, first with grating spectrometers then with Fourier transform instruments. During the early 1970s, scientific concerns emerged about atmospheric composition changes likely to set in as a consequence of the growing usage of nitrogen-containing agricultural fertilisers and the industrial production of chlorine-bearing compounds such as the chlorofluorocarbons and hydrochlorofluorocarbons. Resulting releases to the atmosphere with ensuing photolysis in the stratosphere and catalytic depletion of the protective ozone layer prompted a worldwide consortium of chemical manufacturing companies to solicit the Liege group to help in clarifying these concerns by undertaking specific observations with its existing Jungfraujoch instrumentation. The following pages evoke the main steps that led from quasi full sun-oriented studies to priority investigations of the Earth's atmosphere, in support of both the Montreal and the Kyoto Protocols. (c) 2007 Elsevier B.V. All rights reserved.
C1 [Zander, R.; Mahieu, E.; Demoulin, P.; Duchatelet, P.; Roland, G.; Servais, C.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[De Maziere, M.] Belgian Inst Space Aeron, Brussels, Belgium.
[Rinsland, C. P.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Zander, R (reprint author), Univ Liege, Inst Astrophys & Geophys, 17,Allee 6 Aout, B-4000 Liege, Belgium.
EM r.zander@ulg.ac.be
RI Reimann, Stefan/A-2327-2009;
OI Reimann, Stefan/0000-0002-9885-7138; Mahieu,
Emmanuel/0000-0002-5251-0286
NR 52
TC 40
Z9 41
U1 1
U2 8
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0048-9697
EI 1879-1026
J9 SCI TOTAL ENVIRON
JI Sci. Total Environ.
PD MAR 1
PY 2008
VL 391
IS 2-3
BP 184
EP 195
DI 10.1016/j.scitotenv.2007.10.018
PG 12
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA 261FU
UT WOS:000253065300003
PM 18067951
ER
PT J
AU Fong, R
AF Fong, Ron
TI Goodbye to LD50?
SO SCIENTIST
LA English
DT Letter
C1 NASA, Moffett Field, CA 94035 USA.
RP Fong, R (reprint author), NASA, Moffett Field, CA 94035 USA.
EM ronald.c.fong@nasa.gov
NR 1
TC 0
Z9 0
U1 0
U2 0
PU SCIENTIST INC
PI PHILADELPHIA
PA 3535 MARKET ST, SUITE 200, PHILADELPHIA, PA 19104-3385 USA
SN 0890-3670
J9 SCIENTIST
JI Scientist
PD MAR
PY 2008
VL 22
IS 3
BP 16
EP 17
PG 2
WC Information Science & Library Science; Multidisciplinary Sciences
SC Information Science & Library Science; Science & Technology - Other
Topics
GA 265IL
UT WOS:000253352200010
ER
PT J
AU Michalek, G
Gopalswamy, N
Yashiro, S
AF Michalek, G.
Gopalswamy, N.
Yashiro, S.
TI Space weather application using projected velocity asymmetry of halo
CMEs
SO SOLAR PHYSICS
LA English
DT Article
DE Sun : solar activity; Sun : coronal mass ejections
ID CORONAL MASS EJECTIONS; CONE MODEL; STORMS
AB Halo coronal mass ejections (HCMEs) originating from regions close to the center of the Sun are likely to be responsible for severe geomagnetic storms. It is important to predict geoeffectiveness of HCMEs by using observations when they are still near the Sun. Unfortunately, coronagraphic observations do not provide true speeds of CMEs because of projection effects. In the present paper, we present a new technique to allow estimates of the space speed and approximate source location using projected speeds measured at different position angles for a given HCME (velocity asymmetry). We apply this technique to HCMEs observed during 2001-2002 and find that the improved speeds are better correlated with the travel times of HCMEs to Earth and with the magnitudes of ensuing geomagnetic storms.
C1 [Michalek, G.] Jagiellonian Univ, Astron Observ, Krakow, Poland.
[Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Yashiro, S.] Catholic Univ Amer, Ctr Solar & Space Weather, Washington, DC 20064 USA.
RP Michalek, G (reprint author), Jagiellonian Univ, Astron Observ, Krakow, Poland.
EM michalek@oa.uj.edu.pl
RI Gopalswamy, Nat/D-3659-2012
NR 29
TC 6
Z9 6
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 MAR
PY 2008
VL 248
IS 1
BP 113
EP 123
DI 10.1007/s11207-008-9126-7
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 280QM
UT WOS:000254441300008
ER
PT J
AU Lepping, RP
Wu, CC
Gopalswamy, N
Berdichevsky, DB
AF Lepping, R. P.
Wu, C. -C.
Gopalswamy, N.
Berdichevsky, D. B.
TI Average thickness of magnetosheath upstream of magnetic clouds at 1 AU
versus solar longitude of source
SO SOLAR PHYSICS
LA English
DT Article
DE magnetic clouds; solar wind; shock waves; magnetosheath
ID CORONAL MASS EJECTIONS; MAGNETOSPHERE; ORIGIN; FIELDS; SHOCK; WIND
AB Starting with a large number (N = 100) of Wind magnetic clouds (MCs) and applying necessary restrictions, we find a proper set of N = 29 to investigate the average ecliptic plane projection of the upstream magnetosheath thickness as a function of the longitude of the solar source of the MCs, for those cases of MCs having upstream shock waves. A few of the obvious restrictions on the full set of MCs are the need for there to exist a driven upstream shock wave, knowledge of the MC's solar source, and restriction to only MCs of low axial latitudes. The analysis required splitting this set into two subsets according to average magnetosheath speed: slow/average (300-500 km s(-1)) and fast (500-1100 km s(-1)) speeds. Only the fast set gives plausible results, where the estimated magnetosheath thickness (Delta S) goes from 0.042 to 0.079 AU (at 1 AU) over the longitude sector of 0 degrees (adjusted source-center longitude of the average magnetic cloud) to 40 off center ( East or West), based on N = 11 appropriate cases. These estimates are well determined with a sigma (sigma) for the fit of 0.0055 AU, where s is effectively the same as root(chi- squared) for the appropriate quadratic fit. The associated linear correlation coefficient for Delta S versus vertical bar Longitude vertical bar was very good (c.c. = 0.93) for the fast range, and Delta S at 60 degrees longitude is extrapolated to be 2.7 times the value at 0 degrees. For the slower speeds we obtain the surprising result that Delta S is typically more-or-less constant at 0.040 +/- 0.013 AU at all longitudes, indicating that the MC as a driver, when moving close to the normal solar wind speed, has little influence on magnetosheath thickness. In some cases, the correct choice between two candidate solarsource longitudes for a fast MC might be made by noting the value of the observed Delta S just upstream of the MC. Also, we point out that, for the 29 events, the average sheath speed was well correlated with the quantity Delta V[= (< V-MC > - < V-UPSTREAM >)], and also with both < V-MC > and < V-MC,V-T > , where < V-MC > is the first one-hour average of the MC speed, < V-MC,V-T > is the average MC speed across the full MC, and < V-UPSTREAM > is a five-hour average of the solar wind speed just upstream of the shock.
C1 [Lepping, R. P.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
[Wu, C. -C.] Univ Alabama, Huntsville, AL 35899 USA.
[Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Berdichevsky, D. B.] Sigma Space Corp, Lanham, MD 20706 USA.
RP Lepping, RP (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
EM ronald.p.lepping@nasa.gov
RI Gopalswamy, Nat/D-3659-2012
NR 30
TC 3
Z9 3
U1 0
U2 2
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 MAR
PY 2008
VL 248
IS 1
BP 125
EP 139
DI 10.1007/s11207-007-9111-6
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 280QM
UT WOS:000254441300009
ER
PT J
AU Mckay, CP
AF Mckay, Christopher P.
TI An approach to searching for life on Mars, Europa, and Enceladus
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE life; Mars; Europa; Enceladus; second genesis
ID GLOBAL DISTRIBUTION
AB Near-term missions may be able to access samples of organic material from Mars, Europa, and Enceladus. The challenge for astrobiology will be to determine if this material is the remains of dead microorganisms or merely abiotic organic material. The remains of life that shares a common origin with life on Earth will be straightforward to detect using sophisticated methods such as DNA amplification. These methods are extremely sensitive but specific to Earth-like life. Detecting the remains of alien life-that does not have a genetic or biochemical commonality with Earth life-will be much more difficult. There is a general property of life that can be used to determine if organic material is of biological origin. This general property is the repeated use of a few specific organic molecules for the construction of biopolymers. For example, Earth-like life uses 20 amino acids to construct proteins, 5 nucleotide bases to construct DNA and RNA, and a few sugars to construct polysaccharides. This selectivity will result in a statistically anomalous distribution of organic molecules distinct from organic material of non-biological origin. Such a distinctive pattern, different from the pattern of Earth-like life, will be persuasive evidence for a second genesis of life.
C1 NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Mckay, CP (reprint author), NASA, Ames Res Ctr, Div Space Sci, Mail Stop 245 3, Moffett Field, CA 94035 USA.
EM cmckay@mail.arc.nasa.gov
NR 15
TC 7
Z9 7
U1 2
U2 24
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAR
PY 2008
VL 135
IS 1-4
BP 49
EP 54
DI 10.1007/s11214-007-9229-8
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 322OB
UT WOS:000257384100006
ER
PT J
AU Mahaffy, P
AF Mahaffy, Paul
TI Exploration of the habitability of Mars: Development of analytical
protocols for measurement of organic carbon on the 2009 Mars science
laboratory
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars; organics; Mars Science Laboratory; Sample Analysis at Mars;
investigation; astrobiology
ID MARTIAN METEORITE ALH84001; POLYCYCLIC AROMATIC-HYDROCARBONS;
CHROMATOGRAPHY-MASS-SPECTROMETRY; IN-SITU ANALYSES; AMINO-ACIDS;
ATMOSPHERE; SURFACE; SEARCH; METHANE; ORIGIN
AB The mission goal of the 2009 Mars Science Laboratory is to assess the habitability of a region on Mars. This large rover incorporates an Analytical Laboratory that contributes to this mission objective by means of a detailed characterization of mineralogy and chemistry. The Sample Analysis at Mars instrument suite in the Analytical Laboratory provides the capability to analyze volatiles released from rocks and soils and gases directly sample from the atmosphere. A primary focus of this suite is the detection and identification of organic molecules. The protocols for the extraction and analysis of organics under development for this mission are described as are experiments carried out on Mars analog samples to evaluate these methods.
C1 NASA, Goddard Space Flight Ctr, Atmospher Expt Lab, Greenbelt, MD 20771 USA.
RP Mahaffy, P (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Expt Lab, Greenbelt, MD 20771 USA.
EM Paul.R.Mahaffy@nasa.gov
RI Mahaffy, Paul/E-4609-2012
NR 48
TC 31
Z9 31
U1 0
U2 7
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAR
PY 2008
VL 135
IS 1-4
BP 255
EP 268
DI 10.1007/s11214-007-9223-1
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 322OB
UT WOS:000257384100018
ER
PT J
AU Bada, JL
Ehrenfreund, P
Grunthaner, F
Blaney, D
Coleman, M
Farrington, A
Yen, A
Mathies, R
Amudson, R
Quinn, R
Zent, A
Ride, S
Barron, L
Botta, O
Clark, B
Glavin, D
Hofmann, B
Josset, JL
Rettberg, P
Robert, F
Sephton, M
AF Bada, J. L.
Ehrenfreund, P.
Grunthaner, F.
Blaney, D.
Coleman, M.
Farrington, A.
Yen, A.
Mathies, R.
Amudson, R.
Quinn, R.
Zent, A.
Ride, S.
Barron, L.
Botta, O.
Clark, B.
Glavin, D.
Hofmann, B.
Josset, J. L.
Rettberg, P.
Robert, F.
Sephton, M.
TI Urey: Mars Organic and Oxidant Detector
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars; life detection instrumentation; space research
ID ATACAMA DESERT; MARTIAN SOIL; AMINO-ACIDS; LIFE; ATMOSPHERE;
PRESERVATION; REACTIVITY; MOLECULES; METHANE; SEARCH
AB One of the fundamental challenges facing the scientific community as we enter this new century of Mars research is to understand, in a rigorous manner, the biotic potential both past and present of this outermost terrestrial-like planet in our solar system. Urey: Mars Organic and Oxidant Detector has been selected for the Pasteur payload of the European Space Agency's (ESA's) ExoMars rover mission and is considered a fundamental instrument to achieve the mission's scientific objectives. The instrument is named Urey in recognition of Harold Clayton Urey's seminal contributions to cosmochemistry, geochemistry, and the study of the origin of life. The overall goal of Urey is to search for organic compounds directly in the regolith of Mars and to assess their origin. Urey will perform a groundbreaking investigation of the Martian environment that will involve searching for organic compounds indicative of life and prebiotic chemistry at a sensitivity many orders of magnitude greater than Viking or other in situ organic detection systems. Urey will perform the first in situ search for key classes of organic molecules using state-of-the-art analytical methods that provide part-per-trillion sensitivity. It will ascertain whether any of these molecules are abiotic or biotic in origin and will evaluate the survival potential of organic compounds in the environment using state-of-the-art chemoresistor oxidant sensors.
C1 [Bada, J. L.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Ehrenfreund, P.] Leiden Univ, Leiden Inst Chem, NL-2300 RA Leiden, Netherlands.
[Grunthaner, F.; Blaney, D.; Coleman, M.; Farrington, A.; Yen, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mathies, R.; Amudson, R.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Quinn, R.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Ride, S.] Imaginary Lines Inc, San Diego, CA 92122 USA.
[Barron, L.] Univ Glasgow, Dept Chem, Glasgow G12 8QQ, Lanark, Scotland.
[Botta, O.] Int Space Sci Inst, CH-3012 Bern, Switzerland.
[Clark, B.] Lockheed Martin, Space Explorat Syst, Denver, CO 80201 USA.
[Glavin, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hofmann, B.] Nat Hist Museum Burgergemeinde Bern, CH-3005 Bern, Switzerland.
[Josset, J. L.] Space Explorat Inst SPACE X, Neuchatel, Switzerland.
[Rettberg, P.] Inst Aerosp Med Radiat Biol, D-51147 Cologne, Germany.
[Robert, F.] Museum Natl Hist Nat, LEME NanoAnal, F-75005 Paris, France.
[Sephton, M.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London SW7 2AZ, England.
RP Bada, JL (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
EM jbada@ucsd.edu
RI Glavin, Daniel/D-6194-2012; Rettberg, Petra/K-2378-2015;
OI Glavin, Daniel/0000-0001-7779-7765; Rettberg, Petra/0000-0003-4439-2395;
Sephton, Mark/0000-0002-2190-5402
NR 36
TC 10
Z9 10
U1 4
U2 19
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAR
PY 2008
VL 135
IS 1-4
BP 269
EP 279
DI 10.1007/s11214-007-9213-3
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 322OB
UT WOS:000257384100019
ER
PT J
AU Briggs, C
Little, P
AF Briggs, Clark
Little, Patrick
TI Impacts of organizational culture and personality traits on
decision-making in technical organizations
SO SYSTEMS ENGINEERING
LA English
DT Article
DE organizational culture; decision making; decision analysis
AB Technical organizations in industries such as aerospace or automotive regularly make major decisions regarding software and other tools to support mission-critical activities. These decisions take place at the enterprise level where functional departments must work together in ways not common before. Usually, these are high-impact, tension-filled decision activities that have long term effects. The organization needs a successful decision that stands the test of implementation and a sustained period of effective operation. The processes used in such cases generally follow analytical decision methods aimed at maximizing objectives. Understanding the characteristics of the organization, including the culture and the affected parties, in addition to the technical aspects of the decision may significantly increase the likelihood of success. (C) 2007 Wiley Periodicals, Inc.
C1 [Briggs, Clark] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
[Little, Patrick] Harvey Mudd Coll, Claremont, CA 91711 USA.
RP Briggs, C (reprint author), CALTECH, Jet Prop Lab, NASA, M-S 158-224,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Clark.Briggs@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The research described in this paper was carried out in part at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 23
TC 3
Z9 3
U1 1
U2 4
PU JOHN WILEY & SONS INC
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 1098-1241
J9 SYST ENG
JI Syst. Eng.
PD SPR
PY 2008
VL 11
IS 1
BP 15
EP 26
DI 10.1002/sys.20083
PG 12
WC Engineering, Industrial; Operations Research & Management Science
SC Engineering; Operations Research & Management Science
GA 340RN
UT WOS:000258662800002
ER
PT J
AU Weidman, PD
Davis, AMJ
Kubitschek, DG
AF Weidman, P. D.
Davis, A. M. J.
Kubitschek, D. G.
TI Crocco variable formulation for uniform shear flow over a stretching
surface with transpiration: Multiple solutions and stability
SO ZEITSCHRIFT FUR ANGEWANDTE MATHEMATIK UND PHYSIK
LA English
DT Article
DE shear flow; boundary layer; plate stretching; suction; multiple
solutions; stability
ID BOUNDARY-LAYER FLOW; REVERSE FLOW; MOVING-WALL
AB The simultaneous effects of transpiration through and tangential movement of a semi-infinite flat plate on the self-similar boundary layer flow driven by uniform shear in the far field is considered. Difficulties with standard shooting techniques are overcome using Crocco variables which also serve to better elucidate the solution structure. The stabilities of dual, triple and even quadruple steady flow solutions encountered in different ranges of plate stretching and wall stress are determined using a linear temporal stability analysis for the self-similar flow.
C1 [Weidman, P. D.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA.
[Davis, A. M. J.] Univ Alabama, Dept Math, Tuscaloosa, AL 35487 USA.
[Kubitschek, D. G.] CALTECH, Jet Prop Lab, Opt Navigat Grp, Pasadena, CA 91109 USA.
RP Weidman, PD (reprint author), Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA.
NR 16
TC 10
Z9 10
U1 0
U2 1
PU BIRKHAUSER VERLAG AG
PI BASEL
PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND
SN 0044-2275
J9 Z ANGEW MATH PHYS
JI Z. Angew. Math. Phys.
PD MAR
PY 2008
VL 59
IS 2
BP 313
EP 332
DI 10.1007/s00033-006-6018-2
PG 20
WC Mathematics, Applied
SC Mathematics
GA 269XN
UT WOS:000253684200007
ER
PT J
AU Choi, Y
Wang, YH
Yang, Q
Cunnold, D
Zeng, T
Shim, C
Luo, M
Eldering, A
Bucsela, E
Gleason, J
AF Choi, Yunsoo
Wang, Yuhang
Yang, Qing
Cunnold, Derek
Zeng, Tao
Shim, Changsub
Luo, Ming
Eldering, Annmarie
Bucsela, Eric
Gleason, James
TI Spring to summer northward migration of high O-3 over the western North
Atlantic
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ART.; TRANSPORT; TROPOSPHERE; POLLUTION; OZONE; MODEL
AB Tropospheric O-3 columns retrieved from OMI and MLS measurements, NO2 columns from OMI, and upper tropospheric O-3 concentrations from TES over North America and the western North Atlantic from April to August 2005 are analyzed using the Regional chEmical and trAnsport Model (REAM). Large enhancements of column and upper tropospheric O-3 over the western North Atlantic comparable to those over the eastern United States are found in the satellite measurements and REAM simulations. The O-3 enhancement region migrates northward from spring to summer. Model analysis indicates that the northward migration is driven by seasonal shifts of O-3 transported from the stratosphere and that produced through photochemistry from surface emissions and lightning NOx. As their uncertainties improve, satellite measurements of O-3 and its precursors will be able to provide more quantitative constraints on pollutant outflow from the continents.
C1 [Shim, Changsub; Luo, Ming; Eldering, Annmarie] Jet Prop Lab, Pasadena, CA 91109 USA.
[Choi, Yunsoo; Wang, Yuhang; Yang, Qing; Cunnold, Derek; Zeng, Tao] Georgia Inst Technol, Dept Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Bucsela, Eric; Gleason, James] NASA GSFC, Greenbelt, MD 20771 USA.
RP Choi, Y (reprint author), Jet Prop Lab, Pasadena, CA 91109 USA.
EM yunsoo.choi@jpl.nasa.gov
RI Yang, Qing/H-3275-2011; Gleason, James/E-1421-2012; Wang,
Yuhang/B-5578-2014
OI Yang, Qing/0000-0003-2067-5999;
NR 18
TC 23
Z9 23
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 FEB 29
PY 2008
VL 35
IS 4
AR L04818
DI 10.1029/2007GL032276
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 270IV
UT WOS:000253715400002
ER
PT J
AU Deshler, T
Mercer, JL
Smit, HGJ
Stubi, R
Levrat, G
Johnson, BJ
Oltmans, SJ
Kivi, R
Thompson, AM
Witte, J
Davies, J
Schmidlin, FJ
Brothers, G
Sasaki, T
AF Deshler, Terry
Mercer, Jennifer L.
Smit, Herman G. J.
Stubi, Rene
Levrat, Gilbert
Johnson, Bryan J.
Oltmans, Samuel J.
Kivi, Rigel
Thompson, Anne M.
Witte, Jacquelyn
Davies, Jonathan
Schmidlin, F. J.
Brothers, G.
Sasaki, Toru
TI Atmospheric comparison of electrochemical cell ozonesondes from
different manufacturers, and with different cathode solution strengths:
The Balloon Experiment on Standards for Ozonesondes
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID GROUND-BASED LIDAR; INTERCOMPARISON CAMPAIGN; VERTICAL-DISTRIBUTION;
OZONE PROFILES; STOIC 1989; TROPOSPHERIC OZONE; ECC; PHOTOMETER;
ACCURACY; TRENDS
AB A balloon flight to compare 18 ozonesondes with an ozone photometer and with ozone column measurements from Dobson and Brewer spectrophotometers was completed in April 2004. The core experiment consisted of 12 electrochemical concentration cell ozonesondes, 6 from Science Pump Corporation (SP) and 6 from ENSCI Corporation (ES), prepared with cathode solution concentrations of 0.5% KI (half buffer) and 1.0% KI (full buffer). Auxiliary ozonesondes consisted of two electrochemical concentration cell sondes with 2.0% KI (no buffer), two reconditioned sondes, and two Japanese-KC96 sondes. Precision of each group of similarly prepared ozonesondes was <2-3%. The six ozonesondes prepared according to the manufacturer's recommendations (SP, 1.0% KI, ES 0.5% KI) overestimated the photometer measurements by 5-10% in the stratosphere, but provided ozone columns in good agreement with the ground-based spectrophotometer measurements. This is consistent with the difference (similar to 5%) in ozone photometer and column measurements observed during the experiment. Using cathode cell concentrations of 1.0% KI for ES sondes caused overestimates of the photometer by 10-15% and of ozone column by 5-10%. In contrast, 0.5% KI in SP sondes led to good agreement with the photometer, but underestimates of ozone column. The KC96 sondes underestimated the photometer measurements by about 5-15% at air pressures above 30 hPa. Agreement was within 5% at lower pressures. Diluting the solution concentration and the buffers from 1.0% to 0.5% KI causes an approximately linear pressure-dependent decrease in ozone for both SP and ES sondes, ratio (0.5 KI/1.0 KI) = 0.9 + 0.024* log(10)(Pressure).
C1 [Deshler, Terry; Mercer, Jennifer L.] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA.
[Smit, Herman G. J.] Forschungszentrum Julich, Inst Chem & Dynam Geosphere 2, D-52425 Julich, Germany.
[Stubi, Rene; Levrat, Gilbert] MeteoSwiss, Fed Off Meteorol & Climatol, Aerol Stn Payerne, CH-1530 Payerne, Switzerland.
[Johnson, Bryan J.; Oltmans, Samuel J.] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Kivi, Rigel] Finnish Meteorol Inst, Arctic Res Ctr, FIN-99600 Sodankyla, Finland.
[Thompson, Anne M.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Witte, Jacquelyn] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Schmidlin, F. J.; Brothers, G.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
[Davies, Jonathan] Environm Canada, Air Qual Res Div, Toronto, ON M3H 5T4, Canada.
[Witte, Jacquelyn] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sasaki, Toru] Japan Meteorol Agcy, Tokyo, Japan.
RP Deshler, T (reprint author), Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA.
EM deshler@uwyo.edu; mercer@uwyo.edu; h.smit@fz-juelich.de;
rene.stubi@meteoswiss.ch; bryan.johnson@noaa.gov;
samuel.j.oltmans@noaa.gov; rigel.kivi@fmi.fi; anne@met.psu.edu;
witte@gavial.gsfc.nasa.gov; jonathan.davies@ec.gc.ca;
fjs@osb1.wff.gsfc.gov; tsasaki@naps.kishou.go.jp
RI Smit, Herman/J-2397-2012; Thompson, Anne /C-3649-2014
OI Smit, Herman/0000-0002-2268-4189; Thompson, Anne /0000-0002-7829-0920
NR 45
TC 58
Z9 60
U1 4
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 29
PY 2008
VL 113
IS D4
AR D04307
DI 10.1029/2007JD008975
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 270JA
UT WOS:000253715900004
ER
PT J
AU Yang, YK
Di Girolamo, L
AF Yang, Yuekui
Di Girolamo, Larry
TI Impacts of 3-D radiative effects on satellite cloud detection and their
consequences on cloud fraction and aerosol optical depth retrievals
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CLEAR-SKY REFLECTANCE; SPATIAL-RESOLUTION; ALGORITHM; ISCCP; RADIANCES;
MODIS; CLASSIFICATION; INSTRUMENTS; BRIGHTNESS; VALIDATION
AB We present the first examination on how 3-D radiative transfer impacts satellite cloud detection that uses a single visible channel threshold. The 3-D radiative transfer through predefined heterogeneous cloud fields embedded in a range of horizontally homogeneous aerosol fields have been carried out to generate synthetic nadir-viewing satellite images at a wavelength of 0.67 mu m. The finest spatial resolution of the cloud field is 30 m. We show that 3-D radiative effects cause significant histogram overlap between the radiance distribution of clear and cloudy pixels, the degree to which depends on many factors (resolution, solar zenith angle, surface reflectance, aerosol optical depth (AOD), cloud top variability, etc.). This overlap precludes the existence of a threshold that can correctly separate all clear pixels from cloudy pixels. The region of clear/cloud radiance overlap includes moderately large (up to 5 in our simulations) cloud optical depths. Purpose-driven cloud masks, defined by different thresholds, are applied to the simulated images to examine their impact on retrieving cloud fraction and AOD. Large (up to 100s of %) systematic errors were observed that depended on the type of cloud mask and the factors that influence the clear/cloud radiance overlap, with a strong dependence on solar zenith angle. Different strategies in computing domain-averaged AOD were performed showing that the domain-averaged BRF from all clear pixels produced the smallest AOD biases with the weakest (but still large) dependence on solar zenith angle. The large dependence of the bias on solar zenith angle has serious implications for climate research that uses satellite cloud and aerosol products.
C1 [Yang, Yuekui; Di Girolamo, Larry] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA.
RP Yang, YK (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
EM yuekui@umbc.edu
RI Yang, Yuekui/B-4326-2015
NR 49
TC 22
Z9 22
U1 0
U2 6
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 29
PY 2008
VL 113
IS D4
AR D04213
DI 10.1029/2007JD009095
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 270JA
UT WOS:000253715900007
ER
PT J
AU Comiso, JC
Steffen, K
AF Comiso, Josefino C.
Steffen, Konrad
TI Introduction to special section on Large-Scale Characteristics of the
Sea Ice Cover from AMSR-E and Other Satellite Sensors
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Editorial Material
C1 [Comiso, Josefino C.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA.
[Steffen, Konrad] Univ Colorado, CIRES, Boulder, CO 80309 USA.
RP Comiso, JC (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA.
EM josefino.c.comiso@nasa.gov
RI Steffen, Konrad/C-6027-2013
OI Steffen, Konrad/0000-0001-8658-1026
NR 27
TC 6
Z9 6
U1 0
U2 4
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 29
PY 2008
VL 113
IS C2
AR C02S01
DI 10.1029/2007JC004442
PG 3
WC Oceanography
SC Oceanography
GA 270JH
UT WOS:000253716600004
ER
PT J
AU Nieves-Chinchilla, T
Vinas, AF
AF Nieves-Chinchilla, Teresa
Vinas, Adolfo F.
TI Solar wind electron distribution functions inside magnetic clouds
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID CORONAL MASS EJECTIONS; KAPPA-DISTRIBUTIONS; AU; PARAMETERS; VOYAGER;
PLASMAS; HELIOS; WAVES; CORE
AB This paper presents a study of the kinetic properties of the electron velocity distribution functions within interplanetary magnetic clouds, since they are the dominant thermal component and can contribute as much as 50% of the total electron pressure within the clouds. The study is based on high time resolution data from the Goddard Space Flight Center Wind Solar Wind Experiment vector electron and ion spectrometer. Studies on interplanetary magnetic clouds have shown observational evidence of anticorrelation between the total electron density and temperature, which suggests a polytrope law P(e) = alpha n(e)(gamma) g for electrons with the constant gamma approximate to 0.5 < 1. This anticorrelation and small gamma values are interpreted in the context of the presence of highly non-Maxwellian electron distributions (i.e., nonthermal tails) within magnetic clouds. We have revisited some of the magnetic cloud events previously studied to quantify the nature of the nonthermal electrons by modeling the electron velocity distribution function using Maxwellian and kappa-like distribution functions to characterize the kinetic nonthermal effects. The results show that the electron density-temperature anticorrelation is not a unique feature of magnetic clouds. Within magnetic clouds, k values are generally small, in the range of 1.6-5.4; however, such small values are also typical of regions outside the clouds. We have shown that the density-temperature anticorrelation of the electron moments is persistently consistent with similar density-temperature anticorrelation in the electron halo component of the velocity distribution function and essentially little or no correlation was obtained for the core component. This result clearly shows that the temperature and density of the suprathermal components play a significant role in the temperature-density anticorrelation because of a relative enhancement of the halo component abundance to the total density.
C1 [Nieves-Chinchilla, Teresa; Vinas, Adolfo F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA.
RP Nieves-Chinchilla, T (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Mail Code 673, Greenbelt, MD 20771 USA.
EM adolfo.figueroa-vinas.1@gsfc.nasa.gov
RI Nieves-Chinchilla, Teresa/F-3482-2016
OI Nieves-Chinchilla, Teresa/0000-0003-0565-4890
NR 32
TC 29
Z9 29
U1 0
U2 1
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 28
PY 2008
VL 113
IS A2
AR A02105
DI 10.1029/2007JA012703
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 270JV
UT WOS:000253718000001
ER
PT J
AU Cockell, CS
Mckay, CP
Warren-Rhodes, K
Horneck, G
AF Cockell, Charles S.
Mckay, Christopher P.
Warren-Rhodes, Kim
Horneck, Gerda
TI Ultraviolet radiation-induced limitation to epilithic microbial growth
in and deserts - Dosimetric experiments in the hyperarid core of the
Atacama Desert
SO JOURNAL OF PHOTOCHEMISTRY AND PHOTOBIOLOGY B-BIOLOGY
LA English
DT Article
DE Atacama; desiccation; chroococcidiopsis; dosimetry; weathering
ID UV-RADIATION; CHILE; MARS; LIFE; CHROOCOCCIDIOPSIS; MICROORGANISMS;
CYANOBACTERIA; COMMUNITIES; ANTARCTICA; EXPOSURE
AB Experiments were conducted during November 2003 in the dry core of the Atacama Desert, Yungay, Chile to test the hypothesis that UV radiation, in environments where liquid water is not available, and thus enzymatic repair of UV-induced damage is inhibited, can prevent epilithic colonization. Novel dosimeters made from the cryptoendolithic, desiccation and radiation-resistant cyanobacterium Chroococcidiopsis sp. isolated from the dry Negev desert, Israel, showed that monolayers of this organism were killed within one day. The diurnal profile of microbial loss of viability was investigated with dosimeters of Bacillus subtilis, which similarly showed cell death within one day. Soil grains obtained from south of Yungay where liquid water is more abundant and transported to the hyperarid core showed killing of indigenous vegetative organisms within one day. Gypsum and mineral grain coverings of I mm. were sufficient to prevent measurable UV-induced damage of Chroococcidiopsis and B. subtilis after 8 d exposure. These results show that under extreme desiccation and an ambient UV flux the surface of rocks can potentially be rendered sterile, but that millimetre thick mineral coverings can protect organisms from UV-induced killing, consistent with the observed patterns of lithophytic colonization in the Atacama Desert. These data further show that UV radiation can be an important limiting factor in surface biological rock weathering in and regions. (c) 2007 Elsevier B.V. All rights reserved.
C1 [Cockell, Charles S.] Open Univ, PSSRI, Milton Keynes MK7 6AA, Bucks, England.
[Mckay, Christopher P.; Warren-Rhodes, Kim] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Horneck, Gerda] DLR, Inst Aerospace Med, D-51170 Cologne, Germany.
RP Cockell, CS (reprint author), Open Univ, PSSRI, Milton Keynes MK7 6AA, Bucks, England.
EM c.s.cockell@open.ac.uk
NR 33
TC 38
Z9 39
U1 1
U2 15
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 1011-1344
J9 J PHOTOCH PHOTOBIO B
JI J. Photochem. Photobiol. B-Biol.
PD FEB 27
PY 2008
VL 90
IS 2
BP 79
EP 87
DI 10.1016/j.jphotobiol.2007.11.009
PG 9
WC Biochemistry & Molecular Biology; Biophysics
SC Biochemistry & Molecular Biology; Biophysics
GA 277MH
UT WOS:000254216200001
PM 18191576
ER
PT J
AU Park, ES
Ro, HW
Nguyen, CV
Jaffe, RL
Yoon, DY
AF Park, E. S.
Ro, H. W.
Nguyen, C. V.
Jaffe, R. L.
Yoon, D. Y.
TI Infrared spectroscopy study of microstructures of poly(silsesquioxane)s
SO CHEMISTRY OF MATERIALS
LA English
DT Article
ID LOW-DIELECTRIC-CONSTANT; LOW-K DIELECTRICS; VIBRATIONAL STRUCTURE;
STRUCTURAL CONTROL; THIN-FILMS; POLY(METHYLSILSESQUIOXANE)S;
SILSESQUIOXANES; PRECURSORS
AB Results are presented from theoretical and experimental infrared (IR) spectroscopy studies of the microstructures of poly(silsesquioxane)s (PSSQs) of varying chemical composition. The calculated IR spectra show two distinct asymmetric Si-O-Si stretch vibration bands for models of complete polyhedral cages, incomplete open cages, and short ladder structures. Close analyses of the calculated results indicate that the higher frequency IR band at about 1150 cm(-1) is derived from the parallel asymmetric Si-O-Si stretch vibration mode in the (Si-O)(n) ring subunit while the lower frequency band at about 1050 cm(-1) is due to the asymmetric Si-O-Si stretch symmetric with respect to the inversion point at the center of the (Si-O)(n) ring and is absent in highly symmetric cage structures. Experimentally, poly(methylsilses-quioxane) (PMSQ), poly(isobutylsilsesquioxane) (PiBSQ), and poly(phenylsilsesquioxane) (PPhSQ) exhibit a varying tendency of cage-like structures, rather than ladder structures, in as-polymerized samples. When the thermal conversion (curing) temperature is increased to 400 degrees C, the microstructure of PMSQ in thin solid films transforms from open cage-like structure toward a random network with lower symmetry. This change in microstructure is caused by the secondary condensation reaction and the evaporation of cage structures, and the effect of cage evaporation becomes most pronounced for PiBSQ films, which are mostly comprised of cage-like structures that evaporate around 280 degrees C. In comparison, PPhSQ films retain cage-like structure upon curing to 400 degrees C as a result of the high evaporation temperature (ca. 500 degrees C) of the cages.
C1 [Park, E. S.; Ro, H. W.; Yoon, D. Y.] Seoul Natl Univ, Dept Chem, Seoul 151747, South Korea.
[Nguyen, C. V.] ELORET, NASA, Ames Res Ctr, Moffett Field, CA 94305 USA.
[Jaffe, R. L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Yoon, DY (reprint author), Seoul Natl Univ, Dept Chem, Seoul 151747, South Korea.
EM dyyoon@snu.ac.kr
NR 33
TC 91
Z9 92
U1 4
U2 45
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0897-4756
J9 CHEM MATER
JI Chem. Mat.
PD FEB 26
PY 2008
VL 20
IS 4
BP 1548
EP 1554
DI 10.1021/cm071575z
PG 7
WC Chemistry, Physical; Materials Science, Multidisciplinary
SC Chemistry; Materials Science
GA 264JN
UT WOS:000253283700059
ER
PT J
AU Kambe, E
Ando, H
Sato, B
Izumiura, H
Sekii, T
Paulson, DB
Yanagisawa, K
Masuda, S
Shibahashi, H
Hatzes, AP
Martic, M
Lebrun, JC
Mkrtichian, DE
Kiss, LL
Bruntt, H
O'Toole, SJ
Bedding, TR
AF Kambe, Eiji
Ando, Hiroyasu
Sato, Bun'ei
Izumiura, Hideyuki
Sekii, Takashi
Paulson, Diane B.
Yanagisawa, Kenshi
Masuda, Seiji
Shibahashi, Hiromoto
Hatzes, Artie P.
Martic, Milena
Lebrun, Jean-Claude
Mkrtichian, David E.
Kiss, Laszlo L.
Bruntt, Hans
O'Toole, Simon J.
Bedding, Timothy R.
TI Development of iodine cells for Subaru HDS and Okayama HIDES. III. An
improvement on the radial-velocity measurement technique
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE instrumentation : iodine cell; instrumentation : echelle spectrograph;
stars : radial velocity; stars : planetary systems; stars :
asteroseismology
ID SOLAR-LIKE OSCILLATIONS; PLANET SEARCH PROGRAM; PROCYON-A; MODE
FREQUENCIES; BETA-HYDRI; PRECISION; SPECTROGRAPH; CORE; MASS
AB An improvement of the radial-velocity measurement accuracy is crucial for the detection of tiny stellar oscillations and exoplanets. Through the analysis of week-long extensive observations of solar-type stars (Procyon in 2000, 2002, and 2006/2007 and tau Cet in 2002 and 2006/2007), we have carefully examined, revised, and finely tuned the widely used multiple Gaussian IP fitting method for the spectrograph, HIDES. By determining a necessary and sufficient number of free parameters in the model as well as introducing an iterative process in the radial-velocity analysis, we can reach a precision of below 3 m s(-1), which is much smaller than the precision of 6 m s(-1) officially announced so far for HIDES. We also make our technique refined for the 2002 McDonald Procyon data. Even with our revised method, slow radial velocity variations with an amplitude of about 10 m s(-1) are left in the Procyon data. We emphasize that it is neither due to particular observing instruments nor radial-velocity analysis, and thus could be due to stellar origin. The analysis presented here makes the foundations of our next scientific analysis of the radial-velocity variations of Procyon, which will be presented in our forthcoming papers.
C1 [Kambe, Eiji; Izumiura, Hideyuki; Yanagisawa, Kenshi] Natl Astron Observ Japan, Okayama Astrophys Observ, Asakuchi, Okayama 7190232, Japan.
[Ando, Hiroyasu; Sekii, Takashi] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Sato, Bun'ei] Tokyo Inst Technol, Meguro Ku, Tokyo 152, Japan.
[Paulson, Diane B.] NASA, Goddard Space Flight Ctr, Planetary Syst Branch, Greenbelt, MD 20771 USA.
[Masuda, Seiji] Tokushima Sci Museum, Astumn Land Tokushima, Tokushima 7790111, Japan.
[Shibahashi, Hiromoto] Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Hatzes, Artie P.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany.
[Martic, Milena; Lebrun, Jean-Claude] CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France.
[Mkrtichian, David E.] Sejong Univ, Astrophys Res Ctr Struct & Evolut Cosmos, Seoul 143747, South Korea.
[Mkrtichian, David E.] Odessa Natl Univ, Astron Observ, UA-65014 Odessa, Ukraine.
[Kiss, Laszlo L.; Bruntt, Hans; Bedding, Timothy R.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
[O'Toole, Simon J.] Anglo Australian Observ, Epping, NSW 1710, Australia.
RP Kambe, E (reprint author), Natl Astron Observ Japan, Okayama Astrophys Observ, Asakuchi, Okayama 7190232, Japan.
EM kambe@oao.nao.ac.jp
RI Kiss, Laszlo/A-2539-2008;
OI Bedding, Timothy/0000-0001-5943-1460; Bedding, Tim/0000-0001-5222-4661
NR 34
TC 8
Z9 8
U1 0
U2 2
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 2008
VL 60
IS 1
BP 45
EP 53
DI 10.1093/pasj/60.1.45
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 300IR
UT WOS:000255818000005
ER
PT J
AU Kahn, RA
Chen, Y
Nelson, DL
Leung, FY
Li, QB
Diner, DJ
Logan, JA
AF Kahn, Ralph A.
Chen, Yang
Nelson, David L.
Leung, Fok-Yan
Li, Qinbin
Diner, David J.
Logan, Jennifer A.
TI Wildfire smoke injection heights: Two perspectives from space
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID FOREST-FIRE SMOKE; TRANSPORT; PLUME
AB The elevation at which wildfire smoke is injected into the atmosphere has a strong influence on how the smoke is dispersed, and is a key input to aerosol transport models. Aerosol layer height is derived with great precision from space-borne lidar, but horizontal sampling is very poor on a global basis. Aerosol height derived from space-borne stereo imaging is limited to source plumes having discernable features. But coverage is vastly greater, and captures the cores of major fires, where buoyancy can be sufficient to lift smoke above the near-surface boundary layer. Initial assessment of smoke injection from the Alaska-Yukon region during summer 2004 finds at least about 10% of wildfire smoke plumes reached the free troposphere. Modeling of smoke environmental impacts can benefit from the combined strengths of the stereo and lidar observations.
C1 [Kahn, Ralph A.; Chen, Yang; Li, Qinbin; Diner, David J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Leung, Fok-Yan; Logan, Jennifer A.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Nelson, David L.] Columbus Technol & Serv Inc, Pasadena, CA 91101 USA.
RP Kahn, RA (reprint author), NASA, Goddard Space Flight Ctr, Code 613-2, Greenbelt, MD 20771 USA.
EM ralph.kahn@jpl.nasa.gov
RI Chen, Yang/C-6529-2008; Kahn, Ralph/D-5371-2012
OI Chen, Yang/0000-0002-0993-7081; Kahn, Ralph/0000-0002-5234-6359
NR 13
TC 91
Z9 91
U1 2
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD FEB 22
PY 2008
VL 35
IS 4
AR L04809
DI 10.1029/2007GL032165
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 267TD
UT WOS:000253531200002
ER
PT J
AU Sarantos, M
Killen, RM
Sharma, AS
Slavin, JA
AF Sarantos, Menelaos
Killen, Rosemary M.
Sharma, A. Surjalal
Slavin, James A.
TI Influence of plasma ions on source rates for the lunar exosphere during
passage through the Earth's magnetosphere
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID STIMULATED DESORPTION; SODIUM ATOMS; MOON; SURFACE; ATMOSPHERES;
MAGNETOTAIL; MODEL
AB The total electron flux in the lunar exosphere, measured by the Electron Reflectometer onboard the Lunar Prospector during its passage through the Earth's magnetosphere (June 7-16, 1998), is strongly correlated with variations in the column abundance of equatorial sodium observed coincidentally with the McMath-Pierce solar telescope at Kitt Peak. At the same time, the exospheric temperature increased from a minimum of 1200 K to a maximum of 3000 K at minimum phase angle. A comparison of different source mechanisms, using the measured electron flux as the proxy for the ion flux, provides strong evidence that ion impact enhances the photon-stimulated desorption yield. At the Moon photon-stimulated desorption is shown to be the dominant source of exospheric sodium outside the magnetosphere. Inside the magnetosphere, where the ion flux and the associated photon-stimulated desorption yield decrease, the contributions from impact vaporization to the observed column abundance and temperature are found to be substantial.
C1 [Sarantos, Menelaos; Killen, Rosemary M.; Sharma, A. Surjalal] Univ Maryland, Dept Astron, College Pk, MD 20771 USA.
[Sarantos, Menelaos; Slavin, James A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP Sarantos, M (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20771 USA.
EM sarantos@astro.umd.edu
RI Slavin, James/H-3170-2012; Sarantos, Menelaos/H-8136-2013
OI Slavin, James/0000-0002-9206-724X;
NR 13
TC 23
Z9 24
U1 1
U2 4
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 2008
VL 35
IS 4
AR L04105
DI 10.1029/2007GL032310
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 267TD
UT WOS:000253531200003
ER
PT J
AU Monaghan, AJ
Bromwich, DH
Chapman, W
Comiso, JC
AF Monaghan, Andrew J.
Bromwich, David H.
Chapman, William
Comiso, Josefino C.
TI Recent variability and trends of Antarctic near-surface temperature
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID OCEAN SEA-ICE; HEMISPHERE ANNULAR MODE; POLAR MM5 SIMULATIONS;
SOUTHERN-HEMISPHERE; CLIMATE VARIABILITY; MASS-BALANCE; OSCILLATION;
CIRCULATION; REANALYSIS; ACCUMULATION
AB A new monthly 1 degrees x 1 degrees Antarctic near-surface temperature reconstruction for 1960-2005 is presented. The use of numerical model fields to establish spatial relationships between fifteen continuous observational temperature records and the voids to which they are interpolated inherently accounts for the effects of the atmospheric circulation and topography on temperature variability. Employing a fixed observation network ensures that the reconstruction uncertainty remains constant in time. Comparison with independent observations indicates that the reconstruction and two other gridded observational temperature records are useful for evaluating regional near-surface temperature variability and trends throughout Antarctica. The reconstruction has especially good skill at reproducing temperature trends during the warmest months when melt contributes to ice sheet mass loss. The spatial variability of monthly near-surface temperature trends is strongly dependent on the season and time period analyzed. Statistically insignificant (p > 0.05) positive trends occur over most regions and months during 1960-2005. By contrast, 1970-2005 trends are weakly negative overall, consistent with positive trends in the Southern Hemisphere Annular Mode (SAM) during summer and autumn. Subtle near-surface temperature increases during winter from 1970 to 2000 are consistent with tropospheric warming from radiosonde records and a lack of winter SAM trends. Widespread but statistically insignificant (p > 0.05) warming over Antarctica from 1992 to 2005 coincides with a leveling off of upward SAM trends during summer and autumn since the mid-1990s. Weakly significant annual trends (p < 0.10) of about +1 K decade(-1) are found at three stations in interior and coastal East Antarctica since 1992. The subtle shift toward warming during the past 15 years raises the question of whether the recent trends are linked more closely to anthropogenic influences or multidecadal variability.
C1 [Monaghan, Andrew J.; Bromwich, David H.] Ohio State Univ, Byrd Polar Res Ctr, Polar Meteorol Grp, Columbus, OH 43210 USA.
[Bromwich, David H.] Ohio State Univ, Dept Geog, Atmospher Sci Program, Columbus, OH 43210 USA.
[Chapman, William] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61081 USA.
[Comiso, Josefino C.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA.
RP Monaghan, AJ (reprint author), Ohio State Univ, Byrd Polar Res Ctr, Polar Meteorol Grp, 1090 Carmack Rd, Columbus, OH 43210 USA.
EM monaghan.11@osu.edu
RI Bromwich, David/C-9225-2016;
OI Monaghan, Andrew/0000-0002-8170-2359
NR 52
TC 66
Z9 68
U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD FEB 22
PY 2008
VL 113
IS D4
AR D04105
DI 10.1029/2007JD009094
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 267TI
UT WOS:000253531700006
ER
PT J
AU Comiso, JC
Nishio, F
AF Comiso, Josefino C.
Nishio, Fumihiko
TI Trends in the sea ice cover using enhanced and compatible AMSR-E, SSM/I,
and SMMR data
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID PASSIVE MICROWAVE; SATELLITE; VARIABILITY; PARAMETERS; ALGORITHM;
SURFACE
AB Arguably, the most remarkable manifestation of change in the polar regions is the rapid decline in the Arctic perennial ice cover. Changes in the global sea ice cover, however, have been more modest, being only slightly negative in the Northern Hemisphere and even slightly positive in the Southern Hemisphere, the significance of which has not been adequately assessed because of unknown errors in the satellite historical data. Recent Advanced Microwave Scanning Radiometer (AMSR-E) high-resolution data are used as the baseline for generating an enhanced sea ice data set used in this study. Brightness temperature data from historical Special Scanning Microwave Imager (SSM/I) and Scanning Multichannel Microwave Radiometer (SMMR) sensors were normalized to be consistent with those from AMSR-E, and sea ice parameters were derived from all three data sets using the same algorithm for optimum consistency and accuracy. A small bias in sea ice extent is observed between AMSR- E and SSM/I data which, if uncorrected, causes an error of 0.62%/decade in the Arctic and 0.26%/decade in the Antarctic. Similar corrections are not needed in trend estimates of sea ice area. Biases due to seasonal changes in the accuracy of ice edge determinations, especially during melt periods, were also evaluated, and impacts on the trend results appear to be small. When updated to 2006, the trends in ice extent and area in the Arctic are now slightly more negative at -3.4 +/- 0.2 and -4.0 +/- 0.2% per decade, respectively, while the corresponding trends in the Antarctic remains slight but positive at 0.9 +/- 0.2 and 1.7 +/- 0.3% per decade.
C1 [Comiso, Josefino C.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD USA.
[Nishio, Fumihiko] Chiba Univ, Ctr Environm Remote Sensing, Chiba, Japan.
RP Comiso, JC (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD USA.
NR 30
TC 200
Z9 208
U1 12
U2 52
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 22
PY 2008
VL 113
IS C2
AR C02S07
DI 10.1029/2007JC004257
PG 22
WC Oceanography
SC Oceanography
GA 267TQ
UT WOS:000253532500002
ER
PT J
AU Burlaga, LF
Ness, NF
Acuna, MH
Wang, YM
Sheeley, NR
Wang, C
Richardson, JD
AF Burlaga, L. F.
Ness, N. F.
Acuna, M. H.
Wang, Y. -M.
Sheeley, N. R., Jr.
Wang, C.
Richardson, J. D.
TI Global structure and dynamics of large-scale fluctuations in the solar
wind: Voyager 2 observations during 2005 and 2006
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID MERGED INTERACTION REGION; HELIOSPHERIC MAGNETIC-FIELD; OUTER
HELIOSPHERE; PICKUP IONS; INTERPLANETARY SHOCKS; TERMINATION SHOCK;
COSMIC-RAYS; 95 AU; SPEED; EVOLUTION
AB The Voyager 2 (V2) observations of daily averages of the solar wind during 2005 and 2006 from 75.3 AU to 81.6 AU between approximate to 25.7 degrees S and 27.1 degrees S show both a step-like trend in the speed V(t) and "large-scale fluctuations'' of the magnetic field strength B, speed V, density N and temperature T. The distribution functions of B, N, and NV2 observed by V2 are lognormal and that of V is approximately Gaussian. We introduce a method for specifying the boundary conditions at all latitudes (except near the poles) on a Sun-centered surface of radius of 1 AU, based on solar magnetic field observations. This paper uses only the boundary conditions at the latitude of V2 and a 1-D time-dependent MHD model to calculate the radial evolution of the large-scale fluctuations of B(t), V(t) and N(t) at distances between 1 and 90 AU. This model explains the V2 observations of a lognormal distribution of B and the Gaussian distribution of V, but not the observed lognormal distributions of N and NV2. The lognormal distribution of B observed by V2 was produced primarily by dynamical processes beyond 1 AU.
C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA.
[Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
[Acuna, M. H.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Wang, Y. -M.; Sheeley, N. R., Jr.] USN, Res Lab, Washington, DC 20375 USA.
[Wang, C.] Chinese Acad Sci, Ctr Space Sci & Appl Res, State Key Lab Space Weather, Beijing, Peoples R China.
[Richardson, J. D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 37655 USA.
RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Code 673, Greenbelt, MD 20771 USA.
EM leonard.f.burlaga@nasa.gov
NR 55
TC 4
Z9 4
U1 0
U2 5
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 22
PY 2008
VL 113
IS A2
AR A02104
DI 10.1029/2007JA012796
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 267UK
UT WOS:000253534500005
ER
PT J
AU Forbes, JM
Zhang, X
Palo, S
Russell, J
Mertens, CJ
Mlynczak, M
AF Forbes, J. M.
Zhang, X.
Palo, S.
Russell, J.
Mertens, C. J.
Mlynczak, M.
TI Tidal variability in the ionospheric dynamo region
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID NONMIGRATING DIURNAL TIDES; GENERAL-CIRCULATION MODEL; LATENT-HEAT
RELEASE; UPPER-ATMOSPHERE; SEMIDIURNAL TIDES; MIDDLE ATMOSPHERE;
THERMOSPHERE; TEMPERATURE; WINDS; UARS
AB The seasonal and interannual variability of migrating (Sun-synchronous) and nonmigrating solar atmospheric tides at altitudes between 100 and 116 km are investigated using temperature measurements made with the SABER instrument on the TIMED spacecraft during 2002-2006. Quasi-biennial variations of order +/- 10-15% in migrating diurnal and semidiurnal tidal amplitudes are found, presumably due to modulation by the quasi-biennial oscillation (QBO) as the tides propagate from their troposphere and stratospheric sources to the lower thermosphere. A number of nonmigrating tidal components are found that have the potential to produce significant longitudinal variability of the total tidal fields. The most prominent of these, i.e., those that appear at amplitudes of order 5-10 K in a 5-year mean climatology, include the zonally symmetric (s = 0) diurnal tide (D0); the eastward propagating diurnal and semidiurnal tides with zonal wave numbers s = -2 (DE2 and SE2) and s = -3 (DE3 and SE3); and the following westward propagating waves: diurnal s = 2 (DW2); semidiurnal s = 1 (SW1), s = 3 (SW3), and s = 4 (SW4); and terdiurnal s = 5 (TW5). These waves can be plausibly accounted for by nonlinear interaction between migrating tidal components and stationary planetary waves with s = 1 or s = 2 or by longitudinal variations of tropospheric thermal forcing. Additional waves that occur during some years or undergo phase cancellation within construction of a 5-year climatology include DW5, SE1, SE4, SW6, TE1, TW1, and TW7. It is anticipated that the winds that accompany all of these waves in the 100-170 km region will impose longitudinal variability in the electric fields produced through the ionospheric dynamo mechanism, thereby modulating vertical motion of the equatorial ionosphere and the concomitant plasma densities. In addition to the wave-4 modulation of the equatorial ionosphere that has recently been discovered and replicated in modeling studies, the waves revealed here will generate wave-1 (SW1, SW3, D0, DW2), wave-2 (SW4, TW1), wave-3 (DE2, SE1), wave-4 (DE3, SE2, DW5, SW6, TE1, TW7), wave-5 (SE3), and wave-6 (SE4) components of this ionospheric variability, depending on year and time of year. However, the absolute and relative efficiencies with which these waves produce electric fields remains to be determined.
C1 [Forbes, J. M.; Zhang, X.; Palo, S.] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA.
[Russell, J.] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Mertens, C. J.; Mlynczak, M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Forbes, JM (reprint author), Univ Colorado, Dept Aerosp Engn Sci, UCB 429, Boulder, CO 80309 USA.
EM forbes@colorado.edu
RI Mlynczak, Martin/K-3396-2012;
OI FORBES, JEFFREY/0000-0001-6937-0796; PALO, SCOTT/0000-0002-4729-4929
NR 39
TC 159
Z9 159
U1 3
U2 15
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 22
PY 2008
VL 113
IS A2
AR A02310
DI 10.1029/2007JA012737
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 267UK
UT WOS:000253534500004
ER
PT J
AU Syed, TH
Famiglietti, JS
Rodell, M
Chen, J
Wilson, CR
AF Syed, Tajdarul H.
Famiglietti, James S.
Rodell, Matthew
Chen, Jianli
Wilson, Clark R.
TI Analysis of terrestrial water storage changes from GRACE and GLDAS
SO WATER RESOURCES RESEARCH
LA English
DT Article
ID CLIMATE EXPERIMENT GRACE; TIME-VARIABLE GRAVITY; SOIL-MOISTURE;
MASS-LOSS; RECOVERY; FIELD; EVAPOTRANSPIRATION; VARIABILITY; ILLINOIS;
SYSTEM
AB [1] Since March 2002, the Gravity Recovery and Climate Experiment (GRACE) has provided first estimates of land water storage variations by monitoring the time-variable component of Earth's gravity field. Here we characterize spatial-temporal variations in terrestrial water storage changes (TWSC) from GRACE and compare them to those simulated with the Global Land Data Assimilation System (GLDAS). Additionally, we use GLDAS simulations to infer how TWSC is partitioned into snow, canopy water and soil water components, and to understand how variations in the hydrologic fluxes act to enhance or dissipate the stores. Results quantify the range of GRACE-derived storage changes during the studied period and place them in the context of seasonal variations in global climate and hydrologic extremes including drought and flood, by impacting land memory processes. The role of the largest continental river basins as major locations for freshwater redistribution is highlighted. GRACE-based storage changes are in good agreement with those obtained from GLDAS simulations. Analysis of GLDAS-simulated TWSC illustrates several key characteristics of spatial and temporal land water storage variations. Global averages of TWSC were partitioned nearly equally between soil moisture and snow water equivalent, while zonal averages of TWSC revealed the importance of soil moisture storage at low latitudes and snow storage at high latitudes. Evapotranspiration plays a key role in dissipating globally averaged terrestrial water storage. Latitudinal averages showed how precipitation dominates TWSC variations in the tropics, evapotranspiration is most effective in the midlatitudes, and snowmelt runoff is a key dissipating flux at high latitudes. Results have implications for monitoring water storage response to climate variability and change, and for constraining land model hydrology simulations.
C1 [Syed, Tajdarul H.; Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92717 USA.
[Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
[Chen, Jianli] Univ Texas Austin, Ctr Space Res, Austin, TX 78712 USA.
[Wilson, Clark R.] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA.
RP Syed, TH (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92717 USA.
RI Rodell, Matthew/E-4946-2012; Syed, Tajdarul/G-6731-2014
OI Rodell, Matthew/0000-0003-0106-7437;
NR 48
TC 145
Z9 155
U1 9
U2 72
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 22
PY 2008
VL 44
IS 2
AR W02433
DI 10.1029/2006WR005779
PG 15
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 267VA
UT WOS:000253536100001
ER
PT J
AU Schafer, JS
Eck, TF
Holben, BN
Artaxo, P
Duarte, AF
AF Schafer, J. S.
Eck, T. F.
Holben, B. N.
Artaxo, P.
Duarte, A. F.
TI Characterization of the optical properties of atmospheric aerosols in
Amazonia from long-term AERONET monitoring (1993-1995 and 1999-2006)
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SKY RADIANCE MEASUREMENTS; BIOMASS BURNING AEROSOLS; SINGLE SCATTERING
ALBEDO; SAHARAN DUST; BRAZIL; BASIN; DEPTH; WATER; SUN; VARIABILITY
AB We present a new climatology of atmospheric aerosols (primarily pyrogenic and biogenic) for the Brazilian tropics on the basis of a high-quality data set of spectral aerosol optical depth and directional sky radiance measurements from Aerosol Robotic Network (AERONET) Cimel Sun-sky radiometers at more than 15 sites distributed across the Amazon basin and adjacent Cerrado region. This network is the only long-term project (with a record including observations from more than 11 years at some locations) ever to have provided ground-based remotely-sensed column aerosol properties for this critical region. Distinctive features of the Amazonian area aerosol are presented by partitioning the region into three aerosol regimes: southern Amazonian forest, Cerrado, and northern Amazonian forest. The monitoring sites generally include measurements from the interval 1999-2006, but some sites have measurement records that date back to the initial days of the AERONET program in 1993. Seasonal time series of aerosol optical depth (AOD), angstrom ngstrom exponent, and columnar-averaged microphysical properties of the aerosol derived from sky radiance inversion techniques (single-scattering albedo, volume size distribution, fine mode fraction of AOD, etc.) are described and contrasted for the defined regions. During the wet season, occurrences of mineral dust penetrating deep into the interior were observed.
C1 [Schafer, J. S.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Schafer, J. S.; Eck, T. F.; Holben, B. N.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Eck, T. F.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Artaxo, P.] Univ Sao Paulo, Inst Fis, Dept Fis Aplicada, BR-05508900 Sao Paulo, Brazil.
[Duarte, A. F.] Univ Fed Acre, Dept Ciencias Nat, BR-69915900 Rio Branco, AC, Brazil.
RP Schafer, JS (reprint author), Sci Syst & Applicat Inc, 10210 Greenbelt Rd,Suite 600, Lanham, MD 20706 USA.
EM joel.schafer@nasa.gov
RI Schafer, Joel/A-3978-2010; ECK, THOMAS/D-7407-2012; Artaxo,
Paulo/E-8874-2010
OI Artaxo, Paulo/0000-0001-7754-3036
NR 40
TC 40
Z9 40
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD FEB 21
PY 2008
VL 113
IS D4
AR D04204
DI 10.1029/2007JD009319
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 267TH
UT WOS:000253531600002
ER
PT J
AU Comiso, JC
Parkinson, CL
AF Comiso, Josefino C.
Parkinson, Claire L.
TI Arctic sea ice parameters from AMSR-E data using two techniques and
comparisons with sea ice from SSM/I
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID PASSIVE MICROWAVE; ALGORITHM; COVER; SMMR; GHZ
AB We use two algorithms to process Advanced Microwave Scanning Radiometer for the Earth Observing System (AMSR-E) data in order to determine algorithm dependence, if any, on the estimates of sea ice concentration, ice extent and area, and trends and to evaluate how AMSR-E data compare with historical Special Sensor Microwave Imager (SSM/I) data. The monthly ice concentrations derived from the two algorithms from AMSR-E data (the AMSR-E bootstrap algorithm, or ABA, and the enhanced NASA team algorithm, or NT2), differ on average by about 1-3%, with data from the consolidated ice region being comparable for ABA and NT2 retrievals while data in the marginal ice zones and thin ice regions show slightly higher values when the NT2 algorithm is used. The ice extents and areas derived separately from AMSR-E using these two algorithms are, however, in good agreement, with the differences (ABA - NT2) being about 0.07 x 10(6) km(2) on average for ice extents and -0.07 x 10(6) km(2) for ice area, which are small compared with mean seasonal values of 10.5 x 10(6) and 9.8 x 10(6) for ice extent and area, respectively. Likewise, extents and areas derived from the same algorithm but from AMSR-E and SSM/I data are consistent but differ by about 0.24 x 10(6) km(2) and 0.14 x 10(6) km(2), respectively. The discrepancies are larger with the estimates of extents than area mainly because of differences in channel selection and sensor resolutions. Trends in extent during the AMSR-E era were also estimated, and results from all three data sets are shown to be in good agreement (within errors).
C1 [Comiso, Josefino C.; Parkinson, Claire L.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA.
RP Comiso, JC (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Code 614-1, Greenbelt, MD 20771 USA.
EM josefino.c.comiso@nasa.gov
RI Parkinson, Claire/E-1747-2012
OI Parkinson, Claire/0000-0001-6730-4197
NR 28
TC 18
Z9 20
U1 2
U2 9
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 21
PY 2008
VL 113
IS C2
AR C02S05
DI 10.1029/2007JC004255
PG 16
WC Oceanography
SC Oceanography
GA 267TP
UT WOS:000253532400001
ER
PT J
AU Starling, RLC
O'Brien, PT
Willingale, R
Page, KL
Osborne, JP
De Pasquale, M
Nakagawa, YE
Kuin, NPM
Onda, K
Norris, JP
Ukwatta, TN
Kodaka, N
Burrows, DN
Kennea, JA
Page, MJ
Perri, M
Markwardt, CB
AF Starling, R. L. C.
O'Brien, P. T.
Willingale, R.
Page, K. L.
Osborne, J. P.
De Pasquale, M.
Nakagawa, Y. E.
Kuin, N. P. M.
Onda, K.
Norris, J. P.
Ukwatta, T. N.
Kodaka, N.
Burrows, D. N.
Kennea, J. A.
Page, M. J.
Perri, M.
Markwardt, C. B.
TI Swift captures the spectrally evolving prompt emission of GRB070616
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gamma-rays : bursts
ID GAMMA-RAY-BURSTS; AFTERGLOW EMISSION; HOST-GALAXY; LONG; RADIATION;
BATSE; TELESCOPE; MODELS; DUST; GRBS
AB The origins of gamma-ray burst (GRB) prompt emission are currently not well understood and in this context long, well-observed events are particularly important to study. We present the case of GRB 070616, analysing the exceptionally long-duration multipeaked prompt emission, and later afterglow, captured by all the instruments on-board Swift and by Suzaku Wide-Band All-Sky Monitor (WAM). The high-energy light curve remained generally flat for several hundred seconds before going into a steep decline. Spectral evolution from hard to soft is clearly taking place throughout the prompt emission, beginning at 285 s after the trigger and extending to 1200 s. We track the movement of the spectral peak energy, whilst observing a softening of the low-energy spectral slope. The steep decline in flux may be caused by a combination of this strong spectral evolution and the curvature effect. We investigate origins for the spectral evolution, ruling out a superposition of two power laws and considering instead an additional component dominant during the late prompt emission. We also discuss origins for the early optical emission and the physics of the afterglow. The case of GRB 070616 clearly demonstrates that both broad-band coverage and good time resolution are crucial to pin down the origins of the complex prompt emission in GRBs.
C1 [Starling, R. L. C.; O'Brien, P. T.; Willingale, R.; Page, K. L.; Osborne, J. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[De Pasquale, M.; Kuin, N. P. M.; Page, M. J.] UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Nakagawa, Y. E.] Aoyama Gakuin Univ, Dept Phys & Math, Sagamihara, Kanagawa 2298558, Japan.
[Onda, K.; Kodaka, N.] Saitama Univ, Dept Phys, Saitama 3388570, Japan.
[Norris, J. P.] Univ Denver, Denver Res Inst, Denver, CO 80208 USA.
[Norris, J. P.] Stanford Univ, Stanford, CA 94305 USA.
[Ukwatta, T. N.; Markwardt, C. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ukwatta, T. N.] George Washington Univ, Dept Phys, Ctr Nucl Studies, Washington, DC 20052 USA.
[Burrows, D. N.; Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Perri, M.] ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Markwardt, C. B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Starling, RLC (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England.
EM rlcs1@star.le.ac.uk
RI XRAY, SUZAKU/A-1808-2009;
OI Perri, Matteo/0000-0003-3613-4409
NR 64
TC 19
Z9 20
U1 1
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB 21
PY 2008
VL 384
IS 2
BP 504
EP 514
DI 10.1111/j.1365-2966.2007.12763.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 259HS
UT WOS:000252931000006
ER
PT J
AU Raymond, SN
Barnes, R
Mandell, AM
AF Raymond, Sean N.
Barnes, Rory
Mandell, Avi M.
TI Observable consequences of planet formation models in systems with
close-in terrestrial planets
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Review
DE astrobiology; methods : N-body simulations; methods : numerical;
planetary systems : formation; planetary systems : protoplanetary discs
ID EARTH-LIKE PLANETS; EXTRASOLAR GIANT PLANETS; LOW-MASS STARS;
MAIN-SEQUENCE STARS; T-TAURI STARS; M-CIRCLE-PLUS; M-DWARF STARS; SOLAR
NEBULA; SUPER-EARTHS; PROTOPLANETARY DISKS
AB To date, two planetary systems have been discovered with close-in, terrestrial-mass planets (less than or similar to 5 -10M(circle plus)). Many more such discoveries are anticipated in the coming years with radial velocity and transit searches. Here we investigate the different mechanisms that could form 'hot Earths' and their observable predictions. Models include: (1) in situ accretion; (2) formation at larger orbital distance followed by inward 'type 1' migration; (3) formation from material being 'shepherded' inward by a migrating gas giant planet; (4) formation from material being shepherded by moving secular resonances during dispersal of the protoplanetary disc; (5) tidal circularization of eccentric terrestrial planets with close-in perihelion distances and (6) photoevaporative mass-loss of a close-in giant planet. Models 1-4 have been validated in previous work. We show that tidal circularization can form hot Earths, but only for relatively massive planets (greater than or similar to 5M(circle plus)) with very close-in perihelion distances (less than or similar to 0.025 au), and even then the net inward movement in orbital distance is at most only 0.1-0.15 au. For planets of less than similar to 70M(circle plus), photoevaporation can remove the planet's envelope and leave behind the solid core on a Gyr time-scale, but only for planets inside 0.025-0.05 au. Using two quantities that are observable by current and upcoming missions, we show that these models each produce unique signatures, and can be observationally distinguished. These observables are the planetary system architecture (detectable with radial velocities, transits and transit timing) and the bulk composition of transiting close-in terrestrial planets (measured by transits via the planet's radius).
C1 [Raymond, Sean N.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Barnes, Rory] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Mandell, Avi M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Raymond, SN (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
EM raymond@lasp.colorado.edu
RI Mandell, Avi/F-9361-2012
NR 165
TC 71
Z9 71
U1 1
U2 3
PU BLACKWELL PUBLISHING
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB 21
PY 2008
VL 384
IS 2
BP 663
EP 674
DI 10.1111/j.1365-2966.2007.12712.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 259HS
UT WOS:000252931000019
ER
PT J
AU McGowan, KE
Coe, MJ
Schurch, MPE
Corbet, RHD
Galache, JL
Udalski, A
AF McGowan, K. E.
Coe, M. J.
Schurch, M. P. E.
Corbet, R. H. D.
Galache, J. L.
Udalski, A.
TI Optical and X-ray variability of two Small Magellanic Cloud X-ray binary
pulsars - SXP46.6 and SXP6.85
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars : emission-line, Be; Magellanic Clouds; X-rays : binaries
ID GRAVITATIONAL LENSING EXPERIMENT; MACHO PHOTOMETRY; OUTBURSTS;
ACCRETION; BEHAVIOR; PERIOD; STARS; SMC
AB We present long-term optical and RXTE data of two X-ray binary pulsars in the Small Magellanic Cloud, SXP46.6 and SXP6.85. The optical light curves of both sources show substantial (similar to 0.5-0.8 mag) changes over the time-span of the observations. While the optical data for SXP6.85 do not reveal any periodic behaviour, by detrending the optical measurements for SXP46.6 we find an orbital period of similar to 137 d, consistent with results from the X-ray data. The detection of Type I X-ray outbursts from SXP46.6, combined with the fact that we also see optical outbursts at these times, implies that SXP46.6 is a high orbital eccentricity system. Using contemporaneous optical spectra of SXP46.6, we find that the equivalent width of the H alpha emission line changes over time indicating that the size of the circumstellar disc varies. By studying the history of the colour variations for SXP6.85, we find that the source gets redder as it brightens which can also be attributed to changes in the circumstellar disc. We do not find any correlation between the X-ray and optical data for SXP6.85. The results for SXP6.85 suggest that it is a low-eccentricity binary and that the optical modulations are due to the Be phenomenon.
C1 [McGowan, K. E.; Coe, M. J.; Schurch, M. P. E.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Corbet, R. H. D.] Univ Maryland, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Galache, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Udalski, A.] Warsaw Univ Obsev, PL-00478 Warsaw, Poland.
RP McGowan, KE (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
EM kem@astro.soton.ac.uk
NR 29
TC 18
Z9 18
U1 0
U2 0
PU BLACKWELL PUBLISHING
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB 21
PY 2008
VL 384
IS 2
BP 821
EP 826
DI 10.1111/j.1365-2966.2007.12762.x
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 259HS
UT WOS:000252931000034
ER
PT J
AU Saif, B
Bluth, M
Greenfield, P
Hack, W
Eegholm, BH
Blake, P
Keski-Kuha, R
Feinberg, L
Arenberg, JW
AF Saif, Babak
Bluth, Marcel
Greenfield, Perry
Hack, Warren
Eegholm, Bente Hoffmann
Blake, Peter
Keski-Kuha, Ritva
Feinberg, Lee
Arenberg, Jonathan W.
TI Measurement of large cryogenic structures using a spatially
phase-shifted digital speckle pattern interferometer
SO APPLIED OPTICS
LA English
DT Article
AB The James Webb Space Telescope (JWST) Backplane Stability Test Article (BSTA) was developed to demonstrate large precision cryogenic structures' technology readiness for use in the JWST The thermal stability of the BSTA was measured at cryogenic temperatures at the Marshall Space Flight Center (MSFC) X-Ray Calibration Facility (XRCF) and included nearly continuous measurements over a six-week period in the summer of 2006 covering the temperature range from ambient down to 30 Kusing a spatially phase-shifted digital speckle pattern interferometer (SPS-DSPI). The BSTA is a full size, one-sixth section of the JWST primary mirror backplane assembly (PMBA). The BSTA, measuring almost 3 m across, contains most of the prominent structural elements of the backplane and is to our knowledge the largest structure ever measured with SPS-DSPI at cryogenic conditions. The SPS-DSPI measured rigid body motion and deformations of BSTA to nanometer-level accuracy. The SPS-DSPI was developed specifically for the purposes of this test and other tests of large cryogenic structures for JWST. (c) 2008 Optical Society of America.
C1 [Saif, Babak; Greenfield, Perry; Hack, Warren; Eegholm, Bente Hoffmann] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Bluth, Marcel] Alliant Tech Syst, Space Syst Grp, Magna, UT 84044 USA.
[Blake, Peter; Keski-Kuha, Ritva; Feinberg, Lee] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Arenberg, Jonathan W.] Northrop Grumman Space Technol, Redondo Beach, CA 90278 USA.
RP Eegholm, BH (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM beegholm@stsci.edu
OI Arenberg, Jonathan/0000-0003-1096-5634
NR 10
TC 10
Z9 10
U1 0
U2 2
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 FEB 20
PY 2008
VL 47
IS 6
BP 737
EP 745
DI 10.1364/AO.47.000737
PG 9
WC Optics
SC Optics
GA 276LA
UT WOS:000254141800003
PM 18288221
ER
PT J
AU Winter, LM
Mushotzky, RF
Tueller, J
Markwardt, C
AF Winter, Lisa M.
Mushotzky, Richard F.
Tueller, Jack
Markwardt, Craig
TI X-ray properties of an unbiased hard X-ray-detected sample of active
galactic nuclei
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : active; surveys; X-rays : galaxies
ID XMM-NEWTON OBSERVATIONS; SEYFERT 1 GALAXIES; K-ALPHA LINE; ASCA
OBSERVATIONS; TIME VARIABILITY; COMPTON-THICK; OPTICAL SPECTROSCOPY;
HOST GALAXIES; BRIGHTEST AGN; LOCKMAN HOLE
AB The Swift gamma-ray observatory's Burst Alert Telescope (BAT) has detected a sample of AGNs based solely on their hard X-ray flux (14-195 keV). In this paper we present for the first time XMM-Newton X-ray spectra for 22 BAT AGNs with no previously analyzed X-ray spectra. If our sources are a representative sample of the BAT AGNs, as we claim, our results present for the first time global X-ray properties of an unbiased toward absorption (n(H) < 3 x 10(25) cm(-2)), local (< z > = 0.03), AGN sample. We find 9/22 low-absorption (n(H) < 10(23) cm(-2)), simple power-law model sources, where 4 of these sources have a statistically significant soft component. Among these sources, we find the presence of a warm absorber statistically significant for only one Seyfert 1 source, contrasting with the ASCA results of Reynolds and George and coworkers, who find signatures of warm absorption in half or more of their Seyfert 1 samples at similar redshifts. In addition, the remaining sources (13/22) have more complex spectra, well fitted by an absorbed power law at E > 2.0 keV. Five of the complex sources are classified as Compton-thick candidates. Further, we find four more sources with properties consistent with the hidden/buried AGNs reported by Ueda and coworkers. Finally, we include a comparison of the XMM-Newton EPIC spectra with available Swift X-Ray Telescope (XRT) observations. From these comparisons, we find 6/16 sources with varying column densities, 6/16 sources with varying power-law indices, and 13/16 sources with varying fluxes, over periods of hours to months. Flux and power-law index are correlated for objects where both parameters vary.
C1 [Winter, Lisa M.; Markwardt, Craig] Univ Maryland, College Pk, MD 20742 USA.
[Mushotzky, Richard F.; Tueller, Jack; Markwardt, Craig] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Winter, LM (reprint author), Univ Maryland, College Pk, MD 20742 USA.
EM lwinter@astro.umd.edu
RI Tueller, Jack/D-5334-2012;
OI Winter, Lisa/0000-0002-3983-020X
NR 38
TC 70
Z9 71
U1 0
U2 0
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2008
VL 674
IS 2
BP 686
EP 710
DI 10.1086/525274
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 266RK
UT WOS:000253454500008
ER
PT J
AU Franklin, J
Snell, RL
Kaufman, MJ
Melnick, GJ
Neufeld, DA
Hollenbach, DJ
Bergin, EA
AF Franklin, Jonathan
Snell, Ronald L.
Kaufman, Michael J.
Melnick, Gary J.
Neufeld, David A.
Hollenbach, David J.
Bergin, Edwin A.
TI SWAS observations of water in molecular outflows
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM : abundances; ISM : jets and outflows; ISM : molecules; stars :
formation; stars : winds; outflows
ID WAVE-ASTRONOMY-SATELLITE; SERPENS CLOUD CORE; ORION-KL; C-I; VAPOR
EMISSION; STAR-FORMATION; LINE SURVEY; HH 24-26; GAS; H2O
AB We present detections of the ground-state 1(10) -> 1(01) transition of ortho-H2O at 557 GHz in 18 molecular outflows based on data from the Submillimeter Wave Astronomy Satellite (SWAS). These results are combined with ground-based observations of the J = 1-0 transitions of (CO)-C-12 and (CO)-C-13 obtained at the Five College Radio Astronomy Observatory (FCRAO). Data from Infrared Space Observatory (ISO) for a subset of the outflows are also discussed. Assuming that the SWAS water-line emission originates from the same gas traced by CO emission, we find that the outflowing gas in most outflows has an ortho-H2O abundance relative to H-2 of between similar to 10(-7) and 10(-6). Analysis of the water abundance as a function of outflow velocity reveals a strong dependence. The abundance of ortho-H2O increases with velocity, and at the highest outflow velocities some of the outflows have relative ortho-H2O abundances of order 10(-4). However, the mass of very high velocity gas with such elevated H2O abundances represents less than 1% of the total outflow gas mass. The ISO LWS observations of high-J rotational lines of CO and the 179.5 mu m transition of ortho-H2O provide evidence for a warmer outflow component than required to produce either the SWAS or FCRAO lines. The ISO line-flux ratios can be reproduced with C-shock models with shock velocities of order 25 km s(-1) and pre-shock densities of order 10(5) cm(-3); these C-shocks have postshock relative water abundances greater than 10(-4). The mass associated with the ISO emission is also quite small compared with the total outflow mass and is similar to that responsible for the highest velocity water emission detected by SWAS. Although the gas responsible for the ISO emission has elevated levels of water, the bulk of the outflowing gas has an abundance of ortho-H2O well below what would be expected if the gas has passed through a C-shock with shock velocities greater than 10 km s(-1). Gas-phase water can be depleted in the postshock gas due to freezeout onto grain mantles; however, the rate of freezeout is too slow to explain our results. Therefore, we believe that only a small fraction of the outflowing molecular gas has passed through shocks strong enough to fully convert the gas-phase oxygen to water. This result has implications for the acceleration mechanism of the molecular gas in these outflows.
C1 [Franklin, Jonathan; Snell, Ronald L.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Kaufman, Michael J.] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA.
[Melnick, Gary J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Neufeld, David A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Hollenbach, David J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
RP Franklin, J (reprint author), Univ Massachusetts, Dept Astron, LGRT 619,710 N Pleasant St, Amherst, MA 01003 USA.
NR 54
TC 38
Z9 38
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2008
VL 674
IS 2
BP 1015
EP 1031
DI 10.1086/524924
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 266RK
UT WOS:000253454500028
ER
PT J
AU Trilling, DE
Bryden, G
Beichman, CA
Rieke, GH
Su, KYL
Stansberry, JA
Blaylock, M
Stapelfeldt, KR
Beeman, JW
Haller, EE
AF Trilling, D. E.
Bryden, G.
Beichman, C. A.
Rieke, G. H.
Su, K. Y. L.
Stansberry, J. A.
Blaylock, M.
Stapelfeldt, K. R.
Beeman, J. W.
Haller, E. E.
TI Debris disks around Sun-like stars
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared : stars; planetary systems : formation
ID SOLAR-TYPE STARS; MAIN-SEQUENCE STARS; MULTIBAND IMAGING PHOTOMETER;
SPITZER MIPS SURVEY; BOLOMETRIC CORRECTIONS; INFRARED PHOTOMETRY;
PLANETARY SYSTEM; DWARF STARS; FGK STARS; F-DWARF
AB We have observed nearly 200 FGK stars at 24 and 70 mu m with the Spitzer Space Telescope. We identify excess infrared emission, including a number of cases where the observed flux is more than 10 times brighter than the predicted photospheric flux, and interpret these signatures as evidence of debris disks in those systems. We combine this sample of FGK stars with similar published results to produce a sample of more than 350 main sequence AFGKM stars. The incidence of debris disks is 4.2(-1.1)(+2.0)% at 24 mu m for a sample of 213 Sun-like (FG) stars and 16.4(-2.9)(+2.8)% at 70 mu m for 225 Sun-like (FG) stars. We find that the excess rates for A, F, G, and K stars are statistically indistinguishable, but with a suggestion of decreasing excess rate toward the later spectral types; this may be an age effect. The lack of strong trend among FGK stars of comparable ages is surprising, given the factor of 50 change in stellar luminosity across this spectral range. We also find that the incidence of debris disks declines very slowly beyond ages of 1 billion years.
C1 [Trilling, D. E.; Rieke, G. H.; Su, K. Y. L.; Stansberry, J. A.; Blaylock, M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Bryden, G.; Beichman, C. A.; Stapelfeldt, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Beeman, J. W.; Haller, E. E.] Lawrence Berkeley Natl Lab, Div Mat Sci, Berkeley, CA 94720 USA.
[Haller, E. E.] Univ Calif Berkeley, Dept Mat Sci & Engn, Berkeley, CA 94720 USA.
RP Trilling, DE (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
EM trilling@as.arizona.edu
RI Stapelfeldt, Karl/D-2721-2012;
OI Su, Kate/0000-0002-3532-5580
NR 70
TC 184
Z9 185
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2008
VL 674
IS 2
BP 1086
EP 1105
DI 10.1086/525514
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 266RK
UT WOS:000253454500035
ER
PT J
AU Padmanabhan, N
Schlegel, DJ
Finkbeiner, DP
Barentine, JC
Blanton, MR
Brewington, HJ
Gunn, JE
Harvanek, M
Hogg, DW
Ivezic, Z
Johnston, D
Kent, SM
Kleinman, SJ
Knapp, GR
Krzesinski, J
Long, D
Neilsen, EH
Nitta, A
Loomis, C
Lupton, RH
Roweis, S
Snedden, SA
Strauss, MA
Tucker, DL
AF Padmanabhan, Nikhil
Schlegel, David J.
Finkbeiner, Douglas P.
Barentine, J. C.
Blanton, Michael R.
Brewington, Howard J.
Gunn, James E.
Harvanek, Michael
Hogg, David W.
Ivezic, Zeljko
Johnston, David
Kent, Stephen M.
Kleinman, S. J.
Knapp, Gillian R.
Krzesinski, Jurek
Long, Dan
Neilsen, Eric H., Jr.
Nitta, Atsuko
Loomis, Craig
Lupton, Robert H.
Roweis, Sam
Snedden, Stephanie A.
Strauss, Michael A.
Tucker, Douglas L.
TI An improved photometric calibration of the sloan digital sky survey
imaging data
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE techniques : photometric
ID LUMINOUS RED GALAXIES; LARGE MAGELLANIC CLOUD; DATA RELEASE; STANDARD
STARS; CELESTIAL EQUATOR; SYSTEM; TELESCOPE; CATALOG; EXTINCTION;
EMISSION
AB We present an algorithm to photometrically calibrate wide-field optical imaging surveys, which simultaneously solves for the calibration parameters and relative stellar fluxes using overlapping observations. The algorithm decouples the problem of "relative'' calibrations from that of "absolute'' calibrations; the absolute calibration is reduced to determining a few numbers for the entire survey. We pay special attention to the spatial structure of the calibration errors, allowing one to isolate particular error modes in downstream analyses. Applying this to the SDSS imaging data, we achieve similar to 1% relative calibration errors across 8500 deg(2) in griz; the errors are similar to 2% for the u band. These errors are dominated by unmodeled atmospheric variations at Apache Point Observatory. These calibrations, dubbed "uber-calibration,'' are now public with SDSS Data Release 6 and will be a part of subsequent SDSS data releases.
C1 [Padmanabhan, Nikhil; Schlegel, David J.] Lawrence Berkeley Natl Labs, Div Phys, Berkeley, CA 94720 USA.
[Padmanabhan, Nikhil] Princeton Univ, Joseph Henry Labs, Princeton, NJ 08544 USA.
[Schlegel, David J.; Finkbeiner, Douglas P.; Gunn, James E.; Johnston, David; Knapp, Gillian R.; Loomis, Craig; Lupton, Robert H.; Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Barentine, J. C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Barentine, J. C.; Brewington, Howard J.; Harvanek, Michael; Kleinman, S. J.; Krzesinski, Jurek; Long, Dan; Neilsen, Eric H., Jr.; Nitta, Atsuko; Loomis, Craig; Snedden, Stephanie A.] Apache Point Observ, Sunspot, NM 88349 USA.
[Blanton, Michael R.; Hogg, David W.] NYU, Dept Phys, New York, NY 10003 USA.
[Ivezic, Zeljko] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Johnston, David] Jet Prop Lab, Pasadena, CA 91109 USA.
[Kent, Stephen M.; Neilsen, Eric H., Jr.; Tucker, Douglas L.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Kleinman, S. J.] Subaru Telescope, Hilo, HI 96720 USA.
[Krzesinski, Jurek] Cracow Pedag Univ, Mt Suhora Observ, PL-30084 Krakow, Poland.
[Nitta, Atsuko] Gemini Observ, Hilo, HI 96720 USA.
[Roweis, Sam] Univ Toronto, Dept Comp Sci, Toronto, ON M5S 3G4, Canada.
RP Padmanabhan, N (reprint author), Lawrence Berkeley Natl Labs, Div Phys, Berkeley, CA 94720 USA.
EM npadmanabhan@lbl.gov
RI Padmanabhan, Nikhil/A-2094-2012;
OI Tucker, Douglas/0000-0001-7211-5729; Hogg, David/0000-0003-2866-9403
NR 54
TC 323
Z9 323
U1 0
U2 6
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2008
VL 674
IS 2
BP 1217
EP 1233
DI 10.1086/524677
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 266RK
UT WOS:000253454500048
ER
PT J
AU Ghosh, KK
Punsly, B
AF Ghosh, Kajal K.
Punsly, Brian
TI The discovery of soft X-ray-loud broad absorption line quasars
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; black hole physics; galaxies : jets; quasars
: absorption lines; quasars : general
ID ACTIVE GALACTIC NUCLEI; ROSAT PSPC; EMISSION; GALAXIES; STARS;
ULTRAVIOLET; SEPARATION
AB It has been known for more than a decade that BALQSOs ( broad absorption line quasars) are highly attenuated in the X-ray regime compared to other quasars, especially in the soft band (< 1 keV). Using X-ray selection techniques, we have found "soft X-ray-loud" BALQSOs that, by definition, have soft X-ray (0.3 keV) to UV (3000) flux density ratios that are higher than typical non-BAL radio-quiet quasars. Our sample of three sources includes one LoBALQSO (low-ionization BALQSO), which is generally considered to be the most highly attenuated in X-rays. The three QSOs are the only known BALQSOs that have X-ray observations that are consistent with no intrinsic soft X-ray absorption. The existence of a large X-ray luminosity and the hard ionizing continuum that it presents to potential UV absorption gas is in conflict with the ionization states that are conducive to line-driving forces within BAL winds ( especially for the LoBALs).
C1 [Ghosh, Kajal K.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA.
[Punsly, Brian] ICRANet, I-65100 Pescara, Italy.
RP Ghosh, KK (reprint author), NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, VP62, Huntsville, AL 35812 USA.
EM brian.m.punsly@L-3com.com
NR 23
TC 6
Z9 6
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 20
PY 2008
VL 674
IS 2
BP L69
EP L72
DI 10.1086/529138
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 291YW
UT WOS:000255234500003
ER
PT J
AU Immler, S
Modjaz, M
Landsman, W
Bufano, F
Brown, PJ
Milne, P
Dessart, L
Holland, ST
Koss, M
Pooley, D
Kirshner, RP
Filippenko, AV
Panagia, N
Chevalier, RA
Mazzali, PA
Gehrels, N
Petre, R
Burrows, DN
Nousek, JA
Roming, PWA
Pian, E
Soderberg, AM
Greiner, J
AF Immler, S.
Modjaz, M.
Landsman, W.
Bufano, F.
Brown, P. J.
Milne, P.
Dessart, L.
Holland, S. T.
Koss, M.
Pooley, D.
Kirshner, R. P.
Filippenko, A. V.
Panagia, N.
Chevalier, R. A.
Mazzali, P. A.
Gehrels, N.
Petre, R.
Burrows, D. N.
Nousek, J. A.
Roming, P. W. A.
Pian, E.
Soderberg, A. M.
Greiner, J.
TI Swift and Chandra detections of supernova 2006jc: Evidence for
interaction of the supernova shock with a circumstellar shell
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE circumstellar matter; supernovae : individual (SN 2006jc); X-rays :
general; X rays : individual (SN 2006jc); X rays : ISM; ultraviolet :
ISM
ID TELESCOPE; GALAXY; STAR
AB The peculiar Type Ib supernova (SN) 2006jc has been observed with the UV/Optical Telescope (UVOT) and X-Ray Telescope (XRT) on board the Swift observatory over a period of 19-183 days after the explosion. Signatures of interaction of the outgoing SN shock with dense circumstellar material (CSM) are detected, such as strong X-ray emission (L0.2-10 > 10(39) erg s(-1) ) and the presence of Mg II 2800 angstrom line emission visible in the UV spectra. In combination with a Chandra observation obtained on day 40 after the explosion, the X-ray light curve is constructed, which shows a unique rise of the X-ray emission by a factor of similar to 5 over a period of similar to 4 months, followed by a rapid decline. We interpret the unique X-ray and UV properties as a result of the SN shock interacting with a shell of material that was deposited by an outburst of the SN progenitor 2 years prior to the explosion. Our results are consistent with the explosion of a Wolf-Rayet star that underwent an episodic mass ejection qualitatively similar to those of luminous blue variable stars prior to its explosion. This led to the formation of a dense (similar to 10(7) cm(-3)) shell at a distance of similar to 10(16) cm from the site of the explosion, which expands with the WR wind at a velocity of 1300 +/- 300 km s(-1).
C1 [Immler, S.; Landsman, W.; Bufano, F.; Holland, S. T.; Koss, M.; Gehrels, N.; Petre, R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Immler, S.; Holland, S. T.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
[Immler, S.; Koss, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Modjaz, M.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bufano, F.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Brown, P. J.; Burrows, D. N.; Nousek, J. A.; Roming, P. W. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Milne, P.; Dessart, L.] Steward Observ, Tucson, AZ 85721 USA.
[Holland, S. T.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Pooley, D.; Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Panagia, N.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Chevalier, R. A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Mazzali, P. A.; Pian, E.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy.
[Mazzali, P. A.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Soderberg, A. M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Greiner, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
RP Immler, S (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
EM stefan.immler@nasa.gov
RI Gehrels, Neil/D-2971-2012; Koss, Michael/B-1585-2015;
OI Koss, Michael/0000-0002-7998-9581; Pian, Elena/0000-0001-8646-4858
NR 16
TC 40
Z9 40
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 20
PY 2008
VL 674
IS 2
BP L85
EP L88
DI 10.1086/529373
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 291YW
UT WOS:000255234500007
ER
PT J
AU Sheeley, NR
Herbst, AD
Palatchi, CA
Wang, YM
Howard, RA
Moses, JD
Vourlidas, A
Newmark, JS
Socker, DG
Plunkett, SP
Korendyke, CM
Burlaga, LF
Davila, JM
Thompson, WT
St Cyr, OC
Harrison, RA
Davis, CJ
Eyles, CJ
Halain, JP
Wang, D
Rich, NB
Battams, K
Esfandiari, E
Stenborg, G
AF Sheeley, N. R., Jr.
Herbst, A. D.
Palatchi, C. A.
Wang, Y. -M.
Howard, R. A.
Moses, J. D.
Vourlidas, A.
Newmark, J. S.
Socker, D. G.
Plunkett, S. P.
Korendyke, C. M.
Burlaga, L. F.
Davila, J. M.
Thompson, W. T.
St Cyr, O. C.
Harrison, R. A.
Davis, C. J.
Eyles, C. J.
Halain, J. P.
Wang, D.
Rich, N. B.
Battams, K.
Esfandiari, E.
Stenborg, G.
TI Secchi observations of the Sun's garden-hose density spiral
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun : corona; Sun : coronal mass ejections (CMEs); Sun : magnetic fields
ID CORONA
AB The SECCHI HI2 white-light imagers on the STEREO A and B spacecraft show systematically different proper motions of material moving outward from the Sun in front of high-speed solar wind streams from coronal holes. As a group of ejections enters the eastern (A) field of view, the elements at the rear of the group appear to overrun the elements at the front. (This is a projection effect and does not mean that the different elements actually merge.) The opposite is true in the western (B) field; the elements at the front of the group appear to run away from the elements at the rear. Elongation/ time maps show this effect as a characteristic grouping of the tracks of motion into convergent patterns in the east and divergent patterns in the west, consistent with ejections from a single longitude on the rotating Sun. Evidently, we are observing segments of the "garden-hose" spiral made visible when fast wind from a low-latitude coronal hole compresses blobs of streamer material being shed at the leading edge of the hole.
C1 [Sheeley, N. R., Jr.; Herbst, A. D.; Palatchi, C. A.; Wang, Y. -M.; Howard, R. A.; Moses, J. D.; Vourlidas, A.; Newmark, J. S.; Socker, D. G.; Plunkett, S. P.; Korendyke, C. M.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Burlaga, L. F.; Davila, J. M.; Thompson, W. T.; St Cyr, O. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Harrison, R. A.; Davis, C. J.; Eyles, C. J.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[Eyles, C. J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Halain, J. P.] Univ Liege, Ctr Spatiale Liege, B-4031 Angleur, Belgium.
[Wang, D.; Rich, N. B.; Battams, K.; Esfandiari, E.] Interferometr Inc, Herndon, VA 20171 USA.
[Stenborg, G.] Catholic Univ Amer, Washington, DC 20064 USA.
RP Sheeley, NR (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
EM sheeley@spruce.nrl.navy.mil
RI Vourlidas, Angelos/C-8231-2009; Thompson, William/D-7376-2012; Scott,
Christopher/H-8664-2012
OI Vourlidas, Angelos/0000-0002-8164-5948; Scott,
Christopher/0000-0001-6411-5649
NR 5
TC 42
Z9 42
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 20
PY 2008
VL 674
IS 2
BP L109
EP L112
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 291YW
UT WOS:000255234500013
ER
PT J
AU Wolf, S
Schegerer, A
Beuther, H
Padgett, DL
Stapelfeldt, KR
AF Wolf, S.
Schegerer, A.
Beuther, H.
Padgett, D. L.
Stapelfeldt, K. R.
TI Submillimeter structure of the disk of the Butterfly Star
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE circumstellar matter; planetary systems : formation; planetary systems :
protoplanetary disks; radiative transfer; stars : individual (IRAS
04302+2247); submillimeter
ID YOUNG STELLAR OBJECTS; PROTOPLANETARY DISK; RADIATIVE-TRANSFER; ORIGIN;
ENVELOPES; TAURUS; ARRAY; GAP
AB We present a spatially resolved 894 mm map of the circumstellar disk of the Butterfly Star in Taurus ( IRAS 04302 + 2247), obtained with the Submillimeter Array (SMA). The predicted and observed radial brightness profiles agree well in the outer disk region but differ in the inner region with an outer radius of similar to 80-120 AU. In particular, we find a local minimum of the radial brightness distribution at the center, which can be explained by an increasing density/optical depth combined with the decreasing vertical extent of the disk toward the center. Our finding indicates that young circumstellar disks can be optically thick at wavelengths as long as 894 mm. While earlier modeling lead to general conclusions about the global disk structure and, most importantly, evidence for grain growth in the disk ( Wolf, Padgett, & Stapelfeldt), the presented SMA observations provide more detailed constraints for the disk structure and dust grain properties in the inner, potentially planet-forming region (less than or similar to 80-120 AU) versus the outer disk region (similar to 120-300 AU).
C1 [Wolf, S.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany.
[Wolf, S.; Schegerer, A.; Beuther, H.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Padgett, D. L.] CALTECH, Pasadena, CA 91125 USA.
[Stapelfeldt, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Wolf, S (reprint author), Univ Kiel, Inst Theoret Phys & Astrophys, Leibnizstr 15, D-24098 Kiel, Germany.
EM swolf@mpia.de; schegerer@mpia.de; beuther@mpia.de; dlp@ipac.caltech.edu;
krs@exoplanet.jpl.nasa.gov
RI Stapelfeldt, Karl/D-2721-2012
NR 22
TC 15
Z9 16
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 2008
VL 674
IS 2
BP L101
EP L104
DI 10.1086/529188
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 291YW
UT WOS:000255234500011
ER
PT J
AU Minitti, ME
Leshin, LA
Dyar, MD
Ahrens, TJ
Guan, Y
Luo, SN
AF Minitti, Michelle E.
Leshin, Laurie A.
Dyar, M. Darby
Ahrens, Thomas J.
Guan, Yunbin
Luo, Sheng-Nian
TI Assessment of shock effects on amphibole water contents and hydrogen
isotope compositions: 2. Kaersutitic amphibole experiments
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Mars; Martian meteorites; amphibole; impact shock; hydrogen isotopes
ID IMPLANTED NOBLE-GASES; INDUCED DEVOLATILIZATION; MARTIAN METEORITE;
FRACTIONATION; MANTLE; SERPENTINE; MINERALS; EXCHANGE; ROCKS
AB To constrain the influence of impact shock on water and hydrogen isotope signatures of Martian meteorite kaersutites, we conducted shock recovery experiments on three terrestrial kaersutite crystals. Homogeneous impact shock to 32 GPa, commensurate with shock levels experienced by Martian meteorite kaersutites, led to increases in kaersutite water contents (Delta H2O-0.25-0.89 wt. %), decreases in Fe3+/Sigma Fe (4-20%), and enrichments in hydrogen isotope composition (Delta D=+66 to +87 parts per thousand) relative to pre-shock values. The latter values represent the largest shock-induced hydrogen isotope fractionations measured to date. These observations are explained most completely by a two-step shock process. First, shock-induced devolatilization led to hydrogen isotope enrichment through preferential loss of H relative to D. Second, reaction of the kaersutite with the ambient atmosphere led to increased water contents and reduced Fe. Fe reduction and water addition via the reaction Fe2+ + OH- <-> Fe3+ + O2- + 1/2H(2) explain the Fe3+/Sigma Fe data and some of the water data, Further water addition mechanisms (irreversible adsorption, shock implantation) are necessary to fully explain the increased water contents. Addition of water from the terrestrial atmosphere, which is isotopically light relative to the experimental kaersutite compositions, means the measured hydrogen isotope enrichments are likely minima. The measured (minimum) levels of hydrogen isotope enrichment are relevant to the hydrogen isotope variability within and among Martian kaersutites, but are minor relative to their absolute delta D values. Alternatively, addition of water from the enriched Martian atmosphere could explain both Martian kaersutite hydrogen isotope variability and absolute 6D values. However, the low Martian kaersutite water contents leave little room for significant water addition. The importance of the ambient atmosphere to the outcome of the shock experiments makes it difficult to translate our results to Mars given the unknown influence of its more tenuous atmosphere on the processes observed in the experiments. Our results suggest that shock is a feasible mechanism for influencing
C1 [Minitti, Michelle E.] Arizona State Univ, Res Earth & Space Explorat, Ctr Meteorite Studies, Tempe, AZ 85287 USA.
[Leshin, Laurie A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Dyar, M. Darby] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA.
[Ahrens, Thomas J.; Guan, Yunbin] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Luo, Sheng-Nian] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Minitti, ME (reprint author), Arizona State Univ, Res Earth & Space Explorat, Ctr Meteorite Studies, Tempe, AZ 85287 USA.
EM minitti@asu.edu
RI Luo, Sheng-Nian /D-2257-2010
OI Luo, Sheng-Nian /0000-0002-7538-0541
NR 29
TC 11
Z9 11
U1 0
U2 9
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 20
PY 2008
VL 266
IS 3-4
BP 288
EP 302
DI 10.1016/j.epsl.2007.11.012
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 271QC
UT WOS:000253802800006
ER
PT J
AU Novak, MAM
Watson, IM
Delgado-Granados, H
Rose, WI
Cardenas-Gonzalez, L
Realmuto, VJ
AF Novak, M. A. Matiella
Watson, I. M.
Delgado-Granados, H.
Rose, W. I.
Cardenas-Gonzalez, L.
Realmuto, V. J.
TI Volcanic emissions from Popocatepetl volcano, Mexico, quantified using
Moderate Resolution Imaging Spectroradiometer (MODIS) infrared data: A
case study of the December 2000-January 2001 emissions
SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH
LA English
DT Article
DE Volcanic ash; SO(2); MODIS; infrared; Popocatepetl; remote sensing
ID SULFUR-DIOXIDE EMISSIONS; KILAUEA VOLCANO; ASH CLOUDS; HAWAII; FLUX
AB During December 2000 and January 2001, an increase in activity at Popocatepeti volcano, Mexico, was observed in both ground-based correlation spectrometer (COSPEC) data and in imagery from various satellite sensors, including the Moderate Resolution Imaging Spectroradiometer (MODIS), Total Ozone Mapping Spectrometer (TOMS), Advanced Very High Resolution Radiometer (AVHRR), and Geostationary Satellite 8 (GOES-8). Fine ash abundances detected by MODIS ranged between 6000 and 255,000 metric tons, and fine ash abundances detected by AVHRR, measured at different times, ranged between 4000 and 76,000 metric tons. The difference in ranges of ash mass detected by these two sensors depends largely on the difference in data acquisition time between the two sensors in detecting Popocatepetl's ash clouds. However, the difference could also be partly attributed to differences in spatial resolution and band sensitivity, which are believed to be significantly more favorable for MODIS. Mean effective radii for the two sensors images were typically within 10% of each other; values ranged from 5 to 8 pm and were strongly a function of residence time.
Two types of infrared retrieval were used for the detection and quantification of SO(2) masses - one based on the 7.3 mu m SO(2) absorption feature and the other on the 8.6 mu m absorption feature. SO(2) values were attainable using the 8.6 mu m retrieval for most images, but were problematic using the 7.3 mu m retrieval. Only one SO(2) cloud was successfully measured by the 7.3 mu m retrieval (January 23rd 2001 04:50 UTC). This cloud was at an altitude of approximately 12 km, the highest cloud in the suite of images analyzed, and yielded an SO(2) mass of 16,500 metric tons. This suggests that elevated heights - above similar to 10 km - are required to negate the effects of atmospheric water vapor upon the 7.3 mu m retrieval at tropical latitudes. SO(2) clouds for which the 8.6 mu m retrieval was successful but 7.3 mu m was not were at heights between 6 and 10 km.
Comparison of SO(2) retrievals obtained from MODIS images directly to COSPEC measurements was achieved by taking cross sections of the plume in the MODIS SO, maps. Wind data at the appropriate altitude can then be used to calculate fluxes comparable to those measured by COSPEC in units of tons day(-1). The fluxes calculated from the plume transects fell within the range of fluxes measured by the COSPEC, at 5-32 kT day(-1) and suggest more emissions in mid to late December, and lower emission rates throughout January. The MODIS data also complement a ground-based study on magnetic anomalies in which it was observed that more magma was extruded in the January 23, 2001 eruption than in the eruptions in December of 2000. Ash quantification from MODIS imagery suggests that the majority of fine ash was erupted in January of 2001. (C) 2007 Elsevier B.V. All rights reserved.
C1 [Novak, M. A. Matiella; Watson, I. M.; Rose, W. I.] Michigan Technol Univ, Dept Geog & Min Engn & Sci, Houghton, MI 49931 USA.
[Watson, I. M.] Univ Bristol, Dept Earth Sci, Bristol BS8 IRJ, Avon, England.
[Delgado-Granados, H.] Univ Nacl Autonoma Mexico, Inst Geofis, Mexico City, DF, Mexico.
[Cardenas-Gonzalez, L.] Ctr Nacl Prevenc Desastres, Coyoacan 04360, Mexico.
[Realmuto, V. J.] Jet Prop Lab, Pasadena, CA 91109 USA.
RP Novak, MAM (reprint author), Michigan Technol Univ, Dept Geog & Min Engn & Sci, 1400 Townsend Dr, Houghton, MI 49931 USA.
EM mamatiel@mtu.edu
RI Rose, William/A-7923-2009; Watson, Matt/E-5236-2011; Delgado Granados,
Hugo/J-3056-2013
OI Watson, Matt/0000-0001-9198-2203; Delgado Granados,
Hugo/0000-0001-5263-7968
NR 20
TC 8
Z9 8
U1 0
U2 9
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0377-0273
J9 J VOLCANOL GEOTH RES
JI J. Volcanol. Geotherm. Res.
PD FEB 20
PY 2008
VL 170
IS 1-2
BP 76
EP 85
DI 10.1016/j.jvolgeores.2007.09.010
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA 290FU
UT WOS:000255109500008
ER
PT J
AU Awaki, H
Anabuki, N
Fukazawa, Y
Gallo, LC
Ikeda, S
Isobe, N
Itoh, T
Kunieda, H
Makishima, K
Markowitz, A
Miniutti, G
Mizuno, T
Okajima, T
Ptak, A
Reeves, JN
Takahashi, T
Terashima, Y
Yaqoob, T
AF Awaki, Hisamitsu
Anabuki, Naohisa
Fukazawa, Yasushi
Gallo, Luigi C.
Ikeda, Shinya
Isobe, Naoki
Itoh, Takeshi
Kunieda, Hideyo
Makishima, Kazuo
Markowitz, Alex
Miniutti, Giovanni
Mizuno, Tsunefumi
Okajima, Takashi
Ptak, Andrew
Reeves, James N.
Takahashi, Tadayuki
Terashima, Yuichi
Yaqoob, Tahir
TI Wide-band spectroscopy of the Compton thick Seyfert 2 galaxy Markarian 3
with Suzaku
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE galaxies : active; galaxies : individual (Markarian 3); galaxies :
Seyfert
ID X-RAY-SPECTRUM; ACTIVE GALACTIC NUCLEI; NARROW-LINE REGION; BOARD
SUZAKU; K-LINES; IRON; ABUNDANCES; ALPHA; SPECTROPOLARIMETRY;
PHOTOIONIZATION
AB We obtained a wide-band spectrum of the Compton-thick Seyfert 2 galaxy Mkn 3 with Suzaku. The observed spectrum was clearly resolved into weak, soft power-law emission, a heavily absorbed power-law component, cold reflection, and many emission lines. The heavily absorbed component, absorbed by gas with a column density of 1. 1 x 10(24) cm(-2), has an intrinsic 2-10 keV luminosity of similar to 1. 6 x 10(43) erg s(-1), and is considered to be direct emission from the Mkn 3 nucleus. The reflection component was interpreted as being the reflection of direct light off a cold, thick material; the reflection fraction, R, was 1.36 +/- 0.20. The cold material is inferred to be located > 1 pc from the central black hole of Mkn 3, due to the low ionization parameter of iron ( xi I erg cm s(-1)) and the narrow iron line width (sigma < 22 eV). The weak, soft power-law emission is considered to be scattered light by ionized gas with a scattering fraction of 0.9 +/- 0.2%. The existence of many highly ionized lines in the observed spectrum indicates that the ionized gas has a broad ionized structure, with xi = 10-1000 erg cm s(-1). This high-quality spectrum obtained by Suzaku can be considered to be a template for studies of Seyfert 2 galaxies.
C1 [Awaki, Hisamitsu; Ikeda, Shinya; Terashima, Yuichi] Ehime Univ, Dept Phys, Matsuyama, Ehime 7908577, Japan.
[Anabuki, Naohisa] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan.
[Fukazawa, Yasushi] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Gallo, Luigi C.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Isobe, Naoki; Makishima, Kazuo] RIKEN, Wako, Saitama 3510198, Japan.
[Itoh, Takeshi; Makishima, Kazuo] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Kunieda, Hideyo] Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Markowitz, Alex; Okajima, Takashi; Ptak, Andrew; Reeves, James N.; Yaqoob, Tahir] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Markowitz, Alex; Miniutti, Giovanni; Yaqoob, Tahir] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Miniutti, Giovanni] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Reeves, James N.] Univ Keele, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Takahashi, Tadayuki] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
RP Awaki, H (reprint author), Ehime Univ, Dept Phys, Matsuyama, Ehime 7908577, Japan.
EM awaki@astro.phys.sci.ehime-u.ac.jp
RI Miniutti, Giovanni/L-2721-2014; XRAY, SUZAKU/A-1808-2009
OI Miniutti, Giovanni/0000-0003-0707-4531;
NR 42
TC 26
Z9 26
U1 0
U2 1
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 20
PY 2008
VL 60
SI 1
BP S293
EP S305
DI 10.1093/pasj/60.sp1.S293
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 300IY
UT WOS:000255818700029
ER
PT J
AU Bamba, A
Fukazawa, Y
Hiraga, JS
Hughes, JP
Katagiri, H
Kokubun, M
Koyama, K
Miyata, E
Mizuno, T
Mori, K
Nakajima, H
Ozaki, M
Petre, R
Takahashi, H
Takahashi, T
Tanaka, T
Terada, Y
Uchiyama, Y
Watanabe, S
Yamaguch, H
AF Bamba, Aya
Fukazawa, Yasushi
Hiraga, Junko S.
Hughes, John P.
Katagiri, Hideaki
Kokubun, Motohide
Koyama, Katsuji
Miyata, Emi
Mizuno, Tsunefumi
Mori, Koji
Nakajima, Hiroshi
Ozaki, Masanobu
Petre, Rob
Takahashi, Hiromitsu
Takahashi, Tadayuki
Tanaka, Takaaki
Terada, Yukikatsu
Uchiyama, Yasunobu
Watanabe, Shin
Yamaguch, Hiroya
TI Suzaku wide-band observations of SN 1006
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE acceleration of particles; ISM : individual (SN 1006); X-rays : ISM
ID SUPERNOVA REMNANT SN-1006; X-RAY-DETECTOR; BOARD SUZAKU;
PARTICLE-ACCELERATION; SHOCK ACCELERATION; ELECTRONS; EMISSION; MAXIMUM;
CHANDRA; SN1006
AB We report on the wide-band spectra of SN 1006, as observed by Suzaku. Thermal and nonthermal emissions were successfully resolved thanks to the excellent spectral response of Suzaku's X-ray CCD XIS. The nonthermal emission could not be reproduced by a simple power-law model, but needed a roll-off at 5.7 x 10(16) Hz = 0.23 keV. The roll-off frequency is significantly higher in the northeastern rim than in the southwestern rim. We also placed the most stringent upper limit of the flux above 10 keV using the Hard X-ray Detector.
C1 [Bamba, Aya; Ozaki, Masanobu; Takahashi, Tadayuki; Uchiyama, Yasunobu; Watanabe, Shin] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Dept High Energy Astrophys, Sagamihara, Kanagawa 2298510, Japan.
[Hiraga, Junko S.] RIKEN, Cosm Radiat Grp, Wako, Saitama 3510198, Japan.
[Fukazawa, Yasushi; Katagiri, Hideaki] Hiroshima Univ, Dept Phys, Hiroshima 7398526, Japan.
[Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Koyama, Katsuji; Yamaguch, Hiroya] Kyoto Univ, Grad Sch Sci, Dept Phys, Kyoto 6068502, Japan.
[Miyata, Emi; Nakajima, Hiroshi] Osaka Univ, Fac Sci, Dept Astrophys, Osaka 5600043, Japan.
[Mori, Koji] Miyazaki Univ, Fac Engn, Dept Appl Phys, Miyazaki 8892192, Japan.
[Petre, Rob] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tanaka, Takaaki] Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA.
[Terada, Yukikatsu] Saitama Univ, Sch Sci, Dept Phys, Saitama 3388570, Japan.
RP Bamba, A (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Dept High Energy Astrophys, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan.
EM bamba@astro.isas.jaxa.jp
RI Terada, Yukikatsu/A-5879-2013; Ozaki, Masanobu/K-1165-2013; XRAY,
SUZAKU/A-1808-2009
OI Terada, Yukikatsu/0000-0002-2359-1857;
NR 40
TC 30
Z9 30
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 20
PY 2008
VL 60
SI 1
BP S153
EP S161
DI 10.1093/pasj/60.sp1.S153
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 300IY
UT WOS:000255818700016
ER
PT J
AU Hyodo, Y
Tsujimoto, M
Hamaguchi, K
Koyama, K
Kitamoto, S
Maeda, Y
Tsuboi, Y
Ezoe, Y
AF Hyodo, Yoshiaki
Tsujimoto, Masahiro
Hamaguchi, Kenji
Koyama, Katsuji
Kitamoto, Shunji
Maeda, Yoshitomo
Tsuboi, Yohko
Ezoe, Yuichiro
TI Suzaku spectroscopy of extended X-ray emission in M 17
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE ISM : bubbles; ISM : HII regions; ISM : individual (M 17); X-rays : ISM
ID HIGH-RESOLUTION; BOARD SUZAKU; VORONOI TESSELLATIONS; CORONAL
ABUNDANCES; STELLAR OBJECTS; M17; CHANDRA; NEBULA; REGION; STARS
AB We present the results of a Suzaku spectroscopic study of soft extended X-ray emission in the H II region of M 17. The spectrum of the extended emission was obtained with a high signal-to-noise ratio in a spatially resolved manner using the X-ray Imaging Spectrometer (XIS). We established that contamination by unresolved point sources, the Galactic Ridge X-ray emission, the cosmic X-ray background, and the local hot bubble emission is negligible in the background-subtracted XIS spectrum of the diffuse emission. Half a dozen emission lines were clearly resolved for the first time, including K alpha lines of highly ionized O, Ne, and Mg as well as L-series complex of Fe at 0.5-1.5keV. Based on diagnosis of these lines, we obtained the following results: (1) the extended emission is an optically thin thermal plasma, represented well by a single temperature of similar to 3.0 +/- 0.4 MK, (2) the abundances of elements with emission lines in the diffuse spectrum are 0.1-0.3 solar, while those of bright discrete sources are 0.3-1.5 solar, (3) the metal abundances relative to each other in the diffuse emission are consistent with solar, except for a Ne enhancement of a factor of similar to 2, (4) both the plasma temperature and the chemical composition of the diffuse emission show no spatial variation across the studied spatial scale of similar to 5 pc.
C1 [Hyodo, Yoshiaki; Koyama, Katsuji] Kyoto Univ, Grad Sch Sci, Dept Phys, Kyoto 6068502, Japan.
[Tsujimoto, Masahiro; Kitamoto, Shunji] Rikkyo Univ, Dept Phys, Tokyo 1718501, Japan.
[Tsujimoto, Masahiro] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
CRESST, Greenbelt, MD 20771 USA.
[Hamaguchi, Kenji] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Maeda, Yoshitomo] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Tsuboi, Yohko] Chuo Univ, Dept Sci & Engn, Bunkyo Ku, Tokyo 1128551, Japan.
[Ezoe, Yuichiro] RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan.
RP Hyodo, Y (reprint author), Kyoto Univ, Grad Sch Sci, Dept Phys, Kita Shirakawa Oiwake Cho, Kyoto 6068502, Japan.
EM hyodo@cr.scphys.kyoto-u.ac.jp
RI XRAY, SUZAKU/A-1808-2009
NR 54
TC 15
Z9 15
U1 0
U2 1
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 20
PY 2008
VL 60
SI 1
BP S85
EP S93
DI 10.1093/pasj/60.sp1.S85
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 300IY
UT WOS:000255818700009
ER
PT J
AU Itoh, T
Done, C
Makishima, K
Madejski, G
Awaki, H
Gandhi, P
Isobe, N
Dewangan, GC
Griffthis, RE
Anabuki, N
Okajima, T
Reeves, JN
Takahashi, T
Ueda, Y
Eguchi, S
Yaqoob, T
AF Itoh, Takeshi
Done, Chris
Makishima, Kazuo
Madejski, Grzegorz
Awaki, Hisamitsu
Gandhi, Poshak
Isobe, Naoki
Dewangan, Gulab C.
Griffthis, Richard E.
Anabuki, Naohisa
Okajima, Takashi
Reeves, James N.
Takahashi, Tadayuki
Ueda, Yoshihiro
Eguchi, Satohi
Yaqoob, Tahir
TI Suzaku wide-band X-ray spectroscopy of the Seyfert 2 AGN in NGC 4945
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE galaxies : active; galaxies : individual (NGC 4945); galaxies : Seyfert;
X-rays : galaxies
ID ACTIVE GALACTIC NUCLEI; NGC 4945; XMM-NEWTON; ASCA OBSERVATIONS; GALAXY
NGC-4945; BOARD SUZAKU; EMISSION; SPECTRA; IRON; BEPPOSAX
AB Suzaku observed a nearby Seyfert 2 galaxy, NGC 4945, which hosts one of the brightest active galactic nuclei above 20keV. Combining data from the two detectors aboard Suzaku, the AGN intrinsic nuclear emission and its reprocessed signals were observed simultaneously. The intrinsic emission is highly obscured with an absorbing column of similar to 5 X 10(24) CM-2. The spectrum below 10 keV is dominated by a reflection continuum and emission lines from neutral/ionized material. Along with a neutral iron K alpha line, a neutral iron K alpha line and a neutral nickel Ka line were detected for the first time from this source. The neutral lines and the cold reflection continuum are consistent with both originating in the same location. The Compton down-scattered shoulder in the neutral Fe-K alpha line is similar to 10% in flux of the narrow core, which confirms that the line originates from reflection, rather than transmission. The flux of the intrinsic emission varied by a factor of similar to 2 within similar to 20 ks, which requires the obscuring material to be geometrically thin. Broadband spectral modeling showed that the solid angle of the neutral reflector is less than a few x 10(-2) x 2 pi. All of this evidence regarding the reprocessed signals suggests that a disk-like absorber/reflector is viewed from a near edge-on angle.
C1 [Itoh, Takeshi; Makishima, Kazuo] Univ Tokyo, Fac Sci, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Done, Chris] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Makishima, Kazuo; Gandhi, Poshak; Isobe, Naoki] RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan.
[Madejski, Grzegorz] Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA.
[Awaki, Hisamitsu] Ehime Univ, Dept Phys & Astron, Matsuyama, Ehime 7908577, Japan.
[Dewangan, Gulab C.; Griffthis, Richard E.] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.
[Anabuki, Naohisa] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan.
[Okajima, Takashi; Reeves, James N.] NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA.
[Okajima, Takashi; Reeves, James N.; Yaqoob, Tahir] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Takahashi, Tadayuki] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Ueda, Yoshihiro; Eguchi, Satohi] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Yaqoob, Tahir] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Itoh, T (reprint author), Univ Tokyo, Fac Sci, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
EM titoh@amalthea.phys.s.u-tokyo.ac.jp
RI XRAY, SUZAKU/A-1808-2009; done, chris/D-4605-2016
OI done, chris/0000-0002-1065-7239
NR 69
TC 37
Z9 37
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 20
PY 2008
VL 60
SI 1
BP S251
EP S261
DI 10.1093/pasj/60.sp1.S251
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 300IY
UT WOS:000255818700026
ER
PT J
AU Markowitz, A
Reeves, JN
Miniutti, G
Serlemitsos, P
Kunieda, H
Yaqoob, T
Fabian, AC
Fukazawa, Y
Mushotzky, R
Okajima, T
Gallo, LC
Awaki, H
Griffiths, RE
AF Markowitz, Alex
Reeves, James N.
Miniutti, Giovanni
Serlemitsos, Peter
Kunieda, Hideyo
Yaqoob, Tahir
Fabian, Andrew C.
Fukazawa, Yasushi
Mushotzky, Richard
Okajima, Takashi
Gallo, Luigi C.
Awaki, Hisamitsu
Griffiths, Richard E.
TI The Suzaku observation of NGC 3516: Complex absorption and the broad and
narrow FeK lines
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE galaxies : active; galaxies : individual (NGC 3516); X-rays : galaxies
ID ACTIVE GALACTIC NUCLEI; SEYFERT-GALAXY NGC-3516; X-RAY REFLECTION;
XMM-NEWTON; EMISSION-LINE; BOARD SUZAKU; BLACK-HOLE; ACCRETION DISK;
ALPHA PROFILE; COLD MATTER
AB We present results from a 150 ks Suzaku observation of the Seyfert 1.5 NGC 3516 in 2005 October. The source was in a relatively highly absorbed state. Our best-fit model is consistent with the presence of a low-ionization absorber having a column density near 5 X 1022 cm(-2) and covering most of the X-ray continuum source (covering fraction 96-100%). A high-ionization absorbing component, which yields a narrow absorption feature consistent with Fe xxvi K, is confirmed. A relativistically broadened Fe K alpha line was required in all fits, even after the complex absorption was taken into account; an additional partial-covering component is an inadequate substitute for the continuum curvature associated with the broad Fe line. A narrow Fe Ka emission line has a velocity width consistent with the Broad Line Region. The low-ionization absorber may be responsible for producing the narrow Fe Ka line, though a contribution from additional material out of the line of sight is possible. We include in our model soft band emission lines from He- and H-like ions of N, O, Ne, and Mg, consistent with photo-ionization, though a small contribution from collisionally-ionized emission is possible.
C1 [Markowitz, Alex; Reeves, James N.; Serlemitsos, Peter; Mushotzky, Richard; Okajima, Takashi] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Markowitz, Alex; Reeves, James N.; Yaqoob, Tahir; Okajima, Takashi] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Reeves, James N.] Univ Keele, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England.
[Miniutti, Giovanni; Fabian, Andrew C.] Inst Astron, Cambridge CB3 0HA, England.
[Kunieda, Hideyo] Nagoya Univ, Sch Sci, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Kunieda, Hideyo] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Fukazawa, Yasushi] Hiroshima Univ, Dept Phys, Hiroshima 7398526, Japan.
[Gallo, Luigi C.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Awaki, Hisamitsu] Ehime Univ, Fac Sci, Dept Phys, Matsuyama, Ehime 7908577, Japan.
[Griffiths, Richard E.] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.
RP Markowitz, A (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Code 662, Greenbelt, MD 20771 USA.
RI Miniutti, Giovanni/L-2721-2014; XRAY, SUZAKU/A-1808-2009
OI Miniutti, Giovanni/0000-0003-0707-4531;
NR 65
TC 6
Z9 6
U1 0
U2 1
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 20
PY 2008
VL 60
SI 1
BP S277
EP S291
DI 10.1093/pasj/60.sp1.S277
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 300IY
UT WOS:000255818700028
ER
PT J
AU Miller, ED
Tsunemi, H
Bautz, MW
McCammon, D
Fujimoto, R
Hughes, JP
Katsuda, S
Kokubun, M
Mitsuda, K
Porter, FS
Takei, Y
Tsuboi, Y
Yamasaki, NY
AF Miller, Eric D.
Tsunemi, Hiroshi
Bautz, Mark W.
McCammon, Dan
Fujimoto, Ryuichi
Hughes, John P.
Katsuda, Satoru
Kokubun, Motohide
Mitsuda, Kazuhisa
Porter, F. Scott
Takei, Yoh
Tsuboi, Yohko
Yamasaki, Noriko Y.
TI Suzaku observations of the North Polar Spur: Evidence for nitrogen
enhancement
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE ISM : abundances; ISM : individual (North Polar Spur); ISM : structure;
ISM : supernova remnants; X-rays : ISM
ID X-RAY-EMISSION; GALACTIC-CENTER; INTERSTELLAR-MEDIUM; LOOP-I;
SCORPIO-CENTAURUS; SUPERNOVA REMNANT; STARBURST MODEL; CYGNUS LOOP;
SOLAR-WIND; XMM-NEWTON
AB We present observations of the North Polar Spur (NPS) using the X-ray Imaging Spectrometer (XIS) aboard the Suzaku X-ray satellite. The NPS is a large region of enhanced soft X-ray and radio emission projected above the plane of the Galaxy, likely produced by a series of supernovae and stellar winds from the nearby Sco-Cen OB association. The exceptional sensitivity and spectral resolution of the XIS below 1 keV allow unprecedented probing of low-energy spectral lines, including C VI (0.37 keV) and N VII (0.50 keV), and we have detected highly-ionized nitrogen toward the NPS for the first time. For this single pointing toward the brightest 3/4 keV emission (l = 26.degrees 8, b = +22.degrees 0), the best-fit NPS emission model implies a hot (kT approximate to 0.3 keV), collisional ionization equilibrium (CIE) plasma with depleted C, O, Ne, Mg, and Fe abundances of less than 0.5 solar, but an enhanced N abundance, with N/O = (4.0(-0.5)(+0.4)) times solar. The temperature and total thermal energy of the gas suggest heating by one or more supernovae, while the enhanced nitrogen abundance is best explained by enrichment from stellar material that has been processed by the CNO cycle. Due to the time required to develop AGB stars, we conclude that this N/O enhancement cannot be caused by the Sco-Cen OB association, but may result from a previous enrichment episode in the solar neighborhood.
C1 [Miller, Eric D.; Bautz, Mark W.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Tsunemi, Hiroshi; Katsuda, Satoru] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan.
[McCammon, Dan] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Fujimoto, Ryuichi; Mitsuda, Kazuhisa; Takei, Yoh; Yamasaki, Noriko Y.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Kokubun, Motohide] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Porter, F. Scott] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Takei, Yoh] SRON, NL-3584 CA Utrecht, Netherlands.
[Tsuboi, Yohko] Chuo Univ, Dept Phys, Bunkyo Ku, Tokyo 1128551, Japan.
RP Miller, ED (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM milleric@mit.edu
RI Yamasaki, Noriko/C-2252-2008; Mitsuda, Kazuhisa/C-2649-2008; Porter,
Frederick/D-3501-2012; XRAY, SUZAKU/A-1808-2009
OI Porter, Frederick/0000-0002-6374-1119;
NR 70
TC 14
Z9 14
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 20
PY 2008
VL 60
SI 1
BP S95
EP S106
DI 10.1093/pasj/60.sp1.S95
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 300IY
UT WOS:000255818700010
ER
PT J
AU Ohno, M
Fukazawa, Y
Takahashi, T
Yamaoka, K
Sugita, S
Pal'shin, V
Frederiks, D
Oleynik, P
Ulanov, M
Sakamoto, T
Sato, G
Hurley, K
Tashiro, MS
Urata, Y
Onda, K
Tamagawa, T
Terada, Y
Suzuki, M
Soojing, H
AF Ohno, Masanori
Fukazawa, Yasushi
Takahashi, Takuya
Yamaoka, Kazutaka
Sugita, Satoshi
Pal'shin, Valentin
Frederiks, Dmitry
Oleynik, Philipp
Ulanov, Mikhail
Sakamoto, Takanori
Sato, Goro
Hurley, Kevin
Tashiro, Makoto S.
Urata, Yuji
Onda, Kaori
Tamagawa, Toru
Terada, Yukikatsu
Suzuki, Motoko
Soojing, Hong
TI Spectral properties of prompt emission of four short gamma-ray bursts
observed by the Suzaku-WAM and the Konus-wind
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE gamma rays : burst; gamma rays : observations
ID ALL-SKY MONITOR; LIGHT CURVES; BOARD SUZAKU; CATALOG; HARD; GRB-050709;
PERFORMANCE; AFTERGLOW; BEPPOSAX; DETECTOR
AB We have performed a joint analysis of prompt emission from four bright short gamma-ray bursts (GRBs) with the Suzaku-WAM and the Konus-Wind experiments. This joint analysis allows us to investigate the spectral properties of short-duration bursts over a wider energy band with a higher accuracy. We find that these bursts have a high E-peak, around 1 MeV and have a harder power-law component than that of long GRBs. However, we can not determine whether these spectra follow the cut-off power-law model or the Band model. We also investigated the spectral lag, hardness ratio, inferred isotropic radiation energy and existence of a soft emission hump, in order to classify them into short or long GRBs using several criteria, in addition to the burst duration. We find that all criteria, except for the existence of the soft hump, support the fact that our four GRB samples are correctly classified as belonging to the short class. In addition, our broad-band analysis revealed that there is no evidence of GRBs with a very large hardness ratio, as seen in the BATSE short GRB sample, and that the spectral lag of our four short GRBs is consistent with zero, even in the MeV energy band, unlike long GRBs. Although our short GRB samples are still limited, these results suggest that the spectral hardness of short GRBs might not differ significantly from that of long GRBs, and also that the spectral lag at high energies could be a strong criterion for burst classification.
C1 [Ohno, Masanori; Fukazawa, Yasushi; Takahashi, Takuya] Hiroshima Univ, Sch Sci, Dept Phys Sci, Hiroshima 7398526, Japan.
[Yamaoka, Kazutaka; Sugita, Satoshi] Aoyama Gakuin Univ, Dept Math & Phys, Kanagawa 2298558, Japan.
[Pal'shin, Valentin; Frederiks, Dmitry; Oleynik, Philipp; Ulanov, Mikhail] AF Ioffe Phys Tech Inst, Expt Astrophys Lab, St Petersburg 194021, Russia.
[Sakamoto, Takanori; Sato, Goro] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hurley, Kevin] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Tashiro, Makoto S.; Urata, Yuji; Onda, Kaori] Saitama Univ, Dept Phys, Sakura Ku, Saitama 3388570, Japan.
[Tamagawa, Toru; Terada, Yukikatsu; Suzuki, Motoko] RIKEN, Wako, Saitama 3510198, Japan.
[Soojing, Hong] Nihon Univ, Phys Lab, Coll Sci & Technol, Chiba 2748501, Japan.
RP Ohno, M (reprint author), Hiroshima Univ, Sch Sci, Dept Phys Sci, 1-3-1 Kagamiyama, Hiroshima 7398526, Japan.
EM ohno@hirax7.hepl.hiroshima-u.ac.jp
RI Tashiro, Makoto/J-4562-2012; Terada, Yukikatsu/A-5879-2013; Oleynik,
Philipp/C-1104-2014; Frederiks, Dmitry/C-7612-2014; Pal'shin,
Valentin/F-3973-2014; Ulanov, Mikhail/B-3467-2015; XRAY,
SUZAKU/A-1808-2009
OI Terada, Yukikatsu/0000-0002-2359-1857; Ulanov,
Mikhail/0000-0002-0076-5228;
NR 55
TC 11
Z9 11
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 20
PY 2008
VL 60
SI 1
BP S361
EP S373
DI 10.1093/pasj/60.sp1.S361
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 300IY
UT WOS:000255818700035
ER
PT J
AU Smith, RK
Mushotzky, R
Mukai, K
Kallman, T
Markwardt, CB
Tueller, J
AF Smith, Randall K.
Mushotzky, Richard
Mukai, Koji
Kallman, Tim
Markwardt, Craig B.
Tueller, Jack
TI The symbiotic system SS73 17 seen with Suzaku
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE stars : binaries : symbiotic; stars : individual (SS73 17); X-rays :
stars
ID EMISSION-LINE STARS; CH-CYGNI; VARIABLE-STARS; CATALOG; ASCA;
DIAGNOSTICS; 4U-1954+319; SPECTRUM; BINARIES; SAMPLE
AB We observed with Suzaku the symbiotic star SS73 17, motivated by the discovery by the INTEGRAL satellite and the Swift BAT survey that it emits hard X-rays. Our observations showed a highly-absorbed X-ray spectrum with N-H > 10(23) cm(-2), equivalent to A(v) > 26, although the source has B magnitude 11.3 and is also bright in UV. The source also shows strong, narrow iron lines including fluorescent Fe K as well as Fe xxv and Fe XXVI. The X-ray spectrum can be fit with a thermal model including an absorption component that partially covers the source. Most of the equivalent width of the iron fluorescent line in this model can be explained as a combination of reprocessing in a dense absorber plus reflection off a white dwarf surface, but it is likely that the continuum is partially seen in reflection as well. Unlike other symbiotic systems that show hard X-ray emission (CH Cyg, RT Cru, T CrB, GX 1+4), SS73 17 is not known to have shown nova-like optical variability, X-ray flashes, or pulsations, and has always shown faint soft X-ray emission. As a result, although it is likely a white dwarf, the nature of the compact object in SS73 17 is still uncertain. SS73 17 is probably an extreme example of the recently discovered and relatively small class of hard X-ray emitting symbiotic systems.
C1 [Smith, Randall K.; Mushotzky, Richard; Kallman, Tim; Tueller, Jack] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Smith, Randall K.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Mukai, Koji] CRESST, Greenbelt, MD 20771 USA.
[Mukai, Koji] Univ Maryland, Dept Phys, Baltimore, MD USA.
[Markwardt, Craig B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Smith, RK (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM rsmith@milkway.gsfc.nasa.gov
RI Tueller, Jack/D-5334-2012; XRAY, SUZAKU/A-1808-2009
NR 31
TC 3
Z9 3
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 20
PY 2008
VL 60
SI 1
BP S43
EP S48
DI 10.1093/pasj/60.sp1.S43
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 300IY
UT WOS:000255818700005
ER
PT J
AU Takahashi, H
Fukazawa, Y
Mizuno, T
Hirasawa, A
Kitamoto, S
Sudoh, K
Cigita, T
Kubota, A
Makishima, K
Itoh, T
Parmar, AN
Ebisawa, K
Naik, S
Dotani, T
Kokubun, M
Ohnuki, K
Takahashi, T
Yaqoob, T
Angelini, L
Ueda, Y
Yamaoka, K
Kotani, T
Kawai, N
Namiki, M
Kohmura, T
Negoro, H
AF Takahashi, Hiromitsu
Fukazawa, Yasushi
Mizuno, Tsunefumi
Hirasawa, Ayumi
Kitamoto, Shunji
Sudoh, Keisuke
Cigita, Takayuki
Kubota, Aya
Makishima, Kazuo
Itoh, Takeshi
Parmar, Arvind N.
Ebisawa, Ken
Naik, Sachindra
Dotani, Tadayasu
Kokubun, Motohide
Ohnuki, Kousuke
Takahashi, Tadayuki
Yaqoob, Tahir
Angelini, Lorella
Ueda, Yoshihiro
Yamaoka, Kazutaka
Kotani, Taro
Kawai, Nobuyuki
Namiki, Masaaki
Kohmura, Takayoshi
Negoro, Hitoshi
TI Low/Hard state spectra of GRO J1655-40 observed with Suzaku
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE accretion disks; black hole physics; stars : individual (GRO J1655-40);
X-ray : binaries
ID X-RAY-SPECTRA; ABSORPTION-LINE FEATURES; ACTIVE GALACTIC NUCLEI; CYGNUS
X-1; BLACK-HOLE; SUPERLUMINAL SOURCE; 2005 OUTBURST; BOARD SUZAKU; ASCA
OBSERVATIONS; MAGNETIC FLARES
AB The Galactic black-hole binary GROJ1655-40, a source harboring superluminal jets, was observed with Suzaku on 2005 September 22-23. The source was detected over a broad and continuous energy range of 0.7-300 keV, with an intensity of similar to 50 mCrab at 20 keV At a distance of 3.2 kpc, the 0.7-300 keV luminosity was similar to 5.2 x 10(36) erg s(-1) (similar to 0.7% of the Eddington luminosity for a 6 M-circle dot black hole). The source was in a typical low/hard state, exhibiting a power-law shaped continuum with a photon index of similar to 1.6. During the observation, the source intensity gradually decreased by 25% at energies above similar to 3 keV, and by 35% below 2 keV. This, together with the soft X-ray spectra taken with the X-ray Imaging Spectrometer (XIS), suggests the presence of an independent soft component that can be represented by emission from a cool (similar to 0.2 keV) disk. The hard X-ray spectra obtained with the Hard X-ray Detector reveal a high-energy spectral cutoff, with an e-folding energy of similar to 200 keV. The entire 0.7-300 keV spectrum cannot be reproduced by a single thermal Comptonization model, even when considering reflection effects. Instead, the spectrum (except the soft excess) can be successfully explained by invoking two thermal-Comptonization components with different y-parameters. In contrast to the high/soft state spectra of this object, in which narrow iron absorption lines are detected with equivalent widths of 60-100 eV, the present XIS spectra bear no such features beyond an upper-limit equivalent width of 23 eV.
C1 [Takahashi, Hiromitsu; Fukazawa, Yasushi; Mizuno, Tsunefumi; Hirasawa, Ayumi] Hiroshima Univ, Sch Sci, Dept Phys Sci, Hiroshima 7398526, Japan.
[Kitamoto, Shunji; Sudoh, Keisuke; Cigita, Takayuki] Rikkyo Univ, Dept Phys, Toshima Ku, Tokyo 1718501, Japan.
[Kubota, Aya] Shibaura Inst Technol, Dept Elect Informat Syst, Minami Ku, Saitama 3378570, Japan.
[Makishima, Kazuo] RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan.
[Makishima, Kazuo; Itoh, Takeshi] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Parmar, Arvind N.] European Space Technol Ctr, European Space Agcy, Res & Sci Support Dept, Astrophys Miss Div, NL-2200 AG Noordwijk, Netherlands.
[Ebisawa, Ken; Naik, Sachindra; Dotani, Tadayasu; Kokubun, Motohide; Ohnuki, Kousuke; Takahashi, Tadayuki] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Yaqoob, Tahir] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Angelini, Lorella] NASA, Goddard Space Flight Ctr, Explos Universe Div, Greenbelt, MD 20771 USA.
[Ueda, Yoshihiro] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Yamaoka, Kazutaka] Aoyama Gakuin Univ, Dept Math & Phys, Kanagawa 2298558, Japan.
[Kotani, Taro; Kawai, Nobuyuki] Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan.
[Namiki, Masaaki] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan.
[Kohmura, Takayoshi] Kogakuin Univ, Dept Phys, Tokyo 1920015, Japan.
[Negoro, Hitoshi] Nihon Univ, Coll Sci & Technol, Dept Phys, Chiyoda Ku, Tokyo 1018308, Japan.
RP Takahashi, H (reprint author), Hiroshima Univ, Sch Sci, Dept Phys Sci, Hiroshima 7398526, Japan.
EM hirotaka@hirax7.hepl.hiroshima-u.ac.jp
RI XRAY, SUZAKU/A-1808-2009
NR 58
TC 38
Z9 38
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 20
PY 2008
VL 60
SI 1
BP S69
EP S83
DI 10.1093/pasj/60.sp1.S69
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 300IY
UT WOS:000255818700008
ER
PT J
AU Takahashi, T
Tanaka, T
Uchiyama, Y
Hiraga, JS
Nakazawa, K
Watanabe, S
Bamba, A
Hughes, JP
Katagiri, H
Kataoka, J
Kokubun, M
Koyama, K
Mori, K
Petre, R
Takahashi, H
Tsuboi, Y
AF Takahashi, Tadayuki
Tanaka, Takaaki
Uchiyama, Yasunobu
Hiraga, Junko S.
Nakazawa, Kazuhiro
Watanabe, Shin
Bamba, Aya
Hughes, John P.
Katagiri, Hideaki
Kataoka, Jun
Kokubun, Motohide
Koyama, Katsuji
Mori, Koji
Petre, Robert
Takahashi, Hiromitsu
Tsuboi, Yoko
TI Measuring the broad-band X-ray spectrum from 400 eV to 40 keV in the
southwest part of the supernova remnant RX J1713.7-3946
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE acceleration of particles; ISM : individual (RX J1713.7-3946); ISM :
supernova remnants; X-rays : ISM
ID DIFFUSIVE SHOCK ACCELERATION; MONTE-CARLO SIMULATOR; MAGNETIC-FIELD;
BOARD SUZAKU; COSMIC-RAYS; HIGH-ENERGY; DETECTOR HXD; XMM-NEWTON; SHELL;
EMISSION
AB We report on results from Suzaku broadband X-ray observations of the southwest part of the galactic supernova remnant (SNR) RX J1713.7-3946 with an energy coverage of 0.4-40keV. The X-ray spectrum, presumably of synchrotron origin, is known to be completely lineless, making this SNR ideally suited for a detailed study of the X-ray spectral shape formed through efficient particle acceleration at high-speed shocks. With a sensitive hard X-ray measurement from the HXD PIN aboard Suzaku, we determined the hard X-ray spectrum in the 12-40 keV range to be described by a power law with photon index of Gamma = 3.2 +/- 0.2, significantly steeper than the soft X-ray index of Gamma = 2.4 +/- 0.05 measured previously with ASCA and other missions. We find that a simple power law fails to describe the full spectral range of 0.4-40 keV, and instead a power-law with an exponential cutoff with a hard index of Gamma = 1.50 +/- 0.09 and a high-energy cutoff of epsilon(c) = 1.2 +/- 0.3 keV formally provides an excellent fit over the full bandpass. If we use the so-called SRCUT model, as an alternative model, it gives a best-fit rolloff energy of epsilon(roll) = 0.95 +/- 0.04 keV. Together with the TeV gamma-ray spectrum, ranging from 0.3 to 100 TeV, recently obtained by HESS observations, our Suzaku observations of RX J1713.7-3946 provide stringent constraints on the highest-energy particles accelerated in a supernova shock.
C1 [Takahashi, Tadayuki; Tanaka, Takaaki; Uchiyama, Yasunobu; Watanabe, Shin; Bamba, Aya; Kokubun, Motohide] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Dept High Energy Astrophys, Sagamihara, Kanagawa 2298510, Japan.
[Takahashi, Tadayuki; Nakazawa, Kazuhiro; Watanabe, Shin] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Tanaka, Takaaki] Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA.
[Hiraga, Junko S.] RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan.
[Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Katagiri, Hideaki; Takahashi, Hiromitsu] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Koyama, Katsuji] Kyoto Univ, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan.
[Kataoka, Jun] Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan.
[Mori, Koji] Miyazaki Univ, Dept Appl Phys, Miyazaki 8892198, Japan.
[Petre, Robert] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Tsuboi, Yoko] Chuo Univ, Dept Phys, Bunkyo Ku, Tokyo 1128551, Japan.
RP Takahashi, T (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Dept High Energy Astrophys, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan.
RI XRAY, SUZAKU/A-1808-2009
NR 45
TC 32
Z9 32
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 20
PY 2008
VL 60
SI 1
BP S131
EP S140
DI 10.1093/pasj/60.sp1.S131
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 300IY
UT WOS:000255818700014
ER
PT J
AU Yonetoku, D
Tanabe, S
Murakami, T
Emura, N
Aoyama, Y
Kidamura, T
Kodaira, H
Kodama, Y
Kozaka, R
Nashimoto, T
Okuno, S
Yokota, S
Yoshinari, S
Abe, K
Onda, K
Tashiro, MS
Urata, Y
Nakagawa, YE
Sugita, S
Yamaoka, K
Yoshida, A
Ishimura, T
Kawai, N
Shimokawabe, T
Kinugasa, K
Kohmura, T
Kubota, K
Sugiyasu, K
Ueda, Y
Masui, K
Nakazawa, K
Takahashi, T
Maeno, S
Sonoda, E
Yamauchi, M
Kuwahara, M
Tamagawa, T
Matsuura, D
Suzuki, M
Barthelmy, S
Gehrels, N
Nousek, J
AF Yonetoku, Daisuke
Tanabe, Sachiko
Murakami, Toshio
Emura, Naomi
Aoyama, Yuka
Kidamura, Takashi
Kodaira, Hironobu
Kodama, Yoshiki
Kozaka, Ryota
Nashimoto, Takuro
Okuno, Shinya
Yokota, Satoshi
Yoshinari, Satoru
Abe, Keiichi
Onda, Kaori
Tashiro, Makoto S.
Urata, Yuji
Nakagawa, Yujin E.
Sugita, Satoshi
Yamaoka, Kazutaka
Yoshida, Atsumasa
Ishimura, Takuto
Kawai, Nobuyuki
Shimokawabe, Takashi
Kinugasa, Kenzo
Kohmura, Takayoshi
Kubota, Kaori
Sugiyasu, Kei
Ueda, Yoshihiro
Masui, Kensuke
Nakazawa, Kazuhiro
Takahashi, Tadayuki
Maeno, Shouta
Sonoda, Eri
Yamauchi, Makoto
Kuwahara, Makoto
Tamagawa, Toru
Matsuura, Daisuke
Suzuki, Motoko
Barthelmy, Scott
Gehrels, Neil
Nousek, John
TI Spectral evolution of GRB 060904A observed with swift and Suzaku -
Possibility of inefficient electron acceleration
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE gamma rays : burst; radiation mechanisms : non-thermal; relativistic
jet; X-rays : individual (GRB 060904A); X-rays : stars acceleration of
particles
ID GAMMA-RAY-BURSTS; BOARD SUZAKU; EMISSION; AFTERGLOWS; CATALOG; SHELLS
AB We observed an X-ray afterglow of GRB 060904A with the Swift and Suzaku satellites. We found rapid spectral softening during both the prompt tail phase and the decline phase of an X-ray flare in the Swift/BAT and Swift/XRT +004 data. The observed spectra were fit by power-law photon indices which rapidly changed from Gamma = (+1.51)(-0.03) to Gamma = 5.30(-0.59)(+0.69) within a few hundred seconds. This is one of the steepest X-ray spectra ever observed, making it quite difficult to explain by simple electron-acceleration and synchrotron -radiation processes. We then applied an alternative broken power-law with exponential cutoff (BPEC) model. It is valid to consider the exponential shape is equivalent to a synchrotron cutoff. Since the spectral cutoff appears in the soft X-ray band, we conclude that the electron acceleration must be inefficient in the internal shocks of GRB 060904A. These cutoff spectra suddenly disappeared at the end of the prompt tail. After that, typical afterglow spectra with F = 2.0 have been continuously and preciously monitored by both Swift/XRT and Suzaku/XIS. We could successfully trace the temporal history of two characteristic break energies that have a time dependence of (proportional to t(-3)-t(-4), while the following afterglow spectra are quite stable. This fact indicates that the emitting material of the prompt tail is due to completely different dynamics from the shallow decay component. Therefore, the emission sites of two distinct phenomena obviously differ from each other.
C1 [Yonetoku, Daisuke; Tanabe, Sachiko; Murakami, Toshio; Emura, Naomi; Aoyama, Yuka; Kidamura, Takashi; Kodaira, Hironobu; Kodama, Yoshiki; Kozaka, Ryota; Nashimoto, Takuro; Okuno, Shinya; Yokota, Satoshi; Yoshinari, Satoru] Kanazawa Univ, Dept Phys, Kanazawa, Ishikawa 9201192, Japan.
[Abe, Keiichi; Onda, Kaori; Tashiro, Makoto S.; Urata, Yuji] Saitama Univ, Dept Phys, Sakura Ku, Saitama 3388570, Japan.
[Nakagawa, Yujin E.; Sugita, Satoshi; Yamaoka, Kazutaka; Yoshida, Atsumasa] Aoyama Gakuin Univ, Dept Math & Phys, Kanagawa 2298551, Japan.
[Ishimura, Takuto; Kawai, Nobuyuki; Shimokawabe, Takashi] Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan.
[Kinugasa, Kenzo] Gunma Astron Observ, Takayama, Gunma 3770702, Japan.
[Kohmura, Takayoshi] Kogakuin Univ, Dept Phys, Tokyo 1920015, Japan.
[Kubota, Kaori; Sugiyasu, Kei; Ueda, Yoshihiro] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Masui, Kensuke; Nakazawa, Kazuhiro; Takahashi, Tadayuki] JAXA, Inst Space & Astronaut Sci, Kanagawa 2298510, Japan.
[Maeno, Shouta; Sonoda, Eri; Yamauchi, Makoto] Miyazaki Univ, Miyazaki 8892192, Japan.
[Kuwahara, Makoto; Tamagawa, Toru] RIKEN, Wako, Saitama 3510198, Japan.
[Kuwahara, Makoto; Tamagawa, Toru] Tokyo Univ Sci, Dept Phys, Shinjyuku Ku, Tokyo 1628601, Japan.
[Matsuura, Daisuke] Osaka Univ, Dept Phys, Osaka 5600043, Japan.
[Suzuki, Motoko] Tsukuba Space Ctr, Tsukuba, Ibaraki 3058505, Japan.
[Barthelmy, Scott; Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nousek, John] Penn State Univ, University Pk, PA 16802 USA.
RP Yonetoku, D (reprint author), Kanazawa Univ, Dept Phys, Kanazawa, Ishikawa 9201192, Japan.
EM yonetoku@astro.s.kanazawa-u.ac.jp
RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Tashiro,
Makoto/J-4562-2012; XRAY, SUZAKU/A-1808-2009
NR 30
TC 0
Z9 0
U1 0
U2 1
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 20
PY 2008
VL 60
SI 1
BP S351
EP S360
DI 10.1093/pasj/60.sp1.S351
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 300IY
UT WOS:000255818700034
ER
PT J
AU Cornet, C
Davies, R
AF Cornet, C.
Davies, R.
TI Use of MISR measurements to study the radiative transfer of an isolated
convective cloud: Implications for cloud optical thickness retrieval
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID INDEPENDENT PIXEL APPROXIMATION; ADEOS-POLDER; PART I; RESOLUTION;
STRATOCUMULUS; ALBEDO; VARIABILITY; RADIANCE; BIASES
AB Radiative transfer simulations of an isolated deep convective cloud reconstructed with stereo-techniques from the Multiangle Imaging Spectroradiometer (MISR) are compared with the reflectances measured at the nine MISR viewing angles. The simulations were done using a three dimensional Monte Carlo model, in which ocean reflectance, aerosol and Rayleigh scattering were prescribed to match the surrounding clear-sky MISR measurements. Making reasonable assumptions regarding the vertical and horizontal distribution of the volume extinction coefficient, we were able to reproduce the MISR measurements with the 3D radiative calculations. While the uniqueness of the these distributions cannot be proven, they all lead to retrievals of much larger cloud optical thickness and cloud water content than for a 1D retrieval. Averaged over the cloud, the difference was a factor of about 3, rising to 9 locally. This is a consequence of horizontal photon transport that serves to highlight the inadequacy of 1D retrievals for the case of deep convective cloud. Concerning the internal cloud properties, we noticed the angular distribution of modeled radiances did not match the measured radiances when an ice crystal phase function was applied. Better estimates of the optical depths and water contents of deep convective clouds appear to be obtainable by integrating an estimate of the extinction coefficient over the vertical cloud extent (when this can assessed) than by attempting to invert the radiance measured from a single-angle view using 1D theory.
C1 [Cornet, C.; Davies, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Cornet, C.] Univ Sci & Tech Lille Flandres Artois, Opt Atmospher Lab, Villeneuve Dascq, France.
[Davies, R.] Univ Auckland, Dept Phys, Auckland 1, New Zealand.
RP Cornet, C (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM celine.cornet@loa.univ-lille1.fr
RI Davies, Roger/D-4296-2009
OI Davies, Roger/0000-0002-2991-0409
NR 39
TC 7
Z9 7
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 19
PY 2008
VL 113
IS D4
AR D04202
DI 10.1029/2007JD008921
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 267TF
UT WOS:000253531400003
ER
PT J
AU Naoki, K
Ukita, J
Nishio, F
Nakayama, M
Comiso, JC
Gasiewski, A
AF Naoki, Kazuhiro
Ukita, Jinro
Nishio, Fumihiko
Nakayama, Masashige
Comiso, Josefino C.
Gasiewski, Al
TI Thin sea ice thickness as inferred from passive microwave and in situ
observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID SATELLITE IMAGERY; OKHOTSK SEA; AMSR-E; VARIABILITY; FREQUENCIES;
POLYNYAS; WINTER; WATER; SAR
AB Microwave radiometric signals from sea ice strongly reflect physical conditions of a layer near the ice surface. This study examines the extent to which the relationships of thickness with brightness temperature and with emissivity hold for thin sea ice, approximately <0.2-0.3 m, and how those relationships may arise from changes in brine characteristics through modification of dielectric properties near the ice surface. In order to address these questions we made concurrent measurements of sea ice thickness in the Sea of Okhotsk from a ship and passive microwave radiometry from an over-flying aircraft. The results show that the brightness temperature and emissivity increase with thickness approximately within the thin ice for a frequency range of 10-37 GHz. The relationship is more pronounced at lower frequencies and at the horizontal polarization. We also established an empirical relationship between ice thickness and salinity in the layer near the ice surface from a field experiment, which qualitatively supports the idea that changes in the near-surface brine characteristics contribute to the observed thickness-brightness temperature/emissivity relationship. On the basis of our results, we conclude that for thin ice, passive microwave radiometric signals likely contain indirect information on ice thickness through the dependence of dielectric properties on brine, which provides a plausible and common explanation for previously proposed passive microwave thickness algorithms.
C1 [Naoki, Kazuhiro; Ukita, Jinro; Nishio, Fumihiko] Chiba Univ, Grad Sch Sci & Technol, Chiba 9502181, Japan.
[Naoki, Kazuhiro; Ukita, Jinro; Nishio, Fumihiko] Chiba Univ, Ctr Environm Remote Sensing, Chiba 9502181, Japan.
[Nakayama, Masashige] Kushiro Childrens Museum, Kushiro, Hokkaido 0850017, Japan.
[Comiso, Josefino C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gasiewski, Al] NOAA, Div Phys Sci, Earth Syst Res Lab, Boulder, CO 80305 USA.
RP Naoki, K (reprint author), Chiba Univ, Grad Sch Sci & Technol, 1-33 Yayoi, Chiba 9502181, Japan.
EM naoki@restaff.chiba-u.jp; jukita@env.sc.niigata-u.ac.jp;
fnishio@faculty.chiba-u.jp; nakayama@kodomoyugakukan.jp;
josefino.c.comiso@nasa.gov; al.gasiewski@noaa.gov
NR 34
TC 13
Z9 13
U1 0
U2 3
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 19
PY 2008
VL 113
IS C2
AR C02S16
DI 10.1029/2007JC004270
PG 11
WC Oceanography
SC Oceanography
GA 267TN
UT WOS:000253532200003
ER
PT J
AU Zwally, HJ
Yi, DH
Kwok, R
Zhao, YH
AF Zwally, H. Jay
Yi, Donghui
Kwok, Ron
Zhao, Yunhe
TI ICESat measurements of sea ice freeboard and estimates of sea ice
thickness in the Weddell Sea
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID WINTER SNOW COVER; SOUTHERN-OCEAN; WAVELET ANALYSIS; GLAS ALTIMETRY;
ROSS SEA; VARIABILITY; ANTARCTICA; MOTION; ROUGHNESS; SSM/I
AB Sea ice freeboard heights in the Weddell Sea of Antarctica are derived from the Ice, Cloud, and Land Elevation Satellite (ICESat) laser altimeter measurements, which have a unique range precision to flat surfaces of 2 cm within 70 m footprints spaced at 172 m along track. Although elevations of flat surfaces can be obtained to an accuracy of similar to 10 cm (1 sigma) per footprint, direct determination of freeboard heights is precluded by errors in knowledge of the geoid and temporal variability of the ocean surface. Therefore freeboards are determined relative to an ocean reference level detected over areas of open water and very thin ice within the sea ice pack using an along-track filtering method. The open water/thin ice selections show good agreement in the combined analysis of ICESat segments and Envisat Synthetic Aperture Radar (SAR) imagery. The average residual between the ICESat-measured ocean level and the EGM96 geoid is 1.4 m. Estimates of snow depth on the sea ice from AMSR-E passive microwave data along with nominal densities of snow, water, and sea ice are used to estimate sea ice thickness. Four periods of ICESat data in May-June (fall) and October-November (late winter) of 2004 and 2005 between longitudes 298 degrees E and 360 degrees E are analyzed. In the fall the mean freeboards are 0.28 m in 2004 and 0.29 m in 2005, and the mean thicknesses are 1.33 m in 2004 and 1.52 m in 2005. In late winter the freeboards grew to 0.37 m in 2004 and 0.35 in 2005, and the thicknesses grew to 2.23 m in 2004 and 2.31 m in 2005. The interannual differences in freeboard are small, and the larger interannual change in estimated thickness mainly represents differences in the snow depth estimates. Seasonal changes in the spatial patterns of freeboard and thickness over the 4 months correlate with the expected circulation of sea ice in the Weddell Sea, as indicated by sea ice velocity fields.
C1 [Zwally, H. Jay; Yi, Donghui] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, SGT Inc, Greenbelt, MD 20771 USA.
[Kwok, Ron] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhao, Yunhe] NASA, Goddard Space Flight Ctr, Caelum Res Corp, Oceans Sci Branch, Greenbelt, MD 20771 USA.
RP Zwally, HJ (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, SGT Inc, Code 614-1, Greenbelt, MD 20771 USA.
EM donghui.yi@nasa.gov
RI Kwok, Ron/A-9762-2008
OI Kwok, Ron/0000-0003-4051-5896
NR 44
TC 75
Z9 80
U1 0
U2 14
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 19
PY 2008
VL 113
IS C2
AR C02S15
DI 10.1029/2007JC004284
PG 17
WC Oceanography
SC Oceanography
GA 267TN
UT WOS:000253532200004
ER
PT J
AU Hudman, RC
Murray, LT
Jacob, DJ
Millet, DB
Turquety, S
Wu, S
Blake, DR
Goldstein, AH
Holloway, J
Sachse, GW
AF Hudman, R. C.
Murray, L. T.
Jacob, D. J.
Millet, D. B.
Turquety, S.
Wu, S.
Blake, D. R.
Goldstein, A. H.
Holloway, J.
Sachse, G. W.
TI Biogenic versus anthropogenic sources of CO in the United States
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ATMOSPHERIC CHEMISTRY; CARBONYL-COMPOUNDS; EMISSIONS; FOREST;
FORMALDEHYDE; ISOPRENE; OZONE; MODEL
AB Aircraft observations of carbon monoxide (CO) from the ICARTT campaign over the eastern United States in summer 2004 ( July 1-August 15), interpreted with a global 3-D model of tropospheric chemistry (GEOS-Chem), show that the national anthropogenic emission inventory from the U. S. Environmental Protection Agency (93 Tg CO y(-1)) is too high by 60% in summer. Our best estimate of the CO anthropogenic source for the ICARTT period is 6.4 Tg CO, including 4.6 Tg from direct emission and 1.8 Tg CO from oxidation of anthropogenic volatile organic compounds (VOCs). The biogenic CO source for the same period from the oxidation of isoprene and other biogenic VOCs is 8.3 Tg CO, and is independently constrained by ICARTT observations of formaldehyde (HCHO). Anthropogenic emissions of CO in the U.S. have decreased to the point that they are now lower than the biogenic source in summer.
C1 [Hudman, R. C.; Murray, L. T.; Jacob, D. J.; Wu, S.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02139 USA.
[Blake, D. R.] Univ Calif Irvine, Sch Phys Sci, Irvine, CA 92697 USA.
[Goldstein, A. H.] Univ Calif Berkeley, Div Ecosyst Sci, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA.
[Holloway, J.] NOAA OAR, Earth Syst Res Lab, Boulder, CO USA.
[Millet, D. B.] Univ Minnesota, Dept Soil Water & Climate, St Paul, MN 55108 USA.
[Sachse, G. W.] NASA, Langley Res Ctr, Div Atmospher Sci, Hampton, VA 23681 USA.
[Turquety, S.] Univ Paris 06, IPSL, Serv Aeron, F-75252 Paris 05, France.
RP Hudman, RC (reprint author), Harvard Univ, Sch Engn & Appl Sci, 29 Oxford St, Cambridge, MA 02139 USA.
EM hudman@fas.harvard.edu; ltmurray@fas.harvard.edu;
djacob@fas.harvard.edu; dbm@umn.edu; solene.turquety@aero.jussieu.fr;
wu18@fas.harvard.edu; drblake@uci.edu; agoldstein@nature.berkeley.edu;
john.s.holloway@noaa.gov; glen.w.sachse@nasa.gov
RI Hudman, Rynda/C-6118-2009; Goldstein, Allen/A-6857-2011; Millet,
Dylan/G-5832-2012; Holloway, John/F-9911-2012; Murray, Lee/F-2296-2014;
Chem, GEOS/C-5595-2014
OI Goldstein, Allen/0000-0003-4014-4896; Holloway,
John/0000-0002-4585-9594; Murray, Lee/0000-0002-3447-3952;
NR 23
TC 72
Z9 72
U1 1
U2 20
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 16
PY 2008
VL 35
IS 4
AR L04801
DI 10.1029/2007GL032393
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 263QT
UT WOS:000253232300003
ER
PT J
AU Parkinson, CL
Comiso, JC
AF Parkinson, Claire L.
Comiso, Josefino C.
TI Antarctic sea ice parameters from AMSR-E data using two techniques and
comparisons with sea ice from SSM/I
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID WEDDELL SEA; TIME-SERIES; MICROWAVE; TRENDS; WATER; SMMR
AB Antarctic sea ice concentrations and extents, derived from the satellite passive microwave data of the Advanced Microwave Scanning Radiometer for the Earth Observing System (AMSR-E) are close but not identical depending on which of two major algorithms is used in the calculations. Overall, ice extents tend to be higher and ice concentrations lower when determined from the AMSR-E bootstrap algorithm (ABA) than when determined from the enhanced NASA team (NT2) algorithm, although the differences are within the algorithm error bars. Both algorithms obtain similar negative slopes for the lines of linear least squares fit through the short (4.5-year) AMSR-E data record available so far. When the ABA results are compared with results from the bootstrap algorithm applied over the same time period to data from the Special Sensor Microwave Imager (SSM/I), the two bootstrap results, from different satellites and different instruments, match even more closely than the ABA versus NT2 results from the same AMSR-E instrument. This is encouraging and is likely due to considerable effort to minimize the AMSR-E versus SSM/ I bootstrap differences, in consideration of extending the SSM/I record (which goes back to 1987) with the AMSR-E results.
C1 [Parkinson, Claire L.; Comiso, Josefino C.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA.
RP Parkinson, CL (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Code 614 1, Greenbelt, MD 20771 USA.
EM claire.l.parkinson@nasa.gov
RI Parkinson, Claire/E-1747-2012
OI Parkinson, Claire/0000-0001-6730-4197
NR 22
TC 8
Z9 9
U1 0
U2 6
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 16
PY 2008
VL 113
IS C2
AR C02S06
DI 10.1029/2007JC004253
PG 15
WC Oceanography
SC Oceanography
GA 263SD
UT WOS:000253235900001
ER
PT J
AU Naeye, R
AF Naeye, Robert
TI Density's child
SO NEW SCIENTIST
LA English
DT Article
C1 NASAs Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Naeye, R (reprint author), NASAs Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
NR 0
TC 0
Z9 0
U1 1
U2 1
PU REED BUSINESS INFORMATION LTD
PI SUTTON
PA QUADRANT HOUSE THE QUADRANT, SUTTON SM2 5AS, SURREY, ENGLAND
SN 0262-4079
J9 NEW SCI
JI New Sci.
PD FEB 16
PY 2008
VL 197
IS 2643
BP 34
EP 35
DI 10.1016/S0262-4079(08)60420-0
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 264CG
UT WOS:000253262300030
ER
PT J
AU Pugel, DE
Vispute, RD
Hullavarad, SS
Venkatesan, T
Varughese, B
AF Pugel, D. Elizabeth
Vispute, R. D.
Hullavarad, S. S.
Venkatesan, T.
Varughese, B.
TI Compositional origin of surface roughness variations in air-annealed ZnO
single crystals
SO APPLIED SURFACE SCIENCE
LA English
DT Article
DE ZnO; single crystal; surface morphology; air-annealing
ID OXIDE SURFACES; STABILITY; HYDROGEN
AB We directly investigated the chemical compositional origin of surface roughness variations in air-annealed ZnO single crystal samples for annealing temperatures up to 1000 degrees C. Atomic Force Microscopy (AFM) showed temperature-dependent changes in surface roughness and morphology, with a maximum in surface roughness of 2 nm found for samples annealed at 400 degrees C. The O(1s) line, measured by X-ray Photoelectron Spectroscopy (XPS) showed a maximum for Zn(OH)(2) and a minimum for off-stoichiometric ZnO at 400 degrees C; while the Zn(2p) peaks show an increase in slope at that temperature. These results indicate that the roughness arises from Zn diffusion and loss of surface oxygen. (c) 2007 Elsevier B.V. All rights reserved.
C1 [Pugel, D. Elizabeth; Vispute, R. D.; Venkatesan, T.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Varughese, B.] Univ Maryland, Dept Mat Sci & Engn, College Pk, MD 20742 USA.
[Hullavarad, S. S.] Univ Alaska, Off Elect Miniaturizat, Fairbanks, AK 99701 USA.
RP Pugel, DE (reprint author), NASA, Goddard Space Flight Ctr, Detector Syst Branch, Greenbelt, MD 20771 USA.
EM Diane.E.Pugel@nasa.gov
RI Venkatesan, Thirumalai/E-1667-2013
NR 16
TC 11
Z9 11
U1 0
U2 5
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0169-4332
EI 1873-5584
J9 APPL SURF SCI
JI Appl. Surf. Sci.
PD FEB 15
PY 2008
VL 254
IS 8
BP 2220
EP 2223
DI 10.1016/j.apsusc.2007.07.206
PG 4
WC Chemistry, Physical; Materials Science, Coatings & Films; Physics,
Applied; Physics, Condensed Matter
SC Chemistry; Materials Science; Physics
GA 277FN
UT WOS:000254198200003
ER
PT J
AU Kolasinski, RD
Polk, JE
Goebel, D
Johnson, LK
AF Kolasinski, Robert D.
Polk, James E.
Goebel, Dan
Johnson, Lee K.
TI Carbon sputtering yield measurements at grazing incidence
SO APPLIED SURFACE SCIENCE
LA English
DT Article
DE sputtering; QCM; thin film; ion beam; carbon
ID ENERGY-DEPENDENCE; MONATOMIC SOLIDS; ION-BOMBARDMENT
AB In this investigation, carbon sputtering yields were measured experimentally at varying angles of incidence under Xe+ bombardment. The measurements were obtained by etching a coated quartz crystal microbalance (QCM) with a low energy ion beam. The material properties of the carbon targets were characterized with a scanning electron microscope (SEM) and Raman spectroscopy. C sputtering yields measured under Ar+ and Xe+ bombardment at normal incidence displayed satisfactory agreement with previously published data over an energy range of 200 eV-1 keV. For Xe+ ions, the dependence of the yields on angle of incidence theta was determined for 0 degrees <= theta <= 80 degrees. Over this range, an increase in C sputtering yield by a factor of 4.8 was observed, with the peak in yield occurring at 70 degrees. This is a much higher variation compared to Xe+ -> Mo yields under similar conditions, a difference that may be attributed to higher scattering of the incident particles transverse to the beam direction than in the case of Xe+! C. In addition, the variation of the yields with theta was not strongly energy dependent. Trapping of Xe in the surface was observed, in contrast to observations using the QCM technique with metallic target materials. Finally, target surface roughness was characterized using atomic force microscope measurements to distinguish between the effects of local and overall angle of incidence of the target. (c) 2007 Elsevier B. V. All rights reserved.
C1 [Kolasinski, Robert D.] CALTECH, Pasadena, CA 91125 USA.
[Polk, James E.; Goebel, Dan; Johnson, Lee K.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
RP Kolasinski, RD (reprint author), Sandia Natl Labs, POB 969,MS 9161, Livermore, CA 94551 USA.
EM rkolasi@sandia.gov
NR 28
TC 14
Z9 14
U1 1
U2 6
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0169-4332
J9 APPL SURF SCI
JI Appl. Surf. Sci.
PD FEB 15
PY 2008
VL 254
IS 8
BP 2506
EP 2515
DI 10.1016/j.apsusc.2007.09.082
PG 10
WC Chemistry, Physical; Materials Science, Coatings & Films; Physics,
Applied; Physics, Condensed Matter
SC Chemistry; Materials Science; Physics
GA 277FN
UT WOS:000254198200048
ER
PT J
AU Echer, E
Gonzalez, WD
Tsurutani, BT
AF Echer, E.
Gonzalez, W. D.
Tsurutani, B. T.
TI Interplanetary conditions leading to superintense geomagnetic storms
(Dst <=-250 nT) during solar cycle 23
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MAGNETIC STORMS; INTENSE; DST; GEOEFFECTIVENESS; CRITERIA; MAXIMUM;
CLOUDS
AB The interplanetary causes of superintense geomagnetic storms (superstorms, Dst <= -250 nT) that occurred during solar cycle 23 are studied. Eleven superstorms occurred during the cycle, five close to solar maximum (2000-2001) and six in the post-maximum/declining phase (2003-2004). About 1/3 of the superstorms were caused by magnetic clouds (MCs), 1/3 by a combination of sheath and MC fields, and 1/3 by sheath fields alone. The interplanetary parameter best correlated with peak Dst was the time-integrated E(y) during the storm main phase (in contrast with peak B(s) and/or peak E(y) for less intense geomagnetic storms). The range of peak Dst for these storms was -263 to -422 nT. The storm main phase durations had a range of 3-33 h. We conclude from this study that: (1) only MCs and/or interplanetary sheaths had fields intense enough and with long enough durations to cause superstorms; (2) superstorms occurred only in the maximum and declining phases; (3) the total energy transferred from the solar wind to the magnetosphere is best correlated with the time-integrated solar wind E(y) parameter.
C1 [Echer, E.; Gonzalez, W. D.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, Brazil.
[Tsurutani, B. T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Echer, E (reprint author), Inst Nacl Pesquisas Espaciais, CP 515,Avenida Asrtonautas 1758, BR-12227010 Sao Jose Dos Campos, Brazil.
EM eecher@dge.inpe.br
NR 25
TC 51
Z9 54
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 FEB 15
PY 2008
VL 35
IS 6
AR L06S03
DI 10.1029/2007GL031755
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 263QV
UT WOS:000253232500001
ER
PT J
AU Logan, JA
Megretskaia, I
Nassar, R
Murray, LT
Zhang, L
Bowman, KW
Worden, HM
Luo, M
AF Logan, Jennifer A.
Megretskaia, Inna
Nassar, Ray
Murray, Lee T.
Zhang, Lin
Bowman, Kevin W.
Worden, Helen M.
Luo, Ming
TI Effects of the 2006 El Nino on tropospheric composition as revealed by
data from the Tropospheric Emission Spectrometer (TES)
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID OZONE
AB The Tropospheric Emission Spectrometer (TES) is unique in providing multi-year coincident tropospheric profiles of CO, O(3) and H(2)O. TES data show large differences in these gases over Indonesia and the eastern Indian Ocean in October-December 2006 relative to 2005. In 2006, O3 was higher by 15-30 ppb (30-75%) while CO was higher by > 80 ppb in October and November, and by similar to 25 ppb in December. These differences were caused by high fire emissions from Indonesia in 2006 associated with the lowest rainfall since 1997, reduced convection during the moderate El Nino, and reduced photochemical loss because of lower H2O. The persistence of the O3 difference into December is consistent with higher NO(x) emissions from lightning in 2006. TES CO and O3 enhancements in 2006 were larger than those observed during the weak El Nino of 2004.
C1 [Logan, Jennifer A.; Megretskaia, Inna; Nassar, Ray; Murray, Lee T.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Bowman, Kevin W.; Luo, Ming] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Worden, Helen M.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80305 USA.
[Zhang, Lin] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
RP Logan, JA (reprint author), Harvard Univ, Sch Engn & Appl Sci, 29 Oxford St, Cambridge, MA 02138 USA.
EM jlogan@seas.harvard.edu
RI Zhang, Lin/A-6729-2008; Murray, Lee/F-2296-2014; Zhang, Lin/H-9801-2014;
OI Zhang, Lin/0000-0003-2383-8431; Murray, Lee/0000-0002-3447-3952; Nassar,
Ray/0000-0001-6282-1611
NR 26
TC 77
Z9 79
U1 1
U2 9
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 15
PY 2008
VL 35
IS 3
AR L03816
DI 10.1029/2007GL031698
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 263QQ
UT WOS:000253232000002
ER
PT J
AU Canovas, CR
Hubbard, CG
Olias, M
Nieto, JM
Black, S
Coleman, ML
AF Canovas, C. R.
Hubbard, C. G.
Olias, M.
Nieto, J. M.
Black, S.
Coleman, M. L.
TI Hydrochemical variations and contaminant load in the Rio Tinto (Spain)
during flood events
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE AMD; Rio Tinto; metal load; flood events
ID ACID-MINE DRAINAGE; IBERIAN PYRITE BELT; TRACE-METAL ENRICHMENTS;
SOUTH-WEST SPAIN; SOUTHWESTERN SPAIN; SULFATE MINERALS; ESTUARINE
SYSTEM; IRON-MOUNTAIN; SW SPAIN; RIVER
AB The aim of this work is to study the hydrochemical variations during flood events in the Rio Tinto, SW Spain. Three separate rainfall/flood events were monitored in October 2004 following the dry season. In general, concentrations markedly increased following the first event (Fe from 99 to 1130 mg/L; Q(max) = 0.78 m(3)/s) while dissolved loads peaked in the second event (Fe = 7.5 kg/s, Cu = 0.83 kg/s, Zn = 0.82 kg/s; Q(max) = 77 m(3)/s) and discharge in the third event (Q(max) = 127 m(3)/s). This pattern reflects a progressive depletion of metals and sulphate stored in the dry summer as soluble evaporitic salt minerals and concentrated pore fluids, with dilution by freshwater becoming increasingly dominant as the month progressed. Variations in relative concentrations were attributed to oxyhydroxysulphate Fe precipitation, to relative changes in the sources of acid mine drainage (e.g. salt minerals, mine tunnels, spoil heaps etc.) and to differences in the rainfall distributions along the catchment. The contaminant load carried by the river during October 2004 was enormous, totalling some 770 t of Fe, 420 t of Al, 100 t of Cu, 100 t of Zn and 71 t of Mn. This represents the largest recorded example of this flush-out process in an acid mine drainage setting. Approximately 1000 times more water and 1408 200 times more dissolved elements were carried by the river during October 2004 than during the dry, low-flow conditions of September 2004, highlighting the key role of flood Events in the annual pollutant transport budget of semi-arid and and systems and the need to monitor these events in detail in order to accurately quantify pollutant transport. (c) 2007 Elsevier B.V. All rights reserved.
C1 [Canovas, C. R.; Olias, M.] Univ Huelva, Dept Geodynam & Paleontol, Huelva 21071, Spain.
[Hubbard, C. G.; Black, S.; Coleman, M. L.] Univ Reading, Sch Human & Environm Sci, Reading RG6 6AB, Berks, England.
[Nieto, J. M.] Univ Huelva, Dept Geol, Huelva 21007, Spain.
[Coleman, M. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM carlos.ruiz@dgeo.uhu.es
RI Coleman, Max/A-1303-2007; Black, Stuart/A-1099-2014; Hubbard,
Christopher/J-6150-2014; Olias, Manuel/O-5449-2014; Nieto, Jose
Miguel/K-1935-2014;
OI Coleman, Max/0000-0002-5514-1826; Black, Stuart/0000-0003-1396-4821;
Hubbard, Christopher/0000-0002-8217-8122; Olias,
Manuel/0000-0001-5394-3449; Nieto, Jose Miguel/0000-0002-0086-252X; RUIZ
CANOVAS, CARLOS/0000-0002-2860-5154
NR 64
TC 55
Z9 55
U1 0
U2 16
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 15
PY 2008
VL 350
IS 1-2
BP 25
EP 40
DI 10.1016/j.jhydrol.2007.11.022
PG 16
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA 268SR
UT WOS:000253600200003
ER
PT J
AU Barrie, RL
Gabb, TP
Telesman, J
Kantzos, PT
Prescenzi, A
Biles, T
Bonacuse, PJ
AF Barrie, R. L.
Gabb, T. P.
Telesman, J.
Kantzos, P. T.
Prescenzi, A.
Biles, T.
Bonacuse, P. J.
TI Effectiveness of shot peening in suppressing fatigue cracking at
non-metallic inclusions in Udimet (R) 720
SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES
MICROSTRUCTURE AND PROCESSING
LA English
DT Article
DE shot peening; fatigue; inclusions; superalloy; disk
AB The fatigue lives of modem powder metallurgy disk alloys can be reduced over an order of magnitude by cracking at inherent non-metallic inclusions. The objective of this work was to study the effectiveness of shot peening in suppressing LCF crack initiation and growth at surface non-metallic inclusions. Inclusions were carefully introduced at elevated levels during powder metallurgy processing of the nickel-base disk superalloy Udimet (R) 720. Multiple strain-controlled fatigue tests were then performed on machined specimens with and without shot peened test sections at 427 and 650 degrees C. The low cycle fatigue lives and failure initiation sites varied as functions of inclusion content, shot peening, and fatigue conditions. A large majority of the failures in as-machined specimens with the introduced inclusions occurred at cracks initiating from inclusions intersecting the specimen surface. These inclusions reduced fatigue life by up to 100x, when compared to lives of material without inclusions residing at specimen surface. Large inclusions produced the greatest reductions in life for tests at low strain ranges and high strain ratios. Shot peening improved life in many cases by reducing the most severe effects of inclusions. (C) 2007 Elsevier B.V. All rights reserved.
C1 [Gabb, T. P.; Telesman, J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Barrie, R. L.] USA Aviat & Missile Command, Redstone Arsenal, AL 35895 USA.
[Kantzos, P. T.] Honeywell Engine Syst, Phoenix, AZ 85038 USA.
[Prescenzi, A.] Ohio State Univ, Columbus, OH 43210 USA.
[Biles, T.] Alcoa Wheel & Forged Prod, Cleveland, OH 44105 USA.
[Bonacuse, P. J.] NASA GRC, Army Res Lab, Cleveland, OH 44135 USA.
RP Gabb, TP (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM timothy.p.gabb@nasa.gov
NR 18
TC 13
Z9 15
U1 0
U2 8
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0921-5093
J9 MAT SCI ENG A-STRUCT
JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process.
PD FEB 15
PY 2008
VL 474
IS 1-2
BP 71
EP 81
DI 10.1016/j.msea.2007.03.100
PG 11
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 260SK
UT WOS:000253030500009
ER
PT J
AU Raj, SV
Ghosn, LJ
AF Raj, S. V.
Ghosn, L. J.
TI Failure maps for rectangular 17-4PH stainless steel sandwiched foam
panels
SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES
MICROSTRUCTURE AND PROCESSING
LA English
DT Article
DE 17-4PH; stainless steel; metallic foams; sandwiched foam panel;
theoretical failure maps; design
ID MECHANICAL-BEHAVIOR; CELLULAR MATERIALS; METAL FOAMS; IMPERFECTIONS;
STIFFNESS; FRACTURE; SOLIDS; CREEP; CORES; BEAMS
AB A new and innovative concept is proposed for designing lightweight fan blades for aircraft engines using commercially available 17-4PH precipitation hardened stainless steel. Rotating fan blades in aircraft engines experience a complex loading state consisting of combinations of centrifugal, distributed pressure and torsional loads. Theoretical failure plastic collapse maps, showing plots of the foam relative density versus face sheet thickness, t, normalized by the fan blade span length, L, have been generated for rectangular 17-4PH sandwiched foam panels under these three loading modes assuming three failure plastic collapse modes. These maps show that the 17-4PH sandwiched foam panels can fail by either the yielding of the face sheets, yielding of the foam core or wrinkling of the face sheets depending on foam relative density, the magnitude of t/L and the loading mode. The design envelop of a generic fan blade is superimposed on the maps to provide valuable insights on the probable failure modes in a sandwiched foam fan blade. Published by Elsevier B.V.
C1 [Raj, S. V.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Ghosn, L. J.] Ohio Aerosp Inst, Cleveland, OH 44135 USA.
RP Raj, SV (reprint author), NASA, Glenn Res Ctr, MS 106-5,21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM sai.v.raj@nasa.gov
NR 31
TC 8
Z9 8
U1 0
U2 6
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0921-5093
J9 MAT SCI ENG A-STRUCT
JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process.
PD FEB 15
PY 2008
VL 474
IS 1-2
BP 88
EP 95
DI 10.1016/j.msea.2007.03.102
PG 8
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 260SK
UT WOS:000253030500011
ER
PT J
AU Jackson, TJ
Moran, MS
O'Neill, PE
AF Jackson, T. J.
Moran, M. S.
O'Neill, P. E.
TI Introduction to Soil Moisture Experiments 2004 (SMEX04) Special Issue
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Editorial Material
C1 [Jackson, T. J.; Moran, M. S.] USDA ARS, Washington, DC 20250 USA.
[O'Neill, P. E.] NASA, Goddard Space Flight Ctr, Washington, DC 20546 USA.
RP Jackson, TJ (reprint author), USDA ARS, Washington, DC 20250 USA.
EM tjackson@hydrolab.ars.usda.gov
NR 12
TC 15
Z9 16
U1 2
U2 6
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 2008
VL 112
IS 2
BP 301
EP 303
DI 10.1016/j.rse.2007.01.021
PG 3
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 261GW
UT WOS:000253068100001
ER
PT J
AU Yilmaz, MT
Hunt, ER
Goins, LD
Ustin, SL
Vanderbilt, VC
Jackson, TJ
AF Yilmaz, M. Tugrul
Hunt, E. Raymond, Jr.
Goins, Lyssa D.
Ustin, Susan L.
Vanderbilt, Vern C.
Jackson, Thomas J.
TI Vegetation water content during SMEX04 from ground data and Landsat 5
Thematic Mapper imagery
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE decision tree classification; equivalent water thickness; leaf area
index; normalized difference infrared index; Soil Moisture Experiment
2004
ID LEAF-AREA INDEX; DECISION TREE CLASSIFICATION; REMOTELY-SENSED DATA;
ATMOSPHERIC CORRECTION; REFLECTANCE DATA; FUEL MOISTURE; LIQUID WATER;
LAND-COVER; MODIS; SOIL
AB Vegetation water content is an important parameter for retrieval of soil moisture from microwave data and for other remote sensing applications. Because liquid water absorbs in the shortwave infrared, the normalized difference infrared index (NDII), calculated from Landsat 5 Thematic Mapper band 4 (0.76-0.90 mu m wavelength) and band 5 (1.55-1.65 mu m wavelength), can be used to determine canopy equivalent water thickness (EWT), which is defined as the water volume per leaf area times the leaf area index (LAI). Alternatively, average canopy EWT can be determined using a landcover classification, because different vegetation types have different average LAI at the peak of the growing season. The primary contribution of this study for the Soil Moisture Experiment 2004 was to sample vegetation for the Axizona and Sonora study areas. Vegetation was sampled to achieve a range of canopy EWT; LAI was measured using a plant canopy analyzer and digital hemispherical (fisheye) photographs. NDII was linearly related to measured canopy EWT with an R-2 of 0.601. Landcover of the Arizona, USA, and Sonora, Mexico, study areas were classified with an overall accuracy of 70% using a rule-based decision tree using three dates of Landsat 5 Thematic Mapper imagery and digital elevation data. There was a large range of NDII per landcover class at the peak of the growing season, indicating that canopy EWT should be estimated directly using NDII or other shortwave-infrared vegetation indices. However, landcover classifications will still be necessary to obtain total vegetation water content from canopy EWT and other data, because considerable liquid water is contained in the non-foliar components of vegetation. Published by Elsevier Inc.
C1 [Yilmaz, M. Tugrul; Hunt, E. Raymond, Jr.; Jackson, Thomas J.] USDA ARS, HRSL, Beltsville, MD 20705 USA.
[Goins, Lyssa D.] Univ Arizona, Tucson, AZ USA.
[Ustin, Susan L.] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA.
[Vanderbilt, Vern C.] NASA, Ames Res Ctr, Moffett Field, CA USA.
RP Hunt, ER (reprint author), USDA ARS, HRSL, Bldg 007,Room 104,BARC-W,10300 Baltimore Ave, Beltsville, MD 20705 USA.
EM Raymond.Hunt@ars.usda.gov
NR 53
TC 57
Z9 58
U1 0
U2 13
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 2008
VL 112
IS 2
BP 350
EP 362
DI 10.1016/j.rse.2007.03.029
PG 13
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 261GW
UT WOS:000253068100006
ER
PT J
AU Cheng, YB
Ustin, SL
Riano, D
Vanderbilt, VC
AF Cheng, Yen-Ben
Ustin, Susan L.
Riano, David
Vanderbilt, Vem C.
TI Water content estimation from hyperspectral images and MODIS indexes in
Southeastern Arizona
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE AVIRIS; MODIS; water content; equivalent water thickness; vegetation
index
ID MODEL INVERSION METHODS; FUEL MOISTURE-CONTENT; BIOPHYSICAL PARAMETERS;
VEGETATION INDEXES; MOJAVE-DESERT; WALNUT-GULCH; AVIRIS DATA; LEAF;
REFLECTANCE; CANOPIES
AB Hyperspectral water retrievals from AVIRIS data, equivalent water thickness (EWT), were compared to in situ leaf water content and LAI measurements at a semiarid site in southeastern Arizona. Retrievals of EWT showed good correlation with field canopy water content measurements. Statistical analysis suggested that EWT was significantly different among seven community types, from savanna to agriculture. Four band-ratio indexes (NDVI, EVI, NDWI, and NDII) were derived from MODIS showing strong spatial agreement between maps of AVIRIS EWT and MODIS indexes, and good statistical agreement for the range of habitats at the site. Temporal patterns of these four indexes in all vegetation communities except creosote bush and agriculture showed distinct seasonal patterns that responded to the timing and amount of precipitation. Moreover, these time series captured different ecological responses among the different vegetation communities. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Cheng, Yen-Ben; Ustin, Susan L.; Riano, David] Univ Calif Davis, CSTARS, Dept Land Air & Water Resources, Davis, CA 95616 USA.
[Riano, David] Univ Alcala de Henares, Dept Geog, E-28801 Madrid, Spain.
[Vanderbilt, Vem C.] NASA, Ames Res Ctr, Moffett Field, CA USA.
RP Cheng, YB (reprint author), Univ Calif Davis, CSTARS, 1 Shields Ave, Davis, CA 95616 USA.
EM ybcheng@cstars.ucdavis.edu
RI Cheng, Yen-Ben/G-1311-2012; Riano, David/C-9663-2013
OI Riano, David/0000-0002-0198-1424
NR 54
TC 49
Z9 54
U1 3
U2 22
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 2008
VL 112
IS 2
BP 363
EP 374
DI 10.1016/j.rse.2007.01.023
PG 12
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 261GW
UT WOS:000253068100007
ER
PT J
AU Thoma, DP
Moran, MS
Bryant, R
Rahman, MM
Collins, CDH
Keefer, TO
Noriega, R
Osman, I
Skrivin, SM
Tischler, MA
Bosch, DD
Starks, PJ
Peters-Lidard, CD
AF Thoma, D. P.
Moran, M. S.
Bryant, R.
Rahman, M. M.
Collins, C. D. Holifield
Keefer, T. O.
Noriega, R.
Osman, I.
Skrivin, S. M.
Tischler, M. A.
Bosch, D. D.
Starks, P. J.
Peters-Lidard, C. D.
TI Appropriate scale of soil moisture retrieval from high resolution radar
imagery for bare and minimally vegetated soils
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE radar; soil moisture; scale
ID SAR DATA; SURFACE; BACKSCATTERING; NOISE; MODEL
AB This research investigates the appropriate scale for watershed averaged and site specific soil moisture retrieval from high resolution radar imagery. The first approach involved filtering backscatter for input to a retrieval model that was compared against field measures of soil moisture. The second approach involved spatially averaging raw and filtered imagery in an image-based statistical technique to determine the best scale for site-specific soil moisture retrieval. Field soil moisture was measured at 1225 m(2) sites in three watersheds commensurate with 7 m resolution Radarsat image acquisition. Analysis of speckle reducing block median filters indicated that 5 x 5 filter level was the optimum for watershed averaged estimates of soil moisture. However, median filtering alone did not provide acceptable accuracy for soil moisture retrieval on a site-specific basis. Therefore, spatial averaging of unfiltered and median filtered power values was used to generate backscatter estimates with known confidence for soil moisture retrieval. This combined approach of filtering and averaging was demonstrated at watersheds located in Arizona (AZ), Oklahoma (OK) and Georgia (GA). The optimum ground resolution for AZ, OK and GA study areas was 162 m, 310 m, and 1131 m respectively obtained with unfiltered imagery. This statistical approach does not rely on ground verification of soil moisture for validation and only requires a satellite image and average roughness parameters of the site. When applied at other locations, the resulting optimum ground resolution will depend on the spatial distribution of land surface features that affect radar backscatter. This work offers insight into the accuracy of soil moisture retrieval, and an operational approach to determine the optimal spatial resolution for the required application accuracy. Published by Elsevier Inc.
C1 [Thoma, D. P.; Moran, M. S.; Bryant, R.; Collins, C. D. Holifield; Keefer, T. O.; Skrivin, S. M.] USDA ARS, SW Watershed Res Ctr, Tucson, AZ 85719 USA.
[Rahman, M. M.] Saskatchewan Environm Planning & Risk Analysis Di, Regina, SK, Canada.
[Osman, I.] Univ Arizona, Tucson, AZ 85721 USA.
[Tischler, M. A.] USA, Corps Eng Topog Engn Ctr, Alexandria, VA USA.
[Bosch, D. D.] USDA ARS, SE Watershed Res Ctr, Tifton, GA 31793 USA.
[Starks, P. J.] USDA ARS, Nat Resources Res Unit, El Reno, OK USA.
[Peters-Lidard, C. D.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch Code 6143, Greenbelt, MD USA.
RP Thoma, DP (reprint author), USDA ARS, SW Watershed Res Ctr, Tucson, AZ 85719 USA.
EM dave_thoma@nps.gov
RI Peters-Lidard, Christa/E-1429-2012
OI Peters-Lidard, Christa/0000-0003-1255-2876
NR 29
TC 29
Z9 30
U1 2
U2 11
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 2008
VL 112
IS 2
BP 403
EP 414
DI 10.1016/j.rse.2007.06.021
PG 12
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 261GW
UT WOS:000253068100010
ER
PT J
AU Schroeder, W
Csiszar, I
Morisette, J
AF Schroeder, Wilfrid
Csiszar, Ivan
Morisette, Jeffrey
TI Quantifying the impact of cloud obscuration on remote sensing of active
fires in the Brazilian Amazon
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE vegetation fires; clouds; geostationary satelite; Brazilian amazon
ID BOREAL FOREST REGION; SOUTH-AMERICA; DETECTION ALGORITHMS; RAINFALL
ESTIMATION; TROPICAL FORESTS; VEGETATION FIRE; TRMM VIRS; SCAR-B;
BIOMASS; EMISSIONS
AB Vegetation fires remain as one of the most important processes governing land use and land cover change in tropical areas. The large area extent of fire prone areas associated with human activities makes satellite remote sensing of active fires a valuable tool to help monitor biomass burning in those regions. However, identification of active fire fronts under optically thick clouds is not possible through passive remote sensing, often resulting in omission errors. Previous analyses of fire activity either ignored the cloud obscuration problem or applied corrections based on the assumption that fire occurrence is not impacted by the presence of clouds. In this study we addressed the cloud obscuration problem in the Brazilian Amazon region using a pixel based probabilistic approach, using information on previous fire occurrence, precipitation and land use. We implemented the methodology using data from the geostationary GOES imager, covering the entire diurnal cycle of fire activity and cloud occurrence. Our assessment of the method indicated that the cloud adjustment reproduced the number of potential fires missed within 1.5% and 5% of the true fire counts on annual and monthly bases respectively. Spatially explicit comparison with high resolution burn scar maps in Acre state showed a reduction of omission error (from 58.3% to 43.7%) and only slight increase of commission error (from 6.4% to 8.8%) compared to uncorrected fire counts. A basin-wide analysis of corrected GOES fire counts during 2005 showed a mean cloud adjustment factor of approximately 11%, ranging from negligible adjustment in the central and western part of the Brazilian Amazon to as high as 50% in parts of Roraima, Para and Mato Grosso. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Schroeder, Wilfrid; Csiszar, Ivan] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Morisette, Jeffrey] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Schroeder, W (reprint author), Univ Maryland, Dept Geog, 2181 LeFrak Hall, College Pk, MD 20742 USA.
EM schroeder@hermes.geog.umd.edu
RI Csiszar, Ivan/D-2396-2010; Schroeder, Wilfrid/F-6738-2010
NR 52
TC 29
Z9 29
U1 3
U2 17
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 2008
VL 112
IS 2
BP 456
EP 470
DI 10.1016/j.rse.2007.05.004
PG 15
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 261GW
UT WOS:000253068100014
ER
PT J
AU Tarnavsky, E
Garrigues, S
Brown, ME
AF Tarnavsky, Elena
Garrigues, Sebastien
Brown, Molly E.
TI Multiscale geostatistical analysis of AVHRR, SPOT-VGT, and MODIS global
NDVI products
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE AVHRR; SPOT-VGT; MODIS; Landsat; NDVI; geostatistics; variograms;
variogram modeling; spatial variability; variogram sill; length scale;
EOS sites; global vegetation monitoring; multisensor; multiscale
ID VEGETATION INDEXES; DIGITAL IMAGES; BIOPHYSICAL VARIABLES;
AUTO-CORRELATION; VALIDATION; SURFACE; MODELS; REGULARIZATION;
REFLECTANCE; VARIOGRAMS
AB Global NDVI data are routinely derived from the AVHRR, SPOT-VGT, and MODIS/Terra earth observation records for a range of applications from terrestrial vegetation monitoring to climate change modeling. This has led to a substantial interest in the harmonization of multisensor records. Most evaluations of the internal consistency and continuity of global multisensor NDVI products have focused on time-series harmonization in the spectral domain, often neglecting the spatial domain. We fill this void by applying variogram modeling (a) to evaluate the differences in spatial variability between 8-km AVHRR, 1-km SPOT-VGT, and 1-km, 500-m, and 250-m MODIS NDVI products over eight EOS (Earth Observing System) validation sites, and (b) to characterize the decay of spatial variability as a function of pixel size (i.e. data regularization) for spatially aggregated Landsat ETM+ NDVI products and a real multisensor dataset. First, we demonstrate that the conjunctive analysis of two variogram properties - the sill and the mean length scale metric - provides a robust assessment of the differences in spatial variability between multiscale NDVI products that are due to spatial (nominal pixel size, point spread function, and view angle) and non-spatial (sensor calibration, cloud clearing, atmospheric corrections, and length of multi-day compositing period) factors. Next, we show that as the nominal pixel size increases, the decay of spatial information content follows a logarithmic relationship with stronger fit value for the spatially aggregated NDVI products (R-2 = 0.9321) than for the native resolution AVHRR, SPOT-VGT, and MODIS NDVI products (R-2 = 0.5064). This relationship serves as a reference for evaluation of the differences in spatial variability and length scales in multiscale datasets at native or aggregated spatial resolutions. The outcomes of this study suggest that multisensor NDVI records cannot be integrated into a long-term data record without proper consideration of all factors affecting their spatial consistency. Hence, we propose an approach for selecting the spatial resolution, at which differences in spatial variability between NDVI products from multiple sensors are minimized. This approach provides practical guidance for the harmonization of long-term multisensor datasets. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Tarnavsky, Elena] Kings Coll London, Dept Geog, London, England.
[Garrigues, Sebastien] Univ Maryland, NASA, Goddard Space Flight Ctr, College Pk, MD 20742 USA.
[Brown, Molly E.] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Washington, DC USA.
RP Tarnavsky, E (reprint author), Kings Coll London, Dept Geog, London, England.
EM elena.tarnavsky@kcl.ac.uk
RI Brown, Molly/E-2724-2010; Brown, Molly/M-5146-2013;
OI Brown, Molly/0000-0001-7384-3314; Brown, Molly/0000-0001-7384-3314;
Tarnavsky, Elena/0000-0003-3403-0411
NR 57
TC 84
Z9 93
U1 5
U2 49
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 2008
VL 112
IS 2
BP 535
EP 549
DI 10.1016/j.rse.2007.05.008
PG 15
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 261GW
UT WOS:000253068100020
ER
PT J
AU Garrigues, S
Allard, D
Baret, F
AF Garrigues, S.
Allard, D.
Baret, F.
TI Modeling temporal changes in surface spatial heterogeneity over an
agricultural site
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE spatial heterogeneity; spatio-temporal variogram model; NDVI; phenology;
agricultural site; crop seasonal trajectory; spatial structure;
landscape; high spatial resolution imagery; moderate spatial resolution
imagery; non-linear estimation process; scaling bias
ID REMOTE-SENSING ALGORITHMS; SATELLITE MEASUREMENTS; SOIL-MOISTURE; SCALE;
DISAGGREGATION
AB High temporal frequency remote sensing observations are required to monitor vegetation functioning. These observations are currently provided by moderate resolution sensor (with pixel size ranging from 250 m to 10 km). However, the intra-pixel spatial heterogeneity which may be important at moderate resolution, induces a scaling bias on non-linear estimation processes of land surface variable. A possible strategy to correct this scaling bias consists in using variogram model of high spatial resolution data (e.g. SPOT/HRV 20 m) as a proxy for the spatial heterogeneity within moderate resolution pixel. However, ways have to be found to get prior knowledge of this intra-pixel spatial heterogeneity metric without systematic concurrent high spatial resolution images. This paper aims at proposing a spatio-temporal model of the variogram of high spatial resolution data, which enables us to retrieve the spatial heterogeneity within moderate spatial resolution pixel using a temporal sampling of few high spatial resolution scenes. It capitalizes on variogram modeling of a time series of high spatial resolution NDVI images to quantify and model the temporal changes in landscape spatial heterogeneity over a particular crop site (Fundulea, Romania). We first demonstrate that important temporal variations in surface spatial heterogeneity observed over an agricultural site mainly result from the shift in seasonal trajectories between crop classes (here winter versus summer crops). The mean length scale as measured by the variogram integral range is mainly influenced by the gathering of fields with similar NDVI values. The scene overall spatial variability and the spatial heterogeneity within moderate resolution pixels, as quantified by the variogram. sill and the dispersion variance, respectively, increase with the difference in NDVI between winter and summer crops. The influence of surface spatial heterogeneity on the description of land surface processes is thus critical when the phenological variability between crop classes is maximum, suggesting that the number of high spatial resolution scenes should increase at these periods of the seasonal cycle. Then, based on these observations, we build a model describing the temporal course of surface spatial heterogeneity, i.e. the temporal trajectory of the variogram of high spatial resolution NDVI image, as a function of crop seasonality. Once calibrated from a temporal sampling of few high spatial resolution scenes, this model proves to be powerful to predict the variogram at a date at which the high spatial resolution scene is not available and thus to retrieve the spatial heterogeneity within moderate resolution pixels through the seasonal cycle within a mean relative uncertainty of 20%. (C) 2007 Elsevier Inc. All rights reserved.
C1 [Garrigues, S.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Allard, D.] INRA, Biostatist & Processus Spatiaux, Avignon, France.
[Baret, F.] INRA, UMR1114, Avignon, France.
RP Garrigues, S (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 614 4, Greenbelt, MD 20771 USA.
EM Sebastien.garrigues@gsfc.nasa.gov
RI Baret, Fred/C-4135-2011
OI Baret, Fred/0000-0002-7655-8997
NR 30
TC 11
Z9 14
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
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD FEB 15
PY 2008
VL 112
IS 2
BP 588
EP 602
DI 10.1016/j.rse.2007.05.014
PG 15
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 261GW
UT WOS:000253068100024
ER
PT J
AU Dong, XQ
Minnis, P
Xi, B
Sun-, S
Chen, Y
AF Dong, Xiquan
Minnis, Patrick
Xi, Baike
Sun-Mack, Sunny
Chen, Yan
TI Comparison of CERES-MODIS stratus cloud properties with ground-based
measurements at the DOE ARM southern great plains site
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ENERGY SYSTEM CERES; RADIATIVE PROPERTIES; INFRARED RADIANCES;
SOLAR-RADIATION; SATELLITE; SURFACE; CLIMATE; RADAR; FIRE;
PARAMETERIZATIONS
AB Overcast stratus cloud properties derived for the Clouds and the Earth's Radiant Energy System (CERES) project using Terra and Aqua Moderate Resolution Imaging Spectroradiometer (MODIS) data are compared with observations taken at the Department of Energy (DOE) Atmospheric Radiation Measurement (ARM) Southern Great Plains site from March 2000 through December 2004. Retrievals from ARM surface-based data were averaged over a 1-h interval centered at the time of each satellite overpass, and the CERES-MODIS cloud properties were averaged within a 30 km x 30 km box centered on the ARM SGP site. Two data sets were analyzed: all of the data (ALL), which include multilayered, single-layered, and slightly broken stratus decks and a subset, single-layered unbroken decks (SL). The CERES-MODIS effective cloud heights were determined from effective cloud temperature using a lapse rate method with the surface temperature specified as the 24-h mean surface air temperature. For SL stratus, they are, on average, within the ARM radar-lidar estimated cloud boundaries and are 0.534 +/- 0.542 km and 0.108 +/- 0.480 km lower than the cloud physical tops and centers, respectively, and are comparable for day and night observations. The mean differences and standard deviations are slightly larger for ALL data, but not statistically different to those of SL data. The MODIS-derived effective cloud temperatures are 2.7 +/- 2.4 K less than the surface-observed SL cloud center temperatures with very high correlations (0.86-0.97). Variations in the height differences are mainly caused by uncertainties in the surface air temperatures, lapse rates, and cloud top height variability. The biases are mainly the result of the differences between effective and physical cloud top, which are governed by cloud liquid water content and viewing zenith angle, and the selected lapse rate, -7.1 K km(-1). On the basis of a total of 43 samples, the means and standard deviations of the differences between the daytime Terra and surface retrievals of effective radius re, optical depth, and liquid water path for SL stratus are 0.1 +/- 1.9 mu m (1.2 +/- 23.5%), -1.3 +/- 9.5 (-3.6 +/- 26.2%), and 0.6 +/- 49.9 gm(-2) (0.3 +/- 27%), respectively, while the corresponding correlation coefficients are 0.44, 0.87, and 0.89. For Aqua, they are 0.2 +/- 1.9 mm (2.5 +/- 23.4%), 2.5 +/- 7.8 (7.8 +/- 24.3%), and 28.1 +/- 52.7 gm(-2) (17.2 +/- 32.2%), as well as 0.35, 0.96, and 0.93 from a total of 21 cases. The results for ALL cases are comparable. Although a bias in r(e) was expected because the satellite retrieval of effective radius only represents the top of the cloud, the surface-based radar retrievals revealed that the vertical profile of r(e) is highly variable with smaller droplets occurring at cloud top in some cases. The larger bias in optical depth and liquid water path for Aqua is due, at least partially, to differences in the Terra and Aqua MODIS visible channel calibrations. Methods for improving the cloud top height and microphysical property retrievals are suggested.
C1 [Dong, Xiquan; Xi, Baike] Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA.
[Sun-Mack, Sunny; Chen, Yan] Sci Applicat Int Corp Inc, Hampton, VA 23666 USA.
[Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Dong, XQ (reprint author), Univ N Dakota, Dept Atmospher Sci, 4149 Univ Dr,Stop 9006, Grand Forks, ND 58202 USA.
EM dong@aero.und.edu
RI Minnis, Patrick/G-1902-2010;
OI Minnis, Patrick/0000-0002-4733-6148; Dong, Xiquan/0000-0002-3359-6117
NR 48
TC 46
Z9 49
U1 1
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD FEB 14
PY 2008
VL 113
IS D3
AR D03204
DI 10.1029/2007JD008438
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 263RH
UT WOS:000253233700001
ER
PT J
AU Schwarz, JP
Spackman, JR
Fahey, DW
Gao, RS
Lohmann, U
Stier, P
Watts, LA
Thomson, DS
Lack, DA
Pfister, L
Mahoney, MJ
Baumgardner, D
Wilson, JC
Reeves, JM
AF Schwarz, J. P.
Spackman, J. R.
Fahey, D. W.
Gao, R. S.
Lohmann, U.
Stier, P.
Watts, L. A.
Thomson, D. S.
Lack, D. A.
Pfister, L.
Mahoney, M. J.
Baumgardner, D.
Wilson, J. C.
Reeves, J. M.
TI Coatings and their enhancement of black carbon light absorption in the
tropical atmosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID OPTICAL-PROPERTIES; CLIMATE RESPONSE; SOOT PARTICLES; AEROSOL; CLOUDS;
SCATTERING; TEMPERATURE; ALBEDO
AB Black carbon ( BC) is the dominant aerosol absorber of solar radiation in the atmosphere and is an important component of anthropogenic climate forcing. BC's role is strongly dependent on its physical state, which can influence the way that BC particles may act as ice and cloud nuclei, as well as the way they interact with solar radiation. In situ measurements made with a single-particle soot photometer flown on a NASA high-altitude research aircraft show the mass and size of individual BC particles in the tropics, as well as their propensity to be found mixed with additional materials. Mie theory was used to connect observed light scattering off BC particles to the optical effects of coatings on the particles. The observations indicate that as BC from ground-based emission sources rises in altitude to the lower stratosphere, coatings on BC particles become both thicker and more prevalent, while BC mass mixing ratios decrease dramatically from their values near the ground. Coatings enhance light absorption by the ambient BC column by at least 30%. These results reveal the microphysical state of BC in the atmosphere while providing important constraints for models evaluating BC's role in climate change.
C1 [Schwarz, J. P.; Spackman, J. R.; Fahey, D. W.; Gao, R. S.; Watts, L. A.; Thomson, D. S.; Lack, D. A.] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Baumgardner, D.] Univ Nacl Autonoma Mexico, Ctr Ciencias Atmosfera, Mexico City 04510, DF, Mexico.
[Lohmann, U.] ETH, Inst Atmosphar & Klima, CH-8092 Zurich, Switzerland.
[Mahoney, M. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Pfister, L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Wilson, J. C.; Reeves, J. M.] Univ Denver, Dept Engn, Denver, CO 80208 USA.
[Stier, P.] CALTECH, Dept Environm Sci & Engn, Pasadena, CA 91125 USA.
RP Schwarz, JP (reprint author), NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA.
EM joshua.p.schwarz@noaa.gov
RI Gao, Ru-Shan/H-7455-2013; Watts, Laurel/G-4532-2013; Fahey,
David/G-4499-2013; Lohmann, Ulrike/B-6153-2009; Manager, CSD
Publications/B-2789-2015; Stier, Philip/B-2258-2008; Lack,
Daniel/I-9053-2012; schwarz, joshua/G-4556-2013
OI Watts, Laurel/0000-0002-0834-3329; Fahey, David/0000-0003-1720-0634;
Lohmann, Ulrike/0000-0001-8885-3785; Stier, Philip/0000-0002-1191-0128;
schwarz, joshua/0000-0002-9123-2223
NR 40
TC 123
Z9 126
U1 16
U2 69
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 14
PY 2008
VL 113
IS D3
AR D03203
DI 10.1029/2007JD009042
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 263RH
UT WOS:000253233700002
ER
PT J
AU Liu, X
Shemansky, DE
Malone, CP
Johnson, PV
Ajello, JM
Kanik, I
Heays, AN
Lewis, BR
Gibson, ST
Stark, G
AF Liu, Xianming
Shemansky, Donald E.
Malone, Charles P.
Johnson, Paul V.
Ajello, Joseph M.
Kanik, Isik
Heays, Alan N.
Lewis, Brenton R.
Gibson, Stephen T.
Stark, Glenn
TI Experimental and coupled-channels investigation of the radiative
properties of the N(2)c(4)'(1)Sigma(+)(u)-X-1 Sigma(+)(g) band system
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID ELECTRON-IMPACT EXCITATION; HIGH-RESOLUTION ABSORPTION; ULTRAVIOLET
EMISSION-SPECTRUM; SINGLET UNGERADE STATES; MOLECULAR NITROGEN;
OSCILLATOR-STRENGTHS; RYDBERG STATES; CROSS-SECTION; LIFETIME
MEASUREMENTS; LASER SPECTROSCOPY
AB The emission properties of the N-2 c(4)' (1)Sigma(+)(u) - X (1)Sigma(+)(g) band system have been investigated in a joint experimental and coupled-channels theoretical study. Relative intensities of the c(4)' (1)Sigma(+)(u)(0) - X (1)Sigma(+()(g)v(i)) transitions, measured via electron-impact-induced emission spectroscopy, are combined with a coupled-channel Schrodinger equation (CSE) model of the N-2 molecule, enabling determination of the diabatic electronic transition moment for the c(4)' (1)Sigma(+)(u) - X (1)Sigma(+)(g) system as a function of internuclear distance. The CSE rotational transition probabilities are further verified by comparison with a high-resolution experimental spectrum. Spontaneous transition probabilities of the c(4)' (1)Sigma(+)(u) - X (1)Sigma(+)(g) band system, required for modeling atmospheric emission, can now be calculated reliably.
C1 [Liu, Xianming; Shemansky, Donald E.] Space Environm Technol, Planetary & Space Sci Div, Pasadena, CA 91107 USA.
[Malone, Charles P.; Johnson, Paul V.; Ajello, Joseph M.; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Heays, Alan N.; Lewis, Brenton R.; Gibson, Stephen T.] Australian Natl Univ, Res Sch Phys Sci & Engn, Canberra, ACT 0200, Australia.
[Stark, Glenn] Wellesley Coll, Dept Phys, Wellesley, MA 02181 USA.
RP Liu, X (reprint author), Space Environm Technol, Planetary & Space Sci Div, 320 N Halstead, Pasadena, CA 91107 USA.
EM xliu@spacenvironment.net; dshemansky@spacenvironment.net;
charles.malone@jpl.nasa.gov; paul.v.johnson@jpl.nasa.gov;
alan.heays@anu.edu.au; brenton.lewis@anu.edu.au; gstark@wellesley.edu
RI Malone, Charles/A-6294-2010; Johnson, Paul/D-4001-2009
OI Malone, Charles/0000-0001-8418-1539; Johnson, Paul/0000-0002-0186-8456
NR 84
TC 18
Z9 18
U1 0
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD FEB 14
PY 2008
VL 113
IS A2
AR A02304
DI 10.1029/2007JA012787
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 263SM
UT WOS:000253236800001
ER
PT J
AU Lyatsky, W
Khazanov, GV
AF Lyatsky, Wladislaw
Khazanov, George V.
TI Effect of solar wind density on relativistic electrons at geosynchronous
orbit
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID RADIATION BELT; GEOMAGNETIC STORMS; ACCELERATION; MAGNETOSPHERE;
TIMESCALE
AB We examined the relationship between relativistic (> 2 MeV) electron fluxes at geostationary orbit and two solar wind parameters, the speed and density. For the analysis, we used data of relativistic electron fluxes measured with GOES-8 spacecraft for 1997 - 2002 and GOES-10 spacecraft for 2003 - 2006, and solar wind data, provided by Goddard Space Flight Center. Using the correlation analysis, we found that not only solar wind speed but also solar wind density provides a strong effect on relativistic electrons: the relativistic electron fluxes increase with increasing solar wind speed and decrease with increasing solar wind density. In contrast to solar wind speed that shows the best correlation with electron fluxes after about two days only, the solar wind density shows the best correlation with the electron fluxes after about 15 hours. To separate the effects of solar wind speed and density, we examined events when solar wind speed varied insignificantly; in these events, the effect of solar wind density on the relativistic electrons remained strong. We found that the solar wind density, which may affect the loss of relativistic electrons, effectively controls the magnitude of relativistic electron fluxes at geostationary orbit, so that the strongest fluxes occurred almost exclusively during low-density solar wind conditions. Thus, our study showed that solar wind density is an important parameter that may significantly affect the loss of relativistic electrons and, as a result, the resulting magnitude of the electron fluxes at geostationary orbit. Citation: Lyatsky, W., and G. V. Khazanov ( 2008), Effect of solar wind density on relativistic electrons at geosynchronous orbit.
C1 [Lyatsky, Wladislaw; Khazanov, George V.] NASA Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
RP Lyatsky, W (reprint author), NASA Marshall Space Flight Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM lyatsky@cspar.uah.edu
NR 21
TC 26
Z9 26
U1 0
U2 1
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 13
PY 2008
VL 35
IS 3
AR L03109
DI 10.1029/2007GL032524
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 263QM
UT WOS:000253231600005
ER
PT J
AU Maksym, T
Markus, T
AF Maksym, Ted
Markus, Thorsten
TI Antarctic sea ice thickness and snow-to-ice conversion from atmospheric
reanalysis and passive microwave snow depth
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID OPERATIONAL NUMERICAL-ANALYSES; SURFACE MASS-BALANCE; WESTERN
WEDDELL-SEA; SOUTHERN-OCEAN; TEMPORAL VARIABILITY; PACK ICE;
BELLINGSHAUSEN SEAS; AMUNDSEN SEAS; LATE WINTER; ROSS SEA
AB Passive microwave snow depth, ice concentration, and ice motion estimates are combined with snowfall from the European Centre for Medium-Range Weather Forecasting (ECMWF) reanalysis (ERA-40) from 1979-2001 to estimate the prevalence of snow-to-ice conversion (snow-ice formation) on level sea ice in the Antarctic for April-October. Snow ice is ubiquitous in all regions throughout the growth season. Calculated snow-ice thicknesses fall within the range of estimates from ice core analysis for most regions. However, uncertainties in both this analysis and in situ data limit the usefulness of snow depth and snow-ice production to evaluate the accuracy of ERA-40 snowfall. The East Antarctic is an exception, where calculated snow-ice production exceeds observed ice thickness over wide areas, suggesting that ERA-40 precipitation is too high there. Snow-ice thickness variability is strongly controlled not just by snow accumulation rates, but also by ice divergence. Surprisingly, snow-ice production is largely independent of snow depth, indicating that the latter may be a poor indicator of total snow accumulation. Using the presence of snow-ice formation as a proxy indicator for near-zero freeboard, we examine the possibility of estimating level ice thickness from satellite snow depths. A best estimate for the mean level ice thickness in September is 53 cm, comparing well with 51 cm from ship-based observations. The error is estimated to be 10-20 cm, which is similar to the observed interannual and regional variability. Nevertheless, this is comparable to expected errors for ice thickness determined by satellite altimeters. Improvement in satellite snow depth retrievals would benefit both of these methods.
C1 [Maksym, Ted] British Antarctic Survey, Cambridge CB3 0ET, England.
[Markus, Thorsten] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Maksym, T (reprint author), British Antarctic Survey, Cambridge CB3 0ET, England.
RI Markus, Thorsten/D-5365-2012
NR 85
TC 30
Z9 31
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-OCEANS
JI J. Geophys. Res.-Oceans
PD FEB 13
PY 2008
VL 113
IS C2
AR C02S12
DI 10.1029/2006JC004085
PG 18
WC Oceanography
SC Oceanography
GA 263RZ
UT WOS:000253235500003
ER
PT J
AU Dlugach, JM
Mishchenko, MI
AF Dlugach, Janna M.
Mishchenko, Michael I.
TI Photopolarimetry of planetary atmospheres: what observational data are
essential for a unique retrieval of aerosol microphysics?
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE polarization; scattering; techniques : photometric; techniques :
polarimetric; planets and satellites : individual : Jupiter
ID ELECTROMAGNETIC SCATTERING; LIGHT-SCATTERING; RADIATIVE PROPERTIES;
OPTICAL-PROPERTIES; JOVIAN ATMOSPHERE; POLARIZED-LIGHT; JUPITER;
PARTICLES; CLOUDS; VENUS
AB We analyse the results of computations of the intensity and degree of linear polarization of diffusely reflected sunlight for the centre of a planetary disc in the phase-angle range 0 degrees = 12 degrees. Thus, using Jupiter as a 'proving ground', we conclude that only polatimetric data obtained over a wide range of phase angles (i.e. from spacecraft) may provide definitive constraints on aerosol shape and, as a consequence, ameliorate the ill-posed nature of the inverse remote-sensing problem.
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 Broadwy, New York, NY 10025 USA.
EM mmishchenko@giss.nasa.gov
RI Mishchenko, Michael/D-4426-2012
NR 37
TC 6
Z9 6
U1 0
U2 6
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 11
PY 2008
VL 384
IS 1
BP 64
EP 70
DI 10.1111/j.1365-2966.2007.12679.x
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 264TC
UT WOS:000253312300004
ER
PT J
AU Ade, P
Bock, J
Bowden, M
Brown, ML
Cahill, G
Carlstrom, JE
Castro, PG
Church, S
Culverhouse, T
Friedman, R
Ganga, K
Gear, WK
Hinderks, J
Kovac, J
Lange, AE
Leitch, E
Melhuish, SJ
Murphy, JA
Orlando, A
Schwarz, R
O'Sullivan, C
Piccirillo, L
Pryke, C
Rajguru, N
Rusholme, B
Taylor, AN
Thompson, KL
Wu, EYS
Zemcov, M
AF Ade, P.
Bock, J.
Bowden, M.
Brown, M. L.
Cahill, G.
Carlstrom, J. E.
Castro, P. G.
Church, S.
Culverhouse, T.
Friedman, R.
Ganga, K.
Gear, W. K.
Hinderks, J.
Kovac, J.
Lange, A. E.
Leitch, E.
Melhuish, S. J.
Murphy, J. A.
Orlando, A.
Schwarz, R.
O'Sullivan, C.
Piccirillo, L.
Pryke, C.
Rajguru, N.
Rusholme, B.
Taylor, A. N.
Thompson, K. L.
Wu, E. Y. S.
Zemcov, M.
TI First season QUaD CMB temperature and polarization power spectra
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE polarization
ID PROBE WMAP OBSERVATIONS; COSMIC BACKGROUND IMAGER; 2003 FLIGHT;
MICROWAVE; ANISOTROPY; BOOMERANG
AB QUaD is a bolometric CMB polarimeter sited at the South Pole, operating at frequencies of 100 and 150 GHz. In this paper we report preliminary results from the first season of operation ( austral winter 2005). All six CMB power spectra are presented derived as cross spectra between the 100 and 150 GHz maps using 67 days of observation in a low foreground region of approximately 60 deg(2). These data are a small fraction of the data acquired to date. The measured spectra are consistent with the Lambda CDM cosmological model. We perform jackknife tests that indicate that the observed signal has negligible contamination from instrumental systematics. In addition, by using a frequency jackknife we find no evidence for foreground contamination.
C1 [Ade, P.; Bowden, M.; Gear, W. K.; Melhuish, S. J.; Orlando, A.; Piccirillo, L.; Rajguru, N.; Zemcov, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Bock, J.; Leitch, E.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bock, J.; Kovac, J.; Lange, A. E.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA.
[Bowden, M.; Hinderks, J.; Rusholme, B.; Thompson, K. L.; Wu, E. Y. S.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Brown, M. L.; Castro, P. G.; Taylor, A. N.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Cahill, G.; Murphy, J. A.; O'Sullivan, C.] Natl Univ Ireland Maynooth, Dept Expt Phys, Maynooth, Kildare, Ireland.
[Carlstrom, J. E.; Culverhouse, T.; Friedman, R.; Schwarz, R.; Pryke, C.] Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Ganga, K.] CNRS, Lab APC, F-75205 Paris 13, France.
[Rajguru, N.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
RP Ade, P (reprint author), Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales.
RI Melhuish, Simon/B-1299-2016;
OI Melhuish, Simon/0000-0001-8725-4991; Orlando,
Angiola/0000-0001-8004-5054
NR 24
TC 57
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 FEB 10
PY 2008
VL 674
IS 1
BP 22
EP 28
DI 10.1086/524922
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 266RJ
UT WOS:000253454400003
ER
PT J
AU Kuntz, KD
Snowden, SL
AF Kuntz, K. D.
Snowden, S. L.
TI The X-ray-emitting components toward l=111 degrees: The local hot bubble
and beyond
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE X-rays : diffuse background
ID XMM-NEWTON OBSERVATION; INTERSTELLAR-MEDIUM; MOLECULAR CLOUDS; CHANDRA
OBSERVATIONS; CO SURVEY; EMISSION; SOLAR; GAS; ABSORPTION; GALAXIES
AB We have obtained an XMM-Newton spectrum of the diffuse X-ray emission toward (l, b) (111.14 degrees, 1.11 degrees), a line of sight with a relatively simple distribution of absorbing clouds: > 9 x 10(19) cm(-2) at R > 170 pc, a 6 x 10(21) cm(-2) molecular cloud at 2.5-3.3 kpc, and a total column of 1.2 x 10(22) cm(-2). We find that the analysis of the XMM-Newton spectrum in conjunction with the ROSAT All-Sky Survey (RASS) spectral energy distribution for the same direction requires three thermal components to be well fit: a "standard'' Local Hot Bubble component with kT = 0.095, a component beyond the molecular cloud with kT = 0.57, and a component before the molecular cloud with kT = 0.24. The strength of the O VII 0.56 keV line from the Local Hot Bubble, 1.75 +/- 0.7 photons cm(-2) s(-1) sr(-1), is consistent with other recent measures. The 0.24 keV component has an emission measure of 0.0021 +/- 0.0006 cm(-6) pc and is not localized save as diffuse emission within the Galactic plane. Rough calculations show that only about a quarter of this component is due to unresolved stellar emission; it is the best candidate for a pervasive hot medium. The spatial separation of the similar to 0.2 keV component from the similar to 0.6 keV component suggests that the spectral decompositions of the emission from late-type spiral disks found in the literature do represent real temperature components rather than reflecting more complex temperature distributions.
C1 [Kuntz, K. D.; Snowden, S. L.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Kuntz, K. D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Kuntz, KD (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 662, Greenbelt, MD 20771 USA.
RI Snowden, Steven/D-5292-2012
NR 52
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
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2008
VL 674
IS 1
BP 209
EP 219
DI 10.1086/524719
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 266RJ
UT WOS:000253454400018
ER
PT J
AU Achterberg, A
Ackermann, M
Adams, J
Ahrens, J
Andeen, K
Auffenberg, J
Bahcall, JN
Bai, X
Baret, B
Barwick, SW
Bay, R
Beattie, K
Becka, T
Becker, JK
Becker, KH
Berghaus, P
Berley, D
Bernardini, E
Bertrand, D
Besson, DZ
Blaufuss, E
Boersma, DJ
Bohm, C
Bolmont, J
Boser, S
Botner, O
Bouchta, A
Braun, J
Burgess, C
Burgess, T
Castermans, T
Chirkin, D
Christy, B
Clem, J
Cowen, DF
D'Agostino, MV
Davour, A
Day, CT
De Clercq, C
Demirores, L
Descamps, F
Desiati, P
DeYoung, T
Diaz-Velez, JC
Dreyer, J
Dumm, JP
Duvoort, MR
Edwards, WR
Ehrlich, R
Eisch, J
Ellsworth, RW
Evenson, PA
Fadiran, O
Fazely, AR
Filimonov, K
Foerster, MM
Fox, BD
Franckowiak, A
Gaisser, TK
Gallagher, J
Ganugapati, R
Geenen, H
Gerhardt, L
Goldschmidt, A
Goodman, JA
Gozzini, R
Griesel, T
Gross, A
Grullon, S
Gunasingha, RM
Gurtner, M
Hallgren, A
Halzen, F
Han, K
Hanson, K
Hardtke, D
Hardtke, R
Hart, JE
Hasegawa, Y
Hauschildt, T
Hays, D
Heise, J
Helbing, K
Hellwig, M
Herquet, P
Hill, GC
Hodges, J
Hoffman, KD
Hommez, B
Hoshina, K
Hubert, D
Hughey, B
Hulth, PO
Huss, JP
Hultqvist, K
Hundertmark, S
Inaba, M
Ishihara, A
Jacobsen, J
Japaridze, GS
Johansson, H
Jones, A
Joseph, JM
Kampert, KH
Kappes, A
Karg, T
Karle, A
Kawai, H
Kelley, JL
Kitamura, N
Klein, SR
Klepser, S
Kohnen, G
Kolanoski, H
Pke, LK
Kowalski, M
Kowarik, T
Krasberg, M
Kuehn, K
Labare, M
Landsman, H
Leich, H
Leier, D
Liubarsky, I
Lundberg, J
Lunemann, J
Madsen, J
Mase, K
Matis, HS
McCauley, T
McParland, CP
Meli, A
Messarius, T
Meszaros, P
Miyamoto, H
Mokhtarani, A
Montaruli, T
Morey, A
Morse, R
Movit, SM
Munich, K
Nahnhauer, R
Nam, JW
Niessen, P
Nygren, DR
Ogelman, H
Olivas, A
Patton, S
Pena-Garay, C
Heros, CPL
Piegsa, A
Pieloth, D
Pohl, AC
Porrata, R
Pretz, J
Price, PB
Przybylski, GT
Rawlins, K
Razzaque, S
Resconi, E
Rhode, W
Ribordy, M
Rizzo, A
Robbins, S
Roth, P
Rott, C
Rutledge, D
Ryckbosch, D
Sander, HG
Sarkar, S
Schlenstedt, S
Schmidt, T
Schneider, D
Seckel, D
Semburg, B
Seo, SH
Seunarine, S
Silvestri, A
Smith, AJ
Solarz, M
Song, C
Sopher, JE
Spiczak, GM
Spiering, C
Stamatikos, M
Stanev, T
Steffen, P
Stezelberger, T
Stokstad, RG
Stoufer, MC
Stoyanov, S
Strahler, EA
Straszheim, T
Sulanke, KH
Sullivan, GW
Sumner, TJ
Taboada, I
Tarasova, O
Tepe, A
Thollander, L
Tilav, S
Tluczykont, M
Toale, PA
Turcan, D
Van Eijndhoven, N
Vandenbroucke, J
Van Overloop, A
Viscomi, V
Voigt, B
Wagner, W
Walck, C
Waldmann, H
Walter, M
Wang, YR
Wendt, C
Wiebusch, CH
Wikstrom, G
Williams, DR
Wischnewski, R
Wissing, H
Woschnagg, K
Xu, XW
Yodh, G
Yoshida, S
Zornoza, JD
Boer, M
Cline, T
Crew, G
Feroci, M
Frontera, F
Hurley, K
Lamb, D
Rau, A
Rossi, F
Ricker, G
Von Kienlin, A
AF Achterberg, A.
Ackermann, M.
Adams, J.
Ahrens, J.
Andeen, K.
Auffenberg, J.
Bahcall, J. N.
Bai, X.
Baret, B.
Barwick, S. W.
Bay, R.
Beattie, K.
Becka, T.
Becker, J. K.
Becker, K. -H.
Berghaus, P.
Berley, D.
Bernardini, E.
Bertrand, D.
Besson, D. Z.
Blaufuss, E.
Boersma, D. J.
Bohm, C.
Bolmont, J.
Boeser, S.
Botner, O.
Bouchta, A.
Braun, J.
Burgess, C.
Burgess, T.
Castermans, T.
Chirkin, D.
Christy, B.
Clem, J.
Cowen, D. F.
D'Agostino, M. V.
Davour, A.
Day, C. T.
De Clercq, C.
Demiroeres, L.
Descamps, F.
Desiati, P.
DeYoung, T.
Diaz-Velez, J. C.
Dreyer, J.
Dumm, J. P.
Duvoort, M. R.
Edwards, W. R.
Ehrlich, R.
Eisch, J.
Ellsworth, R. W.
Evenson, P. A.
Fadiran, O.
Fazely, A. R.
Filimonov, K.
Foerster, M. M.
Fox, B. D.
Franckowiak, A.
Gaisser, T. K.
Gallagher, J.
Ganugapati, R.
Geenen, H.
Gerhardt, L.
Goldschmidt, A.
Goodman, J. A.
Gozzini, R.
Griesel, T.
Gross, A.
Grullon, S.
Gunasingha, R. M.
Gurtner, M.
Hallgren, A.
Halzen, F.
Han, K.
Hanson, K.
Hardtke, D.
Hardtke, R.
Hart, J. E.
Hasegawa, Y.
Hauschildt, T.
Hays, D.
Heise, J.
Helbing, K.
Hellwig, M.
Herquet, P.
Hill, G. C.
Hodges, J.
Hoffman, K. D.
Hommez, B.
Hoshina, K.
Hubert, D.
Hughey, B.
Hulth, P. O.
Huess, J. -P.
Hultqvist, K.
Hundertmark, S.
Inaba, M.
Ishihara, A.
Jacobsen, J.
Japaridze, G. S.
Johansson, H.
Jones, A.
Joseph, J. M.
Kampert, K. -H.
Kappes, A.
Karg, T.
Karle, A.
Kawai, H.
Kelley, J. L.
Kitamura, N.
Klein, S. R.
Klepser, S.
Kohnen, G.
Kolanoski, H.
Pke, L. Ko
Kowalski, M.
Kowarik, T.
Krasberg, M.
Kuehn, K.
Labare, M.
Landsman, H.
Leich, H.
Leier, D.
Liubarsky, I.
Lundberg, J.
Luenemann, J.
Madsen, J.
Mase, K.
Matis, H. S.
McCauley, T.
McParland, C. P.
Meli, A.
Messarius, T.
Meszaros, P.
Miyamoto, H.
Mokhtarani, A.
Montaruli, T.
Morey, A.
Morse, R.
Movit, S. M.
Muenich, K.
Nahnhauer, R.
Nam, J. W.
Niessen, P.
Nygren, D. R.
Oegelman, H.
Olivas, A.
Patton, S.
Pena-Garay, C.
De Los Heros, C. Perez
Piegsa, A.
Pieloth, D.
Pohl, A. C.
Porrata, R.
Pretz, J.
Price, P. B.
Przybylski, G. T.
Rawlins, K.
Razzaque, S.
Resconi, E.
Rhode, W.
Ribordy, M.
Rizzo, A.
Robbins, S.
Roth, P.
Rott, C.
Rutledge, D.
Ryckbosch, D.
Sander, H. -G.
Sarkar, S.
Schlenstedt, S.
Schmidt, T.
Schneider, D.
Seckel, D.
Semburg, B.
Seo, S. H.
Seunarine, S.
Silvestri, A.
Smith, A. J.
Solarz, M.
Song, C.
Sopher, J. E.
Spiczak, G. M.
Spiering, C.
Stamatikos, M.
Stanev, T.
Steffen, P.
Stezelberger, T.
Stokstad, R. G.
Stoufer, M. C.
Stoyanov, S.
Strahler, E. A.
Straszheim, T.
Sulanke, K. -H.
Sullivan, G. W.
Sumner, T. J.
Taboada, I.
Tarasova, O.
Tepe, A.
Thollander, L.
Tilav, S.
Tluczykont, M.
Toale, P. A.
Turcan, D.
Van Eijndhoven, N.
Vandenbroucke, J.
Van Overloop, A.
Viscomi, V.
Voigt, B.
Wagner, W.
Walck, C.
Waldmann, H.
Walter, M.
Wang, Y. -R.
Wendt, C.
Wiebusch, C. H.
Wikstroem, G.
Williams, D. R.
Wischnewski, R.
Wissing, H.
Woschnagg, K.
Xu, X. W.
Yodh, G.
Yoshida, S.
Zornoza, J. D.
Boer, M.
Cline, T.
Crew, G.
Feroci, M.
Frontera, F.
Hurley, K.
Lamb, D.
Rau, A.
Rossi, F.
Ricker, G.
Von Kienlin, A.
TI The search for muon neutrinos from northern hemisphere gamma-ray bursts
with amanda
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays : bursts; neutrinos
ID HIGH-ENERGY NEUTRINOS; SUPERNOVAE; CONNECTION; TELESCOPES; DETECTORS;
SELECTION; EMISSION; PARADIGM; BATSE; IB/C
AB We present the results of the analysis of neutrino observations by the Antarctic Muon and Neutrino Detector Array (AMANDA) correlated with photon observations of more than 400 gamma-ray bursts (GRBs) in the northern hemisphere from 1997 to 2003. During this time period, AMANDA's effective collection area for muon neutrinos was larger than that of any other existing detector. After the application of various selection criteria to our data, we expect similar to 1 neutrino event and <2 background events. Based on our observations of zero events during and immediately prior to the GRBs in the data set, we set the most stringent upper limit on muon neutrino emission correlated with GRBs. Assuming a Waxman-Bahcall spectrum and incorporating all systematic uncertainties, our flux upper limit has a normalization at 1 PeV of E-2 Phi(nu) <= 6.3 x 10(-9) GeV cm(-2) s(-1) sr(-1), with 90% of the events expected within the energy range of similar to 10 TeV to similar to 3 PeV. The impact of this limit on several theoretical models of GRBs is discussed, as well as the future potential for detection of GRBs by next-generation neutrino telescopes. Finally, we briefly describe several modifications to this analysis in order to apply it to other types of transient point sources.
C1 [Achterberg, A.; Duvoort, M. R.; Heise, J.; Van Eijndhoven, N.] Univ Utrecht, Dept Phys & Astron, NL-3584 CC Utrecht, Netherlands.
[Ackermann, M.; Bernardini, E.; Bolmont, J.; Boeser, S.; Klepser, S.; Leich, H.; Nahnhauer, R.; Pieloth, D.; Schlenstedt, S.; Steffen, P.; Sulanke, K. -H.; Tarasova, O.; Tluczykont, M.; Voigt, B.; Waldmann, H.; Walter, M.; Wischnewski, R.] Deutsches Elektron Synchrotron, D-15735 Zeuthen, Germany.
[Adams, J.; Han, K.; Spiering, C.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Ahrens, J.; Becka, T.; Gozzini, R.; Griesel, T.; Hellwig, M.; Pke, L. Ko; Kowarik, T.; Piegsa, A.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[Andeen, K.; Boersma, D. J.; Braun, J.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Ganugapati, R.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hodges, J.; Hoshina, K.; Hughey, B.; Ishihara, A.; Kappes, A.; Karle, A.; Kelley, J. L.; Kitamura, N.; Krasberg, M.; Landsman, H.; Morse, R.; Oegelman, H.; Schneider, D.; Stamatikos, M.; Strahler, E. A.; Wang, Y. -R.; Wendt, C.; Zornoza, J. D.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Auffenberg, J.; Becker, K. -H.; Franckowiak, A.; Geenen, H.; Gurtner, M.; Helbing, K.; Kampert, K. -H.; Karg, T.; Robbins, S.; Semburg, B.; Taboada, I.; Tepe, A.; Vandenbroucke, J.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Bai, X.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Baret, B.; De Clercq, C.; Hubert, D.; Labare, M.; Rizzo, A.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Barwick, S. W.; Gerhardt, L.; Kuehn, K.; Nam, J. W.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Bay, R.; Filimonov, K.; Hardtke, D.; Morey, A.; Porrata, R.; Price, P. B.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Beattie, K.; Becker, J. K.; Dreyer, J.; Luenemann, J.; Meli, A.; Messarius, T.; Muenich, K.; Rhode, W.; Wagner, W.] Univ Dortmund, Dept Phys, D-44221 Dortmund, Germany.
[Bertrand, D.] Univ Libre Brussels, Fac Sci, B-1050 Brussels, Belgium.
[Berley, D.; Blaufuss, E.; Ehrlich, R.; Goodman, J. A.; Hoffman, K. D.; Olivas, A.; Pretz, J.; Roth, P.; Schmidt, T.; Smith, A. J.; Straszheim, T.; Sullivan, G. W.; Turcan, D.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Bohm, C.; Burgess, C.; Burgess, T.; Hulth, P. O.; Hultqvist, K.; Hundertmark, S.; Johansson, H.; Thollander, L.; Walck, C.; Wikstroem, G.] Univ Stockholm, Dept Phys, SE-10691 Stockholm, Sweden.
[Botner, O.; Bouchta, A.; Davour, A.; Hallgren, A.; Lundberg, J.; De Los Heros, C. Perez; Pohl, A. C.] Uppsala Univ, Div High Energy Phys, S-75121 Uppsala, Sweden.
[Cowen, D. F.; Fox, B. D.; Hart, J. E.; Meszaros, P.; Rutledge, D.; Seo, S. H.; Toale, P. A.; Viscomi, V.; Williams, D. R.] Univ Mons, B-7000 Mons, Belgium.
[Hommez, B.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Subatom & Radiat Phys, B-9000 Ghent, Belgium.
[Eisch, J.; Hardtke, D.; Madsen, J.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Fadiran, O.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Fazely, A. R.; Gunasingha, R. M.; Xu, X. W.] So Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Resconi, E.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany.
[Hasegawa, Y.; Inaba, M.; Kawai, H.; Mase, K.; Miyamoto, H.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Huess, J. -P.; Wiebusch, C. H.; Wissing, H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52074 Aachen, Germany.
[Kolanoski, H.; Kowalski, M.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Liubarsky, I.; Sumner, T. J.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BW, England.
[Pohl, A. C.] Kalmar Univ, Dept Chem & Biomed Sci, S-39182 Kalmar, Sweden.
[Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Zornoza, J. D.] Univ Valencia, CSIC, IFIC, Valencia 46071, Spain.
[Boer, M.] Observ Haute Provence, St Michel Observ, F-04870 St Michel, France.
[Crew, G.; Ricker, G.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Feroci, M.] CNR, Area Ric Roma Tor Vergata, Inst Nazl Astrofis, Inst Astrofis Spaziale & Fis Cosmica, I-00133 Rome, Italy.
[Lamb, D.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Rau, A.] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA.
[Von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Frontera, F.; Rossi, F.] Univ Ferrara, Dept Phys, I-44100 Ferrara, Italy.
[Stamatikos, M.; Cline, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Beattie, K.; Goldschmidt, A.; Hays, D.; Jacobsen, J.; Jones, A.; Joseph, J. M.; Klein, S. R.; Matis, H. S.; McParland, C. P.; Nygren, D. R.; Patton, S.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.; Stoufer, M. C.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Cowen, D. F.; Meszaros, P.; Movit, S. M.; Razzaque, S.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Foerster, M. M.; Fox, B. D.; Hart, J. E.; Seo, S. H.; Viscomi, V.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Bahcall, J. N.] Inst Adv Study, Princeton, NJ 08540 USA.
RP Achterberg, A (reprint author), Univ Utrecht, Dept Phys & Astron, NL-3584 CC Utrecht, Netherlands.
RI Zornoza, Juan de Dios/L-1604-2014; Sarkar, Subir/G-5978-2011; Song,
Chihwa/A-3455-2008; Hundertmark, Stephan/A-6592-2010; Wiebusch,
Christopher/G-6490-2012; Kowalski, Marek/G-5546-2012; Botner,
Olga/A-9110-2013; Hallgren, Allan/A-8963-2013; Tjus, Julia/G-8145-2012;
Auffenberg, Jan/D-3954-2014
OI Hubert, Daan/0000-0002-4365-865X; Zornoza, Juan de
Dios/0000-0002-1834-0690; Sarkar, Subir/0000-0002-3542-858X; Perez de
los Heros, Carlos/0000-0002-2084-5866; Feroci,
Marco/0000-0002-7617-3421; Wiebusch, Christopher/0000-0002-6418-3008;
Auffenberg, Jan/0000-0002-1185-9094
NR 65
TC 40
Z9 40
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 2008
VL 674
IS 1
BP 357
EP 370
DI 10.1086/524920
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 266RJ
UT WOS:000253454400032
ER
PT J
AU Christodoulou, DM
Contopoulos, I
Kazanas, D
AF Christodoulou, Dimitris M.
Contopoulos, Ioannis
Kazanas, Demosthenes
TI Simulations of the Poynting-Robertson cosmic battery in resistive
accretion disks
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; instabilities; magnetic fields; MHD; plasmas
ID RADIATION MAGNETOHYDRODYNAMICS CODE; CONSERVATIVE DIFFERENCE SCHEME;
MAGNETIZED COUETTE-FLOW; 2 SPACE DIMENSIONS; ASTROPHYSICAL FLOWS;
INTERCHANGE METHOD; BLACK-HOLE; INSTABILITIES; GALAXY; JETS
AB We describe the results of numerical "2.5-dimensional'' MHD simulations of an initially unmagnetized disk orbiting a central point mass and responding to the continual generation of poloidalmagnetic field by a secular source emulating the Poynting-Robertson (PR) drag on electrons in the vicinity of a luminous stellar or compact accreting object. The secular PR term has dual purpose both as the magnetic field source and the trigger of magnetorotational instability (MRI). The disk and surrounding hotter atmosphere fluids have finite resistivity, allowing the magnetic field to diffuse out of its generation sites, while at the same time the disk differential rotation twists the poloidal field and induces a substantial toroidal-field component. For moderate disk resistivity (diffusion timescales up to similar to 16 local dynamical times) and after similar to 100 orbits, the MRI allows the fluid of the disk inner edge along with its magnetic flux to flow toward the central point mass where a new, magnetized, nuclear disk forms. The toroidal field in this nuclear disk is amplified by differential rotation and, when near equipartition, unwinds vertically, producing episodic jetlike outflows. For diffusion times longer than the flow time, the poloidal field in the inner region cannot diffuse out; it grows linearly in time, as the outer sections of new poloidal loops are drawn outward by the MRI while their inner sections continue to accumulate onto the compact inner disk. However, for low resistivity (diffusion timescales larger than similar to 16 local dynamical times), the inflowing matter does not form a nuclear disk or jets and the linear growth of the poloidal magnetic field is interrupted after similar to 20 orbits because of magnetic reconnection and asymmetric outflows.
C1 [Christodoulou, Dimitris M.] Math Methods, Bedford, MA 01730 USA.
[Contopoulos, Ioannis] Acad Athens, Res Ctr Astron, GR-11527 Athens, Greece.
[Kazanas, Demosthenes] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Christodoulou, DM (reprint author), Math Methods, 54 Middlesex Turnpike, Bedford, MA 01730 USA.
EM dimitris@mathmethods.com; icontop@academyofathens.gr;
kazanas@milkyway.gsfc.nasa.gov
NR 36
TC 14
Z9 14
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 10
PY 2008
VL 674
IS 1
BP 388
EP 407
DI 10.1086/524699
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 266RJ
UT WOS:000253454400035
ER
PT J
AU Cackett, EM
Miller, JM
Bhattacharyya, S
Grindlay, JE
Homan, J
Klis, MD
Miller, MC
Strohmayer, TE
Wijnands, R
AF Cackett, Edward M.
Miller, Jon M.
Bhattacharyya, Sudip
Grindlay, Jonathan E.
Homan, Jeroen
Van Der Klis, Michiel
Miller, M. Coleman
Strohmayer, Tod E.
Wijnands, Rudy
TI Relativistic iron emission lines in neutron star low-mass X-ray binaries
as probes of neutron star radii
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; stars : neutron; X-rays : binaries
ID QUASI-PERIODIC OSCILLATIONS; REDSHIFTED ABSORPTION-LINES; FAST-TIME
VARIABILITY; EQUATION-OF-STATE; BLACK-HOLE SPIN; GRO J1655-40; BURST
SPECTRA; LIGHT CURVES; 4U 1820-30; NGC 6624
AB Using Suzaku observations of three neutron star low-mass X-ray binaries ( Ser X-1, 4U 1820-30, and GX 349+2) we have found broad, asymmetric, relativistic Fe K emission lines in all three objects. These Fe K lines can be well fit by a model for lines from a relativistic accretion disk ("diskline''), allowing a measurement of the inner radius of the accretion disk and hence an upper limit on the neutron star radius. These upper limits correspond to 14.5-16.5 km for a 1.4 M-circle dot neutron star. The inner disk radii that we measure with Fe K lines are in good agreement with the inner disk radii implied by kHz QPOs observed in both 4U 1820-30 and GX 349+2, supporting the inner disk origin for kHz QPOs. In addition, the Fe K lines observed in these neutron stars are narrower than those in the black holes that are thought to be close to maximally spinning, as one would expect if inferences for spin are robust.
C1 [Cackett, Edward M.; Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Bhattacharyya, Sudip] NASA, Goddard Space Flight Ctr, CRESST & Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Bhattacharyya, Sudip; Miller, M. Coleman] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Grindlay, Jonathan E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Homan, Jeroen] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Van Der Klis, Michiel; Wijnands, Rudy] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands.
[Strohmayer, Tod E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Cackett, EM (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
EM ecackett@umich.edu
RI XRAY, SUZAKU/A-1808-2009
NR 54
TC 72
Z9 72
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 FEB 10
PY 2008
VL 674
IS 1
BP 415
EP 420
DI 10.1086/524936
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 266RJ
UT WOS:000253454400037
ER
PT J
AU Swain, MR
Bouwman, J
Akeson, RL
Lawler, S
Beichman, CA
AF Swain, M. R.
Bouwman, J.
Akeson, R. L.
Lawler, S.
Beichman, C. A.
TI The mid-infrared spectrum of the transiting exoplanet HD 209458b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods : data analysis; planetary systems; stars : individual (HD
209458); techniques : spectroscopic
ID SPITZER-SPACE-TELESCOPE; SOLAR-TYPE STARS; EXTRASOLAR PLANET; INFRARED
SPECTROGRAPH; SECONDARY ECLIPSE; SEARCH; EMISSION; 189733B; IRS
AB We report the spectroscopic detection of mid-infrared emission from the transiting exoplanet HD 209458b. Using archive data taken with the Spitzer IRS instrument, we have determined the spectrum of HD 209458b between 7.46 and 15.25 mu m. We have used two independent methods to determine the planet spectrum, one differential in wavelength and one absolute, and find the results are in good agreement. Over much of this spectral range, the planet spectrum is consistent with featureless thermal emission. Between 7.5 and 8.5 mu m, we find evidence for an unidentified spectral feature. If this spectral modulation is due to absorption, it implies that the dayside vertical temperature profile of the planetary atmosphere is not entirely isothermal. Using the IRS data, we have determined the broadband eclipse depth to be 0: 00315 +/- 0: 000315, implying significant redistribution of heat from the dayside to the nightside. This work required the development of improved methods for Spitzer IRS data calibration that increase the achievable absolute calibration precision and dynamic range for observations of bright point sources.
C1 [Swain, M. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bouwman, J.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Akeson, R. L.; Lawler, S.; Beichman, C. A.] CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA.
RP Swain, MR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 22
TC 64
Z9 65
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2008
VL 674
IS 1
BP 482
EP 497
DI 10.1086/523832
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 266RJ
UT WOS:000253454400043
ER
PT J
AU Gopalswamy, N
Yashiro, S
Xie, H
Akiyama, S
Aguilar-Rodriguez, E
Kaiser, ML
Howard, RA
Bougeret, JL
AF Gopalswamy, N.
Yashiro, S.
Xie, H.
Akiyama, S.
Aguilar-Rodriguez, E.
Kaiser, M. L.
Howard, R. A.
Bougeret, J. -L.
TI Radio-quiet fast and wide coronal mass ejections
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE solar-terrestrial relations; Sun : corona; Sun : coronal mass ejections
(CMEs); Sun : flares; Sun : particle emission; Sun : radio radiation
ID ENERGETIC PARTICLE EVENTS; LARGE-ANGLE; SOLAR; SPACECRAFT; BURSTS;
WAVES; SHOCK; SUN
AB We report on the properties of radio-quiet (RQ) and radio-loud (RL) coronal mass ejections (CMEs) that are fast and wide (FW). RQ CMEs lack type II radio bursts in the metric and decameter-hectometric (DH) wavelengths. RL CMEs are associated with metric or DH type II bursts. We found that similar to 40% of the FW CMEs from 1996 to 2005 were RQ. The RQ CMEs had an average speed of 1117 km s(-1) compared to 1438 km s(-1) for the RL, bracketing the average speed of all FW CMEs (1303 km s(-1)). The fraction of full halo CMEs (apparent width 360 degrees) was the largest for the RL CMEs (60%), smallest for the RQ CMEs (16%), and intermediate for all FW CMEs (42%). The median soft X-ray flare size for the RQ CMEs (C6.9) was also smaller than that for the RL CMEs (M3.9). About 55% of RQ CMEs were back sided, while the front-sided ones originated close to the limb. The RL CMEs originated generally on the disk with only similar to 25% being back sided. The RQ FW CMEs suggest that the Alfven speed in the low-latitude outer corona can often exceed 1000 km s(-1) and can vary over a factor of >= 3. None of the RQ CMEs was associated with large solar energetic particle events, which is useful information for space weather applications.
C1 [Gopalswamy, N.; Kaiser, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yashiro, S.; Xie, H.; Akiyama, S.; Aguilar-Rodriguez, E.] Catholic Univ Amer, Washington, DC 20064 USA.
[Howard, R. A.] USN, Res Lab, Washington, DC 20375 USA.
[Bougeret, J. -L.] Observ Paris, Meudon, France.
RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RI Gopalswamy, Nat/D-3659-2012;
OI Gopalswamy, Nat/0000-0001-5894-9954
NR 25
TC 47
Z9 47
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2008
VL 674
IS 1
BP 560
EP 569
DI 10.1086/524765
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 266RJ
UT WOS:000253454400050
ER
PT J
AU Wang, AH
Wu, ST
Liu, Y
Hathaway, D
AF Wang, A. H.
Wu, S. T.
Liu, Yang
Hathaway, D.
TI Recovering photospheric velocities from vector magnetograms by using a
three-dimensional, fully magnetohydrodynamic model
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE MHD; Sun : activity; Sun : atmospheric motions; Sun : magnetic fields
ID PROJECTED CHARACTERISTICS; MAGNETIC-FIELDS; ACTIVE-REGION; EVOLUTION;
ENERGY; FLARES; RECONSTRUCTION; FORMULATION; TRACKING; MOTION
AB We use a numerical simulation method for recovering the photospheric velocity field from the vector magnetograms. The traditional method is local correlation tracking (LCT), which is based on measuring the relative displacements of features in blocks of pixels between successive white-light images or magnetograms. Within this method, there are a variety of implementations. One of recently developed implementations is induction local correlation tracking (ILCT) as described by Welsch and coworkers. They employ the normal component of magnetic induction equation as a constraint to assure consistent solutions. Our numerical method uses the fully three-dimensional MHD equations to recover the photospheric velocity field with individual vector magnetograms. We compare our method to the ILCT method using NOAA AR 8210 as an example. The differences and similarities are discussed in detail.
C1 [Wang, A. H.; Wu, S. T.] Univ Alabama, Ctr Space Plasma & Aeronom Res, Huntsville, AL 35899 USA.
[Wang, A. H.; Wu, S. T.] Univ Alabama, Dept Mech & Aerosp Engn, Huntsville, AL 35899 USA.
[Liu, Yang] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Hathaway, D.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Wang, AH (reprint author), Univ Alabama, Ctr Space Plasma & Aeronom Res, Huntsville, AL 35899 USA.
NR 22
TC 8
Z9 8
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 10
PY 2008
VL 674
IS 1
BP L57
EP L60
DI 10.1086/528844
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 291YT
UT WOS:000255234100015
ER
PT J
AU Freund, FT
AF Freund, Friedemann T.
TI Earthquake probabilities and pre-earthquake signals
SO CURRENT SCIENCE
LA English
DT Article
ID EMISSIONS; ANOMALIES; ROCKS
C1 [Freund, Friedemann T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Freund, FT (reprint author), NASA, Ames Res Ctr, MS 242-4, Moffett Field, CA 94035 USA.
EM friedemann.t.freund@nasa.gov
NR 20
TC 2
Z9 2
U1 0
U2 3
PU CURRENT SCIENCE ASSOC
PI BANGALORE
PA C V RAMAN AVENUE, PO BOX 8005, BANGALORE 560 080, INDIA
SN 0011-3891
J9 CURR SCI INDIA
JI Curr. Sci.
PD FEB 10
PY 2008
VL 94
IS 3
BP 311
EP 313
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 264UJ
UT WOS:000253315600017
ER
PT J
AU Howard, AD
Moore, JM
AF Howard, Alan D.
Moore, Jeffrey M.
TI Sublimation-driven erosion on Callisto: A landform simulation model test
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID GALILEAN SATELLITES; DEGRADATION; SURFACE; ATMOSPHERE; MORPHOLOGY;
EVOLUTION
AB Callisto's landscape exhibits widespread erosion from some non-impact-induced process, which is characterized by smooth, undulating dark albedo surfaces with isolated high albedo knobs that are remnants of crater rims. We develop a landform simulation model that incorporates sublimation erosion of exposed bedrock on crater walls, composed of ice-cemented dust, with non-linear mass wasting of the released dust and redeposition of the ice on convex summits. The model reproduces the essential elements of landscapes on Callisto, and lends strong support to the 1999 hypothesis of Moore and his colleagues that volatile sublimation causes slope-forming bedrock disaggregation and subsequent mass wasting while reprecipitation caps and armors local crests with frost.
C1 [Howard, Alan D.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22903 USA.
[Moore, Jeffrey M.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Howard, AD (reprint author), Univ Virginia, Dept Environm Sci, 1156 High St, Charlottesville, VA 22903 USA.
EM jeff.moore@nasa.gov
OI Howard, Alan/0000-0002-5423-1600
NR 21
TC 5
Z9 5
U1 0
U2 3
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 2008
VL 35
IS 3
AR L03203
DI 10.1029/2007GL032618
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 261FK
UT WOS:000253064300004
ER
PT J
AU Grodsky, SA
Carton, JA
McClain, CR
AF Grodsky, Semyon A.
Carton, James A.
McClain, Charles R.
TI Variability of upwelling and chlorophyll in the equatorial Atlantic
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID TROPICAL ATLANTIC; SEASONAL CYCLE; OCEAN; PROJECT; MODEL
AB The primary seasonal phytoplankton bloom in the equatorial Atlantic occurs in boreal summer in response to seasonal strengthening of zonal winds. However, the equatorial Atlantic also has a secondary bloom in late fall - early winter. This secondary bloom is weaker than the primary bloom by a factor of two, but is subject to year-to-year variability that is similar in magnitude. Here, observational evidence, including sea level and SeaWiFS-derived chlorophyll-a concentration, is used to examine several potential causes of this secondary bloom. The secondary bloom varies independently of blooms along the eastern coastal zones. Also, the secondary bloom has a relationship with the cessation of the Northwest African monsoon, which propotes the secondary seasonal strengthening of the trade winds. The variability of the secondary bloom results from perturbations in the depth of the thermocline induced by zonal wind anomalies in the western tropical Atlantic. These wind anomalies are correlated with mean sea level atmospheric pressure anomalies in the region of the northern subtropical high as well as over the Amazon.
C1 [Grodsky, Semyon A.; Carton, James A.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[McClain, Charles R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Grodsky, SA (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
RI carton, james/C-4807-2009; Grodsky, Semyon/F-4929-2010
OI carton, james/0000-0003-0598-5198; Grodsky, Semyon/0000-0002-0670-1356
NR 18
TC 15
Z9 15
U1 2
U2 14
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 8
PY 2008
VL 35
IS 3
AR L03610
DI 10.1029/2007GL032466
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 261FH
UT WOS:000253064000001
ER
EF