FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Gandhi, P
Blain, AW
Russell, DM
Casella, P
Malzac, J
Corbel, S
D'Avanzo, P
Lewis, FW
Markoff, S
Bel, MC
Goldoni, P
Wachter, S
Khangulyan, D
Mainzer, A
AF Gandhi, P.
Blain, A. W.
Russell, D. M.
Casella, P.
Malzac, J.
Corbel, S.
D'Avanzo, P.
Lewis, F. W.
Markoff, S.
Cadolle Bel, M.
Goldoni, P.
Wachter, S.
Khangulyan, D.
Mainzer, A.
TI A VARIABLE MID-INFRARED SYNCHROTRON BREAK ASSOCIATED WITH THE COMPACT
JET IN GX 339-4
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; infrared: general; radiation mechanisms:
non-thermal; stars: individual (GX339-4); X-rays: binaries
ID X-RAY BINARIES; INFRARED-SURVEY-EXPLORER; BLACK-HOLE; LOW/HARD STATE;
TIMING OBSERVATIONS; RELATIVISTIC JETS; ACCRETION RATE; RADIO-SOURCES;
HIGH-ENERGY; EMISSION
AB Many X-ray binaries remain undetected in the mid-infrared, a regime where emission from their compact jets is likely to dominate. Here, we report the detection of the black hole binary GX 339-4 with the Wide-field Infrared Survey Explorer (WISE) during a very bright, hard accretion state in 2010. Combined with a rich contemporaneous multiwavelength data set, clear spectral curvature is found in the infrared, associated with the peak flux density expected from the compact jet. An optically thin slope of similar to-0.7 and a jet radiative power of >6 x 10(35) erg s(-1) (d/8 kpc)(2) are measured. A similar to 24 hr WISE light curve shows dramatic variations in mid-infrared spectral slope on timescales at least as short as the satellite orbital period similar to 95 minutes. There is also significant change during one pair of observations spaced by only 11 s. These variations imply that the spectral break associated with the transition from self-absorbed to optically thin jet synchrotron radiation must be varying across the full wavelength range of similar to 3-22 mu m that WISE is sensitive to, and more. Based on four-band simultaneous mid-infrared detections, the break is constrained to frequencies of approximate to 4.6(-2.0)(+3.5) x 10(13) Hz in at least two epochs of observation, consistent with a magnetic field B approximate to 1.5(+/- 0.8) x 10(4) G assuming a single-zone synchrotron emission region. The observed variability implies that either B or the size of the acceleration zone above the jet base is being modulated by factors of similar to 10 on relatively short timescales.
C1 [Gandhi, P.; Khangulyan, D.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Kanagawa 2525210, Japan.
[Blain, A. W.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Russell, D. M.; Markoff, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Casella, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Malzac, J.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Malzac, J.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Corbel, S.] CEA Saclay, UMR AIM, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Corbel, S.] Univ Paris 07, F-91191 Gif Sur Yvette, France.
[D'Avanzo, P.] INAF Osservatorio Astron Brera, I-23807 Merate, Lc, Italy.
[Lewis, F. W.] Univ Glamorgan, Div Earth Space & Environm, Faulkes Telescope Project, Pontypridd CF37 1DL, M Glam, Wales.
[Cadolle Bel, M.] European Space Astron Ctr, INTEGRAL Sci Operat Ctr, Sci Operat Dept, E-28691 Madrid, Spain.
[Goldoni, P.] Lab Astroparticule & Cosmol, F-75205 Paris 13, France.
[Goldoni, P.] CEA Saclay, Serv Astrophys, IRFU, DSM, F-91191 Gif Sur Yvette, France.
[Wachter, S.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Mainzer, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gandhi, P (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Kanagawa 2525210, Japan.
OI Casella, Piergiorgio/0000-0002-0752-3301
FU National Aeronautics and Space Administration (NASA); NASA's Planetary
Science Division; JAXA; Netherlands Organisation for Scientific
Research; GDR PCHE (France); EU [2009-237722]
FX WISE is a joint project of the University of California, Los Angeles,
and the Jet Propulsion Laboratory (JPL)/California Institute of
Technology (Caltech), funded by the National Aeronautics and Space
Administration (NASA). Data for individual scans are from NEOWISE (e.g.,
Mainzer et al. 2011), a project of JPL/Caltech funded by NASA's
Planetary Science Division. We thank the referee for a prompt report.
Individual support acknowledgments are as follows. P.Ga. acknowledges
JAXA International Top Young Fellowship, D.M.R. and S.M. acknowledge
Netherlands Organisation for Scientific Research Veni and Vidi
Fellowship, respectively, J.M. acknowledges GDR PCHE (France), and P.C.
acknowledges EU Marie Curie Intra-European Fellowship 2009-237722.
Swift/BAT transient monitor results and RXTE HEASARC archive data are
used herein. The Faulkes Telescope South (FTS) is maintained and
operated by Las Cumbres Observatory Global Telescope Network. We thank
Rosa Doran of NUCLIO, Portugal for FTS observations as part of the
EU-Hands on Universe initiative for school scientific education.
NR 50
TC 57
Z9 57
U1 0
U2 8
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 OCT 10
PY 2011
VL 740
IS 1
AR L13
DI 10.1088/2041-8205/740/1/L13
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 824OH
UT WOS:000295210900013
ER
PT J
AU Lin, L
Kouveliotou, C
Gogus, E
van der Horst, AJ
Watts, AL
Baring, MG
Kaneko, Y
Wijers, RAMJ
Woods, PM
Barthelmy, S
Burgess, JM
Chaplin, V
Gehrels, N
Goldstein, A
Granot, J
Guiriec, S
Mcenery, J
Preece, RD
Tierney, D
van der Klis, M
von Kienlin, A
Zhang, SN
AF Lin, Lin
Kouveliotou, Chryssa
Gogus, Ersin
van der Horst, Alexander J.
Watts, Anna L.
Baring, Matthew G.
Kaneko, Yuki
Wijers, Ralph A. M. J.
Woods, Peter M.
Barthelmy, Scott
Burgess, James Michael
Chaplin, Vandiver
Gehrels, Neil
Goldstein, Adam
Granot, Jonathan
Guiriec, Sylvain
Mcenery, Julie
Preece, Robert D.
Tierney, David
van der Klis, Michiel
von Kienlin, Andreas
Zhang, Shuang Nan
TI BURST AND PERSISTENT EMISSION PROPERTIES DURING THE RECENT ACTIVE
EPISODE OF THE ANOMALOUS X-RAY PULSAR 1E 1841-045
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE pulsars: individual (1E 1841-045); X-rays: bursts
ID SOFT GAMMA-REPEATERS; 2002 OUTBURST; SGR 1627-41; 4U 0142+61; KES 73;
MAGNETAR; 1E-1841-045; MONITOR; CHANDRA; SEARCH
AB The Swift/Burst Alert Telescope detected the first burst from 1E 1841-045 in 2010 May with intermittent burst activity recorded through at least 2011 July. Here we present Swift and Fermi/Gamma-ray Burst Monitor observations of this burst activity and search for correlated changes to the persistent X-ray emission of the source. The T-90 durations of the bursts range between 18 and 140 ms, comparable to other magnetar burst durations, while the energy released in each burst ranges between (0.8-25) x 10(38) erg, which is on the low side of soft gamma repeater bursts. We find that the bursting activity did not have a significant effect on the persistent flux level of the source. We argue that the mechanism leading to this sporadic burst activity in 1E 1841-045 might not involve large-scale restructuring (either crustal or magnetospheric) as seen in other magnetar sources.
C1 [Lin, Lin; Zhang, Shuang Nan] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Lin, Lin; Burgess, James Michael; Chaplin, Vandiver; Goldstein, Adam; Guiriec, Sylvain; Preece, Robert D.] Univ Alabama, CSPAR, Huntsville, AL 35805 USA.
[Kouveliotou, Chryssa] NASA, Space Sci Off, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Gogus, Ersin; Kaneko, Yuki] Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey.
[van der Horst, Alexander J.] NSSTC, Univ Space Res Assoc, Huntsville, AL 35805 USA.
[Watts, Anna L.; Wijers, Ralph A. M. J.; van der Klis, Michiel] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Baring, Matthew G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA.
[Woods, Peter M.] Corvid Technol, Huntsville, AL 35806 USA.
[Barthelmy, Scott; Gehrels, Neil; Mcenery, Julie] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Granot, Jonathan] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Tierney, David] Natl Univ Ireland Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[von Kienlin, Andreas] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Zhang, Shuang Nan] Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, Beijing 100049, Peoples R China.
RP Lin, L (reprint author), Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
EM lin198361@gmail.com
RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; McEnery,
Julie/D-6612-2012;
OI Preece, Robert/0000-0003-1626-7335; Burgess, James/0000-0003-3345-9515;
Wijers, Ralph/0000-0002-3101-1808
FU NASA [NNH07ZDA001-GLAST, NNX10AC59A]; Scientific and Technological
Research Council of Turkey (TUBITAK) [109T755]; Netherlands Organisation
for Scientific Research (NWO); European Research Council [247295];
Bundesministeriums fur Wirtschaft und Technologie (BMWi) [50 OG 1101]
FX This publication is part of the GBM/Magnetar Key Project (NASA grant
NNH07ZDA001-GLAST, PI: C. Kouveliotou). E.G. and Y.K. acknowledge the
support from the Scientific and Technological Research Council of Turkey
(TUBITAK) through grant 109T755. A.L.W. acknowledges support from a
Netherlands Organisation for Scientific Research (NWO) Vidi Grant.
M.G.B. acknowledges support from NASA through grant NNX10AC59A.
R.A.M.J.W. acknowledges support from the European Research Council via
Advanced Investigator Grant no. 247295. A.v.K. was supported by the
Bundesministeriums fur Wirtschaft und Technologie (BMWi) through DLR
grant 50 OG 1101.
NR 48
TC 15
Z9 15
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 10
PY 2011
VL 740
IS 1
AR L16
DI 10.1088/2041-8205/740/1/L16
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 824OH
UT WOS:000295210900016
ER
PT J
AU Moor, A
Abraham, P
Juhasz, A
Kiss, C
Pascucci, I
Kospal, A
Apai, D
Henning, T
Csengeri, T
Grady, C
AF Moor, A.
Abraham, P.
Juhasz, A.
Kiss, Cs
Pascucci, I.
Kospal, A.
Apai, D.
Henning, Th
Csengeri, T.
Grady, C.
TI MOLECULAR GAS IN YOUNG DEBRIS DISKS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE circumstellar matter; infrared: stars; stars: individual (HD21997)
ID SUN-LIKE STARS; MAIN-SEQUENCE STARS; PLANETARY SYSTEMS; CO EMISSION;
T-TAURI; NEARBY; EVOLUTION; DISCS; DUST; MASS
AB Gas-rich primordial disks and tenuous gas-poor debris disks are usually considered as two distinct evolutionary phases of the circumstellar matter. Interestingly, the debris disk around the young main-sequence star 49 Ceti possesses a substantial amount of molecular gas and possibly represents the missing link between the two phases. Motivated to understand the evolution of the gas component in circumstellar disks via finding more 49 Ceti-like systems, we carried out a CO J = 3-2 survey with the Atacama Pathfinder EXperiment, targeting 20 infrared-luminous debris disks. These systems fill the gap between primordial and old tenuous debris disks in terms of fractional luminosity. Here we report on the discovery of a second 49 Ceti-like disk around the 30 Myr old A3-type star HD21997, a member of the Columba Association. This system was also detected in the CO(2-1) transition, and the reliable age determination makes it an even clearer example of an old gas-bearing disk than 49 Ceti. While the fractional luminosities of HD21997 and 49 Ceti are not particularly high, these objects seem to harbor the most extended disks within our sample. The double-peaked profiles of HD21997 were reproduced by a Keplerian disk model combined with the LIME radiative transfer code. Based on their similarities, 49 Ceti and HD21997 may be the first representatives of a so far undefined new class of relatively old (greater than or similar to 8 Myr), gaseous dust disks. From our results, neither primordial origin nor steady secondary production from icy planetesimals can unequivocally explain the presence of CO gas in the disk of HD21997.
C1 [Moor, A.; Abraham, P.; Kiss, Cs] Hungarian Acad Sci, Konkoly Observ, H-1525 Budapest, Hungary.
[Juhasz, A.; Kospal, A.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands.
[Pascucci, I.; Apai, D.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Pascucci, I.; Apai, D.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Henning, Th] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Csengeri, T.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Grady, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Grady, C.] Eureka Sci, Oakland, CA 94602 USA.
RP Moor, A (reprint author), Hungarian Acad Sci, Konkoly Observ, POB 67, H-1525 Budapest, Hungary.
EM moor@konkoly.hu
FU Hungarian OTKA [K81966]; Netherlands Organisation for Scientific
Research
FX We thank an anonymous referee whose comments significantly improved the
manuscript. We are grateful to the APEX staff, in particular to Carlos
De Breuck (ESO), for their assistance. This research was partly funded
by the Hungarian OTKA grant K81966. The research of A.K. is supported by
the Netherlands Organisation for Scientific Research.
NR 50
TC 33
Z9 33
U1 0
U2 5
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 OCT 10
PY 2011
VL 740
IS 1
AR L7
DI 10.1088/2041-8205/740/1/L7
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 824OH
UT WOS:000295210900007
ER
PT J
AU Ern, M
Preusse, P
Gille, JC
Hepplewhite, CL
Mlynczak, MG
Russell, JM
Riese, M
AF Ern, M.
Preusse, P.
Gille, J. C.
Hepplewhite, C. L.
Mlynczak, M. G.
Russell, J. M., III
Riese, M.
TI Implications for atmospheric dynamics derived from global observations
of gravity wave momentum flux in stratosphere and mesosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CRYOGENIC INFRARED SPECTROMETERS; BREWER-DOBSON CIRCULATION; ASYNOPTIC
SATELLITE-OBSERVATIONS; DOPPLER-SPREAD PARAMETERIZATION; QUASI-BIENNIAL
OSCILLATION; EQUATORIAL KELVIN WAVES; SPACE-TIME SPECTRA;
MIDDLE-ATMOSPHERE; GENERAL-CIRCULATION; LIMB-SOUNDER
AB In this work absolute values of gravity wave (GW) momentum flux are derived from global temperature measurements by the satellite instruments High Resolution Dynamics Limb Sounder (HIRDLS) and Sounding of the Atmosphere using Broadband Emission Radiometry (SABER). Momentum fluxes in the stratosphere are derived for both instruments and for SABER in the whole mesosphere. The large-scale atmospheric background state is removed by a two-dimensional Fourier decomposition in longitude and time, covering even planetary-scale waves with periods as short as 1-2 days. Therefore, it is possible to provide global distributions of GW momentum flux from observations for the first time in the mesosphere. Seasonal as well as longer-term variations of the global momentum flux distribution are discussed. GWs likely contribute significantly to the equatorward tilt of the polar night jet and to the poleward tilt of the summertime mesospheric jet. Our results suggest that GWs can undergo large latitudinal shifts while propagating upward. In particular, GWs generated by deep convection in the subtropical monsoon regions probably contribute significantly to the mesospheric summertime wind reversal at mid-and high latitudes. Variations in the GW longitudinal distribution caused by those convectively generated GWs are still observed in the mesosphere and could be important for the generation of the quasi two-day wave. Indications for quasi-biennial oscillation (QBO) induced variations of GW momentum flux are found in the subtropics. Also variations at time scales of about one 11-year solar cycle are observed and might indicate a negative correlation between solar flux and GW momentum flux.
C1 [Ern, M.; Preusse, P.; Riese, M.] Forschungszentrum Julich, Inst Energie & Klimaforsch Stratosphare, D-52425 Julich, Germany.
[Gille, J. C.] Univ Colorado, Ctr Limb Atmospher Sounding, Boulder, CO 80309 USA.
[Hepplewhite, C. L.] Univ Oxford, Dept Phys, Oxford OX1 3PU, England.
[Mlynczak, M. G.] NASA Langley Res Ctr, Hampton, VA 23681 USA.
[Russell, J. M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Gille, J. C.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
RP Ern, M (reprint author), Forschungszentrum Julich, Inst Energie & Klimaforsch Stratosphare, D-52425 Julich, Germany.
EM m.ern@fz-juelich.de
RI Mlynczak, Martin/K-3396-2012; Preusse, Peter/A-1193-2013; Riese,
Martin/A-3927-2013; Ern, Manfred/I-8839-2016
OI Preusse, Peter/0000-0002-8997-4965; Riese, Martin/0000-0001-6398-6493;
Ern, Manfred/0000-0002-8565-2125
FU Deutsche Forschungsgemeinschaft (DFG) [ER 474/2-1, SPP-1176]
FX Very helpful comments by three anonymous reviewers are gratefully
acknowledged. The work of M. Ern was supported by the Deutsche
Forschungsgemeinschaft (DFG) within the project GW-EXCITES (grant ER
474/2-1), which is part of the DFG priority program CAWSES (SPP-1176).
This work further largely benefited from the SPARC gravity wave
initiative, as well as "The Gravity Wave Project" (ISSI Team 161) led by
M.J. Alexander and organized by the International Space Science
Institute (ISSI), Bern. The SPARC zonal wind climatology was provided by
the SPARC data center. Monthly Singapore winds were obtained from Free
University of Berlin and monthly solar flux data from NOAA. SABER data
were provided by GATS Inc., and HIRDLS data by NASA. Many thanks also go
to the teams of the HIRDLS and SABER instruments for all their effort to
create the excellent data sets used in this study.
NR 107
TC 87
Z9 87
U1 5
U2 25
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 OCT 8
PY 2011
VL 116
AR D19107
DI 10.1029/2011JD015821
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 833FX
UT WOS:000295869000002
ER
PT J
AU Fortenberry, RC
Huang, XC
Francisco, JS
Crawford, TD
Lee, TJ
AF Fortenberry, Ryan C.
Huang, Xinchuan
Francisco, Joseph S.
Crawford, T. Daniel
Lee, Timothy J.
TI The trans-HOCO radical: Quartic force fields, vibrational frequencies,
and spectroscopic constants
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID AB-INITIO; POLYATOMIC-MOLECULES; WAVE-FUNCTIONS; BASIS-SETS; SPECTRUM;
CO; ABSORPTION; ENERGIES; DYNAMICS; OH
AB In the search for a full mechanism creating CO2 from OH + CO, it has been suggested that creation of the hydroxyformyl or HOCO radical may be a necessary step. This reaction and its transient intermediate may also be responsible for the regeneration of CO2 in such high quantities in the atmosphere of Mars. Past spectroscopic observations of this radical have been limited and a full gas phase set of the fundamental vibrational frequencies of the HOCO radical has not been reported. Using established, highly accurate quantum chemical coupled cluster techniques and quartic force fields, we are able to compute all six fundamental vibrational frequencies and other spectroscopic constants for trans-HOCO in the gas phase. These methods have yielded rotational constants that are within 0.01 cm(-1) for A(0) and 10(-4) cm(-1) for B-0 and C-0 compared with experiment as well as fundamental vibrational frequencies within 4 cm(-1) of the known gas phase experimental nu(1) and nu(2) modes. Such results lead us to conclude that our prediction of the other four fundamental modes of trans-HOCO are also quite reliable for comparison to future experimental observation, though the discrepancy for the torsional mode may be larger since it is fairly anharmonic. With the upcoming European Space Agency/NASA ExoMars Trace Gas Orbiter, these data may help to establish whether HOCO is present in the Martian sky and what role it may play in the retention of a CO2-rich atmosphere. Furthermore, these data may also help to clear up questions built around the fundamental chemical process of how exactly the OH + CO reaction progresses. (C) 2011 American Institute of Physics. [doi:10.1063/1.3643336]
C1 [Fortenberry, Ryan C.; Crawford, T. Daniel] Virginia Tech, Dept Chem, Blacksburg, VA 24061 USA.
[Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA.
[Francisco, Joseph S.] Purdue Univ, Dept Chem, W Lafayette, IN 47907 USA.
[Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Fortenberry, RC (reprint author), Virginia Tech, Dept Chem, Blacksburg, VA 24061 USA.
EM Xinchuan.Huang-1@nasa.gov; crawdad@vt.edu; Timothy.J.Lee@nasa.gov
RI HUANG, XINCHUAN/A-3266-2013; Lee, Timothy/K-2838-2012; Crawford,
Thomas/A-9271-2017
OI Crawford, Thomas/0000-0002-7961-7016
FU U.S. National Science Foundation (NSF) [CHE-1058420]; Multi-User
Chemistry Research Instrumentation and Facility (CRIF:MU) award
[CHE-0741927]; Virginia Space Grant Consortium; NASA [Cycle 0 TR/LA PID
1022, 08-APRA08-0050]; NASA/SETI Institute [NNX09AI49A]
FX The work done by T.D.C. and R.C.F. is supported by the U.S. National
Science Foundation (NSF) award CHE-1058420 and by a Multi-User Chemistry
Research Instrumentation and Facility (CRIF:MU) award CHE-0741927.
R.C.F. also wishes to thank the Virginia Space Grant Consortium for a
Graduate Research Fellowship which he has been grateful to receive for
the past three years and T.J.L. and X.H. for their guidance and patience
with him throughout this research process and during his visit in the
spring of 2011. T.J.L. acknowledges funding from the NASA Herschel GO
Program, Cycle 0 TR/LA PID 1022, and NASA (Grant No. 08-APRA08-0050). X.
H. is funded by NASA/SETI Institute Cooperative Agreement NNX09AI49A. T.
D. C. and R. C. F. wish to thank Dr. Andrew Simmonett of the University
of Georgia for the use of his CheMVP program used to generate Fig. 1.
NR 74
TC 51
Z9 51
U1 0
U2 12
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 OCT 7
PY 2011
VL 135
IS 13
AR 134301
DI 10.1063/1.3643336
PG 8
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 829ZH
UT WOS:000295625400028
PM 21992299
ER
PT J
AU Hartle, RE
Sarantos, M
Sittler, EC
AF Hartle, R. E.
Sarantos, M.
Sittler, E. C., Jr.
TI Pickup ion distributions from three-dimensional neutral exospheres
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID SOLAR-WIND; LUNAR ATMOSPHERE; SODIUM EXOSPHERE; VOYAGER-1; HYDROGEN;
SATURN; TITAN; MODEL; PLANETARY; PHOTOCHEMISTRY
AB Pickup ions formed from ionized neutral exospheres in flowing plasmas have phase space distributions that reflect their source's spatial distributions. Phase space distributions of the ions are derived from the Vlasov equation with a delta function source using three-dimensional neutral exospheres. The ExB drift produced by plasma motion picks up the ions while the effects of magnetic field draping, mass loading, wave particle scattering, and Coulomb collisions near a planetary body are ignored. Previously, one-dimensional exospheres were treated, resulting in closed form pickup ion distributions that explicitly depend on the ratio r(g)/H, where r(g) is the ion gyroradius and H is the neutral scale height at the exobase. In general, the pickup ion distributions, based on three-dimensional neutral exospheres, cannot be written in closed form, but can be computed numerically. They continue to reflect their source's spatial distributions in an implicit way. These ion distributions and their moments are applied to several bodies, including He+ and Na+ at the Moon, H-2(+) and CH4+ at Titan, and H+ at Venus. The best places to use these distributions are upstream of the Moon's surface, the ionopause of Titan, and the bow shock of Venus.
C1 [Hartle, R. E.; Sarantos, M.; Sittler, E. C., Jr.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Hartle, R. E.; Sarantos, M.] NASA, Lunar Sci Inst, Moffett Field, CA USA.
[Sarantos, M.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA.
RP Hartle, RE (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
EM richard.e.hartle@nasa.gov
RI Sarantos, Menelaos/H-8136-2013
NR 40
TC 9
Z9 9
U1 1
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD OCT 7
PY 2011
VL 116
AR A10101
DI 10.1029/2011JA016859
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 832MK
UT WOS:000295808900003
ER
PT J
AU Lim, T
Ahn, SJ
Suh, M
Kwon, OK
Meyyappan, M
Ju, S
AF Lim, Taekyung
Ahn, Seong-Jin
Suh, Misook
Kwon, Oh-Kyong
Meyyappan, Meyya
Ju, Sanghyun
TI A nanowire-based shift register for display scan drivers
SO NANOTECHNOLOGY
LA English
DT Article
ID LIGHT-EMITTING DIODE; BUILDING-BLOCKS; TEMPERATURE; TRANSPARENT;
ELECTRONICS; TRANSISTORS; CIRCUITS
AB The development of display scan drivers is an essential step in the effort to develop transparent and flexible display devices based on nanowire transistors. Here we report a transparent nanowire-based shift register that functions as the standard logic circuit of a display scan driver. To form the shift register circuits using only n-type nanowire transistors, a novel circuit structure was introduced to avoid the output voltage drop typical of purely n-type circuits. A circuit simulation based on the measured nanowire transistor characteristics was developed in the planning phase to verify the circuit operation of the shift register. The shift register successfully produced an output of 0-3 V without an output voltage drop while applying an input of 3 V peak to peak. In addition, the shift register was designed to have multiple channels with a randomly oriented nanowire placement method to enhance the operation yield.
C1 [Lim, Taekyung; Suh, Misook; Ju, Sanghyun] Kyonggi Univ, Dept Phys, Suwon 443760, Gyeonggi Do, South Korea.
[Ahn, Seong-Jin; Kwon, Oh-Kyong] Hanyang Univ, Dept Elect Engn, Seoul 133791, South Korea.
[Meyyappan, Meyya] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Lim, T (reprint author), Kyonggi Univ, Dept Phys, Suwon 443760, Gyeonggi Do, South Korea.
EM shju@kgu.ac.kr
FU National Research Foundation of Korea (NRF); Ministry of Education,
Science and Technology [2011-0003160, 2011-0019133, 2011K000627]
FX This research was supported by the National Research Foundation of Korea
(NRF) funded by the Ministry of Education, Science and Technology
(2011-0003160, 2011-0019133, and 2011K000627).
NR 17
TC 6
Z9 6
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
J9 NANOTECHNOLOGY
JI Nanotechnology
PD OCT 7
PY 2011
VL 22
IS 40
AR 405203
DI 10.1088/0957-4484/22/40/405203
PG 7
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 820ZY
UT WOS:000294945800004
PM 21896980
ER
PT J
AU Spreen, G
Kwok, R
Menemenlis, D
AF Spreen, Gunnar
Kwok, Ron
Menemenlis, Dimitris
TI Trends in Arctic sea ice drift and role of wind forcing: 1992-2009
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MOTION
AB We examine the spatial trends in Arctic sea ice drift speed from satellite data and the role of wind forcing for the winter months of October through May. Between 1992 and 2009, the spatially averaged trend in drift speed within the Arctic Basin is 10.6% +/- 0.9%/decade, and ranges between -4% and 16%/decade depending on the location. The mean trend is dominated by the second half of the period. In fact, for the five years after a clear break point in March 2004, the average trend increased to 46% +/- 5%/decade. Over the 1992-2009 period, averaged trends of wind speed from four atmospheric reanalyses are only 1% to 2%/decade. Regionally, positive trends in wind speed (of up to 9%/decade) are seen over a large fraction of the Central Arctic, where the trends in drift speeds are highest. Spatial correlations between the basin-wide trends in wind and drift speeds are moderate (between 0.40 and 0.52). Our results suggest that changes in wind speed explain a fraction of the observed increase in drift speeds in the Central Arctic but not over the entire basin. In other regions thinning of the ice cover is a more likely cause of the increase in ice drift speed. Citation: Spreen, G., R. Kwok, and D. Menemenlis (2011), Trends in Arctic sea ice drift and role of wind forcing: 1992-2009, Geophys. Res. Lett., 38, L19501, doi: 10.1029/2011GL048970.
C1 [Spreen, Gunnar; Kwok, Ron; Menemenlis, Dimitris] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Spreen, G (reprint author), CALTECH, Jet Prop Lab, M-S 300-323,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM gunnar.spreen@jpl.nasa.gov
RI Spreen, Gunnar/A-4533-2010; Kwok, Ron/A-9762-2008
OI Spreen, Gunnar/0000-0003-0165-8448; Kwok, Ron/0000-0003-4051-5896
FU National Aeronautics and Space Administration
FX Distribution of atmospheric reanalysis data by the Japan Meteorological
Agency (JMA), ECMWF, Reading, UK, and NOAA/OAR/ESRL PSD, Boulder, CO,
USA are acknowledged. SSM/I data were obtained from the National Snow
and Ice Data Center (NSIDC). We thank the three reviewers for useful
comments. This work was performed at the Jet Propulsion Laboratory,
California Institute of Technology under contract with the National
Aeronautics and Space Administration.
NR 18
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U1 3
U2 23
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 OCT 6
PY 2011
VL 38
AR L19501
DI 10.1029/2011GL048970
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 832JS
UT WOS:000295801600003
ER
PT J
AU Kelly, BJ
Baker, JG
Boggs, WD
McWilliams, ST
Centrella, J
AF Kelly, Bernard J.
Baker, John G.
Boggs, William D.
McWilliams, Sean T.
Centrella, Joan
TI Mergers of black-hole binaries with aligned spins: Waveform
characteristics
SO PHYSICAL REVIEW D
LA English
DT Article
ID 3-DIMENSIONAL CARTESIAN GRIDS; APPARENT-HORIZON FINDER;
GRAVITATIONAL-WAVES; INITIAL DATA; NUMERICAL RELATIVITY; FINAL SPIN;
COALESCENCE; EVOLUTION; SCHEME
AB We conduct a descriptive analysis of the multipolar structure of gravitational-radiation waveforms from equal-mass aligned-spin mergers, following an approach first presented in the complementary context of nonspinning black holes of varying mass ratio [J. G. Baker et al., Phys. Rev. D 78, 044046 (2008).]. We find that, as with the nonspinning mergers, the dominant waveform mode phases evolve together in lock-step through inspiral and merger, supporting the previous waveform description in terms of an adiabatically rigid rotator driving gravitational-wave emission-an implicit rotating source. We further apply the late-time merger-ringdown model for the rotational frequency introduced in [J. G. Baker et al., Phys. Rev. D 78, 044046 (2008).], along with an improved amplitude model appropriate for the dominant (2, +/- 2) modes. This provides a quantitative description of the merger-ringdown waveforms, and suggests that the major features of these waveforms can be described with reference only to the intrinsic parameters associated with the state of the final black hole formed in the merger. We provide an explicit model for the merger-ringdown radiation, and demonstrate that this model agrees to fitting factors better than 95% with the original numerical waveforms for system masses above similar to 150M(circle dot). This model may be directly applicable to gravitational-wave detection of intermediate-mass black-hole mergers.
C1 [Kelly, Bernard J.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Kelly, Bernard J.] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA.
[Kelly, Bernard J.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Baker, John G.; Centrella, Joan] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA.
[Boggs, William D.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McWilliams, Sean T.] Columbia Univ, ISCAP, New York, NY 10027 USA.
[McWilliams, Sean T.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
RP Kelly, BJ (reprint author), NASA, Goddard Space Flight Ctr, CRESST, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RI Kelly, Bernard/G-7371-2011;
OI Kelly, Bernard/0000-0002-3326-4454
FU NASA [08-ATFP08-0126, 09-ATP09-0136]; NASA through the NASA Advanced
Supercomputing (NAS) Division at Ames Research Center
FX This work was supported by NASA grants 08-ATFP08-0126 and 09-ATP09-0136.
Resources supporting this work were provided by the NASA High-End
Computing (HEC) Program through the NASA Advanced Supercomputing (NAS)
Division at Ames Research Center.
NR 86
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U1 1
U2 1
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 OCT 5
PY 2011
VL 84
IS 8
AR 084009
DI 10.1103/PhysRevD.84.084009
PG 19
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 841PR
UT WOS:000296525300003
ER
PT J
AU Zimmerman, MI
Farrell, WM
Stubbs, TJ
Halekas, JS
Jackson, TL
AF Zimmerman, M. I.
Farrell, W. M.
Stubbs, T. J.
Halekas, J. S.
Jackson, T. L.
TI Solar wind access to lunar polar craters: Feedback between surface
charging and plasma expansion
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID VACUUM
AB Determining the plasma environment within permanently shadowed lunar craters is critical to understanding local processes such as surface charging, electrostatic dust transport, volatile sequestration, and space weathering. In order to investigate the nature of this plasma environment, the first two-dimensional kinetic simulations of solar wind expansion into a lunar crater with a self-consistent plasma-surface interaction have been undertaken. The present results reveal how the plasma expansion into a crater couples with the electrically-charged lunar surface to produce a quasi-steady wake structure. In particular, there is a negative feedback between surface charging and ambipolar wake potential that allows an equilibrium to be achieved, with secondary electron emission strongly moderating the process. A range of secondary electron yields is explored, and two distinct limits are highlighted in which either surface charging or ambipolar expansion is responsible for determining the overall wake structure. Citation: Zimmerman, M. I., W. M. Farrell, T. J. Stubbs, J. S. Halekas, and T. L. Jackson ( 2011), Solar wind access to lunar polar craters: Feedback between surface charging and plasma expansion, Geophys. Res. Lett., 38, L19202, doi:10.1029/2011GL048880.
C1 [Zimmerman, M. I.; Farrell, W. M.; Stubbs, T. J.; Jackson, T. L.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Zimmerman, M. I.; Farrell, W. M.; Stubbs, T. J.; Halekas, J. S.; Jackson, T. L.] NASA Ames Res Ctr, NASA Lunar Sci Inst, Moffett Field, CA USA.
[Stubbs, T. J.] Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21228 USA.
[Halekas, J. S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Zimmerman, MI (reprint author), NASA Goddard Space Flight Ctr, Code 695, Greenbelt, MD 20771 USA.
EM michael.i.zimmerman@nasa.gov
RI Jackson, Telana/E-9102-2012; Stubbs, Timothy/I-5139-2013; Farrell,
William/I-4865-2013;
OI Stubbs, Timothy/0000-0002-5524-645X; Halekas, Jasper/0000-0001-5258-6128
FU NASA Lunar Science Institute; DREAM virtual institute [NNX09AG78A]; NASA
at the Goddard Space Flight Center; [NNX08AN76G]
FX This research was supported by an appointment to the NASA Postdoctoral
Program at the Goddard Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA. The support of
LPROPS grant NNX08AN76G and the NASA Lunar Science Institute and DREAM
virtual institute through grant NNX09AG78A are gratefully acknowledged.
NR 14
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U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD OCT 5
PY 2011
VL 38
AR L19202
DI 10.1029/2011GL048880
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 832JR
UT WOS:000295801500001
ER
PT J
AU Szeto, M
Werdell, PJ
Moore, TS
Campbell, JW
AF Szeto, M.
Werdell, P. J.
Moore, T. S.
Campbell, J. W.
TI Are the world's oceans optically different?
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID FLUORESCENCE EXCITATION-SPECTRA; DISSOLVED ORGANIC-MATTER; BIOOPTICAL
PROPERTIES; SURFACE SEDIMENTS; PACIFIC-OCEAN; ABSORPTION-SPECTRA;
CALCIUM-CARBONATE; COASTAL WATERS; ATLANTIC OCEAN; SOUTHERN-OCEAN
AB Regional differences in the Sea-viewing Wide Field-of-view Sensor chlorophyll algorithm uncertainty were observed in a large global data set containing coincident in situ measurements of chlorophyll a concentration (Chla) and spectral radiometry. The uncertainty was found to be systematic when the data were sorted by ocean: Atlantic, Pacific, Southern, and Indian Oceans. Artifacts associated with different instrumentation and analytical methods had been previously ruled out. Given these oceanic biases in the chlorophyll algorithm, we hypothesized that the oceans may be optically different, and their optical differences may be intrinsically related to regional differences in phytoplankton community structure or biogeochemical processes. The oceanic biases, originally observed using radiometric measurements, were independently verified using total absorption measurements in a subset of the data. Moreover, they were explained through oceanic differences in the absorption of colored detrital matter (CDM) and phytoplankton. Both effects were considered together in explaining the ocean biases through a stepwise linear regression analysis. Significant oceanic differences in the amount of CDM and in phytoplankton cell sizes and pigmentation would give rise to optical differences, but we raise a concern for the spatial coverage of the data. We do not suggest the application of ocean-based algorithms but rather emphasize the importance of consolidating regional data sets before reaching this conclusion.
C1 [Szeto, M.; Moore, T. S.; Campbell, J. W.] Univ New Hampshire, Inst Study Earth Oceans & Space, Ocean Proc Anal Lab, Durham, NH 03824 USA.
[Werdell, P. J.] NASA, Goddard Space Flight Ctr, Ocean Biol Proc Grp, Greenbelt, MD 20771 USA.
RP Szeto, M (reprint author), Univ New Hampshire, Inst Study Earth Oceans & Space, Ocean Proc Anal Lab, 8 Coll Rd,Morse Hall,Rm 142, Durham, NH 03824 USA.
EM mimi.szeto@unh.edu; jeremy.werdell@nasa.gov; timothy.moore@unh.edu;
janet.campbell@unh.edu
RI Werdell, Jeremy/D-8265-2012
FU Research and Discover Fellowship Program; NASA [NNX08AG80A]; University
of New Hampshire
FX This work was funded by the Research and Discover Fellowship Program
cosponsored by NASA and the University of New Hampshire and a NASA grant
to J. W. Campbell (NNX08AG80A). The authors would like to thank all of
the Ocean Biology Processing Group members at NASA Goddard Space Flight
Center for their guidance, as well as the contributors to the SeaBASS
archive, making the comprehensive NOMAD data set available for analysis.
Much gratitude also goes to the three anonymous reviewers of the
manuscript, whose comments greatly strengthened the work and motivated a
deeper investigation of the underlying questions.
NR 58
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Z9 37
U1 0
U2 18
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 OCT 4
PY 2011
VL 116
AR C00H04
DI 10.1029/2011JC007230
PG 14
WC Oceanography
SC Oceanography
GA 832RZ
UT WOS:000295825900005
ER
PT J
AU Battaglia, A
Augustynek, T
Tanelli, S
Kollias, P
AF Battaglia, A.
Augustynek, T.
Tanelli, S.
Kollias, P.
TI Multiple scattering identification in spaceborne W-band radar
measurements of deep convective cores
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID DOPPLER RADAR; TROPICAL TROPOPAUSE; VELOCITY-MEASUREMENTS; GLOBAL
DISTRIBUTION; CLOUD; RAINFALL; UNCERTAINTIES; AIRBORNE; SURFACE; RANGE
AB CloudSat observations have indicated that multiple scattering affects 94 GHz spaceborne radar observations. The ESA EarthCARE explorer mission scheduled to launch in 2015 features also a spaceborne 94-GHz radar with Doppler capability for providing a global data set of convective motions and particle sedimentation rates. Vertical velocity measurements will be collected in all cloud conditions, including deep convection where multiple-scattering is expected to contaminate the signal. Thus, before the spaceborne Doppler radars are used for science application, it is imperative to develop a method to identify radar range gates contaminated by multiple scattering contributions. Based on simulations, a criterion to identify the onset of multiple scattering is presented in this paper; the cumulative integrated reflectivity from the top of the atmosphere is a proxy of the multiple scattering enhancement and can be confidently used to detect the onset of multiple scattering. Analysis of a limited (two months) CloudSat data set reveals that, for deep tropical convective cores, the onset of significant multiple scattering typically occurs in the region between 9-10 km and more than 35% of the range bins above the freezing level height and with reflectivity above -20 dBZ are not affected by multiple scattering. This assessment offers a conservative upper limit for EarthCARE 94-GHz radar multiple scattering effects due to the narrower field of view of the Doppler radar compared to CloudSat's radar. Identification of multiple scattering contamination in the CloudSat and EarthCARE radar observations facilitates the following objectives: (1) to constrain the region of validity of currently developed CloudSat products based on single scattering theory (e.g. 2B-CWC-RO, 2B-CWC-RVOD) and (2) to filter out multiple scattering affected range bins in any analysis aimed at the assessment of the feasibility and of the accuracy of the EarthCARE Doppler estimates within deep convective cores.
C1 [Battaglia, A.; Augustynek, T.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Tanelli, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kollias, P.] McGill Univ, Dept Atmospher & Ocean Sci, Montreal, PQ H3A 2K6, Canada.
RP Battaglia, A (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England.
EM a.battaglia@le.ac.uk
OI Battaglia, Alessandro/0000-0001-9243-3484
FU European Space Agency; STSE program; Jet Propulsion Laboratory under
National Aeronautics and Space Administration; Advanced Information
Systems Technology Program; NASA SALMON/USPI; Department of Physics and
Astronomy, University of Leicester
FX This work was supported by the European Space Agency under the Doppler
Air Motion Estimate project funded by the STSE program. A. Battaglia's
travel and publication costs were covered by the NCEO EO Mission
Support. The contributions by Simone Tanelli were performed at the Jet
Propulsion Laboratory under contract with the National Aeronautics and
Space Administration. Support for the "Instrument Simulator Suite for
Atmospheric Remote Sensing" project from the Advanced Information
Systems Technology Program, and for the "Doppler Velocity Products for
the EarthCARE mission" from the NASA SALMON/USPI program are gratefully
acknowledged. The financial and educational support of the Department of
Physics and Astronomy, University of Leicester for Augustynek's Ph.D.
are also greatly acknowledged.
NR 39
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U1 2
U2 14
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 OCT 4
PY 2011
VL 116
AR D19201
DI 10.1029/2011JD016142
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 833FS
UT WOS:000295868400005
ER
PT J
AU Abbasi, R
Abdou, Y
Abu-Zayyad, T
Adams, J
Aguilar, JA
Ahlers, M
Altmann, D
Andeen, K
Auffenberg, J
Bai, X
Baker, M
Barwick, SW
Bay, R
Alba, JLB
Beattie, K
Beatty, JJ
Bechet, S
Becker, JK
Becker, KH
Benabderrahmane, ML
BenZvi, S
Berdermann, J
Berghaus, P
Berley, D
Bernardini, E
Bertrand, D
Besson, DZ
Bindig, D
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohm, C
Bose, D
Boser, S
Botner, O
Brown, AM
Buitink, S
Caballero-Mora, KS
Carson, M
Chirkin, D
Christy, B
Clem, J
Clevermann, F
Cohen, S
Colnard, C
Cowen, DF
D'Agostino, MV
Danninger, M
Daughhetee, J
Davis, JC
De Clercq, C
Demirors, L
Denger, T
Depaepe, O
Descamps, F
Desiati, P
de Vries-Uiterweerd, G
DeYoung, T
Diaz-Velez, JC
Dierckxsens, M
Dreyer, J
Dumm, JP
Ehrlich, R
Eisch, J
Ellsworth, RW
Engdegard, O
Euler, S
Evenson, PA
Fadiran, O
Fazely, AR
Fedynitch, A
Feintzeig, J
Feusels, T
Filimonov, K
Finley, C
Fischer-Wasels, T
Foerster, MM
Fox, BD
Franckowiak, A
Franke, R
Gaisser, TK
Gallagher, J
Gerhardt, L
Gladstone, L
Glusenkamp, T
Goldschmidt, A
Goodman, JA
Gora, D
Grant, D
Griesel, T
Gross, A
Grullon, S
Gurtner, M
Ha, C
Hajismail, A
Hallgren, A
Halzen, F
Han, K
Hanson, K
Heinen, D
Helbing, K
Herquet, P
Hickford, S
Hill, GC
Hoffman, KD
Homeier, A
Hoshina, K
Hubert, D
Huelsnitz, W
Hulss, JP
Hulth, PO
Hultqvist, K
Hussain, S
Ishihara, A
Jacobsen, J
Japaridze, GS
Johansson, H
Joseph, JM
Kampert, KH
Kappes, A
Karg, T
Karle, A
Kenny, P
Kiryluk, J
Kislat, F
Klein, SR
Kohne, JH
Kohnen, G
Kolanoski, H
Kopke, L
Kopper, S
Koskinen, DJ
Kowalski, M
Kowarik, T
Krasberg, M
Krings, T
Kroll, G
Kurahashi, N
Kuwabara, T
Labare, M
Lafebre, S
Laihem, K
Landsman, H
Larson, MJ
Lauer, R
Lunemann, J
Madsen, J
Majumdar, P
Marotta, A
Maruyama, R
Mase, K
Matis, HS
Meagher, K
Merck, M
Meszaros, P
Meures, T
Middell, E
Milke, N
Miller, J
Montaruli, T
Morse, R
Movit, SM
Nahnhauer, R
Nam, JW
Naumann, U
Niessen, P
Nygren, DR
Odrowski, S
Olivas, A
Olivo, M
O'Murchadha, A
Ono, M
Panknin, S
Paul, L
de los Heros, CP
Petrovic, J
Piegsa, A
Pieloth, D
Porrata, R
Posselt, J
Price, PB
Przybylski, GT
Rawlins, K
Redl, P
Resconi, E
Rhode, W
Ribordy, M
Rizzo, A
Rodrigues, JP
Roth, P
Rothmaier, F
Rott, C
Ruhe, T
Rutledge, D
Ruzybayev, B
Ryckbosch, D
Sander, HG
Santander, M
Sarkar, S
Schatto, K
Schmidt, T
Schonwald, A
Schukraft, A
Schultes, A
Schulz, O
Schunck, M
Seckel, D
Semburg, B
Seo, SH
Sestayo, Y
Seunarine, S
Silvestri, A
Slipak, A
Spiczak, GM
Spiering, C
Stamatikos, M
Stanev, T
Stephens, G
Stezelberger, T
Stokstad, RG
Stossl, A
Stoyanov, S
Strahler, EA
Straszheim, T
Stur, M
Sullivan, GW
Swillens, Q
Taavola, H
Taboada, I
Tamburro, A
Tepe, A
Ter-Antonyan, S
Tilav, S
Toale, PA
Toscano, S
Tosi, D
Turcan, D
van Eijndhoven, N
Vandenbroucke, J
Van Overloop, A
van Santen, J
Vehring, M
Voge, M
Walck, C
Waldenmaier, T
Wallraff, M
Walter, M
Weaver, C
Wendt, C
Westerhoff, S
Whitehorn, N
Wiebe, K
Wiebusch, CH
Williams, DR
Wischnewski, R
Wissing, H
Wolf, M
Wood, TR
Woschnagg, K
Xu, C
Xu, XW
Yodh, G
Yoshida, S
Zarzhitsky, P
Zoll, M
AF Abbasi, R.
Abdou, Y.
Abu-Zayyad, T.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Altmann, D.
Andeen, K.
Auffenberg, J.
Bai, X.
Baker, M.
Barwick, S. W.
Bay, R.
Alba, J. L. Bazo
Beattie, K.
Beatty, J. J.
Bechet, S.
Becker, J. K.
Becker, K. -H.
Benabderrahmane, M. L.
BenZvi, S.
Berdermann, J.
Berghaus, P.
Berley, D.
Bernardini, E.
Bertrand, D.
Besson, D. Z.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohm, C.
Bose, D.
Boeser, S.
Botner, O.
Brown, A. M.
Buitink, S.
Caballero-Mora, K. S.
Carson, M.
Chirkin, D.
Christy, B.
Clem, J.
Clevermann, F.
Cohen, S.
Colnard, C.
Cowen, D. F.
D'Agostino, M. V.
Danninger, M.
Daughhetee, J.
Davis, J. C.
De Clercq, C.
Demiroers, L.
Denger, T.
Depaepe, O.
Descamps, F.
Desiati, P.
de Vries-Uiterweerd, G.
DeYoung, T.
Diaz-Velez, J. C.
Dierckxsens, M.
Dreyer, J.
Dumm, J. P.
Ehrlich, R.
Eisch, J.
Ellsworth, R. W.
Engdegard, O.
Euler, S.
Evenson, P. A.
Fadiran, O.
Fazely, A. R.
Fedynitch, A.
Feintzeig, J.
Feusels, T.
Filimonov, K.
Finley, C.
Fischer-Wasels, T.
Foerster, M. M.
Fox, B. D.
Franckowiak, A.
Franke, R.
Gaisser, T. K.
Gallagher, J.
Gerhardt, L.
Gladstone, L.
Gluesenkamp, T.
Goldschmidt, A.
Goodman, J. A.
Gora, D.
Grant, D.
Griesel, T.
Gross, A.
Grullon, S.
Gurtner, M.
Ha, C.
Hajismail, A.
Hallgren, A.
Halzen, F.
Han, K.
Hanson, K.
Heinen, D.
Helbing, K.
Herquet, P.
Hickford, S.
Hill, G. C.
Hoffman, K. D.
Homeier, A.
Hoshina, K.
Hubert, D.
Huelsnitz, W.
Huelss, J. -P.
Hulth, P. O.
Hultqvist, K.
Hussain, S.
Ishihara, A.
Jacobsen, J.
Japaridze, G. S.
Johansson, H.
Joseph, J. M.
Kampert, K. -H.
Kappes, A.
Karg, T.
Karle, A.
Kenny, P.
Kiryluk, J.
Kislat, F.
Klein, S. R.
Koehne, J. -H.
Kohnen, G.
Kolanoski, H.
Koepke, L.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Kowarik, T.
Krasberg, M.
Krings, T.
Kroll, G.
Kurahashi, N.
Kuwabara, T.
Labare, M.
Lafebre, S.
Laihem, K.
Landsman, H.
Larson, M. J.
Lauer, R.
Luenemann, J.
Madsen, J.
Majumdar, P.
Marotta, A.
Maruyama, R.
Mase, K.
Matis, H. S.
Meagher, K.
Merck, M.
Meszaros, P.
Meures, T.
Middell, E.
Milke, N.
Miller, J.
Montaruli, T.
Morse, R.
Movit, S. M.
Nahnhauer, R.
Nam, J. W.
Naumann, U.
Niessen, P.
Nygren, D. R.
Odrowski, S.
Olivas, A.
Olivo, M.
O'Murchadha, A.
Ono, M.
Panknin, S.
Paul, L.
de los Heros, C. Perez
Petrovic, J.
Piegsa, A.
Pieloth, D.
Porrata, R.
Posselt, J.
Price, P. B.
Przybylski, G. T.
Rawlins, K.
Redl, P.
Resconi, E.
Rhode, W.
Ribordy, M.
Rizzo, A.
Rodrigues, J. P.
Roth, P.
Rothmaier, F.
Rott, C.
Ruhe, T.
Rutledge, D.
Ruzybayev, B.
Ryckbosch, D.
Sander, H. -G.
Santander, M.
Sarkar, S.
Schatto, K.
Schmidt, T.
Schoenwald, A.
Schukraft, A.
Schultes, A.
Schulz, O.
Schunck, M.
Seckel, D.
Semburg, B.
Seo, S. H.
Sestayo, Y.
Seunarine, S.
Silvestri, A.
Slipak, A.
Spiczak, G. M.
Spiering, C.
Stamatikos, M.
Stanev, T.
Stephens, G.
Stezelberger, T.
Stokstad, R. G.
Stoessl, A.
Stoyanov, S.
Strahler, E. A.
Straszheim, T.
Stuer, M.
Sullivan, G. W.
Swillens, Q.
Taavola, H.
Taboada, I.
Tamburro, A.
Tepe, A.
Ter-Antonyan, S.
Tilav, S.
Toale, P. A.
Toscano, S.
Tosi, D.
Turcan, D.
van Eijndhoven, N.
Vandenbroucke, J.
Van Overloop, A.
van Santen, J.
Vehring, M.
Voge, M.
Walck, C.
Waldenmaier, T.
Wallraff, M.
Walter, M.
Weaver, Ch
Wendt, C.
Westerhoff, S.
Whitehorn, N.
Wiebe, K.
Wiebusch, C. H.
Williams, D. R.
Wischnewski, R.
Wissing, H.
Wolf, M.
Wood, T. R.
Woschnagg, K.
Xu, C.
Xu, X. W.
Yodh, G.
Yoshida, S.
Zarzhitsky, P.
Zoll, M.
TI Search for a diffuse flux of astrophysical muon neutrinos with the
IceCube 40-string detector
SO PHYSICAL REVIEW D
LA English
DT Article
ID COSMIC-RAYS; MODEL; TELESCOPES; SELECTION; AMANDA; ICE
AB The IceCube Neutrino Observatory is a 1 km(3) detector currently taking data at the South Pole. One of the main strategies used to look for astrophysical neutrinos with IceCube is the search for a diffuse flux of high-energy neutrinos from unresolved sources. A hard energy spectrum of neutrinos from isotropically distributed astrophysical sources could manifest itself as a detectable signal that may be differentiated from the atmospheric neutrino background by spectral measurement. This analysis uses data from the IceCube detector collected in its half completed configuration which operated between April 2008 and May 2009 to search for a diffuse flux of astrophysical muon neutrinos. A total of 12 877 upward-going candidate neutrino events have been selected for this analysis. No evidence for a diffuse flux of astrophysical muon neutrinos was found in the data set leading to a 90% C. L. upper limit on the normalization of an E-2 astrophysical nu(mu) flux of 8.9 x 10(-9) GeV cm(-2) s(-1) sr(-1). The analysis is sensitive in the energy range between 35 TeV and 7 PeV. The 12 877 candidate neutrino events are consistent with atmospheric muon neutrinos measured from 332 GeV to 84 TeV and no evidence for a prompt component to the atmospheric neutrino spectrum is found.
C1 [Abbasi, R.; Aguilar, J. A.; Andeen, K.; Baker, M.; BenZvi, S.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Feintzeig, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hoshina, K.; Jacobsen, J.; Karle, A.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; Merck, M.; Montaruli, T.; Morse, R.; O'Murchadha, A.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Altmann, D.; Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Gluesenkamp, T.; Heinen, D.; Huelss, J. -P.; Krings, T.; Laihem, K.; Paul, L.; Schukraft, A.; Schunck, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
[Toale, P. A.; Williams, D. R.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Rawlins, K.] Univ Alaska, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Fadiran, O.; Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Bay, R.; D'Agostino, M. V.; Filimonov, K.; Gerhardt, L.; Kiryluk, J.; Klein, S. R.; Porrata, R.; Price, P. B.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Beattie, K.; Buitink, S.; Gerhardt, L.; Goldschmidt, A.; Joseph, J. M.; Kiryluk, J.; Klein, S. R.; Matis, H. S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
[Kappes, A.; Kolanoski, H.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Becker, J. K.; Dreyer, J.; Fedynitch, A.; Olivo, M.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Boeser, S.; Denger, T.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.; Stuer, M.; Voge, M.] Univ Bonn, Inst Phys 1, D-53115 Bonn, Germany.
[Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados.
[Bechet, S.; Bertrand, D.; Dierckxsens, M.; Hanson, K.; Marotta, A.; Meures, T.; Petrovic, J.; Swillens, Q.] Univ Libre Bruxelles, Sci Fac CP230, B-1050 Brussels, Belgium.
[Bose, D.; De Clercq, C.; Depaepe, O.; Hubert, D.; Labare, M.; Rizzo, A.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Davis, J. C.; Ishihara, A.; Mase, K.; Ono, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Adams, J.; Brown, A. M.; Gross, A.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Berley, D.; Blaufuss, E.; Christy, B.; Ehrlich, R.; Ellsworth, R. W.; Goodman, J. A.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Roth, P.; Schmidt, T.; Straszheim, T.; Sullivan, G. W.; Turcan, D.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Beatty, J. J.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Clevermann, F.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Grant, D.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
[Abdou, Y.; Carson, M.; Descamps, F.; de Vries-Uiterweerd, G.; Feusels, T.; Hajismail, A.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium.
[Colnard, C.; Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.; Wolf, M.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany.
[Barwick, S. W.; Nam, J. W.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Cohen, S.; Demiroers, L.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland.
[Besson, D. Z.; Kenny, P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Griesel, T.; Koepke, L.; Kowarik, T.; Kroll, G.; Luenemann, J.; Piegsa, A.; Rothmaier, F.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[Herquet, P.; Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Bai, X.; Berghaus, P.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bai, X.; Berghaus, P.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Ahlers, M.; Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Abu-Zayyad, T.; Madsen, J.; Spiczak, G. M.; Tamburro, A.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Caballero-Mora, K. S.; Cowen, D. F.; DeYoung, T.; Foerster, M. M.; Fox, B. D.; Ha, C.; Koskinen, D. J.; Lafebre, S.; Larson, M. J.; Meszaros, P.; Rutledge, D.; Slipak, A.; Stephens, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Botner, O.; Engdegard, O.; Hallgren, A.; Miller, J.; de los Heros, C. Perez; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Auffenberg, J.; Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Kampert, K. -H.; Karg, T.; Kopper, S.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Montaruli, T.] Sezione Ist Nazl Fis Nucl, I-70124 Bari, Italy.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Alba, J. L. Bazo; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Franke, R.; Gora, D.; Han, K.; Kislat, F.; Lauer, R.; Majumdar, P.; Middell, E.; Nahnhauer, R.; Schoenwald, A.; Spiering, C.; Stoessl, A.; Tosi, D.; Walter, M.; Wischnewski, R.] DESY, D-15735 Zeuthen, Germany.
RP Grullon, S (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.
EM grullon@icecube.wisc.edu
RI Wiebusch, Christopher/G-6490-2012; Kowalski, Marek/G-5546-2012;
Tamburro, Alessio/A-5703-2013; Botner, Olga/A-9110-2013; Hallgren,
Allan/A-8963-2013; Tjus, Julia/G-8145-2012; Auffenberg, Jan/D-3954-2014;
Koskinen, David/G-3236-2014; Aguilar Sanchez, Juan Antonio/H-4467-2015;
Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011; Beatty,
James/D-9310-2011; Taavola, Henric/B-4497-2011;
OI Wiebusch, Christopher/0000-0002-6418-3008; Perez de los Heros,
Carlos/0000-0002-2084-5866; Auffenberg, Jan/0000-0002-1185-9094;
Koskinen, David/0000-0002-0514-5917; Aguilar Sanchez, Juan
Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X;
Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952;
Taavola, Henric/0000-0002-2604-2810; Buitink, Stijn/0000-0002-6177-497X;
Carson, Michael/0000-0003-0400-7819; Hubert, Daan/0000-0002-4365-865X;
Benabderrahmane, Mohamed Lotfi/0000-0003-4410-5886
FU U.S. National Science Foundation-Office of Polar Programs; U.S. National
Science Foundation-Physics Division, University of Wisconsin Alumni
Research Foundation; Grid Laboratory of Wisconsin (GLOW) grid
infrastructure at the University of Wisconsin-Madison; Open Science Grid
(OSG) grid infrastructure; U.S. Department of Energy; National Energy
Research Scientific Computing Center; Louisiana Optical Network
Initiative (LONI); National Science and Engineering Research Council of
Canada; Swedish Research Council; Swedish Polar Research Secretariat;
Swedish National Infrastructure for Computing (SNIC); Knut and Alice
Wallenberg Foundation, Sweden; German Ministry for Education and
Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Research
Department of Plasmas with Complex Interactions (Bochum), Germany; Fund
for Scientific Research (FNRS-FWO); FWO Odysseus programme; Flanders
Institute; Belgian Federal Science Policy Office (Belspo); University of
Oxford, United Kingdom; Marsden Fund, New Zealand; Japan Society for
Promotion of Science (JSPS); Swiss National Science Foundation (SNSF),
Switzerland; EU Marie Curie OIF Program; Capes Foundation; Ministry of
Education of Brazil
FX We acknowledge the support from the following agencies: U.S. National
Science Foundation-Office of Polar Programs, U.S. National Science
Foundation-Physics Division, University of Wisconsin Alumni Research
Foundation, the Grid Laboratory of Wisconsin (GLOW) grid infrastructure
at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid
infrastructure; U.S. Department of Energy, and National Energy Research
Scientific Computing Center, the Louisiana Optical Network Initiative
(LONI) grid computing resources; National Science and Engineering
Research Council of Canada; Swedish Research Council, Swedish Polar
Research Secretariat, Swedish National Infrastructure for Computing
(SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German
Ministry for Education and Research (BMBF), Deutsche
Forschungsgemeinschaft (DFG), Research Department of Plasmas with
Complex Interactions (Bochum), Germany; Fund for Scientific Research
(FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage
scientific and technological research in industry (IWT), Belgian Federal
Science Policy Office (Belspo); University of Oxford, United Kingdom;
Marsden Fund, New Zealand; Japan Society for Promotion of Science
(JSPS); the Swiss National Science Foundation (SNSF), Switzerland; A.
Gross acknowledges support by the EU Marie Curie OIF Program; J. P.
Rodrigues acknowledges support by the Capes Foundation, Ministry of
Education of Brazil.
NR 48
TC 82
Z9 83
U1 2
U2 9
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 OCT 3
PY 2011
VL 84
IS 8
AR 082001
DI 10.1103/PhysRevD.84.082001
PG 20
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 841PG
UT WOS:000296523900001
ER
PT J
AU Abbasi, R
Abdou, Y
Abu-Zayyad, T
Adams, J
Aguilar, JA
Ahlers, M
Andeen, K
Auffenberg, J
Bai, X
Baker, M
Barwick, SW
Bay, R
Alba, JLB
Beattie, K
Beatty, JJ
Bechet, S
Becker, JK
Becker, KH
Benabderrahmane, ML
BenZvi, S
Berdermann, J
Berghaus, P
Berley, D
Bernardini, E
Bertrand, D
Besson, DZ
Bindig, D
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohm, C
Bose, D
Boser, S
Botner, O
Braun, J
Brown, AM
Buitink, S
Carson, M
Chirkin, D
Christy, B
Clem, J
Clevermann, F
Cohen, S
Colnard, C
Cowen, DF
D'Agostino, MV
Danninger, M
Daughhetee, J
Davis, JC
De Clercq, C
Demirors, L
Depaepe, O
Descamps, F
Desiati, P
de Vries-Uiterweerd, G
DeYoung, T
Diaz-Velez, JC
Dierckxsens, M
Dreyer, J
Dumm, JP
Ehrlich, R
Eisch, J
Ellsworth, RW
Engdegard, O
Euler, S
Evenson, PA
Fadiran, O
Fazely, AR
Fedynitch, A
Feusels, T
Filimonov, K
Finley, C
Fischer-Wasels, T
Foerster, MM
Fox, BD
Franckowiak, A
Franke, R
Gaisser, TK
Gallagher, J
Geisler, M
Gerhardt, L
Gladstone, L
Glusenkamp, T
Goldschmidt, A
Goodman, JA
Grant, D
Griesel, T
Gross, A
Grullon, S
Gurtner, M
Ha, C
Hallgren, A
Halzen, F
Han, K
Hanson, K
Heinen, D
Helbing, K
Herquet, P
Hickford, S
Hill, GC
Hoffman, KD
Homeier, A
Hoshina, K
Hubert, D
Huelsnitz, W
Hulss, JP
Hulth, PO
Hultqvist, K
Hussain, S
Ishihara, A
Jacobsen, J
Japaridze, GS
Johansson, H
Joseph, JM
Kampert, KH
Kappes, A
Karg, T
Karle, A
Kelley, JL
Kemming, N
Kenny, P
Kiryluk, J
Kislat, F
Klein, SR
Kohne, JH
Kohnen, G
Kolanoski, H
Kopke, L
Kopper, S
Koskinen, DJ
Kowalski, M
Kowarik, T
Krasberg, M
Krings, T
Kroll, G
Kuehn, K
Kuwabara, T
Labare, M
Lafebre, S
Laihem, K
Landsman, H
Larson, MJ
Lauer, R
Lehmann, R
Lunemann, J
Madsen, J
Majumdar, P
Marotta, A
Maruyama, R
Mase, K
Matis, HS
Meagher, K
Merck, M
Meszaros, P
Meures, T
Middell, E
Milke, N
Miller, J
Montaruli, T
Morse, R
Movit, SM
Nahnhauer, R
Nam, JW
Naumann, U
Niessen, P
Nygren, DR
Odrowski, S
Olivas, A
Olivo, M
O'Murchadha, A
Ono, M
Panknin, S
Paul, L
de los Heros, CP
Petrovic, J
Piegsa, A
Pieloth, D
Porrata, R
Posselt, J
Price, PB
Prikockis, M
Przybylski, GT
Rawlins, K
Redl, P
Resconi, E
Rhode, W
Ribordy, M
Rizzo, A
Rodrigues, JP
Roth, P
Rothmaier, F
Rott, C
Ruhe, T
Rutledge, D
Ruzybayev, B
Ryckbosch, D
Sander, HG
Santander, M
Sarkar, S
Schatto, K
Schmidt, T
Schoenwald, A
Schukraft, A
Schultes, A
Schulz, O
Schunck, M
Seckel, D
Semburg, B
Seo, SH
Sestayo, Y
Seunarine, S
Silvestri, A
Slipak, A
Spiczak, GM
Spiering, C
Stamatikos, M
Stanev, T
Stephens, G
Stezelberger, T
Stokstad, RG
Stoyanov, S
Strahler, EA
Straszheim, T
Sullivan, GW
Swillens, Q
Taavola, H
Taboada, I
Tamburro, A
Tarasova, O
Tepe, A
Ter-Antonyan, S
Tilav, S
Toale, PA
Toscano, S
Tosi, D
Turcan, D
van Eijndhoven, N
Vandenbroucke, J
Van Overloop, A
van Santen, J
Vehring, M
Voge, M
Voigt, B
Walck, C
Waldenmaier, T
Wallraff, M
Walter, M
Weaver, C
Wendt, C
Westerhoff, S
Whitehorn, N
Wiebe, K
Wiebusch, CH
Williams, DR
Wischnewski, R
Wissing, H
Wolf, M
Woschnagg, K
Xu, C
Xu, XW
Yodh, G
Yoshida, S
Zarzhitsky, P
AF Abbasi, R.
Abdou, Y.
Abu-Zayyad, T.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Andeen, K.
Auffenberg, J.
Bai, X.
Baker, M.
Barwick, S. W.
Bay, R.
Alba, J. L. Bazo
Beattie, K.
Beatty, J. J.
Bechet, S.
Becker, J. K.
Becker, K-H
Benabderrahmane, M. L.
BenZvi, S.
Berdermann, J.
Berghaus, P.
Berley, D.
Bernardini, E.
Bertrand, D.
Besson, D. Z.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohm, C.
Bose, D.
Boeser, S.
Botner, O.
Braun, J.
Brown, A. M.
Buitink, S.
Carson, M.
Chirkin, D.
Christy, B.
Clem, J.
Clevermann, F.
Cohen, S.
Colnard, C.
Cowen, D. F.
D'Agostino, M. V.
Danninger, M.
Daughhetee, J.
Davis, J. C.
De Clercq, C.
Demiroers, L.
Depaepe, O.
Descamps, F.
Desiati, P.
de Vries-Uiterweerd, G.
DeYoung, T.
Diaz-Velez, J. C.
Dierckxsens, M.
Dreyer, J.
Dumm, J. P.
Ehrlich, R.
Eisch, J.
Ellsworth, R. W.
Engdegard, O.
Euler, S.
Evenson, P. A.
Fadiran, O.
Fazely, A. R.
Fedynitch, A.
Feusels, T.
Filimonov, K.
Finley, C.
Fischer-Wasels, T.
Foerster, M. M.
Fox, B. D.
Franckowiak, A.
Franke, R.
Gaisser, T. K.
Gallagher, J.
Geisler, M.
Gerhardt, L.
Gladstone, L.
Gluesenkamp, T.
Goldschmidt, A.
Goodman, J. A.
Grant, D.
Griesel, T.
Gross, A.
Grullon, S.
Gurtner, M.
Ha, C.
Hallgren, A.
Halzen, F.
Han, K.
Hanson, K.
Heinen, D.
Helbing, K.
Herquet, P.
Hickford, S.
Hill, G. C.
Hoffman, K. D.
Homeier, A.
Hoshina, K.
Hubert, D.
Huelsnitz, W.
Huelss, J-P
Hulth, P. O.
Hultqvist, K.
Hussain, S.
Ishihara, A.
Jacobsen, J.
Japaridze, G. S.
Johansson, H.
Joseph, J. M.
Kampert, K-H
Kappes, A.
Karg, T.
Karle, A.
Kelley, J. L.
Kemming, N.
Kenny, P.
Kiryluk, J.
Kislat, F.
Klein, S. R.
Koehne, J-H
Kohnen, G.
Kolanoski, H.
Koepke, L.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Kowarik, T.
Krasberg, M.
Krings, T.
Kroll, G.
Kuehn, K.
Kuwabara, T.
Labare, M.
Lafebre, S.
Laihem, K.
Landsman, H.
Larson, M. J.
Lauer, R.
Lehmann, R.
Luenemann, J.
Madsen, J.
Majumdar, P.
Marotta, A.
Maruyama, R.
Mase, K.
Matis, H. S.
Meagher, K.
Merck, M.
Meszaros, P.
Meures, T.
Middell, E.
Milke, N.
Miller, J.
Montaruli, T.
Morse, R.
Movit, S. M.
Nahnhauer, R.
Nam, J. W.
Naumann, U.
Niessen, P.
Nygren, D. R.
Odrowski, S.
Olivas, A.
Olivo, M.
O'Murchadha, A.
Ono, M.
Panknin, S.
Paul, L.
de los Heros, C. Perez
Petrovic, J.
Piegsa, A.
Pieloth, D.
Porrata, R.
Posselt, J.
Price, P. B.
Prikockis, M.
Przybylski, G. T.
Rawlins, K.
Redl, P.
Resconi, E.
Rhode, W.
Ribordy, M.
Rizzo, A.
Rodrigues, J. P.
Roth, P.
Rothmaier, F.
Rott, C.
Ruhe, T.
Rutledge, D.
Ruzybayev, B.
Ryckbosch, D.
Sander, H-G
Santander, M.
Sarkar, S.
Schatto, K.
Schmidt, T.
Schoenwald, A.
Schukraft, A.
Schultes, A.
Schulz, O.
Schunck, M.
Seckel, D.
Semburg, B.
Seo, S. H.
Sestayo, Y.
Seunarine, S.
Silvestri, A.
Slipak, A.
Spiczak, G. M.
Spiering, C.
Stamatikos, M.
Stanev, T.
Stephens, G.
Stezelberger, T.
Stokstad, R. G.
Stoyanov, S.
Strahler, E. A.
Straszheim, T.
Sullivan, G. W.
Swillens, Q.
Taavola, H.
Taboada, I.
Tamburro, A.
Tarasova, O.
Tepe, A.
Ter-Antonyan, S.
Tilav, S.
Toale, P. A.
Toscano, S.
Tosi, D.
Turcan, D.
van Eijndhoven, N.
Vandenbroucke, J.
Van Overloop, A.
van Santen, J.
Vehring, M.
Voge, M.
Voigt, B.
Walck, C.
Waldenmaier, T.
Wallraff, M.
Walter, M.
Weaver, Ch.
Wendt, C.
Westerhoff, S.
Whitehorn, N.
Wiebe, K.
Wiebusch, C. H.
Williams, D. R.
Wischnewski, R.
Wissing, H.
Wolf, M.
Woschnagg, K.
Xu, C.
Xu, X. W.
Yodh, G.
Yoshida, S.
Zarzhitsky, P.
CA IceCube Collaboration
TI First search for atmospheric and extraterrestrial neutrino-induced
cascades with the IceCube detector
SO PHYSICAL REVIEW D
LA English
DT Article
ID HIGH-ENERGY NEUTRINOS; AMANDA-II; SCATTERING; SELECTION; SPECTRUM; ICE
AB We report on the first search for atmospheric and for diffuse astrophysical neutrino-induced showers (cascades) in the IceCube detector using 257 days of data collected in the year 2007-2008 with 22 strings active. A total of 14 events with energies above 16 TeV remained after event selections in the diffuse analysis, with an expected total background contribution of 8.3 +/- 3.6. At 90% confidence we set an upper limit of E-2 Phi(90%CL) < 3.6 x 10(-7) GeV.cm(-2).s(-1).sr(-1) on the diffuse flux of neutrinos of all flavors in the energy range between 24 TeV and 6.6 PeV assuming that Phi proportional to E-2 and the flavor composition of the nu(e):nu(mu):nu(tau) flux is 1:1:1 at the Earth. The atmospheric neutrino analysis was optimized for lower energies. A total of 12 events were observed with energies above 5 TeV. The observed number of events is consistent with the expected background, within the uncertainties.
C1 [Beattie, K.; Buitink, S.; Gerhardt, L.; Goldschmidt, A.; Joseph, J. M.; Kiryluk, J.; Klein, S. R.; Matis, H. S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Geisler, M.; Gluesenkamp, T.; Heinen, D.; Huelss, J-P; Krings, T.; Laihem, K.; Meures, T.; Paul, L.; Schukraft, A.; Schunck, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
[Williams, D. R.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Rawlins, K.] Univ Alaska, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Fadiran, O.; Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Bay, R.; D'Agostino, M. V.; Filimonov, K.; Gerhardt, L.; Kiryluk, J.; Klein, S. R.; Porrata, R.; Price, P. B.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Kappes, A.; Kemming, N.; Kolanoski, H.; Lehmann, R.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Becker, J. K.; Dreyer, J.; Fedynitch, A.; Olivo, M.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Boeser, S.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
[Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados.
[Bechet, S.; Bertrand, D.; Dierckxsens, M.; Hanson, K.; Marotta, A.; Petrovic, J.; Swillens, Q.] Univ Libre Bruxelles, Fac Sci, B-1050 Brussels, Belgium.
[Bose, D.; De Clercq, C.; Depaepe, O.; Hubert, D.; Labare, M.; Rizzo, A.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Ishihara, A.; Mase, K.; Ono, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Adams, J.; Brown, A. M.; Gross, A.; Han, K.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Berley, D.; Blaufuss, E.; Christy, B.; Ehrlich, R.; Ellsworth, R. W.; Goodman, J. A.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Roth, P.; Schmidt, T.; Straszheim, T.; Sullivan, G. W.; Turcan, D.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Beatty, J. J.; Davis, J. C.; Kuehn, K.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Kuehn, K.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Clevermann, F.; Koehne, J-H; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Grant, D.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
[Abdou, Y.; Carson, M.; Descamps, F.; de Vries-Uiterweerd, G.; Feusels, T.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Subatom & Radiat Phys, B-9000 Ghent, Belgium.
[Colnard, C.; Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.; Voge, M.; Wolf, M.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany.
[Barwick, S. W.; Nam, J. W.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Cohen, S.; Demiroers, L.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland.
[Besson, D. Z.; Kenny, P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Abbasi, R.; Aguilar, J. A.; Andeen, K.; Baker, M.; BenZvi, S.; Berghaus, P.; Braun, J.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hoshina, K.; Jacobsen, J.; Karle, A.; Kelley, J. L.; Krasberg, M.; Landsman, H.; Maruyama, R.; Merck, M.; Montaruli, T.; Morse, R.; O'Murchadha, A.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Griesel, T.; Koepke, L.; Kowarik, T.; Kroll, G.; Luenemann, J.; Piegsa, A.; Rothmaier, F.; Sander, H-G; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[Herquet, P.; Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Bai, X.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bai, X.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Ahlers, M.; Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Abu-Zayyad, T.; Madsen, J.; Spiczak, G. M.; Tamburro, A.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Cowen, D. F.; DeYoung, T.; Foerster, M. M.; Fox, B. D.; Ha, C.; Koskinen, D. J.; Lafebre, S.; Larson, M. J.; Meszaros, P.; Prikockis, M.; Rutledge, D.; Slipak, A.; Stephens, G.; Toale, P. A.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Botner, O.; Engdegard, O.; Hallgren, A.; Miller, J.; Olivo, M.; de los Heros, C. Perez; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Auffenberg, J.; Becker, K-H; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Kampert, K-H; Karg, T.; Kopper, S.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Alba, J. L. Bazo; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Franke, R.; Kislat, F.; Lauer, R.; Majumdar, P.; Middell, E.; Nahnhauer, R.; Schoenwald, A.; Spiering, C.; Tarasova, O.; Tosi, D.; Voigt, B.; Walter, M.; Wischnewski, R.] DESY, D-15735 Zeuthen, Germany.
[Montaruli, T.] Univ Bari, Dipartmento Fis, Sez INFN, I-70126 Bari, Italy.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kiryluk, J (reprint author), Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
EM JKiryluk@lbl.gov
RI Taavola, Henric/B-4497-2011; Tamburro, Alessio/A-5703-2013; Botner,
Olga/A-9110-2013; Hallgren, Allan/A-8963-2013; Tjus, Julia/G-8145-2012;
Auffenberg, Jan/D-3954-2014; Koskinen, David/G-3236-2014; Aguilar
Sanchez, Juan Antonio/H-4467-2015; Maruyama, Reina/A-1064-2013; Sarkar,
Subir/G-5978-2011; Beatty, James/D-9310-2011; Wiebusch,
Christopher/G-6490-2012; Kowalski, Marek/G-5546-2012
OI Ter-Antonyan, Samvel/0000-0002-5788-1369; Schukraft,
Anne/0000-0002-9112-5479; Perez de los Heros,
Carlos/0000-0002-2084-5866; Taavola, Henric/0000-0002-2604-2810;
Buitink, Stijn/0000-0002-6177-497X; Carson, Michael/0000-0003-0400-7819;
Hubert, Daan/0000-0002-4365-865X; Benabderrahmane, Mohamed
Lotfi/0000-0003-4410-5886; Auffenberg, Jan/0000-0002-1185-9094;
Koskinen, David/0000-0002-0514-5917; Aguilar Sanchez, Juan
Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X;
Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952;
Actis, Oxana/0000-0001-8851-3983; Wiebusch,
Christopher/0000-0002-6418-3008;
FU U.S. National Science Foundation-Office of Polar Programs; U.S. National
Science Foundation-Physics Division; University of Wisconsin Alumni
Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid
infrastructure at the University of Wisconsin-Madison; Open Science Grid
(OSG) grid infrastructure; U.S. Department of Energy, and National
Energy Research Scientific Computing Center; Louisiana Optical Network
Initiative (LONI) grid computing resources; National Science and
Engineering Research Council of Canada; Swedish Research Council;
Swedish Polar Research Secretariat; Swedish National Infrastructure for
Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German
Ministry for Education and Research (BMBF); Deutsche
Forschungsgemeinschaft (DFG); Research Department of Plasmas with
Complex Interactions (Bochum), Germany; Fund for Scientific Research
(FNRS-FWO); FWO; Flanders Institute to encourage scientific and
technological research in industry (IWT); Belgian Federal Science Policy
Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New
Zealand; Japan Society for Promotion of Science (JSPS); Swiss National
Science Foundation (SNSF), Switzerland; EU; Capes Foundation, Ministry
of Education of Brazil
FX We acknowledge the support from the following agencies: U.S. National
Science Foundation-Office of Polar Programs, U.S. National Science
Foundation-Physics Division, University of Wisconsin Alumni Research
Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure
at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid
infrastructure; U.S. Department of Energy, and National Energy Research
Scientific Computing Center, the Louisiana Optical Network Initiative
(LONI) grid computing resources; National Science and Engineering
Research Council of Canada; Swedish Research Council, Swedish Polar
Research Secretariat, Swedish National Infrastructure for Computing
(SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German
Ministry for Education and Research (BMBF), Deutsche
Forschungsgemeinschaft (DFG), Research Department of Plasmas with
Complex Interactions (Bochum), Germany; Fund for Scientific Research
(FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage
scientific and technological research in industry (IWT), Belgian Federal
Science Policy Office (Belspo); University of Oxford, United Kingdom;
Marsden Fund, New Zealand; Japan Society for Promotion of Science
(JSPS); the Swiss National Science Foundation (SNSF), Switzerland; A.
Gross acknowledges support by the EU Marie Curie OIF Program; J. P.
Rodrigues acknowledges support by the Capes Foundation, Ministry of
Education of Brazil.
NR 53
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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 OCT 3
PY 2011
VL 84
IS 7
AR 072001
DI 10.1103/PhysRevD.84.072001
PG 15
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 828YL
UT WOS:000295541100001
ER
PT J
AU Chen, YH
Miller, JR
Francis, JA
Russell, GL
AF Chen, Yonghua
Miller, James R.
Francis, Jennifer A.
Russell, Gary L.
TI Projected regime shift in Arctic cloud and water vapor feedbacks
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE Arctic; feedback; sensitivity; clouds; water vapor; radiation
ID CLIMATE-CHANGE; RIVER FLOW; MODEL; OCEAN
AB The Arctic climate is changing faster than any other large-scale region on Earth. A variety of positive feedback mechanisms are responsible for the amplification, most of which are linked with changes in snow and ice cover, surface temperature (T-s), atmospheric water vapor (WV), and cloud properties. As greenhouse gases continue to accumulate in the atmosphere, air temperature and water vapor content also increase, leading to a warmer surface and ice loss, which further enhance evaporation and WV. Many details of these interrelated feedbacks are poorly understood, yet are essential for understanding the pace and regional variations in future Arctic change. We use a global climate model (Goddard Institute for Space Studies, Atmosphere-Ocean Model) to examine several components of these feedbacks, how they vary by season, and how they are projected to change through the 21st century. One positive feedback begins with an increase in T-s that produces an increase in WV, which in turn increases the downward longwave flux (DLF) and T-s, leading to further evaporation. Another associates the expected increases in cloud cover and optical thickness with increasing DLF and Ts. We examine the sensitivities between DLF and other climate variables in these feedbacks and find that they are strongest in the non-summer seasons, leading to the largest amplification in Ts during these months. Later in the 21st century, however, DLF becomes less sensitive to changes in WV and cloud optical thickness, as they cause the atmosphere to emit longwave radiation more nearly as a black body. This regime shift in sensitivity implies that the amplified pace of Arctic change relative to the northern hemisphere could relax in the future.
C1 [Chen, Yonghua] Columbia Univ, New York, NY 10027 USA.
[Chen, Yonghua] Inst Space Studies, New York, NY USA.
[Miller, James R.; Francis, Jennifer A.] Rutgers State Univ, Dept Marine & Coastal Sci, New Brunswick, NJ 08901 USA.
[Russell, Gary L.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Chen, YH (reprint author), Columbia Univ, New York, NY 10027 USA.
EM yc2268@columbia.edu
FU NASA [NAG5-11720]; New Jersey Agricultural Experiment Station; NSF/ARCSS
[0628818]
FX We would like to acknowledge support for this study from NASA grant
NAG5-11720. Partial support for James R Miller was provided by Project
#32103 of the New Jersey Agricultural Experiment Station, and for J
Francis from NSF/ARCSS grant 0628818. The ERA-40 reanalysis data were
obtained from the ECWMF data server. We are also grateful to Elias
Hunter for providing some of the ERA-40 data. The authors thank two
reviewers for their comments that improved this study.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD OCT-DEC
PY 2011
VL 6
IS 4
AR 044007
DI 10.1088/1748-9326/6/4/044007
PG 8
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 870MX
UT WOS:000298674700012
ER
PT J
AU Gopalakrishnan, R
Bala, G
Jayaraman, M
Cao, L
Nemani, R
Ravindranath, NH
AF Gopalakrishnan, Ranjith
Bala, Govindsamy
Jayaraman, Mathangi
Cao, Long
Nemani, Ramakrishna
Ravindranath, N. H.
TI Sensitivity of terrestrial water and energy budgets to CO2-physiological
forcing: an investigation using an offline land model
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE CO2-physiological effect; CO2-fertilization; canopy transpiration; water
cycle; runoff; climate change
ID STOMATAL CONDUCTANCE MODEL; CARBON-DIOXIDE; ATMOSPHERIC CO2; RISING CO2;
CLIMATE; PHOTOSYNTHESIS; LEAF; EVAPOTRANSPIRATION; TRANSPIRATION; RUNOFF
AB Increasing concentrations of atmospheric carbon dioxide (CO2) influence climate by suppressing canopy transpiration in addition to its well- known greenhouse gas effect. The decrease in plant transpiration is due to changes in plant physiology (reduced opening of plant stomata). Here, we quantify such changes in water flux for various levels of CO2 concentrations using the National Center for Atmospheric Research's (NCAR) Community Land Model. We find that photosynthesis saturates after 800 ppmv (parts per million, by volume) in this model. However, unlike photosynthesis, canopy transpiration continues to decline at about 5.1% per 100 ppmv increase in CO2 levels. We also find that the associated reduction in latent heat flux is primarily compensated by increased sensible heat flux. The continued decline in canopy transpiration and subsequent increase in sensible heat flux at elevated CO2 levels implies that incremental warming associated with the physiological effect of CO2 will not abate at higher CO2 concentrations, indicating important consequences for the global water and carbon cycles from anthropogenic CO2 emissions.
C1 [Gopalakrishnan, Ranjith; Jayaraman, Mathangi; Ravindranath, N. H.] Indian Inst Sci, Ctr Sustainable Technol, Bangalore 560012, Karnataka, India.
[Bala, Govindsamy] Indian Inst Sci, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India.
[Bala, Govindsamy] Indian Inst Sci, Divecha Ctr Climate Change, Bangalore 560012, Karnataka, India.
[Cao, Long] Carnegie Inst, Dept Global Ecol, Stanford, CA 94305 USA.
[Nemani, Ramakrishna] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Gopalakrishnan, R (reprint author), Indian Inst Sci, Ctr Sustainable Technol, Bangalore 560012, Karnataka, India.
EM ranjith.gopalakrishnan@gmail.com
FU Department of Science and Technology; Royal Norwegian Embassy
FX This research is funded by Department of Science and Technology grant
DST0948, the project 'Impact of climate change on tropical forest
ecosystems and biodiversity in India' funded by the Royal Norwegian
Embassy in collaboration with CICERO, Oslo and the NATCOM project.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD OCT-DEC
PY 2011
VL 6
IS 4
AR 044013
DI 10.1088/1748-9326/6/4/044013
PG 7
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 870MX
UT WOS:000298674700018
ER
PT J
AU Kharuk, VI
Ranson, KJ
Dvinskaya, ML
Im, ST
AF Kharuk, Viacheslav I.
Ranson, Kenneth J.
Dvinskaya, Maria L.
Im, Sergey T.
TI Wildfires in northern Siberian larch dominated communities
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE wildfires; larch forests; fire return interval; climate change
ID BOREAL FOREST; FIRE REGIMES; USA; FREQUENCY; LANDSCAPE; TRENDS
AB The fire history of the northern larch forests within the permafrost zone in a portion of northern Siberia (similar to 66 degrees N, 100 degrees E) was studied. Since there is little to no human activity in this area, fires within the study area were mostly caused by lightning. Fire return intervals (FRI) were estimated on the basis of burn marks on tree stems and dates of tree natality. FRI values varied from 130 to 350 yr with a 200 +/- 50 yr mean. For southerly larch dominated communities, FRI was found to be shorter (77 +/- 20 yr at similar to 61 degrees N, and 82 +/- 7 at 64 degrees N), and it was longer at the northern boundary (similar to 71 degrees) of larch stands (320 +/- 50 yr). During the Little Ice Age period in the 16th-18th centuries, FRI was approximately twice as long those as recorded in this study. Fire caused changes in the soil including increases in soil drainage and permafrost thawing depth, and a radial growth increase to about twice the background value (with more than six times observed in extreme cases). This effect may simulate the predicted warming impact on the larch growth in the permafrost zone.
C1 [Kharuk, Viacheslav I.; Dvinskaya, Maria L.; Im, Sergey T.] VN Sukachev Inst Forest, Krasnoyarsk 660036, Russia.
[Ranson, Kenneth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kharuk, VI (reprint author), VN Sukachev Inst Forest, Krasnoyarsk 660036, Russia.
EM kharuk@ksc.krasn.ru
RI Ranson, Kenneth/G-2446-2012; Im, Sergei/J-2736-2016
OI Ranson, Kenneth/0000-0003-3806-7270; Im, Sergei/0000-0002-5794-7938
FU Siberian Branch of the Russian Academy of Sciences [27.33]; NASA HQ
FX This work was supported by the Siberian Branch of the Russian Academy of
Sciences Project No. 27.33 and NASA HQ Terrestrial Ecology Program.
NR 32
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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 OCT-DEC
PY 2011
VL 6
IS 4
AR 045208
DI 10.1088/1748-9326/6/4/045208
PG 6
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 870MX
UT WOS:000298674700046
ER
PT J
AU Mitchard, ETA
Saatchi, SS
Lewis, SL
Feldpausch, TR
Gerard, FF
Woodhouse, IH
Meir, P
AF Mitchard, E. T. A.
Saatchi, S. S.
Lewis, S. L.
Feldpausch, T. R.
Gerard, F. F.
Woodhouse, I. H.
Meir, P.
TI Comment on 'A first map of tropical Africa's above-ground biomass
derived from satellite imagery'
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Editorial Material
DE aboveground biomass; Africa; AGB; carbon; GLAS; LiDAR; MODIS; random
forest; regression tree; remote sensing; savanna; tropical forest
ID FORESTS
AB We present a critical evaluation of the above-ground biomass (AGB) map of Africa published in this journal by Baccini et al (2008 Environ. Res. Lett. 3 045011). We first test their map against an independent dataset of 1154 scientific inventory plots from 16 African countries, and find only weak correspondence between our field plots and the AGB value given for the surrounding 1 km pixel by Baccini et al. Separating our field data using a continental landcover classification suggests that the Baccini et al map underestimates the AGB of forests and woodlands, while overestimating the AGB of savannas and grasslands. Secondly, we compare their map to 216 000 x 0.25 ha spaceborne LiDAR footprints. A comparison between Lorey's height (basal-area-weighted average height) derived from the LiDAR data for 1 km pixels containing at least five LiDAR footprints again does not support the hypothesis that the Baccini et al map is accurate, and suggests that it significantly underestimates the AGB of higher AGB areas. We conclude that this is due to the unsuitability of some of the field data used by Baccini et al to create their map, and overfitting in their model, resulting in low accuracies outside the small areas from which their field data are drawn.
C1 [Mitchard, E. T. A.; Woodhouse, I. H.; Meir, P.] Univ Edinburgh, Sch Geosci, Edinburgh EH8 9XP, Midlothian, Scotland.
[Saatchi, S. S.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
[Lewis, S. L.; Feldpausch, T. R.] Univ Leeds, Sch Geog, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England.
[Gerard, F. F.] Ctr Ecol & Hydrol, Wallingford OX10 8BB, Oxon, England.
RP Mitchard, ETA (reprint author), Univ Edinburgh, Sch Geosci, Drummond St, Edinburgh EH8 9XP, Midlothian, Scotland.
EM edward.mitchard@ed.ac.uk
RI Gerard, France/D-8428-2012; Lewis, Simon/I-9025-2012; Meir,
Patrick/J-8344-2012; Woodhouse, Iain/B-1790-2009
OI Feldpausch, Ted R./0000-0002-6631-7962; Mitchard,
Edward/0000-0002-5690-4055; Lewis, Simon/0000-0002-8066-6851;
NR 17
TC 16
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U1 9
U2 46
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 OCT-DEC
PY 2011
VL 6
IS 4
AR 049001
DI 10.1088/1748-9326/6/4/049001
PG 6
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 870MX
UT WOS:000298674700066
ER
PT J
AU Peng, SS
Chen, AP
Xu, L
Cao, CX
Fang, JY
Myneni, RB
Pinzon, JE
Tucker, CJ
Piao, SL
AF Peng, Shushi
Chen, Anping
Xu, Liang
Cao, Chunxiang
Fang, Jingyun
Myneni, Ranga B.
Pinzon, Jorge E.
Tucker, Compton J.
Piao, Shilong
TI Recent change of vegetation growth trend in China
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE climate change; NDVI; vegetation growth; drought; grassland; desert;
vegetation greening; vegetation browning; turning point; China
ID NET ECOSYSTEM EXCHANGE; INTERANNUAL VARIATIONS; CLIMATE-CHANGE; BOREAL
FOREST; NDVI DATA; SATELLITE; INCREASE; INDEX
AB Using satellite-derived normalized difference vegetation index (NDVI) data, several previous studies have indicated that vegetation growth significantly increased in most areas of China during the period 1982-99. In this letter, we extended the study period to 2010. We found that at the national scale the growing season (April-October) NDVI significantly increased by 0.0007 yr(-1) from 1982 to 2010, but the increasing trend in NDVI over the last decade decreased in comparison to that of the 1982-99 period. The trends in NDVI show significant seasonal and spatial variances. The increasing trend in April and May (AM) NDVI (0.0013 yr(-1)) is larger than those in June, July and August (JJA) (0.0003 yr(-1)) and September and October (SO) (0.0008 yr(-1)). This relatively small increasing trend of JJA NDVI during 1982-2010 compared with that during 1982-99 (0.0012 yr(-1)) (Piao et al 2003 J. Geophys. Res.-Atmos. 108 4401) implies a change in the JJA vegetation growth trend, which significantly turned from increasing (0.0039 yr(-1)) to slightly decreasing (0 : 0002 yr(-1)) in 1988. Regarding the spatial pattern of changes in NDVI, the growing season NDVI increased (over 0.0020 yr(-1)) from 1982 to 2010 in southern China, while its change was close to zero in northern China, as a result of a significant changing trend reversal that occurred in the 1990s and early 2000s. In northern China, the growing season NDVI significantly increased before the 1990s as a result of warming and enhanced precipitation, but decreased after the 1990s due to drought stress strengthened by warming and reduced precipitation. Our results also show that the responses of vegetation growth to climate change vary across different seasons and ecosystems.
C1 [Peng, Shushi; Fang, Jingyun; Piao, Shilong] Peking Univ, Coll Urban & Environm Sci, Beijing 100871, Peoples R China.
[Chen, Anping] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA.
[Xu, Liang; Myneni, Ranga B.] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA.
[Cao, Chunxiang] Chinese Acad Sci, Inst Remote Sensing Applicat, Beijing, Peoples R China.
[Pinzon, Jorge E.; Tucker, Compton J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Peng, SS (reprint author), Peking Univ, Coll Urban & Environm Sci, Beijing 100871, Peoples R China.
EM slpiao@pku.edu.cn
RI Xu, Liang/D-1247-2013; Peng, Shushi/J-4779-2014; Myneni,
Ranga/F-5129-2012; Chen, Anping/H-9960-2014
OI Peng, Shushi/0000-0001-5098-726X;
FU National Natural Science Foundation of China [41125004, 30970511];
Foundation for Sino-EU research cooperation of the Ministry of Science
and Technology of China [1003]; EU [242316]; Foundation for the Author
of National Excellent Doctoral Dissertation of PR China [FANEDD-200737];
National Basic Research Program of China [2010CB950601]
FX This study was supported by the National Natural Science Foundation of
China (grants 41125004 and 30970511), Foundation for Sino-EU research
cooperation of the Ministry of Science and Technology of China (1003),
CARBONES EU FP7 foundation (242316), Foundation for the Author of
National Excellent Doctoral Dissertation of PR China (FANEDD-200737) and
National Basic Research Program of China (Grant No. 2010CB950601).
NR 40
TC 62
Z9 74
U1 11
U2 94
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 OCT-DEC
PY 2011
VL 6
IS 4
AR 044027
DI 10.1088/1748-9326/6/4/044027
PG 13
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 870MX
UT WOS:000298674700032
ER
PT J
AU Shen, SH
Leptoukh, GG
AF Shen, Suhung
Leptoukh, Gregory G.
TI Estimation of surface air temperature over central and eastern Eurasia
from MODIS land surface temperature
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE surface air temperature; land surface temperature; remote sensing; land
cover types
AB Surface air temperature (T(a)) is a critical variable in the energy and water cycle of the Earth-atmosphere system and is a key input element for hydrology and land surface models. This is a preliminary study to evaluate estimation of T(a) from satellite remotely sensed land surface temperature (T(s)) by using MODIS-Terra data over two Eurasia regions: northern China and fUSSR. High correlations are observed in both regions between station-measured T(a) and MODIS T(s). The relationships between the maximum T(a) and daytime T(s) depend significantly on land cover types, but the minimum T(a) and nighttime T(s) have little dependence on the land cover types. The largest difference between maximum T(a) and daytime T(s) appears over the barren and sparsely vegetated area during the summer time. Using a linear regression method, the daily maximum T(a) were estimated from 1 km resolution MODIS T(s) under clear-sky conditions with coefficients calculated based on land cover types, while the minimum T(a) were estimated without considering land cover types. The uncertainty, mean absolute error (MAE), of the estimated maximum T(a) varies from 2.4 degrees C over closed shrublands to 3.2 degrees C over grasslands, and the MAE of the estimated minimum T(a) is about 3.0 degrees C.
C1 [Shen, Suhung; Leptoukh, Gregory G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Shen, Suhung] George Mason Univ, Fairfax, VA 22030 USA.
RP Shen, SH (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Suhung.shen@nasa.gov
FU NASA ROSES [NNH08ZD-A001N-LCLUC]
FX This work was supported by NASA ROSES 2008 NNH08ZD-A001N-LCLUC. The
fUSSR station data are from NOAA NCDC provided by Dr Pavel Y Groisman.
The authors are grateful to the NASA GES DISC S4PA team for
preprocessing the data used in this research. Part of the visualization
and initial analysis in this study was conducted by using the NASA
Giovanni online data system [21, 22].
NR 22
TC 20
Z9 20
U1 7
U2 38
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 OCT-DEC
PY 2011
VL 6
IS 4
AR 045206
DI 10.1088/1748-9326/6/4/045206
PG 8
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 870MX
UT WOS:000298674700044
ER
PT J
AU Tchebakova, NM
Parfenova, EI
Lysanova, GI
Soja, AJ
AF Tchebakova, N. M.
Parfenova, E. I.
Lysanova, G. I.
Soja, A. J.
TI Agroclimatic potential across central Siberia in an altered twenty-first
century
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE climate warming; central Siberia; agriculture; crop range and production
AB Humans have traditionally cultivated steppe and forest-steppe on fertile soils for agriculture. Forests are predicted to shift northwards in a warmer climate and are likely to be replaced by forest-steppe and steppe ecosystems. We analyzed potential climate change impacts on agriculture in south-central Siberia believing that agriculture in traditionally cold Siberia may benefit from warming. Simple models determining crop range and regression models determining crop yields were constructed and applied to climate change scenarios for various time frames: pre-1960, 1960-90 and 1990-2010 using historic data and data taken from 2020 and 2080 HadCM3 B1 and A2 scenarios. From 50 to 85% of central Siberia is predicted to be climatically suitable for agriculture by the end of the century, and only soil potential would limit crop advance and expansion to the north. Crop production could increase twofold. Future Siberian climatic resources could provide the potential for a great variety of crops to grow that previously did not exist on these lands. Traditional Siberian crops could gradually shift as far as 500 km northwards (about 50-70 km/decade) within suitable soil conditions, and new crops nonexistent today may be introduced in the dry south that would necessitate irrigation. Agriculture in central Siberia would likely benefit from climate warming. Adaptation measures would sustain and promote food security in a warmer Siberia.
C1 [Tchebakova, N. M.; Parfenova, E. I.] Russian Acad Sci, Siberian Branch, VN Sukachev Inst Forest, Krasnoyarsk 660036, Russia.
[Lysanova, G. I.] Russian Acad Sci, Siberian Branch, Inst Geog, Irkutsk, Russia.
[Soja, A. J.] NASA, Langley Res Ctr, NIA, Hampton, VA 23681 USA.
RP Tchebakova, NM (reprint author), Russian Acad Sci, Siberian Branch, VN Sukachev Inst Forest, Krasnoyarsk 660036, Russia.
EM ncheby@forest.akadem.ru; lyeti@ksc.krasn.ru; lysanova@irigs.irk.ru;
Amber.J.Soja@nasa.gov
FU NASA [NNH09ZDA001N-IDS]; Russian Foundation for Basic Research
[10-05-00941]
FX We would like to recognize the Northern Eurasian Earth Science
Partnership Initiative (NEESPI) and the NASA Land Cover Land Use Change
(LCLUC) program for providing the background that made this work
possible. We are greatly appreciative of the current support for this
work provided by the NASA InterDisciplinary Science grant
NNH09ZDA001N-IDS and the Russian Foundation for Basic Research grant
10-05-00941. We thank our two anonymous reviewers for their very helpful
comments.
NR 38
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U1 1
U2 12
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 OCT-DEC
PY 2011
VL 6
IS 4
AR 045207
DI 10.1088/1748-9326/6/4/045207
PG 11
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 870MX
UT WOS:000298674700045
ER
PT J
AU Yasunari, TJ
AF Yasunari, Teppei J.
TI What influences climate and glacier change in southwestern China?
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Editorial Material
ID HIMALAYAN GLACIERS; SPECTRAL ALBEDO; TIBETAN PLATEAU; SNOW ALBEDO;
MODEL; SENSITIVITY; IMPACT; COVER
C1 [Yasunari, Teppei J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yasunari, Teppei J.] Univ Space Res Assoc, Columbia, MD 21044 USA.
RP Yasunari, TJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM teppei.j.yasunari@nasa.gov
RI Yasunari, Teppei/E-5374-2010
OI Yasunari, Teppei/0000-0002-9896-9404
NR 24
TC 2
Z9 2
U1 1
U2 9
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 OCT-DEC
PY 2011
VL 6
IS 4
AR 041001
DI 10.1088/1748-9326/6/4/041001
PG 3
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 870MX
UT WOS:000298674700002
ER
PT J
AU Bauer, P
Auligne, T
Bell, W
Geer, A
Guidard, V
Heilliette, S
Kazumori, M
Kim, MJ
Liu, EHC
McNally, AP
Macpherson, B
Okamoto, K
Renshaw, R
Riishojgaard, LP
AF Bauer, Peter
Auligne, Thomas
Bell, William
Geer, Alan
Guidard, Vincent
Heilliette, Sylvain
Kazumori, Masahiro
Kim, Min-Jeong
Liu, Emily H. -C.
McNally, Anthony P.
Macpherson, Bruce
Okamoto, Kozo
Renshaw, Richard
Riishojgaard, Lars-Peter
TI Satellite cloud and precipitation assimilation at operational NWP
centres
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE data assimilation; satellite observations
ID NUMERICAL WEATHER PREDICTION; VARIATIONAL DATA ASSIMILATION; AFFECTED
MICROWAVE RADIANCES; DIRECT 4D-VAR ASSIMILATION; FLUX CONVECTION SCHEME;
MOIST PHYSICS SCHEMES; LARGE-SCALE MODELS; 1D+4D-VAR ASSIMILATION;
METEOROLOGICAL SERVICE; CLEARED RADIANCES
AB The status of current efforts to assimilate cloud- and precipitation-affected satellite data is summarised with special focus on infrared and microwave radiance data obtained from operational Earth observation satellites. All global centres pursue efforts to enhance infrared radiance data usage due to the limited availability of temperature observations in cloudy regions where forecast skill is estimated to strongly depend on the initial conditions. Most systems focus on the sharpening of weighting functions at cloud top providing high vertical resolution temperature increments to the analysis, mainly in areas of persistent high and low cloud cover. Microwave radiance assimilation produces impact on the deeper atmospheric moisture structures as well as cloud microphysics and, through control variable and background-error formulation, also on temperature but to lesser extent than infrared data. Examples of how the impacts of these two observation types are combined are shown for subtropical low-level cloud regimes. The overall impact of assimilating such data on forecast skill is measurably positive despite the fact that the employed assimilation systems have been constructed and optimized for clear-sky data. This leads to the conclusion that a better understanding and modelling of model processes in cloud-affected areas and data assimilation system enhancements through inclusion of moist processes and their error characterization will contribute substantially to future forecast improvement. Copyright (C) 2011 Royal Meteorological Society, Crown in the right of Canada, and British Crown copyright, the Met Office
C1 [Bauer, Peter; Bell, William; Geer, Alan; McNally, Anthony P.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
[Auligne, Thomas] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Guidard, Vincent] Meteo France, Toulouse, France.
[Heilliette, Sylvain] Environm Canada, Dorval, PQ, Canada.
[Kazumori, Masahiro; Okamoto, Kozo] Japan Meteorol Agcy, Tokyo, Japan.
[Kim, Min-Jeong] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
[Liu, Emily H. -C.] NOAA, NCEP, EMC, Camp Springs, MD USA.
[Liu, Emily H. -C.] Syst Res Grp, Colorado Springs, CO USA.
[Macpherson, Bruce; Renshaw, Richard] Met Off, Exeter, Devon, England.
[Riishojgaard, Lars-Peter] NASA, JCSDA, GMAO, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Bauer, P (reprint author), ECMWF, Shinfield Pk, Reading RG2 9AX, Berks, England.
EM peter.bauer@ecmwf.int
FU EUMETSAT Fellowship programme; Joint Center for Satellite Data
Assimilation
FX Alan Geer was funded by the EUMETSAT Fellowship programme, and Min-Jeong
Kim by the Joint Center for Satellite Data Assimilation. The authors are
grateful for the valuable comments and suggestions from two reviewers.
The work of Rob Hine on improving the figures is greatly appreciated.
NR 101
TC 36
Z9 36
U1 2
U2 14
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 OCT
PY 2011
VL 137
IS 661
SI SI
BP 1934
EP 1951
DI 10.1002/qj.905
PN B
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 866OA
UT WOS:000298389300002
ER
PT J
AU Sridhara, DM
Nakagawa, H
Cucinotta, FA
Pluth, JM
AF Sridhara, D. M.
Nakagawa, H.
Cucinotta, F. A.
Pluth, J. M.
TI Cell Type and 3-D Context Prominently Influence Response to HZE
Radiation
SO ENVIRONMENTAL AND MOLECULAR MUTAGENESIS
LA English
DT Meeting Abstract
CT 42nd Annual Meeting of the Environmental-Mutagen-Society on
Environmental Impacts on the Genome and Epigenome - Mechanisms and Risks
CY OCT 15-19, 2011
CL Montreal, CANADA
SP Environm Mutagen Soc
C1 [Sridhara, D. M.; Pluth, J. M.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Nakagawa, H.] Univ Penn, Philadelphia, PA 19104 USA.
[Cucinotta, F. A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
NR 0
TC 0
Z9 0
U1 0
U2 2
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0893-6692
J9 ENVIRON MOL MUTAGEN
JI Environ. Mol. Mutagen.
PD OCT
PY 2011
VL 52
SU 1
BP S80
EP S80
PG 1
WC Environmental Sciences; Genetics & Heredity; Toxicology
SC Environmental Sciences & Ecology; Genetics & Heredity; Toxicology
GA 860DU
UT WOS:000297929800274
ER
PT J
AU Whalen, MK
Sridharan, DM
Wilson, W
Chapell, L
Cucinotta, FA
Pluth, JM
AF Whalen, M. K.
Sridharan, D. M.
Wilson, W.
Chapell, L.
Cucinotta, F. A.
Pluth, J. M.
TI Analyzing the Relationship between Radiation-Induced Phospho-Protein
Signaling and Surrogate Cancer Endpoints Using Novel Flow-Based Assays
SO ENVIRONMENTAL AND MOLECULAR MUTAGENESIS
LA English
DT Meeting Abstract
CT 42nd Annual Meeting of the Environmental-Mutagen-Society on
Environmental Impacts on the Genome and Epigenome - Mechanisms and Risks
CY OCT 15-19, 2011
CL Montreal, CANADA
SP Environm Mutagen Soc
C1 [Whalen, M. K.; Sridharan, D. M.; Wilson, W.; Pluth, J. M.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Chapell, L.; Cucinotta, F. A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
NR 0
TC 0
Z9 0
U1 0
U2 3
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0893-6692
J9 ENVIRON MOL MUTAGEN
JI Environ. Mol. Mutagen.
PD OCT
PY 2011
VL 52
SU 1
BP S41
EP S41
PG 1
WC Environmental Sciences; Genetics & Heredity; Toxicology
SC Environmental Sciences & Ecology; Genetics & Heredity; Toxicology
GA 860DU
UT WOS:000297929800115
ER
PT J
AU Fogarty, L
Thatte, N
Tecza, M
Clarke, F
Goodsall, T
Houghton, R
Salter, G
Davies, RL
Kassin, SA
AF Fogarty, L.
Thatte, N.
Tecza, M.
Clarke, F.
Goodsall, T.
Houghton, R.
Salter, G.
Davies, R. L.
Kassin, S. A.
TI SWIFT observations of the Arp 147 ring galaxy system
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE instrumentation: spectrographs; galaxies: individual: Arp 147
ID H-II REGIONS; STAR-FORMATION; MULTIWAVELENGTH OBSERVATIONS; ABUNDANCE
ANALYSIS; MODELS; CARTWHEEL; IMAGES
AB We present observations of Arp 147, a galaxy system comprising a collisionally created ring galaxy and an early-type galaxy, using the Oxford SWIFT integral field spectrograph (IFS) at the 200-inch Hale telescope. We derive spatially resolved kinematics from the IFS data and use these to study the interaction between the two galaxies. We find the edge-to-edge expansion velocity of the ring is 225 +/- 8 km s(-1), implying an upper limit on the time-scale for the collision of 50 Myr. We also calculate that the angle of impact for the collision is between , where 0 degrees would imply a perpendicular collision. The ring galaxy is strongly star forming with the star formation likely to have been triggered by the collision between the two galaxies.
We also measure some key physical parameters in an integrated and spatially resolved manner for the ring galaxy. Using the observed B - I colours and the Ha equivalent widths, we conclude that two stellar components (a young and an old population) are required everywhere in the ring to simultaneously match both observed quantities. We are able to constrain the age range, light and mass fractions of the young star formation activity in the ring, finding a modest age range, a light fraction of less than a third, and a negligible (<1 per cent) mass fraction. We postulate that the redder colours observed in the south-east corner of the ring galaxy could correspond to the nuclear bulge of the original disc galaxy from which the ring was created, consistent with the stellar mass in the south-east quadrant being 30-50 per cent of the total. The ring appears to have been a typical disc galaxy prior to the encounter.
The ring shows electron densities consistent with typical values for star-forming H II regions. The eastern half of the ring exhibits a metallicity a factor of similar to 2 higher than the western half. The ionization parameter, measured across the ring, roughly follows the previously observed trend with metallicity.
C1 [Fogarty, L.; Thatte, N.; Tecza, M.; Clarke, F.; Goodsall, T.; Houghton, R.; Salter, G.; Davies, R. L.; Kassin, S. A.] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England.
[Goodsall, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Fogarty, L (reprint author), Univ Oxford, Subdept Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England.
EM lmrf@astro.ox.ac.uk
FU European Commission [MEXT-CT-2003-002792]; University of Oxford Physics
Department; John Fell OUP; Caltech Optical Observatories; NASA
[NAS5-26555]; NASA Office of Space Science [NNX09AFO8G]; Balliol
College, Oxford; STFC
FX The Oxford SWIFT integral field spectrograph is directly supported by a
Marie Curie Excellence Grant from the European Commission
(MEXT-CT-2003-002792, Team Leader: N. Thatte). It is also supported by
additional funds from the University of Oxford Physics Department and
the John Fell OUP Research Fund. Additional funds to host and support
SWIFT at the 200-inch Hale Telescope on Palomar are provided by Caltech
Optical Observatories.; Some of the data presented in this paper were
obtained from the Multimission Archive at the Space Telescope Science
Institute (MAST). STScI is operated by the Association of Universities
for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support
for MAST for non-HST data is provided by the NASA Office of Space
Science via grant NNX09AFO8G and by other grants and contracts.; L.
Fogarty would like to thank Professor M. Livio(STScI) for interesting
discussions regarding the ring geometry, and acknowledge the generous
support of the Foley-Bejar Scholarship through Balliol College, Oxford
and the support of the STFC.
NR 40
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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 OCT
PY 2011
VL 417
IS 2
BP 835
EP 844
DI 10.1111/j.1365-2966.2011.19066.x
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848HR
UT WOS:000297043000003
ER
PT J
AU Nemec, JM
Smolec, R
Benko, JM
Moskalik, P
Kolenberg, K
Szabo, R
Kurtz, DW
Bryson, S
Guggenberger, E
Chadid, M
Jeon, YB
Kunder, A
Layden, AC
Kinemuchi, K
Kiss, LL
Poretti, E
Christensen-Dalsgaard, J
Kjeldsen, H
Caldwell, D
Ripepi, V
Derekas, A
Nuspl, J
Mullally, F
Thompson, SE
Borucki, WJ
AF Nemec, J. M.
Smolec, R.
Benko, J. M.
Moskalik, P.
Kolenberg, K.
Szabo, R.
Kurtz, D. W.
Bryson, S.
Guggenberger, E.
Chadid, M.
Jeon, Y. -B.
Kunder, A.
Layden, A. C.
Kinemuchi, K.
Kiss, L. L.
Poretti, E.
Christensen-Dalsgaard, J.
Kjeldsen, H.
Caldwell, D.
Ripepi, V.
Derekas, A.
Nuspl, J.
Mullally, F.
Thompson, S. E.
Borucki, W. J.
TI Fourier analysis of non-Blazhko ab-type RR Lyrae stars observed with the
Kepler space telescope
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; stars: abundances; stars: evolution; stars: fundamental
parameters; stars: Population II; stars: variables: RR Lyrae
ID HORIZONTAL-BRANCH STARS; GALACTIC GLOBULAR-CLUSTERS;
LARGE-MAGELLANIC-CLOUD; STELLAR EVOLUTION DATABASE; PERIOD-AMPLITUDE
RELATION; COLOR-MAGNITUDE DIAGRAM; POPULATION 2 STARS; RED GIANT BRANCH;
METAL-POOR STARS; LIGHT CURVES
AB Nineteen of the similar to 40 RR Lyr stars in the Kepler field have been identified as candidate non-Blazhko (or unmodulated) stars. In this paper we present the results of Fourier decomposition of the time-series photometry of these stars acquired during the first 417 d of operation (Q0Q5) of the Kepler telescope. Fourier parameters based on similar to 18 400 long-cadence observations per star (and similar to 150 000 short-cadence observations for FN Lyr and for AW Dra) are derived. None of the stars shows the recently discovered period-doubling effect seen in Blazhko variables; however, KIC 7021124 has been found to pulsate simultaneously in the fundamental and second overtone modes with a period ratio P2/P0 similar to 0.593 05 and is similar to the double-mode star V350 Lyr. Period change rates are derived from O - C diagrams spanning, in some cases, over 100 years; these are compared with high-precision periods derived from the Kepler data alone. Extant Fourier correlations by Kovacs, Jurcsik et al. (with minor transformations from the V to the Kp passband) have been used to derive underlying physical characteristics for all the stars. This procedure seems to be validated through comparisons of the Kepler variables with Galactic and Large Magellanic Cloud (LMC) RR Lyr stars. The most metal-poor star in the sample is NR Lyr, with [Fe/H] =-2.3 dex; and the four most metal-rich stars have [Fe/H] ranging from -0.6 to +0.1 dex. Pulsational luminosities and masses are found to be systematically smaller than L and values derived from stellar evolution models, and are favoured over the evolutionary values when periods are computed with the Warsaw linear hydrodynamics code. Finally, the Fourier parameters are compared with theoretical values derived using the Warsaw non-linear convective pulsation code.
C1 [Nemec, J. M.] Camosun Coll, Dept Phys & Astron, Victoria, BC V8P 5J2, Canada.
[Nemec, J. M.] Int Stat & Res Corp, Brentwood Bay, BC V8M 1R3, Canada.
[Smolec, R.; Kolenberg, K.; Guggenberger, E.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Benko, J. M.; Szabo, R.; Kiss, L. L.; Derekas, A.; Nuspl, J.] Hungarian Acad Sci, Konkoly Observ, H-1121 Budapest, Hungary.
[Moskalik, P.] Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Kolenberg, K.] Harvard Coll Observ, Cambridge, MA 02138 USA.
[Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst Astrophys, Preston PR1 2HE, Lancs, England.
[Bryson, S.; Kinemuchi, K.; Borucki, W. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Chadid, M.] Univ Nice Sophia Antipolis, UMR 6525, Observ Cote Azur, F-06108 Nice 02, France.
[Jeon, Y. -B.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Kunder, A.] Cerro Tololo Interamer Observ, La Serena, Chile.
[Layden, A. C.] Bowling Green State Univ, Dept Phys & Astron, Bowling Green, OH 43403 USA.
[Poretti, E.] Osserv Astron Brera, I-23807 Merate, Italy.
[Christensen-Dalsgaard, J.; Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Caldwell, D.; Mullally, F.; Thompson, S. E.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94025 USA.
[Ripepi, V.] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy.
RP Nemec, JM (reprint author), Camosun Coll, Dept Phys & Astron, Victoria, BC V8P 5J2, Canada.
EM nemec@camosun.bc.ca
RI Smolec, Radoslaw/F-1435-2013; Caldwell, Douglas/L-7911-2014; Derekas,
Aliz/G-2091-2016;
OI Smolec, Radoslaw/0000-0001-7217-4884; Caldwell,
Douglas/0000-0003-1963-9616; Derekas, Aliz/0000-0002-6526-9444; Kunder,
Andrea/0000-0002-2808-1370; Poretti, Ennio/0000-0003-1200-0473; Benko,
Jozsef/0000-0003-3851-6603; Szabo, Robert/0000-0002-3258-1909
FU NASA; Austrian Fonds zur Forderung der wissenschaftlichen Forschung [AP
21205-N16, T359-N16, P19962]; Hungarian Academy of Sciences (HAS); OTKA
[K76816, K83790, MB08C 81013]; European Community [FP7/20072013, 269194]
FX Funding for this Discovery mission is provided by NASA's Science Mission
Directorate. The authors acknowledge the entire Kepler team, whose
outstanding efforts have made these results possible. JMN gratefully
acknowledges Dr. Amanda F. Linnell Nemec (International Statistics &
Research Corporation) for a critical reading of the paper, and the
Camosun College Faculty Association for funding his attendance at the
3rd KASC Workshop held in Aarhus, Denmark, in 2010 June; he also thanks
Dr. Geza Kovacs for his software and discussions on Fourier methods, and
Dr. Dorota Szczygiel for discussions on the ASAS data. Also, we thank
Dr. K. Mighell for sending us his Guest Observer LC:Q2-Q4 data for FN
Lyr, and the anonymous referee for a very thoughtful, knowledgeable and
helpful report. KK, EG and RSm acknowledge support from the Austrian
Fonds zur Forderung der wissenschaftlichen Forschung,project numbers AP
21205-N16 (RSm), T359-N16 and P19962 (KK and EG). RSz and JB are
supported by the Lenthilet program of the Hungarian Academy of Sciences
(HAS) and OTKA Grants K76816 and K83790 and MB08C 81013. RSz
acknowledges support of the Janos Bolyai Research Scholarship of the
HAS. The research leading to these results has received funding from the
European Community's Seventh Framework Programme (FP7/20072013) under
grant agreement no. 269194. Finally, as this paper was nearing
completion we learned of the death of Dr. Allan Sandage this paper is
dedicated to his memory.
NR 144
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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 OCT
PY 2011
VL 417
IS 2
BP 1022
EP 1053
DI 10.1111/j.1365-2966.2011.19317.x
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848HR
UT WOS:000297043000014
ER
PT J
AU Dunne, L
Gomez, HL
da Cunha, E
Charlot, S
Dye, S
Eales, S
Maddox, SJ
Rowlands, K
Smith, DJB
Auld, R
Baes, M
Bonfield, DG
Bourne, N
Buttiglione, S
Cava, A
Clements, DL
Coppin, KEK
Cooray, A
Dariush, A
de Zotti, G
Driver, S
Fritz, J
Geach, J
Hopwood, R
Ibar, E
Ivison, RJ
Jarvis, MJ
Kelvin, L
Pascale, E
Pohlen, M
Popescu, C
Rigby, EE
Robotham, A
Rodighiero, G
Sansom, AE
Serjeant, S
Temi, P
Thompson, M
Tuffs, R
van der Werf, P
Vlahakis, C
AF Dunne, L.
Gomez, H. L.
da Cunha, E.
Charlot, S.
Dye, S.
Eales, S.
Maddox, S. J.
Rowlands, K.
Smith, D. J. B.
Auld, R.
Baes, M.
Bonfield, D. G.
Bourne, N.
Buttiglione, S.
Cava, A.
Clements, D. L.
Coppin, K. E. K.
Cooray, A.
Dariush, A.
de Zotti, G.
Driver, S.
Fritz, J.
Geach, J.
Hopwood, R.
Ibar, E.
Ivison, R. J.
Jarvis, M. J.
Kelvin, L.
Pascale, E.
Pohlen, M.
Popescu, C.
Rigby, E. E.
Robotham, A.
Rodighiero, G.
Sansom, A. E.
Serjeant, S.
Temi, P.
Thompson, M.
Tuffs, R.
van der Werf, P.
Vlahakis, C.
TI Herschel -ATLAS: rapid evolution of dust in galaxies over the last 5
billion years
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE ISM: evolution; galaxies: evolution; galaxies: ISM; submillimetre:
galaxies
ID STAR-FORMATION RATE; INITIAL MASS FUNCTION; INFRARED LUMINOSITY
FUNCTIONS; SCIENCE DEMONSTRATION PHASE; KEPLERS SUPERNOVA REMNANT; COLD
DUST; INTERSTELLAR-MEDIUM; SUBMILLIMETER LUMINOSITY; FORMING GALAXIES;
STELLAR MASS
AB We present the first direct and unbiased measurement of the evolution of the dust mass function of galaxies over the past 5 billion years of cosmic history using data from the Science Demonstration Phase of the Herschel-Astrophysical Terahertz Large Area Survey (Herschel-ATLAS). The sample consists of galaxies selected at 250 m which have reliable counterparts from the Sloan Digital Sky Survey (SDSS) at z < 0.5, and contains 1867 sources. Dust masses are calculated using both a single-temperature grey-body model for the spectral energy distribution and also a model with multiple temperature components. The dust temperature for either model shows no trend with redshift. Splitting the sample into bins of redshift reveals a strong evolution in the dust properties of the most massive galaxies. At z= 0.40.5, massive galaxies had dust masses about five times larger than in the local Universe. At the same time, the dust-to-stellar mass ratio was about three to four times larger, and the optical depth derived from fitting the UV-sub-mm data with an energy balance model was also higher. This increase in the dust content of massive galaxies at high redshift is difficult to explain using standard dust evolution models and requires a rapid gas consumption time-scale together with either a more top-heavy initial mass function (IMF), efficient mantle growth, less dust destruction or combinations of all three. This evolution in dust mass is likely to be associated with a change in overall interstellar medium mass, and points to an enhanced supply of fuel for star formation at earlier cosmic epochs.
C1 [Dunne, L.; Maddox, S. J.; Rowlands, K.; Smith, D. J. B.; Bourne, N.; Rigby, E. E.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Gomez, H. L.; Dye, S.; Eales, S.; Auld, R.; Dariush, A.; Pascale, E.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[da Cunha, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[da Cunha, E.] Univ Crete, Dept Phys, Iraklion 71003, Greece.
[Charlot, S.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Bonfield, D. G.; Jarvis, M. J.; Thompson, M.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys, Hatfield AL10 9AB, Herts, England.
[Buttiglione, S.; de Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain.
[Clements, D. L.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Coppin, K. E. K.; Geach, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Coppin, K. E. K.; Geach, J.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England.
[Cooray, A.; Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England.
[de Zotti, G.] SISSA, I-34136 Trieste, Italy.
[Driver, S.; Kelvin, L.; Robotham, A.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Ibar, E.; Ivison, R. J.; van der Werf, P.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Popescu, C.; Sansom, A. E.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Rodighiero, G.] Univ Padua, Dept Astron, I-35122 Padua, Italy.
[Serjeant, S.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Temi, P.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[Tuffs, R.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Vlahakis, C.] Univ Chile, Dept Astron, Santiago, Chile.
RP Dunne, L (reprint author), Univ Nottingham, Sch Phys & Astron, Univ Pk Campus, Nottingham NG7 2RD, England.
EM loretta.dunne@nottingham.ac.uk
RI Gomez, Haley/C-2800-2009; Baes, Maarten/I-6985-2013; Robotham,
Aaron/H-5733-2014; Driver, Simon/H-9115-2014; Ivison, R./G-4450-2011;
Cava, Antonio/C-5274-2017;
OI Rodighiero, Giulia/0000-0002-9415-2296; da Cunha,
Elisabete/0000-0001-9759-4797; Dye, Simon/0000-0002-1318-8343; Smith,
Daniel/0000-0001-9708-253X; Baes, Maarten/0000-0002-3930-2757; Robotham,
Aaron/0000-0003-0429-3579; Driver, Simon/0000-0001-9491-7327; Ivison,
R./0000-0001-5118-1313; Cava, Antonio/0000-0002-4821-1275; Maddox,
Stephen/0000-0001-5549-195X
FU STFC (UK); ARC (Australia); AAO; ALMA-CONICYT Fund for the Development
of Chilean Astronomy [31090013]; Center of Excellence in Astrophysics
and Associated Technologies [PBF06]
FX HLG acknowledges useful discussions with Mike Edmunds. The H-ATLAS is a
project with Herschel, which is an ESA space observatory with science
instruments provided by European-led Principal Investigator consortia
andwith important participation from NASA. The H-ATLAS web-site
ishttp://www.h-atlas.org. GAMA is a joint European-Australasian project
based around a spectroscopic campaign using the Anglo-Australian
Telescope. The GAMA input catalogue is based on data taken from the SDSS
and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the
GAMA regions is being obtained by a number of independent survey
programmes including GALEX MIS, VST KIDS, VISTA VIKING, WISE, H-ATLAS,
GMRT and ASKAP providing UV to radio coverage. GAMA is funded by the
STFC (UK), the ARC (Australia), the AAO and the participating
institutions. The GAMA web-site is http://www.gama-survey.org/. This
work received support from the ALMA-CONICYT Fund for the Development of
Chilean Astronomy (Project 31090013) and from the Center of Excellence
in Astrophysics and Associated Technologies (PBF06).
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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 OCT
PY 2011
VL 417
IS 2
BP 1510
EP 1533
DI 10.1111/j.1365-2966.2011.19363.x
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848HR
UT WOS:000297043000046
ER
PT J
AU Parris, MG
Sharma, CA
Demara, RF
AF Parris, Matthew G.
Sharma, Carthik A.
Demara, Ronald F.
TI Progress in Autonomous Fault Recovery of Field Programmable Gate Arrays
SO ACM COMPUTING SURVEYS
LA English
DT Article
DE Design; Performance; Reliability; FPGA; evolvable hardware; autonomous
systems; self-test; reconfigurable architectures
ID FPGA LOGIC BLOCKS; RELIABILITY; METHODOLOGIES
AB The capabilities of current fault-handling techniques for Field Programmable Gate Arrays (FPGAs) develop a descriptive classification ranging from simple passive techniques to robust dynamic methods. Fault-handling methods not requiring modification of the FPGA device architecture or user intervention to recover from faults are examined and evaluated against overhead-based and sustainability-based performance metrics such as additional resource requirements, throughput reduction, fault capacity, and fault coverage. This classification alongside these performance metrics forms a standard for confident comparisons.
C1 [Parris, Matthew G.] NASA, NE A3, Kennedy Space Ctr, Kennedy Space Ctr, FL 32899 USA.
[Sharma, Carthik A.; Demara, Ronald F.] Univ Cent Florida, Sch Elect Engn & Comp Sci, Orlando, FL 32816 USA.
RP Parris, MG (reprint author), NASA, NE A3, Kennedy Space Ctr, Kennedy Space Ctr, FL 32899 USA.
EM matthew.g.parris@nasa.gov
OI DeMara, Ronald/0000-0001-6864-7255
FU NASA Intelligent Systems NRA [NNA04CL07A]
FX This research was supported in part by NASA Intelligent Systems NRA
Contract NNA04CL07A.
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U2 4
PU ASSOC COMPUTING MACHINERY
PI NEW YORK
PA 2 PENN PLAZA, STE 701, NEW YORK, NY 10121-0701 USA
SN 0360-0300
EI 1557-7341
J9 ACM COMPUT SURV
JI ACM Comput. Surv.
PD OCT
PY 2011
VL 43
IS 4
AR 31
DI 10.1145/1978802.1978810
PG 30
WC Computer Science, Theory & Methods
SC Computer Science
GA 849SN
UT WOS:000297145500008
ER
PT J
AU Hickman, JE
Havlikova, M
Kroeze, C
Palm, CA
AF Hickman, Jonathan E.
Havlikova, Martina
Kroeze, Carolien
Palm, Cheryl A.
TI Current and future nitrous oxide emissions from African agriculture
SO CURRENT OPINION IN ENVIRONMENTAL SUSTAINABILITY
LA English
DT Review
ID CROP-LIVESTOCK SYSTEMS; NITRIC-OXIDE; MILLENNIUM VILLAGES; NATURAL
SAVANNA; SOIL EMISSIONS; BURKINA-FASO; N2O; KENYA; FERTILIZER; DATABASE
AB Most emission estimates of the greenhouse gas nitrous oxide (N(2)O) from African agriculture at a continental scale are based on emission factors, such as those developed by the IPCC Guidelines. Here we present estimates from Africa from the EDGAR database, which is derived from the IPCC emission factors. Resulting estimates indicate that N(2)O emissions from agriculture represented 42% of total emissions from Africa (though that rises to 71% if all savannah and grassland burning is included), or roughly 6% of global anthropogenic N(2)O emissions (or 11% including burning). Emissions from African agriculture are dominated by grazing livestock; 74% of agricultural N(2)O excluding biomass burning was from paddocks, ranges, and pasture. Direct soil emissions represent 15% of agricultural emissions; substantial changes in direct emissions from North Africa helped drive a 47% continental increase in direct soil emissions from 1970 to 2005. Future trends based on the Millennium Ecosystem Assessment scenarios indicate that agricultural N(2)O emissions may double in Africa by 2050 from 2000 levels. Any regional or continental estimates for Africa are, however, necessarily limited by a paucity of direct measurements of emissions in sub-Saharan agro-ecosystems, and the heavy reliance on emission factors and other default assumptions about nitrogen cycling in African agriculture. In particular, a better understanding of livestock-related N inputs and N(2)O emissions will help improve regional and continental estimates. As fertilizer use increases in sub-Saharan Africa, emission estimates should consider several unusual elements of African agriculture: farmer practices that differ fundamentally from that of large scale farms, the long history of N depletion from agricultural soils, seasonal emission pulses, and emission factors that vary with the amount of N added.
C1 [Hickman, Jonathan E.; Havlikova, Martina; Palm, Cheryl A.] Columbia Univ, Earth Inst, Trop Agr & Rural Environm Program, Palisades, NY 10964 USA.
[Hickman, Jonathan E.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Kroeze, Carolien] Wageningen Univ, NL-6700 AA Wageningen, Netherlands.
[Kroeze, Carolien] Open Univ Netherlands, Sch Sci, Heerlen, Netherlands.
RP Hickman, JE (reprint author), Columbia Univ, Earth Inst, Trop Agr & Rural Environm Program, Lamont Campus,Lamont Hall,9W Route 61, Palisades, NY 10964 USA.
EM jeh2179@columbia.edu
NR 70
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U1 4
U2 39
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1877-3435
J9 CURR OPIN ENV SUST
JI Curr. Opin. Environ. Sustain.
PD OCT
PY 2011
VL 3
IS 5
BP 370
EP 378
DI 10.1016/j.cosust.2011.08.001
PG 9
WC GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY; Environmental Sciences
SC Science & Technology - Other Topics; Environmental Sciences & Ecology
GA 843QE
UT WOS:000296686300011
ER
PT J
AU Wildes, SL
Vollenweider, JJ
Nguyen, HT
Guyon, JR
AF Wildes, Sharon L.
Vollenweider, Johanna J.
Nguyen, Hanhvan T.
Guyon, Jeffrey R.
TI Genetic variation between outer-coastal and fjord populations of Pacific
herring (Clupea pallasii) in the eastern Gulf of Alaska
SO FISHERY BULLETIN
LA English
DT Article
ID MICROSATELLITE LOCI; MARINE FISH; DIFFERENTIATION; HARENGUS; SOFTWARE
AB Pacific herring (Clupea pallasii) from the Gulf of Alaska were screened for temporal and spatial genetic variation with 15 microsatellite loci. Thirteen collections were examined in this study: 11 from Southeast Alaska and 2 from Prince William Sound, Alaska. Although F(ST) values were low, a neighbor-joining tree based on genetic distance, homogeneity, and F(ST) values revealed that collectively, the Berners Bay and Lynn Canal (interior) collections were genetically distinct from Sitka Sound and Prince of Wales Island (outer-coastal) collections. Temporal genetic variation within regions (among three years of Berners Bay spawners and between the two Sitka Sound spawners) was zero, whereas 0.05% was attributable to genetic variation between Berners Bay and Sitka Sound. This divergence may be attributable to environmental differences between interior archipelago waters and outer-coast habitats, such as differences in temperature and salinity. Early spring collections of nonspawning Lynn Canal herring were nearly genetically identical to collections of spawning herring in Berners Bay two months later-an indication that Berners Bay spawners over-winter in Lynn Canal. Southeast Alaskan herring (collectively) were significantly different from those in Prince William Sound. This study illustrates that adequate sample size is needed to detect variation in pelagic fish species with a large effective population size, and microsatellite markers may be useful in detecting low-level genetic divergence in Pacific herring in the Gulf of Alaska.
C1 [Wildes, Sharon L.; Vollenweider, Johanna J.; Nguyen, Hanhvan T.; Guyon, Jeffrey R.] Natl Marine Fisheries Serv, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Ocean & Atmospher Adm, Juneau, AK 99801 USA.
RP Wildes, SL (reprint author), Natl Marine Fisheries Serv, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Ocean & Atmospher Adm, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA.
EM Sharon.Wildes@noaa.gov
NR 33
TC 7
Z9 7
U1 0
U2 6
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 OCT
PY 2011
VL 109
IS 4
BP 382
EP 393
PG 12
WC Fisheries
SC Fisheries
GA 839UT
UT WOS:000296395600003
ER
PT J
AU Talaat, ER
Mayr, HG
AF Talaat, E. R.
Mayr, H. G.
TI Model of semidiurnal pseudo-tide in the high-latitude upper mesosphere
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Mesosphere; Gravity waves; Modeling; Atmospheric dynamics
ID DOPPLER-SPREAD PARAMETERIZATION; NONMIGRATING DIURNAL TIDES;
GENERAL-CIRCULATION MODEL; WAVE MOMENTUM DEPOSITION; LARGE-SCALE
DYNAMICS; MIDDLE ATMOSPHERE; LOWER THERMOSPHERE; GRAVITY-WAVES;
SOUTH-POLE; 12-HOUR OSCILLATION
AB We present numerical results for the m=1 meridional winds of semidiurnal oscillations in the high-latitude upper mesosphere, which are generated in the Numerical Spectral Model (NSM) without solar excitations of the tides. Identified with heuristic computer runs, the pseudo-tides attain amplitudes that are, at times, as large as the non-migrating tides produced with standard solar forcing. Under the influence of parameterized gravity waves, the nonlinear NSM generates internal oscillations like the quasi-biennial oscillation, which are produced with periods favored by the dynamical properties of the system. The Coriolis force would favor at polar latitudes the excitation of 12 h periodicity. This oscillation may help explain the large non-migrating semidiurnal tides that are observed in the region with ground-based and satellite measurements. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Talaat, E. R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Mayr, H. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Talaat, ER (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
EM elsayed.talaat@jhuapl.edu
FU National Science Foundation [0640864, 0946902]
FX This work was supported by National Science Foundation Grants 0640864
and 0946902. The authors are indebted to a reviewer for critical and
constructive comments that contributed significantly to improve the
paper.
NR 49
TC 1
Z9 1
U1 0
U2 2
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 OCT
PY 2011
VL 73
IS 16
BP 2386
EP 2391
DI 10.1016/j.jastp.2011.08.008
PG 6
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 849QY
UT WOS:000297141400015
ER
PT J
AU Hudson, HS
Woods, TN
Chamberlin, PC
Fletcher, L
Del Zanna, G
Didkovsky, L
Labrosse, N
Graham, D
AF Hudson, H. S.
Woods, T. N.
Chamberlin, P. C.
Fletcher, L.
Del Zanna, G.
Didkovsky, L.
Labrosse, N.
Graham, D.
TI The EVE Doppler Sensitivity and Flare Observations
SO SOLAR PHYSICS
LA English
DT Article
DE Sun: flares; Sun: photosphere
ID SOLAR-FLARES; ATOMIC DATABASE; EMISSION-LINES; SPECTROMETER; HYDROGEN;
CHIANTI; PLASMA
AB The Extreme-ultraviolet Variability Experiment (EVE; see Woods et al., 2009) obtains continuous EUV spectra of the Sun viewed as a star. Its primary objective is the characterization of solar spectral irradiance, but its sensitivity and stability make it extremely interesting for observations of variability on time scales down to the limit imposed by its basic 10 s sample interval. In this paper we characterize the Doppler sensitivity of the EVE data. We find that the 30.4 nm line of He II has a random Doppler error below 0.001 nm (1 pm, better than 10 km s(-1) as a redshift), with ample stability to detect the orbital motion of its satellite, the Solar Dynamics Observatory (SDO). Solar flares also displace the spectrum, both because of Doppler shifts and because of EVE's optical layout, which (as with a slitless spectrograph) confuses position and wavelength. As a flare develops, the centroid of the line displays variations that reflect Doppler shifts and therefore flare dynamics. For the impulsive phase of the flare SOL2010-06-12, we find the line centroid to have a redshift of 16.8 +/- 5.9 km s(-1) relative to that of the flare gradual phase (statistical errors only). We find also that high-temperature lines, such as Fe XXIV 19.2 nm, have well-determined Doppler components for major flares, with decreasing apparent blueshifts as expected from chromospheric evaporation flows.
C1 [Hudson, H. S.] UC Berkeley, SSL, Berkeley, CA 94720 USA.
[Hudson, H. S.; Fletcher, L.; Labrosse, N.; Graham, D.] Univ Glasgow, Sch Phys & Astron, SUPA, Glasgow, Lanark, Scotland.
[Woods, T. N.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA.
[Chamberlin, P. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Didkovsky, L.] Univ So Calif, Ctr Space Sci, Los Angeles, CA 90089 USA.
[Del Zanna, G.] Univ Cambridge, Cambridge, England.
RP Hudson, HS (reprint author), UC Berkeley, SSL, Berkeley, CA 94720 USA.
EM hhudson@ssl.berkeley.edu
RI Chamberlin, Phillip/C-9531-2012; Labrosse, Nicolas/B-2670-2010
OI Chamberlin, Phillip/0000-0003-4372-7405; Labrosse,
Nicolas/0000-0002-4638-157X
FU NASA [NAS5-98033]; International Space Science Institute (Bern); Science
and Technology Facilities Council [STFC/F002941/1]; Leverhulme
Foundation [F00-179A]; EU via the HESPE [FP7-2010-SPACE-1/26]; STFC DTA
FX This work was supported by NASA via Contract NAS5-98033 for RHESSI.
Authors Fletcher and Hudson thank the International Space Science
Institute (Bern) for support. This work was supported by the Science and
Technology Facilities Council grant STFC/F002941/1, by Leverhulme
Foundation Grant F00-179A and by the EU via the HESPE project
FP7-2010-SPACE-1/26; author DG also acknowledges support from an STFC
DTA studentship.
NR 21
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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 OCT
PY 2011
VL 273
IS 1
BP 69
EP 80
DI 10.1007/s11207-011-9862-y
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 849KZ
UT WOS:000297125700005
ER
PT J
AU Jian, LK
Russell, CT
Luhmann, JG
MacNeice, PJ
Odstrcil, D
Riley, P
Linker, JA
Skoug, RM
Steinberg, JT
AF Jian, L. K.
Russell, C. T.
Luhmann, J. G.
MacNeice, P. J.
Odstrcil, D.
Riley, P.
Linker, J. A.
Skoug, R. M.
Steinberg, J. T.
TI Comparison of Observations at ACE and Ulysses with Enlil Model Results:
Stream Interaction Regions During Carrington Rotations 2016-2018
SO SOLAR PHYSICS
LA English
DT Article
DE Coronal model; Corotating interaction region; Heliospheric model; Radial
evolution; Solar wind; Space weather
ID CORONAL MASS EJECTIONS; GROUP GONG PROJECT; SOLAR-WIND SPEED;
MAGNETIC-FIELDS; INNER HELIOSPHERE; 5 AU; INTERPLANETARY; EVOLUTION;
MISSION; SHOCKS
AB During the latitudinal alignment in 2004, ACE and Ulysses encountered two stream interaction regions (SIRs) each Carrington rotation from 2016 to 2018, at 1 and 5.4 AU, respectively. More SIR-driven shocks were observed at 5.4 AU than at 1 AU. Three small SIRs at 1 AU merged to form a strong SIR at 5.4 AU. We compare the Enlil model results with spacecraft observations from four aspects: i) the accuracy of the latest versions of models (WSA v2.2 and Enlil v2.7) vs. old versions (WSA v1.6 and Enlil v2.6), ii) the sensitivity to different solar magnetograms (MWO vs. NSO), iii) the sensitivity to different coronal models (WSA vs. MAS), iv) the predictive capability at 1 AU vs. 5.4 AU. We find the models can capture field sector boundaries with some time offset. Although the new versions have improved the SIR timing prediction, the time offset can be up to two days at 1 AU and four days at 5.4 AU. The models cannot capture some small-scale structures, including shocks and small SIRs at 1 AU. For SIRs, the temperature and total pressure are often underestimated, while the density compression is overestimated. For slow wind, the density is usually overestimated, while the temperature, magnetic field, and total pressure are often underestimated. The new versions have improved the prediction of the speed and density, but they need more robust scaling factors for magnetic field. The Enlil model results are very sensitive to different solar magnetograms and coronal models. It is hard to determine which magnetogram-coronal model combination is superior to others. Higher-resolution solar and coronal observations, a mission closer to the Sun, together with simulations of greater resolution and added physics, are ways to make progress for the solar wind modeling.
C1 [Jian, L. K.; Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[MacNeice, P. J.; Odstrcil, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Riley, P.; Linker, J. A.] Predict Sci Inc, San Diego, CA 92121 USA.
[Skoug, R. M.; Steinberg, J. T.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Jian, LK (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
EM jlan@igpp.ucla.edu
RI MacNeice, Peter/F-5587-2012; Russell, Christopher/E-7745-2012; Jian,
Lan/B-4053-2010
OI Russell, Christopher/0000-0003-1639-8298; Jian, Lan/0000-0002-6849-5527
FU NSF SHINE [AGS-1062105]; NASA STEREO [NAS5-03131]; U.S. Department of
Energy; NASA; NSF Science and Technology Center [ATM-0120950]
FX This research is supported by the NSF SHINE program through Award
AGS-1062105 and NASA STEREO program through Grant NAS5-03131
administered by UC Berkeley. We appreciate CCMC staff for running the
coronal and heliospheric models. We thank all the PIs of ACE and Ulysses
for making the data available. We acknowledge the MWO and NSO staff for
providing the photospheric magnetic data. We thank Nick Arge for
providing the WSA coronal model at the CCMC. Work at Los Alamos was
performed under the auspices of the U.S. Department of Energy, with
financial support from the NASA ACE and STEREO programs. CISM (Center
for Integrated Space Weather Modeling), supported by the NSF Science and
Technology Center Program through Fund ATM-0120950 to Boston University,
has contributed to the development of several of the models applied in
this report.
NR 53
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U1 1
U2 6
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 OCT
PY 2011
VL 273
IS 1
BP 179
EP 203
DI 10.1007/s11207-011-9858-7
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 849KZ
UT WOS:000297125700012
ER
PT J
AU Hathaway, DH
AF Hathaway, D. H.
TI A Standard Law for the Equatorward Drift of the Sunspot Zones
SO SOLAR PHYSICS
LA English
DT Article
DE Solar cycle, observations; Sunspots, statistics; Sunspots, velocity
ID DEEP MERIDIONAL FLOW; SOLAR-CYCLE; MINIMUM
AB The latitudinal location of the sunspot zones in each hemisphere is determined by calculating the centroid position of sunspot areas for each solar rotation from May 1874 to June 2011. When these centroid positions are plotted and analyzed as functions of time from each sunspot cycle maximum, there appear to be systematic differences in the positions and equatorward drift rates as a function of sunspot cycle amplitude. If, instead, these centroid positions are plotted and analyzed as functions of time from each sunspot cycle minimum, then most of the differences in the positions and equatorward drift rates disappear. The differences that remain disappear entirely if curve fitting is used to determine the starting times (which vary by as much as eight months from the times of minima). The sunspot zone latitudes and equatorward drift measured relative to this starting time follow a standard path for all cycles with no dependence upon cycle strength or hemispheric dominance. Although Cycle 23 was peculiar in its length and the strength of the polar fields it produced, it too shows no significant variation from this standard. This standard law, and the lack of variation with sunspot cycle characteristics, is consistent with dynamo wave mechanisms but not consistent with current flux transport dynamo models for the equatorward drift of the sunspot zones.
C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Hathaway, DH (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM david.hathaway@nasa.gov
FU NASA
FX The author would like to thank NASA for its support of this research
through a grant from the Heliophysics Causes and Consequences of the
Minimum of Solar Cycle 23/24 Program to NASA Marshall Space Flight
Center. He is also indebted to Lisa Rightmire, Ron Moore, and an
anonymous referee whose comments and suggestions improved both the
figures and the manuscript. Most importantly, he would like to thank the
American taxpayers for supporting scientific research in general and
this research in particular.
NR 23
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U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD OCT
PY 2011
VL 273
IS 1
BP 221
EP 230
DI 10.1007/s11207-011-9837-z
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 849KZ
UT WOS:000297125700014
ER
PT J
AU Sorooshian, S
AghaKouchak, A
Arkin, P
Eylander, J
Foufoula-Georgiou, E
Harmon, R
Hendrickx, JMH
Imam, B
Kuligowski, R
Skahill, B
Skofronick-Jackson, G
AF Sorooshian, Soroosh
AghaKouchak, Amir
Arkin, Phillip
Eylander, John
Foufoula-Georgiou, Efi
Harmon, Russell
Hendrickx, Jan M. H.
Imam, Bisher
Kuligowski, Robert
Skahill, Brian
Skofronick-Jackson, Gail
TI ADVANCING THE REMOTE SENSING OF PRECIPITATION
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
C1 [AghaKouchak, Amir] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA 92717 USA.
[Arkin, Phillip] Univ Maryland, College Pk, MD 20742 USA.
[Eylander, John] USA, Engineer Res & Dev Ctr, Hanover, NH USA.
[Foufoula-Georgiou, Efi] Univ Minnesota, Minneapolis, MN USA.
[Harmon, Russell] USA, Res Lab, Durham, NC USA.
[Hendrickx, Jan M. H.] New Mexico Inst Min & Technol, Socorro, NM USA.
[Kuligowski, Robert] NOAA, NESDIS, STAR, Camp Springs, MD USA.
[Skahill, Brian] USA, Engineer Res & Dev Ctr, Vicksburg, MS USA.
[Skofronick-Jackson, Gail] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP AghaKouchak, A (reprint author), Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA 92717 USA.
EM amir.a@uci.edu
RI sorooshian, soroosh/B-3753-2008; Skofronick-Jackson, Gail/D-5354-2012;
Kuligowski, Robert/C-6981-2009
OI sorooshian, soroosh/0000-0001-7774-5113; Kuligowski,
Robert/0000-0002-6909-2252
FU U.S. Army Research Office
FX We are pleased to acknowledge that the funding for the Advanced Concepts
Workshop on Remote Sensing of Precipitation was provided by the U.S.
Army Research Office.
NR 0
TC 13
Z9 13
U1 0
U2 16
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 OCT
PY 2011
VL 92
IS 10
BP 1271
EP 1272
DI 10.1175/BAMS-D-11-00116.1
PG 2
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 848UI
UT WOS:000297080200006
ER
PT J
AU Mims, FM
Chambers, LH
Brooks, DR
AF Mims, Forrest M., III
Chambers, Lin Hartung
Brooks, David R.
TI MEASURING TOTAL COLUMN WATER VAPOR BY POINTING AN INFRARED THERMOMETER
AT THE SKY
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID SUN PHOTOMETER; PRECIPITABLE WATER; GPS METEOROLOGY; DESIGN; IR;
CALIBRATION; MONITOR; SYSTEM
AB A 2-yr study affirms that the temperature indicated by an inexpensive ($20-$60) IR thermometer pointed at the cloud-free zenith sky (Tz) is a proxy for total column water vapor [precipitable water (PW)]. From 8 September 2008 to 18 October 2010 Tz was measured either at or near solar noon, and occasionally at night, at a field in south-central Texas. PW was measured by a MICROTOPS II sun photometer. The coefficient of correlation (r(2)) of PW and Tz was 0.90, and the rms difference was 3.2 mm. A comparison of Tz with PW from a GPS site 31 km north-northeast yielded an r(2) of 0.79 and an rms difference of 5.8 mm. An expanded study compared Tz from eight IR thermometers with PW at various times during the day and night from 17 May to 18 October 2010, mainly at the Texas site, with an additional 10 days at Hawaii's Mauna Loa Observatory. The best results were provided by two IR thermometers that yielded an r(2) of 0.96 and an rms difference with PW of 2.7 mm. The results of both the ongoing 2-yr study and the 5-month comparison show that IR thermometers can measure PW with an accuracy (rms difference/mean PW) approaching 10%, which is the accuracy typically ascribed to sun photometers. The simpler IR method, which works during both day and night, can be easily mastered by students, amateur scientists, and cooperative weather observers.
C1 [Mims, Forrest M., III] Geronimo Creek Observ, Seguin, TX USA.
[Chambers, Lin Hartung] NASA, Langley Res Ctr, Climate Sci Branch, Sci Directorate, Hampton, VA 23665 USA.
[Brooks, David R.] Inst Earth Sci Res & Educ, Eagleville, PA USA.
RP Mims, FM (reprint author), 433 Twin Oak Rd, Seguin, TX 78155 USA.
EM forrest.mims@ieee.org
FU Science Directorate of NASA's Langley Research Center (LaRC); NOAA;
Solar Light Company
FX Preparation of this paper was supported in part by a contract from the
Science Directorate of NASA's Langley Research Center (LaRC). Annika
Jersild assisted with the LaRC measurements. We are grateful for
suggestions that greatly improved the manuscript provided by John Barnes
of the Mauna Loa Observatory, Peter A. Parker of LaRC, Seth Gutman and
Kirk L. Holub of NOAA's Ground-Based GPS-IPW Project, and, especially,
the three anonymous reviewers.; Trade names and product manufacturers
listed in this paper are provided solely for informational purposes and
imply no endorsement by the authors or NASA. The first author discloses
that he receives a royalty from Solar Light Company for sales of
MICROTOPS II sun photometers.
NR 28
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U1 2
U2 9
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 OCT
PY 2011
VL 92
IS 10
BP 1311
EP +
DI 10.1175/2011BAMS3215.1
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 848UI
UT WOS:000297080200013
ER
PT J
AU Sorooshian, S
AghaKouchak, A
Arkin, P
Eylander, J
Foufoula-Georgiou, E
Harmon, R
Hendrickx, JMH
Imam, B
Kuligowski, R
Skahill, B
Skofronick-Jackson, G
AF Sorooshian, Soroosh
AghaKouchak, Amir
Arkin, Phillip
Eylander, John
Foufoula-Georgiou, Efi
Harmon, Russell
Hendrickx, Jan M. H.
Imam, Bisher
Kuligowski, Robert
Skahill, Brian
Skofronick-Jackson, Gail
TI ADVANCED CONCEPTS ON REMOTE SENSING OF PRECIPITATION AT MULTIPLE SCALES
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID PASSIVE MICROWAVE; RAINFALL; SYSTEM
C1 [Sorooshian, Soroosh] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA 92697 USA.
[Arkin, Phillip] Univ Maryland, College Pk, MD 20742 USA.
[Eylander, John] USA, Engineer Res & Dev Ctr, Hanover, NH USA.
[Foufoula-Georgiou, Efi] Univ Minnesota, Minneapolis, MN USA.
[Harmon, Russell] USA, Res Lab, Durham, NC USA.
[Hendrickx, Jan M. H.] New Mexico Inst Min & Technol, Socorro, NM USA.
[Kuligowski, Robert] NOAA, NESDIS, STAR, Camp Springs, MD USA.
[Skahill, Brian] USA, Engineer Res & Dev Ctr, Vicksburg, MS USA.
[Skofronick-Jackson, Gail] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sorooshian, S (reprint author), Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA 92697 USA.
EM soroosh@uci.edu
RI Skofronick-Jackson, Gail/D-5354-2012; sorooshian, soroosh/B-3753-2008;
Kuligowski, Robert/C-6981-2009
OI sorooshian, soroosh/0000-0001-7774-5113; Kuligowski,
Robert/0000-0002-6909-2252
FU U.S. Army Research Office
FX We are pleased to acknowledge that a major portion of the funding for
this workshop was provided by the U.S. Army Research Office. Our deepest
gratitude goes to Dr. Russell Harmon for his unyielding support
throughout the planning and organization of the workshop. We offer
special thanks to Diane Hohnbaum for organizing and coordinating the
workshop activities. Finally, we are very thankful to CHRS graduate
students Jingjing Li, Rebeka Sultana, Qing Xia, Ali Zahraei, Tsou Chun
Jaw, Nasrin Nasrollahi, and Hamed Ashouri, who offered so generously
their time summarizing group discussions throughout the workshop. The
contents of this article are solely the opinions of the authors and do
not constitute a statement of policy, decision, or position on behalf of
the U.S. Army, NOAA, NASA, or the U.S. government.
NR 13
TC 56
Z9 57
U1 3
U2 17
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 OCT
PY 2011
VL 92
IS 10
BP 1353
EP 1357
DI 10.1175/2011BAMS3158.1
PG 5
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 848UI
UT WOS:000297080200017
ER
PT J
AU Rincon, RF
Vega, MA
Buenfil, M
Geist, A
Hilliard, L
Racette, P
AF Rincon, Rafael F.
Vega, Manuel A.
Buenfil, Manuel
Geist, Alessandro
Hilliard, Lawrence
Racette, Paul
TI NASA's L-Band Digital Beamforming Synthetic Aperture Radar
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article; Proceedings Paper
CT 8th European Conference on Synthetic Aperture Radar (EUSAR)
CY JUN, 2010
CL Aachen, GERMANY
SP German Assoc Elect, Elect, and Informat Technol/Informat Technol Soc (VDE/ITG), FHR, DLR, Cassidian, European Aeronaut Def & Space Co Astrium, IEEE Geosci & Remote Sensing Soc, IEEE Aerosp & Elect Syst Soc (AESS)
DE Altimeter; digital beamformimg; synthetic aperture radar (SAR);
scatterometer
AB The Digital Beamforming Synthetic Aperture Radar (DBSAR) is a state-of-the-art L-band radar that employs advanced radar technology and a customized data acquisition and real-time processor in order to enable multimode measurement techniques in a single radar platform. DBSAR serves as a test bed for the development, implementation, and testing of digital beamforming radar techniques applicable to Earth science and planetary measurements. DBSAR flew its first field campaign on board the National Aeronautics and Space Administration P3 aircraft in October 2008, demonstrating enabling techniques for scatterometry, synthetic aperture, and altimetry.
C1 [Rincon, Rafael F.; Vega, Manuel A.; Buenfil, Manuel; Geist, Alessandro; Hilliard, Lawrence; Racette, Paul] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
RP Rincon, RF (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
EM raafael.rincon@nasa.gov; manuel.vega@nasa.gov;
manuel.buenfil-1@nasa.gov; alessandro.d.geist@nasa.gov;
lawrence.m.hilliard@nasa.gov; paul.e.racette@nasa.gov
NR 14
TC 7
Z9 8
U1 1
U2 3
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 OCT
PY 2011
VL 49
IS 10
SI SI
BP 3622
EP 3628
DI 10.1109/TGRS.2011.2157971
PN 1
PG 7
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 846HS
UT WOS:000296888400012
ER
PT J
AU Wu, XQ
Jezek, KC
Rodriguez, E
Gogineni, S
Rodriguez-Morales, F
Freeman, A
AF Wu, Xiaoqing
Jezek, Kenneth C.
Rodriguez, Ernesto
Gogineni, Sivaprasad
Rodriguez-Morales, Fernando
Freeman, Anthony
TI Ice Sheet Bed Mapping With Airborne SAR Tomography
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article; Proceedings Paper
CT 8th European Conference on Synthetic Aperture Radar (EUSAR)
CY JUN, 2010
CL Aachen, GERMANY
SP German Assoc Elect, Elect, and Informat Technol/Informat Technol Soc (VDE/ITG), FHR, DLR, Cassidian, European Aeronaut Def & Space Co Astrium, IEEE Geosci & Remote Sensing Soc, IEEE Aerosp & Elect Syst Soc
DE Ice sheet; radar; sounder; synthetic aperture radar (SAR) tomography
ID SYNTHETIC-APERTURE RADAR; WEST ANTARCTICA; PROJECTION; SOUNDER; GLACIER
AB We develop and then demonstrate a 3-D tomographic ice sounding method applied to very high frequency (VHF) radar data that produces swath measurements of ice sheet surface topography, ice thickness, and radar reflectivity of both the surface and bed of the ice sheet. First, we formulate the ice sheet imaging problem as a problem of estimating signal arrival angles and illustrate how the method resolves ambiguous echoes arriving simultaneously from the left and right sides of the aircraft, as well as from the surface and base of the ice sheet. We then discuss why we chose the time-domain subaperture method for 2-D image formation for ice sounding. We apply the tomographic technique to the data that we collected in May 2006 and again in July 2008 from a multiple-phase-center VHF radar system. We present 3-D images of the upper and lower surfaces of the ice sheet and compare the estimated surface topography with Ice, Cloud, and land Elevation Satellite altimeter nadir track measurements and the measured swath ice thickness with independent nadir depth sounder tracks. We achieved a 5-m surface topography accuracy and a 14-m ice thickness accuracy.
C1 [Wu, Xiaoqing; Rodriguez, Ernesto; Freeman, Anthony] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Jezek, Kenneth C.] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA.
[Gogineni, Sivaprasad; Rodriguez-Morales, Fernando] Univ Kansas, Ctr Remote Sensing Ice Sheets, Lawrence, KS 66045 USA.
RP Wu, XQ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Xiaoqing.Wu@jpl.nasa.gov; jezek.1@osu.edu;
ernesto.rodriguez@jpl.nasa.gov; gogineni@cresis.ku.edu;
frodriguez@cresis.ku.edu; Anthony.Freeman@jpl.nasa.gov
NR 28
TC 28
Z9 30
U1 2
U2 9
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD OCT
PY 2011
VL 49
IS 10
SI SI
BP 3791
EP 3802
DI 10.1109/TGRS.2011.2132802
PN 1
PG 12
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 846HS
UT WOS:000296888400029
ER
PT J
AU Jacquinet-Husson, N
Crepeau, L
Armante, R
Boutammine, C
Chedin, A
Scott, NA
Crevoisier, C
Capelle, V
Boone, C
Poulet-Crovisier, N
Barbe, A
Campargue, A
Benner, DC
Benilan, Y
Bezard, B
Boudon, V
Brown, LR
Coudert, LH
Coustenis, A
Dana, V
Devi, VM
Fally, S
Fayt, A
Flaud, JM
Goldman, A
Herman, M
Harris, GJ
Jacquemart, D
Jolly, A
Kleiner, I
Kleinbohl, A
Kwabia-Tchana, F
Lavrentieva, N
Lacome, N
Xu, LH
Lyulin, OM
Mandin, JY
Maki, A
Mikhailenko, S
Miller, CE
Mishina, T
Moazzen-Ahmadi, N
Muller, HSP
Nikitin, A
Orphal, J
Perevalov, V
Perrin, A
Petkie, DT
Predoi-Cross, A
Rinsland, CP
Remedios, JJ
Rotger, M
Smith, MAH
Sung, K
Tashkun, S
Tennyson, J
Toth, RA
Vandaele, AC
Vander Auwera, J
AF Jacquinet-Husson, N.
Crepeau, L.
Armante, R.
Boutammine, C.
Chedin, A.
Scott, N. A.
Crevoisier, C.
Capelle, V.
Boone, C.
Poulet-Crovisier, N.
Barbe, A.
Campargue, A.
Benner, D. Chris
Benilan, Y.
Bezard, B.
Boudon, V.
Brown, L. R.
Coudert, L. H.
Coustenis, A.
Dana, V.
Devi, V. M.
Fally, S.
Fayt, A.
Flaud, J. -M.
Goldman, A.
Herman, M.
Harris, G. J.
Jacquemart, D.
Jolly, A.
Kleiner, I.
Kleinboehl, A.
Kwabia-Tchana, F.
Lavrentieva, N.
Lacome, N.
Xu, Li-Hong
Lyulin, O. M.
Mandin, J. -Y.
Maki, A.
Mikhailenko, S.
Miller, C. E.
Mishina, T.
Moazzen-Ahmadi, N.
Mueller, H. S. P.
Nikitin, A.
Orphal, J.
Perevalov, V.
Perrin, A.
Petkie, D. T.
Predoi-Cross, A.
Rinsland, C. P.
Remedios, J. J.
Rotger, M.
Smith, M. A. H.
Sung, K.
Tashkun, S.
Tennyson, J.
Toth, R. A.
Vandaele, A. -C.
Vander Auwera, J.
TI The 2009 edition of the GEISA spectroscopic database
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE GEISA; Spectroscopic database; Molecular spectroscopy; Line parameters;
Cross-sections; Atmospheric absorption; Atmospheric aerosols;
Atmospheric radiative transfer; Earth's and planetary atmospheres
ID ABSORPTION CROSS-SECTIONS; ABSOLUTE LINE-INTENSITIES; DIODE-LASER
MEASUREMENTS; FOURIER-TRANSFORM SPECTROSCOPY; MU-M REGION;
HIGH-RESOLUTION FOURIER; SELF-BROADENING COEFFICIENTS; CW-CAVITY
RINGDOWN; INTEGRATED BAND INTENSITIES; PRESSURE-SHIFT COEFFICIENTS
AB The updated 2009 edition of the spectroscopic database GEISA (Gestion et Etude des Informations Spectroscopiques Atmospheriques; Management and Study of Atmospheric Spectroscopic Information) is described in this paper. GEISA is a computer-accessible system comprising three independent sub-databases devoted, respectively, to: line parameters, infrared and ultraviolet/visible absorption cross-sections, microphysical and optical properties of atmospheric aerosols. In this edition, 50 molecules are involved in the line parameters sub-database, including 111 isotopologues, for a total of 3,807,997 entries, in the spectral range from 10(-6) to 35,877.031 cm(-1).
The successful performances of the new generation of hyperspectral sounders depend ultimately on the accuracy to which the spectroscopic parameters of the optically active atmospheric gases are known, since they constitute an essential input to the forward radiative transfer models that are used to interpret their observations. Currently, GEISA is involved in activities related to the assessment of the capabilities of IASI (Infrared Atmospheric Sounding Interferometer; http://smsc.cnes.fr/lASI/index.htm) on board the METOP European satellite through the GEISA/IASI database derived from GEISA. Since the Metop-A (http://www.eumetsat.int) launch (19 October 2006), GEISA is the reference spectroscopic database for the validation of the level-1 IASI data. Also, GEISA is involved in planetary research, i.e., modeling of Titan's atmosphere, in the comparison with observations performed by Voyager, or by ground-based telescopes, and by the instruments on board the Cassini-Huygens mission.
GEISA, continuously developed and maintained at LMD (Laboratoire de Meteorologie Dynamique, France) since 1976, is implemented on the IPSL/CNRS (France) "Ether" Products and Services Centre WEB site (http://ether.ipsl.jussieu.fr), where all archived spectroscopic data can be handled through general and user friendly associated management software facilities. More than 350 researchers are registered for on line use of GEISA. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Jacquinet-Husson, N.; Crepeau, L.; Armante, R.; Boutammine, C.; Chedin, A.; Scott, N. A.; Crevoisier, C.; Capelle, V.] Univ Paris 06, CNRS, Ecole Polytech, Lab Meteorol Dynam,IPSL,UMR 8539, F-91128 Palaiseau, France.
[Boone, C.; Poulet-Crovisier, N.] Univ Paris 06, Inst Pierre Simon Laplace, F-75252 Paris, France.
[Barbe, A.; Rotger, M.] Univ Reims, CNRS, Grp Spectrometrie Mol & Atmospher, UMR 6089, F-51687 Reims, France.
[Campargue, A.] Univ Grenoble 1, CNRS, Spectrometrie Phys Lab, UMR LIPHY 5588, F-38402 Grenoble, France.
[Benner, D. Chris; Devi, V. M.] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
[Benilan, Y.; Coudert, L. H.; Flaud, J. -M.; Jolly, A.; Kleiner, I.; Perrin, A.] Univ Paris 07, CNRS, Lab Interuniv Syst Atmospher, UMR 7583, F-94010 Creteil, France.
[Benilan, Y.; Coudert, L. H.; Flaud, J. -M.; Jolly, A.; Kleiner, I.; Perrin, A.] Univ Paris EST Creteil UPEC, F-94010 Creteil, France.
[Bezard, B.; Coustenis, A.] Univ Paris 06, CNRS, Lab Etud Spatiales & Instrumentat Astrophys, UMR 8109, F-92195 Meudon, France.
[Bezard, B.; Coustenis, A.] Univ Paris 07, Observ Paris Meudon, F-92195 Meudon, France.
[Boudon, V.] Univ Bourgogne, CNRS, Lab Interdisciplinaire Carnot de Bourgogne, UMR 5209, F-21078 Dijon, France.
[Brown, L. R.; Kleinboehl, A.; Miller, C. E.; Sung, K.; Toth, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dana, V.; Mandin, J. -Y.] Univ Paris 06, CNRS, Lab Phys Mol Atmosphere & Astrophys, UMR 7092, F-75252 Paris, France.
[Fally, S.; Vandaele, A. -C.] Inst Aeron Spatiale Belgique, B-1180 Brussels, Belgium.
[Fayt, A.] Catholic Univ Louvain, Lab Spect Mol, B-1348 Louvain, Belgium.
[Goldman, A.] Univ Denver, Dept Phys, Denver, CO 80208 USA.
[Herman, M.; Vander Auwera, J.] Univ Libre Brussels, Serv Chim Quant & Photophys, B-1050 Brussels, Belgium.
[Harris, G. J.; Tennyson, J.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Jacquemart, D.; Kwabia-Tchana, F.; Lacome, N.] Univ Paris 06, CNRS, Lab Dynam Interact & Reactivite, UMR 7075, F-75252 Paris, France.
[Lavrentieva, N.; Lyulin, O. M.; Mikhailenko, S.; Mishina, T.; Nikitin, A.; Perevalov, V.; Tashkun, S.] VE Zuev Inst Atmospher Opt, Tomsk 634021, Russia.
[Xu, Li-Hong] Univ New Brunswick, Ctr Laser Atom & Mol Sci CLAMS, Dept Phys, St John, NB E2L 4L5, Canada.
[Moazzen-Ahmadi, N.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
[Mueller, H. S. P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
[Orphal, J.] Univ KIT, Res Ctr Karlsruhe, Inst Meteorol & Climate Res, D-76021 Karlsruhe, Germany.
[Petkie, D. T.] Wright State Univ, Dept Phys, Dayton, OH 45435 USA.
[Predoi-Cross, A.] Univ Lethbridge, Dept Phys & Astron, Lethbridge, AB T1K 3M4, Canada.
[Rinsland, C. P.; Smith, M. A. H.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
[Remedios, J. J.] Univ Leicester, Dept Phys & Astron, Space Res Ctr, EOS, Leicester LE1 7RH, Leics, England.
RP Jacquinet-Husson, N (reprint author), Univ Paris 06, CNRS, Ecole Polytech, Lab Meteorol Dynam,IPSL,UMR 8539, F-91128 Palaiseau, France.
EM jacquinet@lmd.polytechnique.fr
RI Tennyson, Jonathan/I-2222-2012; Orphal, Johannes/A-8667-2012; BOUDON,
Vincent/A-4504-2010; Lavrentieva, Nina/A-4010-2014; Nikitin,
Andrei/K-2624-2013; Tashkun, Sergey/E-8682-2014; Xu,
Li-Hong/J-5095-2015; Sung, Keeyoon/I-6533-2015;
OI Tennyson, Jonathan/0000-0002-4994-5238; Orphal,
Johannes/0000-0002-1943-4496; Nikitin, Andrei/0000-0002-4280-4096;
Mueller, Holger/0000-0002-0183-8927
FU CNES; CNRS/INSU; BIRA/IASB; National Fund for Scientific Research (FNRS
FRFC) [2.4536.01]; Belgian Federal Science Policy Office [S09/09/2010
19:5709/09/2010 20:00:10SD]; Communaute Francaise de Belgique (Actions
de Recherche Concertees); Fonds de to Recherche Scientifique (FRS-FNRS,
Belgium, contracts FRFC); Action de Recherches Concertees of the
Communaute francaise de Belgique; Cologne Database for Molecular
Spectroscopy, CDMS; Deutsches Zentrum fur Luft- und Raumfahrt (DLR);
Natural Sciences and Engineering Research Council of Canada
FX This study is supported by CNES and CNRS/INSU with associated
encouragements of EUMETSAT. Part of this research was carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. Support
for the co-authors from BIRA/IASB has been given by the National Fund
for Scientific Research (FNRS FRFC convention no. 2.4536.01), the
Belgian Federal Science Policy Office (S09/09/2010 19:5709/09/2010
20:00:10SD program) and the Communaute Francaise de Belgique (Actions de
Recherche Concertees). J. Vander Auwera acknowledges financial support
from the Fonds de to Recherche Scientifique (FRS-FNRS, Belgium,
contracts FRFC) and the Action de Recherches Concertees of the
Communaute francaise de Belgique. H.S.P. Muller is very grateful to the
Bundesministerium fur Bildung und Forschung (BMBF) for financial support
aimed at maintaining the Cologne Database for Molecular Spectroscopy,
CDMS. This support has been administered by the Deutsches Zentrum fur
Luft- und Raumfahrt (DLR). Li-Hong Xu thanks the Natural Sciences and
Engineering Research Council of Canada for financial support of this
research program.
NR 518
TC 198
Z9 202
U1 3
U2 56
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 OCT
PY 2011
VL 112
IS 15
BP 2395
EP 2445
DI 10.1016/j.jqsrt.2011.06.004
PG 51
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 824ZK
UT WOS:000295240500001
ER
PT J
AU Choi, S
Datta, A
Alonso, JJ
AF Choi, Seongim
Datta, Anubhav
Alonso, Juan J.
TI Prediction of Helicopter Rotor Loads Using Time-Spectral Computational
Fluid Dynamics and an Exact Fluid-Structure Interface
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
ID VALIDATION; DISCRETIZATION; FLOWS
AB The objectives of this paper are to introduce time-spectral computational fluid dynamics (CFD) for the analysis of helicopter rotor flows in level flight and to introduce an exact fluid-structure interface for coupled CFD/computational structural dynamics (CSD) analysis. The accuracy and efficiency of time-spectral CFD are compared with conventional time-marching computations. The exact interface is equipped with an exact delta coupling procedure that bypasses the requirement for sectional airloads. Predicted loads are compared between time-spectral and time-marching CFD using both interfaces and validated using UH-60A flight data for high-vibration and dynamic stall conditions. It is concluded that time-spectral CFD can indeed predict rotor performance and peak-to-peak structural loads efficiently, and hence, open opportunity for blade shape optimization. The vibratory and dynamic stall loads, however, require a large number of time instances, which reduces its efficiency. The exact interface and delta procedure allow coupling to be implemented for arbitrary grids and advanced structural models exactly, without the requirement for two-dimensional sectional airloads.
C1 [Choi, Seongim; Alonso, Juan J.] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA.
[Datta, Anubhav] USA, Sci & Technol Corp, Aeroflightdynam Directorate, NASA Ames Res Ctr, Moffett Field, CA USA.
RP Choi, S (reprint author), Korea Adv Inst Sci & Technol, Dept Aerosp Engn, Taejon 305701, South Korea.
EM schoi1@kaist.ac.kr
RI Choi, Seongim/C-1825-2011
FU U.S. DoD HPC Modernization Program Office
FX This research was conducted at the U.S. Army Aeroflightdynamics
Directorate as part of the High Performance Computing Institute of
Advanced Rotorcraft Modeling and Simulation (HI-ARMS) program supported
by the U.S. DoD HPC Modernization Program Office and directed by Dr.
Roger Strawn. The authors wish to thank Wayne Johnson (NASA Ames) for
his insightful comments and discussions.
NR 29
TC 3
Z9 3
U1 0
U2 0
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
EI 2161-6027
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD OCT
PY 2011
VL 56
IS 4
AR 042001
DI 10.4050/JAHS.56.042001
PG 15
WC Engineering, Aerospace
SC Engineering
GA 846OC
UT WOS:000296912100001
ER
PT J
AU Yeo, H
Potsdam, M
Ormiston, RA
AF Yeo, Hyeonsoo
Potsdam, Mark
Ormiston, Robert A.
TI Rotor Aeroelastic Stability Analysis Using Coupled Computational Fluid
Dynamics/Computational Structural Dynamics
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
AB Computational fluid dynamics/computational structural dynamics (CFD/CSD) coupling was successfully applied to the rotor aeroelastic stability problem to calculate lead-lag regressing mode damping of a hingeless rotor in hover and forward flight. A direct time domain numerical integration of the equations in response to suitable excitation was solved using a tight CFD/CSD coupling. Two different excitation methods-swashplate cyclic pitch and blade tip lead-lag force excitations-were investigated to provide suitable blade transient responses. The free decay transient response time histories were postprocessed using the moving-block method to determine the damping as a function of the rotor operating conditions. Coupled CFD/CSD analysis results are compared with the experimentally measured stability data obtained for a 7.5-ft-diameter Mach-scale hingeless rotor model as well as stability predictions using the comprehensive analysis Rotorcraft Comprehensive Analysis System (RCAS). The coupled CFD/CSD predictions agreed more closely with the experimental lead-lag damping measurements than RCAS predictions based on conventional aerodynamic methods, better capturing key features in the damping trends.
C1 [Yeo, Hyeonsoo; Potsdam, Mark; Ormiston, Robert A.] USA, Aeroflightdynam Directorate AMRDEC, Res Dev & Engn Command, Ames Res Ctr, Moffett Field, CA USA.
RP Yeo, H (reprint author), USA, Aeroflightdynam Directorate AMRDEC, Res Dev & Engn Command, Ames Res Ctr, Moffett Field, CA USA.
EM hyeonsoo.yeo@us.army.mil
NR 26
TC 1
Z9 1
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 OCT
PY 2011
VL 56
IS 4
AR 042003
DI 10.4050/JAHS.56.042003
PG 16
WC Engineering, Aerospace
SC Engineering
GA 846OC
UT WOS:000296912100003
ER
PT J
AU Yeo, H
Romander, EA
Norman, TR
AF Yeo, Hyeonsoo
Romander, Ethan A.
Norman, Thomas R.
TI Investigation of Rotor Performance and Loads of a UH-60A Individual
Blade Control System
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
ID COMPREHENSIVE ANALYSIS; ACTIVE CONTROLS; ENHANCEMENT; PREDICTION;
HELICOPTER; AIRLOADS
AB Wind tunnel measurements of performance, loads, and vibration of a full-scale UH-60A Black Hawk main rotor with an individual blade control (IBC) system are compared with calculations obtained using the comprehensive helicopter analysis CAMRAD II and a coupled CAMRAD II/OVERFLOW 2 analysis. Measured data show a 5.1% rotor power reduction (8.6% rotor lift to effective-drag ratio increase) using 2/rev IBC actuation with 2.0. amplitude at mu = 0.4. At the optimum IBC phase for rotor performance, IBC actuator force (pitch link force) decreased, and neither flap nor chord bending moments changed significantly. CAMRAD II predicts the rotor power variations with the IBC phase reasonably well at mu = 0.35. However, the correlation degrades at mu = 0.4. Coupled CAMRAD II/OVERFLOW 2 shows excellent correlation with the measured rotor power variations with the IBC phase at both mu = 0.35 and mu = 0.4. Maximum reduction of IBC actuator force is better predicted with CAMRAD II, but general trends are better captured with the coupled analysis. The correlation of vibratory hub loads is generally poor by both methods, although the coupled analysis somewhat captures general trends.
C1 [Yeo, Hyeonsoo] USA, Aeroflightdynam Directorate AMRDEC, Res Dev & Engn Command, Ames Res Ctr, Moffett Field, CA USA.
[Romander, Ethan A.; Norman, Thomas R.] Natl Aeronaut & Space Adm, Flight Vehicle Res & Technol Div, Ames Res Ctr, Moffett Field, CA USA.
RP Yeo, H (reprint author), USA, Aeroflightdynam Directorate AMRDEC, Res Dev & Engn Command, Ames Res Ctr, Moffett Field, CA USA.
EM hyeonsoo.yeo@us.army.mil
NR 29
TC 4
Z9 4
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 OCT
PY 2011
VL 56
IS 4
AR 042006
DI 10.4050/JAHS.56.042006
PG 18
WC Engineering, Aerospace
SC Engineering
GA 846OC
UT WOS:000296912100006
ER
PT J
AU Kilaru, K
Ramsey, BD
Gubarev, MV
Gregory, DA
AF Kilaru, Kiranmayee
Ramsey, Brian D.
Gubarev, Mikhail V.
Gregory, Don A.
TI Differential deposition technique for figure corrections in
grazing-incidence x-ray optics
SO OPTICAL ENGINEERING
LA English
DT Article
DE grazing-incidence x-ray optics; figure profile improvement;
spatial-frequency deviations; differential deposition
AB A differential deposition technique was investigated as a way to minimize axial figure errors in full-shell, grazing-incidence, reflective x-ray optics. These types of optics use a combination of off-axis conic segments-hyperbolic, parabolic, and/or elliptical, to reflect and image x-rays. Several such mirrors or "shells" of decreasing diameter are typically concentrically nested to form a single focusing unit. Individual mirrors are currently produced at Marshall Space Flight Center using an electroforming technique, in which the shells are replicated off figured and superpolished mandrels. Several factors in this fabrication process lead to low-and mid-spatial frequency deviations in the surface profile of the shell that degrade the imaging quality of the optics. A differential deposition technique, discussed in this paper, seeks to improve the achievable resolution of the optics by correcting the surface profile deviations of the shells after fabrication. As a proof of concept, the technique was implemented on small-animal radionuclide-imaging x-ray optics being considered for medical applications. This paper discusses the deposition technique, its implementation, and the experimental results obtained to date. (C) 2011 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.3631851]
C1 [Kilaru, Kiranmayee; Gregory, Don A.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Ramsey, Brian D.; Gubarev, Mikhail V.] NASA, MSFC, Huntsville, AL 35812 USA.
RP Kilaru, K (reprint author), Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
NR 7
TC 13
Z9 13
U1 0
U2 3
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 0091-3286
J9 OPT ENG
JI Opt. Eng.
PD OCT
PY 2011
VL 50
IS 10
AR 106501
DI 10.1117/1.3631851
PG 6
WC Optics
SC Optics
GA 842BA
UT WOS:000296559700032
ER
PT J
AU Watson, WR
Jones, MG
AF Watson, W. R.
Jones, M. G.
TI New Numerical Procedure for Impedance Eduction in Ducts Containing Mean
Flow
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT 15th AIAA/CEAS Aeroacoustics Conference
CY MAY 11-13, 2009
CL Miami, FL
SP Amer Inst Aeronaut & Astronaut (AIAA), CEAS
ID LINER IMPEDANCE; HYDRODYNAMIC INSTABILITY; ACOUSTIC PROPERTIES; GRAZING
FLOW; VALIDATION; WALL; MINIMIZATION
AB A new impedance eduction method is presented and validated against a benchmark method, and the effects of measurement uncertainty errors on the impedances educed with this new method are assessed. Unique features of the new method include the following: 1) the upstream and downstream boundary conditions contain higher-order duct modes, 2) the impedance spectra of unique nonuniform test liners on opposite walls may be educed simultaneously, and 3) the measured data for the impedance eduction are acquired only at the source and duct termination planes. The validation exercise is performed with a rigid-wall insert and a conventional liner over a range of frequencies and flow Mach numbers in the NASA Langley Research Center's grazing flow impedance tube. The primary conclusions of the study are that the impedance spectra of the rigid-wall insert and the conventional liner that were educed from the new method are in very good agreement with those that were educed by using the benchmark method. However, the effects of measurement uncertainty on the educed impedance are greater at the lower frequencies and the higher Mach numbers for the new method. All indications are that this occurs because the new method 1) uses significantly less data to perform the impedance eduction than the benchmark and 2) is currently based on a rather crude approximation to the measured pressure gradient, which is more sensitive to the refractive effects of the boundary layer than the measured lower-wall pressure that is required in the benchmark method.
C1 [Watson, W. R.] NASA, Langley Res Ctr, Res & Technol Directorate, Computat Aerosci Branch,Liner Phys Grp, Hampton, VA 23681 USA.
[Jones, M. G.] NASA, Langley Res Ctr, Res & Technol Directorate, Struct Acoust Branch,Head Liner Phys Grp, Hampton, VA 23681 USA.
RP Watson, WR (reprint author), NASA, Langley Res Ctr, Res & Technol Directorate, Computat Aerosci Branch,Liner Phys Grp, Hampton, VA 23681 USA.
NR 44
TC 4
Z9 4
U1 2
U2 5
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 OCT
PY 2011
VL 49
IS 10
BP 2109
EP 2122
DI 10.2514/1.J050317
PG 14
WC Engineering, Aerospace
SC Engineering
GA 833DM
UT WOS:000295862000004
ER
PT J
AU Jenerette, GD
Harlan, SL
Stefanov, WL
Martin, CA
AF Jenerette, G. Darrel
Harlan, Sharon L.
Stefanov, William L.
Martin, Chris A.
TI Ecosystem services and urban heat riskscape moderation: water, green
spaces, and social inequality in Phoenix, USA
SO ECOLOGICAL APPLICATIONS
LA English
DT Article
DE climate change; economic stratification; ecosystem services; extreme
heat events; urban heat riskscape; vegetated cooling
ID CLIMATE-CHANGE; UNITED-STATES; SURFACE-TEMPERATURE; METROPOLITAN
PHOENIX; ENVIRONMENTAL-CHANGE; CARBON-DIOXIDE; AIR-POLLUTION; SHADE
TREES; ENERGY USE; ISLAND
AB Urban ecosystems are subjected to high temperatures-extreme heat events, chronically hot weather, or both-through interactions between local and global climate processes. Urban vegetation may provide a cooling ecosystem service, although many knowledge gaps exist in the biophysical and social dynamics of using this service to reduce climate extremes. To better understand patterns of urban vegetated cooling, the potential water requirements to supply these services, and differential access to these services between residential neighborhoods, we evaluated three decades (1970-2000) of land surface characteristics and residential segregation by income in the Phoenix, Arizona, USA metropolitan region. We developed an ecosystem service trade-offs approach to assess the urban heat riskscape, defined as the spatial variation in risk exposure and potential human vulnerability to extreme heat. In this region, vegetation provided nearly a 25 degrees C surface cooling compared to bare soil on low-humidity summer days; the magnitude of this service was strongly coupled to air temperature and vapor pressure deficits. To estimate the water loss associated with land-surface cooling, we applied a surface energy balance model. Our initial estimates suggest 2.7 mm/d of water may be used in supplying cooling ecosystem services in the Phoenix region on a summer day. The availability and corresponding resource use requirements of these ecosystem services had a strongly positive relationship with neighborhood income in the year 2000. However, economic stratification in access to services is a recent development: no vegetation-income relationship was observed in 1970, and a clear trend of increasing correlation was evident through 2000. To alleviate neighborhood inequality in risks from extreme heat through increased vegetation and evaporative cooling, large increases in regional water use would be required. Together, these results suggest the need for a systems evaluation of the benefits, costs, spatial structure, and temporal trajectory for the use of ecosystem services to moderate climate extremes. Increasing vegetation is one strategy for moderating regional climate changes in urban areas and simultaneously providing multiple ecosystem services. However, vegetation has economic, water, and social equity implications that vary dramatically across neighborhoods and need to be managed through informed environmental policies.
C1 [Jenerette, G. Darrel] Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA.
[Harlan, Sharon L.] Arizona State Univ, Sch Evolut & Human Change, Tempe, AZ 85287 USA.
[Stefanov, William L.] Lyndon B Johnson Space Ctr, Image Sci & Anal Lab, Houston, TX 77058 USA.
[Martin, Chris A.] Arizona State Univ, Dept Appl Sci & Math, Glendale, AZ 85306 USA.
RP Jenerette, GD (reprint author), Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA.
EM darrel.jenerette@ucr.edu
RI Romero, Luz/E-7993-2012; Namikawa, Laercio/C-5559-2013
OI Namikawa, Laercio/0000-0001-7847-1804
FU NSF Dynamics of Coupled Natural and Human Systems [GEO-0919006,
GEO-0816168]; Central Arizona-Phoenix Long-Term Ecological Research [DEB
9714833, DEB-096169]
FX We greatly appreciate the ongoing discussions and specific feedback
provided by Tony Brazel, Juan Declet-Barreto, Susanne Grossman-Clarke,
Stephanie Pincetl, Tim Lant, and Lorraine Weller. This research was
supported by the NSF Dynamics of Coupled Natural and Human Systems
(Grant No. GEO-0919006 and Grant No. GEO-0816168), Central
Arizona-Phoenix Long-Term Ecological Research (DEB 9714833), and
Ecosystems (DEB-096169) programs. Any opinions, findings, and
conclusions or recommendations expressed in this article are those of
the authors and do not necessarily reflect the views of the National
Science Foundation. We thank the Astromaterials Research and Exploration
Science Directorate, NASA Johnson Space Center, for providing
computational resources used in this research.
NR 101
TC 91
Z9 95
U1 14
U2 169
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA
SN 1051-0761
J9 ECOL APPL
JI Ecol. Appl.
PD OCT
PY 2011
VL 21
IS 7
BP 2637
EP 2651
PG 15
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 836UP
UT WOS:000296139200023
PM 22073649
ER
PT J
AU Kis, KI
Taylor, PT
Wittmann, G
Toronyi, B
Puszta, S
AF Kis, K. I.
Taylor, P. T.
Wittmann, G.
Toronyi, B.
Puszta, S.
TI Inversion of magnetic measurements of the CHAMP satellite over the
Pannonian Basin
SO JOURNAL OF APPLIED GEOPHYSICS
LA English
DT Article
DE CHAMP; Pannonian Basin; Total and vertical gradient magnetic anomalies;
Downward continuation; Inversion
ID NATURAL REMANENT MAGNETIZATION; CRUSTAL GRANULITE XENOLITHS; LAMELLAR
MAGNETISM; BAYESIAN-ESTIMATION; SEISMIC INVERSION; PART; TITANOHEMATITE;
HUNGARY
AB The Pannonian Basin is a deep intra-continental basin that formed as part of the Alpine orogeny. In order to study the nature of the crustal basement we used the long-wavelength magnetic anomalies acquired by the CHAMP satellite. The anomalies were distributed in a spherical shell, some 107,927 data recorded between January 1 and December 31 of 2008. They covered the Pannonian Basin and its vicinity. These anomaly data were interpolated into a spherical grid of 0.5 degrees x 0.5 degrees, at the elevation of 324 km by the Gaussian weight function. The vertical gradient of these total magnetic anomalies was also computed and mapped to the surface of a sphere at 324 km elevation. The former spherical anomaly data at 425 km altitude continued downward to 324 km. To interpret these data at the elevation of 324 km we used an inversion method. A polygonal prism forward model was used for the inversion. The minimum problem was solved numerically by the Simplex and Simulated annealing methods; a L(2) norm in the case of Gaussian distribution parameters and a L(1) norm was used in the case of Laplace distribution parameters. We interpret that the magnetic anomaly was produced by several sources and the effect of the sable magnetization of the exsolution of hemo-ilmenite minerals in the upper crustal metamorphic rocks. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Kis, K. I.] Eotvos Lorand Univ, Geophys & Space Sci Dept, H-1117 Budapest, Hungary.
[Taylor, P. T.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Wittmann, G.] MOL Hungarian Oil & Gas Co, H-1117 Budapest, Hungary.
[Toronyi, B.] Inst Geodesy Cartog & Remote Sensing, H-1149 Budapest, Hungary.
[Puszta, S.] Earthquake Observ, Geodet & Geophys Res Inst, H-1112 Budapest, Hungary.
RP Kis, KI (reprint author), Eotvos Lorand Univ, Geophys & Space Sci Dept, Pazmany Peter Setany 1-C, H-1117 Budapest, Hungary.
EM kisk@ludens.elte.hu
RI Taylor, Patrick/D-4707-2012
OI Taylor, Patrick/0000-0002-1212-9384
NR 36
TC 2
Z9 2
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0926-9851
J9 J APPL GEOPHYS
JI J. Appl. Geophys.
PD OCT
PY 2011
VL 75
IS 2
BP 412
EP 418
DI 10.1016/j.jappgeo.2011.07.018
PG 7
WC Geosciences, Multidisciplinary; Mining & Mineral Processing
SC Geology; Mining & Mineral Processing
GA 845KY
UT WOS:000296822800028
ER
PT J
AU Sepka, SA
Wright, M
AF Sepka, Steven A.
Wright, Michael
TI Monte Carlo Approach to FIAT Uncertainties with Applications for Mars
Science Laboratory
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article
AB A new scripted Monte Carlo analysis software tool has been developed for use with the fully implicit ablation and thermal response program thermal-protection-system-sizing code. This paper describes the new software tool and gives examples of its increased utility and useful insights on many aeroshell heatshield design considerations, such as maximum bond line temperature, recession, isotherm depth, surface temperature, and char depth. Finally, results are presented that illustrate the effect of uncertainties in key parameters that were used in the Mars Science Laboratory aeroshell thermal protection system design. The parameters having the greatest influence on bond line temperature dispersion for the Mars Science Laboratory backshell are virgin material thermal density (34%), initial material temperature (20%), virgin material conductivity (17%), and char density (13%).
C1 [Sepka, Steven A.] NASA, Ames Res Ctr, ERC Corp, Thermal Protect Mat Branch, Moffett Field, CA 94035 USA.
[Wright, Michael] NASA, Ames Res Ctr, Aerothermodynam Branch, Moffett Field, CA 94035 USA.
RP Sepka, SA (reprint author), NASA, Ames Res Ctr, ERC Corp, Thermal Protect Mat Branch, MS 234-1, Moffett Field, CA 94035 USA.
FU Thermal Protection Materials Branch; Aerothermodynamics Branch of NASA
Ames Research Center, through NASA [NNA10DE12C]
FX The authors gratefully acknowledge the support provided by the Thermal
Protection Materials Branch and the Aerothermodynamics Branch of NASA
Ames Research Center, through NASA contract no. NNA10DE12C to the ERC
Corporation.
NR 11
TC 1
Z9 2
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 OCT-DEC
PY 2011
VL 25
IS 4
BP 516
EP 522
DI 10.2514/1.49804
PG 7
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA 835YQ
UT WOS:000296073600004
ER
PT J
AU Daryabeigi, K
Cunnington, GR
Knutson, JR
AF Daryabeigi, Kamran
Cunnington, George R.
Knutson, Jeffrey R.
TI Combined Heat Transfer in High-Porosity High-Temperature Fibrous
Insulation: Theory and Experimental Validation
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article
ID RADIATIVE-TRANSFER; FIBER ORIENTATION; CONDUCTION; MODELS; MEDIA
AB Combined radiation and conduction heat transfer through various types of high-temperature, high-porosity, flexible fibrous insulation was modeled based on first principles. The relevant parameters needed for the heat transfer model were derived from experimental data. A semi-empirical formulation was used to model the solid conduction contribution of heat transfer in fibrous insulation, with the relevant parameters inferred from thermal conductivity measurements at cryogenic temperatures in a vacuum. The diffusion approximation was used for modeling the radiation component of heat transfer. The specific extinction coefficient for radiation heat transfer was obtained from high-temperature steady-state thermal measurements with large temperature differences maintained across the sample thickness in a vacuum. Standard gas conduction modeling was used in the heat transfer formulation. This heat transfer modeling methodology was applied to silica, two types of alumina, and a zirconia-based fibrous insulation. The heat transfer modeling methodology was evaluated by comparison with more rigorous analytical solutions and with standard thermal conductivity measurements. The developed heat transfer model is applicable over the temperature range of 300 to 1360K, pressure range of 0.001 to 760 torr, and density range of the various types of insulation studied here.
C1 [Daryabeigi, Kamran] NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA.
[Cunnington, George R.] Cunnington & Associates, Palo Alto, CA 94303 USA.
[Knutson, Jeffrey R.] NASA, Langley Res Ctr, Syst Integrat & Test Branch, Hampton, VA 23681 USA.
RP Daryabeigi, K (reprint author), NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Mail Stop 190, Hampton, VA 23681 USA.
FU NASA
FX The authors wish to express their gratitude to following individuals for
their invaluable contributions: Wayne Geouge, NASA Langley Research
Center, for fabrication and instrumentation of steady-state test setup,
and Jozef Gembarovic, TPRL, Inc., for providing transient radiant
step-heating technique thermal conductivity measurements. This work was
funded through the NASA Fundamental Aeronautics Hypersonic Program.
NR 35
TC 8
Z9 8
U1 1
U2 20
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 OCT-DEC
PY 2011
VL 25
IS 4
BP 536
EP 546
DI 10.2514/1.T3616
PG 11
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA 835YQ
UT WOS:000296073600006
ER
PT J
AU Kim, SS
Bargar, JR
Nealson, KH
Flood, BE
Kirschvink, JL
Raub, TD
Tebo, BM
Villalobos, M
AF Kim, Soon Sam
Bargar, John R.
Nealson, Kenneth H.
Flood, Beverly E.
Kirschvink, Joseph L.
Raub, Timothy D.
Tebo, Bradley M.
Villalobos, Mario
TI Searching for Biosignatures Using Electron Paramagnetic Resonance (EPR)
Analysis of Manganese Oxides
SO ASTROBIOLOGY
LA English
DT Article
DE Spectroscopic biosignatures
ID SP STRAIN SG-1; MARINE BACILLUS SP.; LEPTOTHRIX-DISCOPHORA; MULTICOPPER
OXIDASE; MAGNETIC-PROPERTIES; PSEUDOMONAS-PUTIDA; DESERT VARNISH;
OXIDATION; MN; RAMSDELLITE
AB Manganese oxide (Mn oxide) minerals from bacterial sources produce electron paramagnetic resonance (EPR) spectral signatures that are mostly distinct from those of synthetic simulants and abiogenic mineral Mn oxides. Biogenic Mn oxides exhibit only narrow EPR spectral linewidths (similar to 500 G), whereas abiogenic Mn oxides produce spectral linewidths that are 2-6 times broader and range from 1200 to 3000 G. This distinction is consistent with X-ray structural observations that biogenic Mn oxides have abundant layer site vacancies and edge terminations and are mostly of single ionic species [i.e., Mn(IV)], all of which favor narrow EPR linewidths. In contrast, abiogenic Mn oxides have fewer lattice vacancies, larger particle sizes, and mixed ionic species [Mn(III) and Mn(IV)], which lead to the broader linewidths. These properties could be utilized in the search for extraterrestrial physicochemical biosignatures, for example, on Mars missions that include a miniature version of an EPR spectrometer.
C1 [Kim, Soon Sam] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bargar, John R.] SLAC, Stanford Synchrotron Radiat Lab, Stanford, CA USA.
[Nealson, Kenneth H.] Univ So Calif, Los Angeles, CA USA.
[Flood, Beverly E.] Univ Minnesota, Minneapolis, MN USA.
[Tebo, Bradley M.] Oregon Hlth & Sci Univ, Div Environm & Biomol Syst, Beaverton, OR USA.
[Villalobos, Mario] Univ Nacl Autonoma Mexico, Fac Quim, Environm Biogeochem Grp, Mexico City 04510, DF, Mexico.
[Villalobos, Mario] Univ Nacl Autonoma Mexico, Inst Geol, Mexico City 04510, DF, Mexico.
RP Kim, SS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Soonsam.Kim@jpl.nasa.gov
RI Tebo, Bradley/A-8432-2017;
OI Tebo, Bradley/0000-0002-6301-4325; Raub, Timothy/0000-0002-7471-0246
FU IFS [W/3912]; National Aeronautics and Space Administration
FX S.S.K. is deeply grateful to George Rossman (Caltech) for the samples of
desert varnish. M.V. is grateful to the IFS, project no. W/3912, for
providing funds to synthesize and characterize synthetic Mn oxides. The
research conducted by the Jet Propulsion Laboratory, California
Institute of Technology was done under a contract with the National
Aeronautics and Space Administration. Copyright 2011. All rights
reserved.
NR 51
TC 9
Z9 10
U1 4
U2 32
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD OCT
PY 2011
VL 11
IS 8
BP 775
EP 786
DI 10.1089/ast.2011.0619
PG 12
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 839RS
UT WOS:000296387500004
PM 21970705
ER
PT J
AU Andersson, BG
Pintado, O
Potter, SB
Straizys, V
Charcos-Llorens, M
AF Andersson, B-G
Pintado, O.
Potter, S. B.
Straizys, V.
Charcos-Llorens, M.
TI Angle-dependent radiative grain alignment Confirmation of a magnetic
field - radiation anisotropy angle dependence on the efficiency of
interstellar grain alignment
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE polarization; dust, extinction; ISM: magnetic fields
ID CHAMELEON-I; POLARIZATION; CONSTRAINTS; EXTINCTION; TORQUES; CLOUDS
AB Context. Interstellar grain alignment studies are currently experiencing a renaissance due to the development of a new quantitative theory based on radiative alignment torques (RAT). One of the distinguishing predictions of this theory is a dependence of the grain alignment efficiency on the relative angle (Psi) between the magnetic field and the anisotropy direction of the radiation field. In an earlier study we found observational evidence for such an effect from observations of the polarization around the star HD 97300 in the Chamaeleon I cloud. However, due to the large uncertainties in the measured visual extinctions, the result was uncertain.
Aims. By acquiring explicit spectral classification of the polarization targets, we have sought to perform a more precise reanalysis of the existing polarimetry data.
Methods. We have obtained new spectral types for the stars in our for our polarization sample, which we combine with photometric data from the literature to derive accurate visual extinctions for our sample of background field stars. This allows a high accuracy test of the grain alignment efficiency as a function of Psi.
Results. We confirm and improve the measured accuracy of the variability of the grain alignment efficiency with Psi, seen in the earlier study. We note that the grain temperature (heating) also shows a dependence on Psi which we interpret as a natural effect of the projection of the grain surface to the illuminating radiation source. This dependence also allows us to derive an estimate of the fraction of aligned grains in the cloud.
C1 [Andersson, B-G; Charcos-Llorens, M.] NASA, USRA SOFIA Sci Ctr, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Pintado, O.] Consejo Nacl Invest Cient & Tecn, Inst Super Corellac Geol, RA-4000 San Miguel De Tucuman, Tucuman, Argentina.
[Potter, S. B.] S African Astron Observ, ZA-7935 Cape Town, South Africa.
[Straizys, V.] Vilnius Univ, Inst Theoret Phys & Astron, LT-01108 Vilnius, Lithuania.
RP Andersson, BG (reprint author), NASA, USRA SOFIA Sci Ctr, Ames Res Ctr, Mail Stop N211-3, Moffett Field, CA 94035 USA.
EM bg@sofia.usra.edu
OI Andersson, B-G/0000-0001-6717-0686
FU CASLEO observatory; CONICET [PIP0348]
FX We gratefully acknowledge the time allocation and support of the staff
of the CASLEO observatory. O.I.P. contribution to this paper was
partially supported by PIP0348 by CONICET.
NR 38
TC 13
Z9 13
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 OCT
PY 2011
VL 534
AR A19
DI 10.1051/0004-6361/201117670
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 841ZS
UT WOS:000296554800134
ER
PT J
AU Campante, TL
Handberg, R
Mathur, S
Appourchaux, T
Bedding, TR
Chaplin, WJ
Garcia, RA
Mosser, B
Benomar, O
Bonanno, A
Corsaro, E
Fletcher, ST
Gaulme, P
Hekker, S
Karoff, C
Regulo, C
Salabert, D
Verner, GA
White, TR
Houdek, G
Brandao, IM
Creevey, OL
Dogan, G
Bazot, M
Christensen-Dalsgaard, J
Cunha, MS
Elsworth, Y
Huber, D
Kjeldsen, H
Lundkvist, M
Molenda-Zakowicz, J
Monteiro, MJPFG
Stello, D
Clarke, BD
Girouard, FR
Hall, JR
AF Campante, T. L.
Handberg, R.
Mathur, S.
Appourchaux, T.
Bedding, T. R.
Chaplin, W. J.
Garcia, R. A.
Mosser, B.
Benomar, O.
Bonanno, A.
Corsaro, E.
Fletcher, S. T.
Gaulme, P.
Hekker, S.
Karoff, C.
Regulo, C.
Salabert, D.
Verner, G. A.
White, T. R.
Houdek, G.
Brandao, I. M.
Creevey, O. L.
Dogan, G.
Bazot, M.
Christensen-Dalsgaard, J.
Cunha, M. S.
Elsworth, Y.
Huber, D.
Kjeldsen, H.
Lundkvist, M.
Molenda-Zakowicz, J.
Monteiro, M. J. P. F. G.
Stello, D.
Clarke, B. D.
Girouard, F. R.
Hall, J. R.
TI Asteroseismology from multi-month Kepler photometry: the evolved
Sun-like stars KIC 10273246 and KIC 10920273
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: oscillations; methods: data analysis; asteroseismology; stars:
solar-type; stars: individual: KIC 10273246; stars: individual: KIC
10920273
ID SOLAR-LIKE OSCILLATIONS; MAIN-SEQUENCE STARS; P-MODE PARAMETERS; STELLAR
OSCILLATIONS; RED GIANTS; RADIUS DETERMINATION; SPECTRAL-ANALYSIS; LIGHT
CURVES; TIME-SERIES; SPACED DATA
AB Context. The evolved main-sequence Sun-like stars KIC 10273246 (F-type) and KIC 10920273 (G-type) were observed with the NASA Kepler satellite for approximately ten months with a duty cycle in excess of 90%. Such continuous and long observations are unprecedented for solar-type stars other than the Sun.
Aims. We aimed mainly at extracting estimates of p-mode frequencies - as well as of other individual mode parameters - from the power spectra of the light curves of both stars, thus providing scope for a full seismic characterization.
Methods. The light curves were corrected for instrumental effects in a manner independent of the Kepler science pipeline. Estimation of individual mode parameters was based both on the maximization of the likelihood of a model describing the power spectrum and on a classic prewhitening method. Finally, we employed a procedure for selecting frequency lists to be used in stellar modeling.
Results. A total of 30 and 21 modes of degree l = 0, 1, 2 - spanning at least eight radial orders - have been identified for KIC 10273246 and KIC 10920273, respectively. Two avoided crossings (l = 1 ridge) have been identified for KIC 10273246, whereas one avoided crossing plus another likely one have been identified for KIC 10920273. Good agreement is found between observed and predicted mode amplitudes for the F-type star KIC 10273246, based on a revised scaling relation. Estimates are given of the rotational periods, the parameters describing stellar granulation and the global asteroseismic parameters Delta nu and nu(max).
C1 [Campante, T. L.; Brandao, I. M.; Bazot, M.; Cunha, M. S.; Monteiro, M. J. P. F. G.] Univ Porto, Fac Ciencias, DFA, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Campante, T. L.; Handberg, R.; Karoff, C.; Dogan, G.; Christensen-Dalsgaard, J.; Kjeldsen, H.; Lundkvist, M.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Mathur, S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Appourchaux, T.; Benomar, O.; Gaulme, P.] Univ Paris 11, CNRS UMR8617, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Bedding, T. R.; White, T. R.; Huber, D.; Stello, D.] Univ Sydney, Sch Phys, SIfA, Sydney, NSW 2006, Australia.
[Chaplin, W. J.; Hekker, S.; Verner, G. A.; Elsworth, Y.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Garcia, R. A.] Univ Paris Diderot, Ctr Saclay, IRFU SAp, CNRS,CEA DSM,Lab AIM, F-91191 Gif Sur Yvette, France.
[Mosser, B.] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA,Observ Paris, F-92195 Meudon, France.
[Bonanno, A.; Corsaro, E.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy.
[Fletcher, S. T.] Sheffield Hallam Univ, Fac Arts Comp Engn & Sci, Mat Engn Res Inst, Sheffield S1 1WB, S Yorkshire, England.
[Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Regulo, C.; Salabert, D.; Creevey, O. L.] Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38206, Spain.
[Regulo, C.; Salabert, D.; Creevey, O. L.] Inst Astrofis Canarias, Tenerife 38200, Spain.
[Verner, G. A.] Univ London, Astron Unit, London E1 4NS, England.
[White, T. R.] Australian Astron Observ, Epping, NSW 1710, Australia.
[Houdek, G.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Molenda-Zakowicz, J.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland.
[Clarke, B. D.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Girouard, F. R.; Hall, J. R.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
RP Campante, TL (reprint author), Univ Porto, Fac Ciencias, DFA, Ctr Astrofis, Rua Estrelas, P-4150762 Oporto, Portugal.
EM campante@astro.up.pt
RI Brandao, Isa/M-5172-2013; Monteiro, Mario J.P.F.G./B-4715-2008;
OI Brandao, Isa/0000-0002-1153-0942; Monteiro, Mario
J.P.F.G./0000-0003-0513-8116; Bazot, Michael/0000-0003-0166-1540;
Bonanno, Alfio/0000-0003-3175-9776; Bedding,
Timothy/0000-0001-5943-1460; Cunha, Margarida/0000-0001-8237-7343;
Bedding, Tim/0000-0001-5222-4661; Garcia, Rafael/0000-0002-8854-3776
FU NASA's Science Mission Directorate; FCT/MCTES, Portugal
[SFRH/BD/36240/2007, PTDC/CTE-AST/098754/2008]
FX Funding for this mission is provided by NASA's Science Mission
Directorate. The authors wish to thank the entire Kepler team, without
whom these results would not be possible. T.L.C. is supported by grant
with reference number SFRH/BD/36240/2007 from FCT/MCTES, Portugal. This
work was supported by the project PTDC/CTE-AST/098754/2008 funded by
FCT/MCTES, Portugal.
NR 97
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2011
VL 534
AR A6
DI 10.1051/0004-6361/201116620
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 841ZS
UT WOS:000296554800019
ER
PT J
AU Defrere, D
Absil, O
Augereau, JC
di Folco, E
Berger, JP
du Foresto, VC
Kervella, P
Le Bouquin, JB
Lebreton, J
Millan-Gabet, R
Monnier, JD
Olofsson, J
Traub, W
AF Defrere, D.
Absil, O.
Augereau, J-C.
di Folco, E.
Berger, J-P.
du Foresto, V. Coude
Kervella, P.
Le Bouquin, J-B.
Lebreton, J.
Millan-Gabet, R.
Monnier, J. D.
Olofsson, J.
Traub, W.
TI Hot exozodiacal dust resolved around Vega with IOTA/IONIC
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE instrumentation: high angular resolution; techniques: interferometric;
circumstellar matter
ID INFRARED INTERFEROMETRIC SURVEY; MAIN-SEQUENCE STARS; DEBRIS DISKS;
NULLING INTERFEROMETRY; STELLAR INTERFEROMETRY; ABSOLUTE CALIBRATION;
INTEGRATED-OPTICS; BEAM COMBINER; SYSTEM; CHARA/FLUOR
AB Context. Although debris discs have been detected around a significant number of main-sequence stars, only a few of them are known to harbour hot dust in their inner part where terrestrial planets may have formed. Thanks to infrared interferometric observations, it is possible to obtain a direct measurement of these regions, which are of prime importance for preparing future exo-Earth characterisation missions.
Aims. We resolve the exozodiacal dust disc around Vega with the help of infrared stellar interferometry and estimate the integrated H-band flux originating from the first few AUs of the debris disc.
Methods. Precise H-band interferometric measurements were obtained on Vega with the 3-telescope IOTA/IONIC interferometer (Mount Hopkins, Arizona). Thorough modelling of both interferometric data (squared visibility and closure phase) and spectral energy distribution was performed to constrain the nature of the near-infrared excess emission.
Results. Resolved circumstellar emission within similar to 6 AU from Vega is identified at the 3-sigma level. The most straightforward scenario consists in a compact dust disc producing a thermal emission that is largely dominated by small grains located between 0.1 and 0.3 AU from Vega and accounting for 1.23 +/- 0.45% of the near-infrared stellar flux for our best-fit model. This flux ratio is shown to vary slightly with the geometry of the model used to fit our interferometric data (variations within +/- 0.19%).
Conclusions. The presence of hot exozodiacal dust in the vicinity of Vega, initially revealed by K-band CHARA/FLUOR observations, is confirmed by our H-band IOTA/IONIC measurements. Whereas the origin of the dust is still uncertain, its presence and the possible connection with the outer disc suggest that the Vega system is currently undergoing major dynamical perturbations.
C1 [Defrere, D.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Absil, O.] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Liege, Belgium.
[Augereau, J-C.; Le Bouquin, J-B.; Lebreton, J.] CNRS INSU, IPAG, UMR 5274, UJF Grenoble 1, F-38041 Grenoble, France.
[di Folco, E.] Univ Paris Diderot, CNRS, DSM, Serv Astrophys,Lab AIM,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Berger, J-P.] European So Observ, Vitacura 3107, Chile.
[di Folco, E.; du Foresto, V. Coude; Kervella, P.] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris,UMR 8109, F-92195 Meudon, France.
[Millan-Gabet, R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Monnier, J. D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Olofsson, J.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Traub, W.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Defrere, D (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM ddefrere@mpifr-bonn.mpg.de
FU International Space Science Institute (ISSI) in Bern, Switzerland;
Belgian National Science Foundation ("FRIA"); MPIFR; F.R.S.-FNRS;
Communaute francaise de Belgique - Actions de recherche concertees -
Academie universitaire Wallonie-Europe; French National Research Agency
(ANR) [ANR-2010 BLAN-0505-01]; ONERA; Observatoire de Paris; CNRS;
University Denis Diderot Paris 7
FX The authors acknowledge Sylvestre Lacour (LESIA) and Ettore Pedretti
(St. Andrews) for sharing dispersed calibrator data of 2006. The authors
are also grateful to Arnaud Magette, Charles Hanot, Pierre Riaud, and
Jean Surdej (IAGL), Bertrand Mennesson (NASA/JPL), Jason Aufdenberg
(ERAU), Gerd Weigelt (MPIFR), and Paul Lepoulpe for helpful advice. This
research was supported by the International Space Science Institute
(ISSI) in Bern, Switzerland ("Exozodiacal Dust discs and Darwin" working
group, http://www.issibern.ch/teams/exodust/). D.D. acknowledges the
support of the Belgian National Science Foundation ("FRIA"), of EII
(Fizeau programme), and the MPIFR. O.A. acknowledges the support from an
F.R.S.-FNRS Postdoctoral Fellowship. D.D. and O.A. acknowledge support
from the Communaute francaise de Belgique - Actions de recherche
concertees - Academie universitaire Wallonie-Europe. D.D., O.A., and
J.C.A. thank the French National Research Agency (ANR) for financial
support through contract ANR-2010 BLAN-0505-01 (EXOZODI). This research
received the support of PHASE, the high angular resolution partnership
between ONERA, Observatoire de Paris, CNRS, and University Denis Diderot
Paris 7.
NR 61
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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 OCT
PY 2011
VL 534
AR A5
DI 10.1051/0004-6361/201117017
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 841ZS
UT WOS:000296554800043
ER
PT J
AU Ferrari, C
Intema, HT
Orru, E
Govoni, F
Murgia, M
Mason, B
Bourdin, H
Asad, KM
Mazzotta, P
Wise, MW
Mroczkowski, T
Croston, JH
AF Ferrari, C.
Intema, H. T.
Orru, E.
Govoni, F.
Murgia, M.
Mason, B.
Bourdin, H.
Asad, K. M.
Mazzotta, P.
Wise, M. W.
Mroczkowski, T.
Croston, J. H.
TI Discovery of the correspondence between intra-cluster radio emission and
a high pressure region detected through the Sunyaev-Zel'dovich effect
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: clusters: individual: RX J1347-1145; radio continuum:
galaxies; X-rays: galaxies: clusters; cosmic background radiation
ID GALAXY CLUSTERS; RX J1347.5-1145; PARTICLE REACCELERATION; SHOCK-WAVES;
SKY SURVEY; CORE; PLASMA; HALOS; GAS
AB We analyzed new 237 MHz and 614 MHz GMRT data of the most X-ray luminous galaxy cluster, RXJ1347-1145. Our radio results are compared with the MUSTANG 90 GHz Sunyaev-Zel'dovich effect map and with re-processed Chandra and XMM-Newton archival data of this cluster. We point out for the first time in an unambiguous way the correspondence between a radio excess in a diffuse intra-cluster radio source and a hot region detected through both Sunyaev-Zel'dovich effect and X-ray observations. Our result indicates that electron re-acceleration in the excess emission of the radio mini-halo at the center of RXJ1347-1145 is most likely related to a shock front propagating into the intra-cluster medium.
C1 [Ferrari, C.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Cassiopee, Nice, France.
[Intema, H. T.; Mason, B.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Orru, E.] Radboud Univ Nijmegen, NL-6525 AJ Nijmegen, Netherlands.
[Govoni, F.; Murgia, M.] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, Ca, Italy.
[Bourdin, H.; Mazzotta, P.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Mazzotta, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Wise, M. W.] ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Wise, M. W.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands.
[Mroczkowski, T.] Univ Penn, Philadelphia, PA 19104 USA.
[Mroczkowski, T.] NASA, Washington, DC USA.
[Croston, J. H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
RP Ferrari, C (reprint author), Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Cassiopee, Nice, France.
EM chiara.ferrari@oca.eu
RI Mazzotta, Pasquale/B-1225-2016;
OI Mroczkowski, Tony/0000-0003-3816-5372; Mazzotta,
Pasquale/0000-0002-5411-1748; Murgia, Matteo/0000-0002-4800-0806;
Govoni, Federica/0000-0003-3644-3084
FU Agence Nationale de la Recherche [ANR-09-JCJC-0001-01]; BQR program of
Observatoire de la Cote d'Azur; Laboratoire Cassiopee [UMR 6202]
FX We thank the anonymous referee for her/his useful comments. We are
grateful to Giulia Macario for helpful suggestions in the radio data
reduction phase. We warmly thank Monique Arnaud for very useful
discussions. We would like to thank the staff of the GMRT that made
these observations possible. GMRT is run by the National Centre for
Radio Astrophysics of the Tata Institute of Fundamental Research. CF
acknowledges financial support by the "Agence Nationale de la Recherche"
through grant ANR-09-JCJC-0001-01. This work was supported by the BQR
program of Observatoire de la Cote d'Azur and by Laboratoire Cassiopee
(UMR 6202).
NR 27
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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 OCT
PY 2011
VL 534
AR L12
DI 10.1051/0004-6361/201117788
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 841ZS
UT WOS:000296554800146
ER
PT J
AU Giacintucci, S
Dallacasa, D
Venturi, T
Brunetti, G
Cassano, R
Markevitch, M
Athreya, RM
AF Giacintucci, S.
Dallacasa, D.
Venturi, T.
Brunetti, G.
Cassano, R.
Markevitch, M.
Athreya, R. M.
TI An unlikely radio halo in the low X-ray luminosity galaxy cluster RXC
J1514.9-1523 (Research Note)
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE radiation mechanisms: non-thermal; galaxies: clusters: general;
galaxies: clusters: individual: RXCJ1514.9-1523; radio continuum:
general
ID VLA SKY SURVEY; DEEP 1.4 GHZ; COSMIC-RAYS; RELIC CANDIDATES; HADRONIC
MODELS; EMISSION; REACCELERATION; SPECTRUM; COMA; ACCELERATION
AB We report the discovery of a giant radio halo in the galaxy cluster RXCJ1514.9-1523 at z = 0.22 with a relatively low X-ray luminosity, LX[0.1-2.4 kev] similar to 7 x 10(44) erg s(-1). This faint, diffuse radio source is detected with the Giant Metrewave Radio Telescope at 327 MHz. The source is barely detected at 1.4 GHz in a NVSS pointing that we have reanalyzed. The integrated radio spectrum of the halo is quite steep, with a slope alpha = 1.6 between 327 MHz and 1.4 GHz. While giant radio halos are common in more X-ray luminous cluster mergers, there is a less than 10% probability to detect a halo in systems with L-X less than or similar to 8 x 10(44) erg s(-1). The detection of a new giant halo in this borderline luminosity regime can be particularly useful for discriminating between the competing theories for the origin of ultrarelativistic electrons in clusters. Furthermore, if our steep radio spectral index is confirmed by future deeper radio observations, this cluster would provide another example of the recently discovered population of ultra-steep spectrum radio halos, predicted by the model in which the cluster cosmic ray electrons are produced by turbulent reacceleration.
C1 [Giacintucci, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Giacintucci, S.; Markevitch, M.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Dallacasa, D.; Venturi, T.; Brunetti, G.; Cassano, R.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Dallacasa, D.] Univ Bologna, Dept Astron, I-40127 Bologna, Italy.
[Markevitch, M.] NASA, Astrophys Sci Div, High Energy Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Athreya, R. M.] Indian Inst Sci Educ & Res, Pune 411021, Maharashtra, India.
RP Giacintucci, S (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM simona@astro.umd.edu
OI Venturi, Tiziana/0000-0002-8476-6307
FU NASA [PF0-110071]; Chandra X-ray Center (CXC)
FX We thank the staff of the GMRT for their help during the observations.
GMRT is run by the National Centre for Radio Astrophysics of the Tata
Institute of Fundamental Research. S. G. acknowledges the support of
NASA through Einstein Postdoctoral Fellowship PF0-110071 awarded by the
Chandra X-ray Center (CXC), which is operated by SAO. The National Radio
Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc.
NR 38
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FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2011
VL 534
AR A57
DI 10.1051/0004-6361/201117820
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 841ZS
UT WOS:000296554800151
ER
PT J
AU Kruhler, T
Greiner, J
Schady, P
Savaglio, S
Afonso, PMJ
Clemens, C
Elliott, J
Filgas, R
Gruber, D
Kann, DA
Klose, S
Kupcu-Yoldas, A
McBreen, S
Olivares, F
Pierini, D
Rau, A
Rossi, A
Nardini, M
Guelbenzu, AN
Sudilovsky, V
Updike, AC
AF Kruehler, T.
Greiner, J.
Schady, P.
Savaglio, S.
Afonso, P. M. J.
Clemens, C.
Elliott, J.
Filgas, R.
Gruber, D.
Kann, D. A.
Klose, S.
Kuepcue-Yoldas, A.
McBreen, S.
Olivares, F.
Pierini, D.
Rau, A.
Rossi, A.
Nardini, M.
Guelbenzu, A. Nicuesa
Sudilovsky, V.
Updike, A. C.
TI The SEDs and host galaxies of the dustiest GRB afterglows
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gamma-ray burst: general; dust, extinction; galaxies: star formation
ID GAMMA-RAY BURST; STAR-FORMING GALAXIES; STELLAR MASS FUNCTION;
SIMILAR-TO 2; SWIFT-ERA; DARK BURSTS; OPTICAL AFTERGLOWS; COLUMN
DENSITIES; HIGH-REDSHIFT; PHOTOMETRIC REDSHIFTS
AB Context. The afterglows and host galaxies of long gamma-ray bursts (GRBs) offer unique opportunities to study star-forming galaxies in the high-z Universe. Until recently, however, the information inferred from GRB follow-up observations was mostly limited to optically bright afterglows, biasing all demographic studies against sight-lines that contain large amounts of dust.
Aims. Here we present afterglow and host observations for a sample of bursts that are exemplary of previously missed ones because of high visual extinction (A(V)(GRB) >= 1 mag) along the sight-line. This facilitates an investigation of the properties, geometry, and location of the absorbing dust of these poorly-explored host galaxies, and a comparison to hosts from optically-selected samples.
Methods. This work is based on GROND optical/NIR and Swift/XRT X-ray observations of the afterglows, and multi-color imaging for eight GRB hosts. The afterglow and galaxy spectral energy distributions yield detailed insight into physical properties such as the dust and metal content along the GRB sight-line and galaxy-integrated characteristics such as the host's stellar mass, luminosity, color-excess, and star-formation rate.
Results. For the eight afterglows considered in this study, we report for the first time the redshift of GRB 081109 (z = 0.9787 +/- 0.0005), and the visual extinction towards GRBs 081109 (A(V)(GRB) = 3.4(-0.3)(+0.4) mag) and 100621A (A(V)(GRB) = 3.8 +/- 0.2mag), which are among the largest ever derived for GRB afterglows. Combined with non-extinguished GRBs, there is a strong anti-correlation between the afterglow's metal-to-dust ratio and visual extinction. The hosts of the dustiest afterglows are diverse in their properties, but on average redder (<(R -K)(AB)> similar to 1.6 mag), more luminous (< L > similar to 0.9 L*), and massive (< log M*[M-circle dot]> similar to 9.8) than the hosts of optically-bright events. Hence, we probe a different galaxy population, suggesting that previous host samples miss most of the massive and metal-rich members. This also indicates that the dust along the sight-line is often related to host properties, and thus probably located in the diffuse ISM or interstellar clouds and not in the immediate GRB environment. Some of the hosts in our sample, are blue, young, or of low stellar mass illustrating that even apparently non-extinguished galaxies possess very dusty sight-lines owing to a patchy dust distribution.
Conclusions. The afterglows and host galaxies of the dustiest GRBs provide evidence of a complex dust geometry in star-forming galaxies. In addition, they establish a population of luminous, massive, and correspondingly chemically evolved GRB hosts. This suggests that GRBs trace the global star-formation rate better than studies based on optically selected host samples indicate, and that the previously claimed deficiency of high-mass hosts was at least partially a selection effect.
C1 [Kruehler, T.; Greiner, J.; Schady, P.; Savaglio, S.; Afonso, P. M. J.; Clemens, C.; Elliott, J.; Filgas, R.; Gruber, D.; Olivares, F.; Rau, A.; Nardini, M.; Sudilovsky, V.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Kruehler, T.] Tech Univ Munich, D-85748 Garching, Germany.
[Kruehler, T.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Afonso, P. M. J.] Amer River Coll, Phys & Astron Dpt, Sacramento, CA 95841 USA.
[Kann, D. A.; Klose, S.; Rossi, A.; Guelbenzu, A. Nicuesa] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany.
[Kuepcue-Yoldas, A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[McBreen, S.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Nardini, M.] Univ Milano Bicocca, I-20126 Milan, Italy.
[Updike, A. C.] NASA GSFC, CRESST, Greenbelt, MD 20771 USA.
[Updike, A. C.] NASA GSFC, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Updike, A. C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Kruhler, T (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
EM kruehler@mpe.mpg.de
RI Rossi, Andrea/N-4674-2015;
OI Rossi, Andrea/0000-0002-8860-6538; Kruehler, Thomas/0000-0002-8682-2384;
Savaglio, Sandra/0000-0003-2354-3238
FU DFG cluster of excellence; European Commission; Leibniz-Prize [HA
1850/28-1]; Danish National Research Foundation; DFG [SA 2001/1-1, Kl
766/16-1]; MPG [Ext 00003]; BLANCEFLOR Boncompagni-Ludovisi, nee Bildt
foundation; European Union [PERG04-GA-2008-239176]
FX We thank the referee for valuable comments. We also acknowledge helpful
comments from S. Shore, R. Salvaterra, M. Michalowski and E.
Ramirez-Ruiz. T. K. acknowledges support by the DFG cluster of
excellence "Origin and Structure of the Universe" and support by the
European Commission under the Marie Curie IEF Programme in FP7. Part of
the funding for GROND (both hardware as well as personnel) was
generously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG
grant HA 1850/28-1). The Dark Cosmology Centre is funded by the Danish
National Research Foundation. P. S. acknowledges support by DFG grant SA
2001/1-1. S. S. acknowledges support through project M. FE. A. Ext 00003
of the MPG. S. K., D. A. K. and A. N. G. acknowledge support by DFG
grant Kl 766/16-1. A. Ro. acknowledges support from the BLANCEFLOR
Boncompagni-Ludovisi, nee Bildt foundation. S. M. B. acknowledges
support of a European Union Marie Curie European Reintegration Grant
within the 7th Program under contract number PERG04-GA-2008-239176. This
work made use of data supplied by the UK Swift Science Data Centre at
the University of Leicester.
NR 175
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U2 4
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2011
VL 534
AR A108
DI 10.1051/0004-6361/201117428
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 841ZS
UT WOS:000296554800099
ER
PT J
AU Pagani, C
Beardmore, AP
Abbey, AF
Mountford, C
Osborne, JP
Capalbi, M
Perri, M
Angelini, L
Burrows, DN
Campana, S
Cusumano, G
Evans, PA
Kennea, JA
Moretti, A
Page, KL
Starling, RLC
AF Pagani, C.
Beardmore, A. P.
Abbey, A. F.
Mountford, C.
Osborne, J. P.
Capalbi, M.
Perri, M.
Angelini, L.
Burrows, D. N.
Campana, S.
Cusumano, G.
Evans, P. A.
Kennea, J. A.
Moretti, A.
Page, K. L.
Starling, R. L. C.
TI Recovering Swift-XRT energy resolution through CCD charge trap mapping
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays: general; instrumentation: detectors; methods: numerical
ID GAMMA-RAY BURST; X-RAY; RADIATION-DAMAGE; COUPLED-DEVICES; REDSHIFT;
TELESCOPE; EVOLUTION; GALAXY
AB The X-ray telescope on board the Swift satellite for gamma-ray burst astronomy has been exposed to the radiation of the space environment since launch in November 2004. Radiation causes damage to the detector, with the generation of dark current and charge trapping sites that result in the degradation of the spectral resolution and an increase of the instrumental background. The Swift team has a dedicated calibration program with the goal of recovering a significant proportion of the lost spectroscopic performance. Calibration observations of supernova remnants with strong emission lines are analysed to map the detector charge traps and to derive position-dependent corrections to the measured photon energies. We have achieved a substantial recovery in the XRT resolution by implementing these corrections in an updated version of the Swift XRT gain file and in corresponding improvements to the Swift XRT HEAsoft software. We provide illustrations of the impact of the enhanced energy resolution, and show that we have recovered most of the spectral resolution lost since launch.
C1 [Pagani, C.; Beardmore, A. P.; Abbey, A. F.; Mountford, C.; Osborne, J. P.; Evans, P. A.; Page, K. L.; Starling, R. L. C.] Univ Leicester, Dept Phys & Astron, Xray & Observat Astron Grp, Leicester LE1 7RH, Leics, England.
[Capalbi, M.; Perri, M.] ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Angelini, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Campana, S.; Moretti, A.] State Univ, University Pk, PA 16802 USA.
[Cusumano, G.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy.
INAF Ist Astrofis Spaziale & Fis Cosm, Sez Palermo, I-90146 Palermo, Italy.
RP Pagani, C (reprint author), Univ Leicester, Dept Phys & Astron, Xray & Observat Astron Grp, Leicester LE1 7RH, Leics, England.
EM cp232@star.le.ac.uk
OI Campana, Sergio/0000-0001-6278-1576; Cusumano,
Giancarlo/0000-0002-8151-1990; moretti, alberto/0000-0002-9770-0315;
Perri, Matteo/0000-0003-3613-4409
FU UK Space Agency; ASI [I/R/011/07/0]; NASA [NAS5-00136]
FX We thank the Swift science planners, Jonathan Gelbord, Craig Swenson,
Michael Stroh, and Chris Wolf, for their efforts in scheduling the long
and complex trap mapping calibration observations. C.P., A.P.B., A.F.A.,
C.M., J.P.O., P.A.E., K.L.P., gratefully acknowledge the support of the
UK Space Agency. This work is supported at INAF by funding from ASI
through grant I/R/011/07/0. D.N.B. and J.A.K. acknowledge support by
NASA contract NAS5-00136. This work made use of the data supplied by the
UK Swift Science Data Centre at the University of Leicester. This
research has made use of the XRT Data Analysis Software (XRTDAS)
developed under the responsibility of the ASI Science Data Center
(ASDC), Italy.
NR 33
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2011
VL 534
AR A20
DI 10.1051/0004-6361/201117660
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 841ZS
UT WOS:000296554800133
ER
PT J
AU Raiteri, CM
Villata, M
Aller, MF
Gurwell, MA
Kurtanidze, OM
Lahteenmaki, A
Larionov, VM
Romano, P
Vercellone, S
Agudo, I
Aller, HD
Arkharov, AA
Bach, U
Benitez, E
Berdyugin, A
Blinov, DA
Borisova, EV
Bottcher, M
Calle, OJAB
Buemi, CS
Calcidese, P
Carosati, D
Casas, R
Chen, WP
Efimova, NV
Gomez, JL
Gusbar, C
Hawkins, K
Heidt, J
Hiriart, D
Hsiao, HY
Jordan, B
Jorstad, SG
Joshi, M
Kimeridze, GN
Koptelova, E
Konstantinova, TS
Kopatskaya, EN
Kurtanidze, SO
Larionova, EG
Larionova, LV
Leto, P
Li, Y
Ligustri, R
Lindfors, E
Lister, M
Marscher, AP
Molina, SN
Morozova, DA
Nieppola, E
Nikolashvili, MG
Nilsson, K
Palma, N
Pasanen, M
Reinthal, R
Roberts, V
Ros, JA
Roustazadeh, P
Sadun, AC
Sakamoto, T
Schwartz, RD
Sigua, LA
Sillanpaa, A
Takalo, LO
Tammi, J
Taylor, B
Tornikoski, M
Trigilio, C
Troitsky, IS
Umana, G
Volvach, A
Yuldasheva, TA
AF Raiteri, C. M.
Villata, M.
Aller, M. F.
Gurwell, M. A.
Kurtanidze, O. M.
Lahteenmaki, A.
Larionov, V. M.
Romano, P.
Vercellone, S.
Agudo, I.
Aller, H. D.
Arkharov, A. A.
Bach, U.
Benitez, E.
Berdyugin, A.
Blinov, D. A.
Borisova, E. V.
Casas, R.
Calle, O. J. A. Bravo
Buemi, C. S.
Calcidese, P.
Carosati, D.
Casas, R.
Chen, W-P.
Efimova, N. V.
Gomez, J. L.
Gusbar, C.
Hawkins, K.
Heidt, J.
Hiriart, D.
Hsiao, H. Y.
Jordan, B.
Jorstad, S. G.
Joshi, M.
Kimeridze, G. N.
Koptelova, E.
Konstantinova, T. S.
Kopatskaya, E. N.
Kurtanidze, S. O.
Larionova, E. G.
Larionova, L. V.
Leto, P.
Li, Y.
Ligustri, R.
Lindfors, E.
Lister, M.
Marscher, A. P.
Molina, S. N.
Morozova, D. A.
Nieppola, E.
Nikolashvili, M. G.
Nilsson, K.
Palma, N.
Pasanen, M.
Reinthal, R.
Roberts, V.
Ros, J. A.
Roustazadeh, P.
Sadun, A. C.
Sakamoto, T.
Schwartz, R. D.
Sigua, L. A.
Sillanpaa, A.
Takalo, L. O.
Tammi, J.
Taylor, B.
Tornikoski, M.
Trigilio, C.
Troitsky, I. S.
Umana, G.
Volvach, A.
Yuldasheva, T. A.
TI The long-lasting activity of 3C 454.3 GASP-WEBT and satellite
observations in 2008-2010
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; quasars: general; quasars: individual: 3C 454.3;
galaxies: jets
ID SPACE-TELESCOPE OBSERVATIONS; GAMMA-RAY FLARE; GALACTIC NUCLEI;
BL-LACERTAE; BLAZAR 3C-454.3; MULTIWAVELENGTH OBSERVATIONS; INFRARED
OBSERVATIONS; RADIO VARIABILITY; AGILE DETECTION; CRAZY-DIAMOND
AB Context. The blazar 3C 454.3 is one of the most active sources from the radio to the gamma-ray frequencies observed in the past few years.
Aims. We present multiwavelength observations of this source from April 2008 to March 2010. The radio to optical data are mostly from the GASP-WEBT, UV and X-ray data from Swift, and gamma-ray data from the AGILE and Fermi satellites. The aim is to understand the connection among emissions at different frequencies and to derive information on the emitting jet.
Methods. Light curves in 18 bands were carefully assembled to study flux variability correlations. We improved the calibration of optical-UV data from the UVOT and OM instruments and estimated the Ly alpha flux to disentangle the contributions from different components in this spectral region.
Results. The observations reveal prominent variability above 8 GHz. In the optical-UV band, the variability amplitude decreases with increasing frequency due to a steadier radiation from both a broad line region and an accretion disc. The optical flux reaches nearly the same levels in the 2008-2009 and 2009-2010 observing seasons; the mm one shows similar behaviour, whereas the gamma and X-ray flux levels rise in the second period. Two prominent gamma-ray flares in mid 2008 and late 2009 show a double-peaked structure, with a variable gamma/optical flux ratio. The X-ray flux variations seem to follow the gamma-ray and optical ones by about 0.5 and 1 d, respectively.
Conclusions. We interpret the multifrequency behaviour in terms of an inhomogeneous curved jet, where synchrotron radiation of increasing wavelength is produced in progressively outer and wider jet regions, which can change their orientation in time. In particular, we assume that the long-term variability is due to this geometrical effect. By combining the optical and mm light curves to fit the gamma and X-ray ones, we find that the gamma (X-ray) emission may be explained by inverse-Comptonisation of synchrotron optical (IR) photons by their parent relativistic electrons (SSC process). A slight, variable misalignment between the synchrotron and Comptonisation zones would explain the increased gamma and X-ray flux levels in 2009-2010, as well as the change in the gamma/optical flux ratio during the outbursts peaks. The time delays of the X-ray flux changes after the gamma, and optical ones are consistent with the proposed scenario.
C1 [Raiteri, C. M.; Villata, M.] Osserv Astron Torino, INAF, Turin, Italy.
[Aller, M. F.; Aller, H. D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kurtanidze, O. M.; Kimeridze, G. N.; Kurtanidze, S. O.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, Abastumani, Rep of Georgia.
[Lahteenmaki, A.; Nieppola, E.; Tammi, J.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, Kylmala, Finland.
[Larionov, V. M.; Blinov, D. A.; Borisova, E. V.; Calle, O. J. A. Bravo; Efimova, N. V.; Jorstad, S. G.; Konstantinova, T. S.; Kopatskaya, E. N.; Larionova, E. G.; Larionova, L. V.; Morozova, D. A.; Troitsky, I. S.; Yuldasheva, T. A.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia.
[Larionov, V. M.; Arkharov, A. A.; Efimova, N. V.] Pulkovo Observ, St Petersburg, Russia.
[Larionov, V. M.; Blinov, D. A.] St Petersburg Branch, Isaac Newton Inst Chile, St Petersburg, Russia.
[Romano, P.; Vercellone, S.] INAF IASF Palermo, Palermo, Italy.
[Agudo, I.; Gomez, J. L.; Molina, S. N.] CSIC, Inst Astrofis Andalucia, Granada, Spain.
[Agudo, I.; Jorstad, S. G.; Joshi, M.; Marscher, A. P.; Taylor, B.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
[Bach, U.] Max Planck Inst Radioastron, D-5300 Bonn, Germany.
[Benitez, E.; Hiriart, D.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Berdyugin, A.; Lindfors, E.; Pasanen, M.; Reinthal, R.; Sillanpaa, A.; Takalo, L. O.] Univ Turku, Tuorla Observ, Piikkio, Finland.
[Casas, R.; Gusbar, C.; Hawkins, K.; Li, Y.; Palma, N.; Roberts, V.; Roustazadeh, P.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA.
[Buemi, C. S.; Leto, P.; Trigilio, C.; Umana, G.] Osserv Astrofis Catania, INAF, Catania, Italy.
[Calcidese, P.] Osservatorio Astron Reg Autonoma Valle dAosta, St Barthelemy, Italy.
[Carosati, D.] EPT Observ, Tijarafe, La Palma, Spain.
[Carosati, D.] TNG Fdn Galileo Galilei, INAF, La Palma, Spain.
[Casas, R.] Inst Ciencies Espai CSIC IEEC, Barcelona, Spain.
[Casas, R.; Ros, J. A.] Agrupacio Astron Sabadell, Sabadell, Spain.
[Chen, W-P.; Hsiao, H. Y.; Koptelova, E.] Natl Cent Univ, Grad Inst, Jhongli, Taiwan.
[Heidt, J.] Landessternwarte Heidelberg Konigstuhl, ZAH, Heidelberg, Germany.
[Hsiao, H. Y.] Natl Cent Univ, Lulin Observ, Jhongli, Taiwan.
[Jordan, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin, Ireland.
[Koptelova, E.] Natl Taiwan Univ, Dept Phys, Taipei, Taiwan.
[Ligustri, R.] Circolo Astrofili Talmassons, Talmassons, Italy.
[Lister, M.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Nieppola, E.; Nilsson, K.] Univ Turku, Finnish Ctr Astron ESO FINCA, Piikkio, Finland.
[Palma, N.] Univ Nacl Autonoma Honduras, Fac Ciencias Espaciales, Tegucigalpa Mdc, Honduras.
[Sadun, A. C.] Univ Colorado Denver, Dept Phys, Denver, CO USA.
[Sakamoto, T.] NASA, Ctr Res & Explorat Space Sci & Technol, GSFC, Greenbelt, MD USA.
[Schwartz, R. D.] Galaxy View Observ, Sequim, WA USA.
[Taylor, B.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Volvach, A.] Crimean Astrophys Observ, Radio Astron Lab, Crimea, Ukraine.
RP Raiteri, CM (reprint author), Osserv Astron Torino, INAF, Turin, Italy.
EM raiteri@oato.inaf.it; villata@oato.inaf.it
RI Kurtanidze, Omar/J-6237-2014; Molina, Sol Natalia/F-9968-2015; Agudo,
Ivan/G-1701-2015; Morozova, Daria/H-1298-2013; Larionov,
Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Larionova,
Elena/H-7287-2013; Troitskiy, Ivan/K-7979-2013; Jorstad,
Svetlana/H-6913-2013; Efimova, Natalia/I-2196-2013; Blinov,
Dmitry/G-9925-2013; Lahteenmaki, Anne/L-5987-2013; Grishina,
Tatiana/H-6873-2013;
OI Molina, Sol Natalia/0000-0002-4112-2157; Agudo,
Ivan/0000-0002-3777-6182; Morozova, Daria/0000-0002-9407-7804; Larionov,
Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X;
Larionova, Elena/0000-0002-2471-6500; Troitskiy,
Ivan/0000-0002-4218-0148; Jorstad, Svetlana/0000-0001-9522-5453;
Efimova, Natalia/0000-0002-8071-4753; Blinov,
Dmitry/0000-0003-0611-5784; Grishina, Tatiana/0000-0002-3953-6676;
Villata, Massimo/0000-0003-1743-6946; Larionova,
Liudmila/0000-0002-0274-1481; Leto, Paolo/0000-0003-4864-2806;
Vercellone, Stefano/0000-0003-1163-1396; Raiteri, Claudia
Maria/0000-0003-1784-2784
FU ASI-INAF I/009/10/0; Russian RFBR foundation [09-02-00092]; Georgian
National Science Foundation [GNSF/ST08/4-404]; Academy of Finland
[212656, 210338, 121148]; NASA [NNX09AU16G, NNX10AP16G, NNX08AV65G,
NNX08AV61G, NNX09AT99G]; NSF [AST-0607523, AST-0907893]; University of
Michigan; MICIIN (Spain) [AYA2010-14844]; CEIC (Andalucia)
[P09-FQM-4784]; Smithsonian Institution; Academia Sinica; BU; Lowell
Observatory
FX C.M.R. is grateful to Stefania Rasetti from the Torino Observatory
Computer Centre for her assistance. We thank the Fermi-LAT team for
providing Fermi data. We acknowledge the use of public data from the
Swift data archive. We acknowledge financial contribution from the
agreement ASI-INAF I/009/10/0. St.-Petersburg University team
acknowledges support from Russian RFBR foundation via grant 09-02-00092.
Abastumani Observatory team acknowledges financial support by the
Georgian National Science Foundation through grant GNSF/ST08/4-404. The
Metsahovi team acknowledges the support from the Academy of Finland to
our observing projects (numbers 212656, 210338, 121148, and others). The
University of Michigan team acknowledges financial support through the
NASA Fermi grants NNX09AU16G, NNX10AP16G, and NSF grant AST-0607523. The
operation of UMRAO is funded by the University of Michigan. This paper
is partly based on observations carried out at the German-Spanish Calar
Alto Observatory, which is jointly operated by the MPIA and the
IAA-CSIC. Acquisition of the MAPCAT data is supported in part by MICIIN
(Spain) grant and AYA2010-14844, and by CEIC (Andalucia) grant
P09-FQM-4784. Partly based on observations with the Medicina and Noto
telescopes operated by INAF - Istituto di Radioastronomia. This research
has made use of NASA's Astrophysics Data System and of the XRT Data
Analysis Software (XRTDAS) developed under the responsibility of the ASI
Science Data Center (ASDC), Italy. This research has made use of data
from the MOJAVE database that is maintained by the MOJAVE team (Lister
et al. 2009). The Submillimeter Array is a joint project between the
Smithsonian Astrophysical Observatory and the Academia Sinica Institute
of Astronomy and Astrophysics and is funded by the Smithsonian
Institution and the Academia Sinica. The research at Boston U. was
supported by NSF grant AST-0907893 and NASA Fermi GI grants NNX08AV65G,
NNX08AV61G, and NNX09AT99G. The PRISM camera at Lowell Observatory was
developed by K. Janes et al. at BU and Lowell Observatory, with funding
from the NSF, BU, and Lowell Observatory.
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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 OCT
PY 2011
VL 534
AR A87
DI 10.1051/0004-6361/201117026
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 841ZS
UT WOS:000296554800047
ER
PT J
AU Uytterhoeven, K
Moya, A
Grigahcene, A
Guzik, JA
Gutierrez-Soto, J
Smalley, B
Handler, G
Balona, LA
Niemczura, E
Machado, LF
Benatti, S
Chapellier, E
Tkachenko, A
Szabo, R
Suarez, JC
Ripepi, V
Pascual, J
Mathias, P
Martin-Ruiz, S
Lehmann, H
Jackiewicz, J
Hekker, S
Gruberbauer, M
Garcia, RA
Dumusque, X
Diaz-Fraile, D
Bradley, P
Antoci, V
Roth, M
Leroy, B
Murphy, SJ
De Cat, P
Cuypers, J
Kjeldsen, H
Christensen-Dalsgaard, J
Breger, M
Pigulski, A
Kiss, LL
Still, M
Thompson, SE
Van Cleve, J
AF Uytterhoeven, K.
Moya, A.
Grigahcene, A.
Guzik, J. A.
Gutierrez-Soto, J.
Smalley, B.
Handler, G.
Balona, L. A.
Niemczura, E.
Fox Machado, L.
Benatti, S.
Chapellier, E.
Tkachenko, A.
Szabo, R.
Suarez, J. C.
Ripepi, V.
Pascual, J.
Mathias, P.
Martin-Ruiz, S.
Lehmann, H.
Jackiewicz, J.
Hekker, S.
Gruberbauer, M.
Garcia, R. A.
Dumusque, X.
Diaz-Fraile, D.
Bradley, P.
Antoci, V.
Roth, M.
Leroy, B.
Murphy, S. J.
De Cat, P.
Cuypers, J.
Kjeldsen, H.
Christensen-Dalsgaard, J.
Breger, M.
Pigulski, A.
Kiss, L. L.
Still, M.
Thompson, S. E.
Van Cleve, J.
TI The Kepler characterization of the variability among A- and F-type stars
I. General overview
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: oscillations; stars: fundamental parameters; binaries: general;
asteroseismology; stars: variables: delta Scuti; stars: statistics
ID GAMMA-DORADUS STARS; DELTA-SCUTI STARS; HIGH-RESOLUTION SPECTROSCOPY;
TIME-SERIES ANALYSIS; MAIN-SEQUENCE STARS; RR LYRAE STARS;
FIELD-OF-VIEW; SPECTRAL CLASSIFICATION; FUNDAMENTAL PARAMETERS;
ASTEROSEISMIC TARGETS
AB Context. The Kepler spacecraft is providing time series of photometric data with micromagnitude precision for hundreds of A-F type stars.
Aims. We present a first general characterization of the pulsational behaviour of A-F type stars as observed in the Kepler light curves of a sample of 750 candidate A-F type stars, and observationally investigate the relation between gamma Doradus (gamma Dor), delta Scuti (delta Sct), and hybrid stars.
Methods. We compile a database of physical parameters for the sample stars from the literature and new ground-based observations. We analyse the Kepler light curve of each star and extract the pulsational frequencies using different frequency analysis methods. We construct two new observables, "energy" and "efficiency", related to the driving energy of the pulsation mode and the convective efficiency of the outer convective zone, respectively.
Results. We propose three main groups to describe the observed variety in pulsating A-F type stars: gamma Dor, delta Sct, and hybrid stars. We assign 63% of our sample to one of the three groups, and identify the remaining part as rotationally modulated/active stars, binaries, stars of different spectral type, or stars that show no clear periodic variability. 23% of the stars (171 stars) are hybrid stars, which is a much higher fraction than what has been observed before. We characterize for the first time a large number of A-F type stars (475 stars) in terms of number of detected frequencies, frequency range, and typical pulsation amplitudes. The majority of hybrid stars show frequencies with all kinds of periodicities within the gamma Dor and delta Sct range, also between 5 and 10 d(-1), which is a challenge for the current models. We find indications for the existence of delta Sct and gamma Dor stars beyond the edges of the current observational instability strips. The hybrid stars occupy the entire region within the delta Sct and gamma Dor instability strips and beyond. Non-variable stars seem to exist within the instability strips. The location of gamma Dor and delta Sct classes in the (T-eff, log g)-diagram has been extended. We investigate two newly constructed variables, "efficiency" and "energy", as a means to explore the relation between gamma Dor and delta Sct stars.
Conclusions. Our results suggest a revision of the current observational instability strips of delta Sct and gamma Dor stars and imply an investigation of pulsation mechanisms to supplement the kappa mechanism and convective blocking effect to drive hybrid pulsations. Accurate physical parameters for all stars are needed to confirm these findings.
C1 [Uytterhoeven, K.; Garcia, R. A.] Univ Paris Diderot, Lab AIM, CEA DSM CNRS, IRFU,SAp,Ctr Saclay, F-91191 Gif Sur Yvette, France.
[Uytterhoeven, K.; Roth, M.] Kiepenheuer Inst Sonnenphys, D-79104 Freiburg, Germany.
[Uytterhoeven, K.] Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain.
[Uytterhoeven, K.] Inst Astrofis Canarias, Tenerife 38200, Spain.
[Moya, A.] INTA CSIC, LAEX CAB, Madrid 28691, Spain.
[Grigahcene, A.; Dumusque, X.] Univ Porto, Ctr Astrofis, Fac Ciencias, P-4150762 Oporto, Portugal.
[Guzik, J. A.; Bradley, P.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Gutierrez-Soto, J.; Suarez, J. C.; Pascual, J.; Martin-Ruiz, S.; Diaz-Fraile, D.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Gutierrez-Soto, J.; Leroy, B.] Univ Paris Diderot, UPMC, LESIA, Observ Paris,CNRS, F-92195 Meudon, France.
[Gutierrez-Soto, J.] Valentian Int Univ, Castellon De La Plana 12006, Spain.
[Smalley, B.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Handler, G.; Gruberbauer, M.; Antoci, V.; Breger, M.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Handler, G.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Balona, L. A.] S African Astron Observ, ZA-7935 Observatory, South Africa.
[Niemczura, E.; Pigulski, A.] Uniwersytet Wroclawski, Inst Astron, PL-51622 Wroclaw, Poland.
[Fox Machado, L.] UNAM, Observ Astron Nacl, Inst Astron, Ensenada, Baja California, Mexico.
[Benatti, S.] Univ Padua, CISAS, I-35131 Padua, Italy.
[Benatti, S.] INAF Astron Observ Padova, I-35122 Padua, Italy.
[Chapellier, E.] UNS, CNRS, OCA, UMR H Fizeau 6525, F-06108 Nice 2, France.
[Tkachenko, A.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Szabo, R.; Kiss, L. L.] Hungarian Acad Sci, Konkoly Observ, H-1525 Budapest, Hungary.
[Ripepi, V.] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy.
[Mathias, P.] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-65000 Tarbes, France.
[Lehmann, H.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany.
[Jackiewicz, J.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88001 USA.
[Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Hekker, S.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Gruberbauer, M.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Dumusque, X.] Univ Geneva, Observ Geneve, CH-1290 Sauverny, Switzerland.
[Murphy, S. J.] Univ Cent Lancashire, Jeremiah Horrocks Inst Astrophys, Preston PR1 2HE, Lancs, England.
[De Cat, P.; Cuypers, J.] Royal Observ Belgium, B-1180 Brussels, Belgium.
[Kjeldsen, H.; Christensen-Dalsgaard, J.] Univ Aarhus, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Breger, M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Kiss, L. L.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia.
[Still, M.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Thompson, S. E.; Van Cleve, J.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
RP Uytterhoeven, K (reprint author), Univ Paris Diderot, Lab AIM, CEA DSM CNRS, IRFU,SAp,Ctr Saclay, F-91191 Gif Sur Yvette, France.
EM katrien@iac.es
RI Martin-Ruiz, Susana/B-6768-2013; Gutierrez-Soto, Juan/H-9620-2015;
Suarez, Juan Carlos/C-1015-2009;
OI Gutierrez-Soto, Juan/0000-0001-6736-0551; Suarez, Juan
Carlos/0000-0003-3649-8384; Murphy, Simon/0000-0002-5648-3107; Antoci,
Victoria/0000-0002-0865-3650; Bradley, Paul/0000-0001-6229-6677; Szabo,
Robert/0000-0002-3258-1909; Garcia, Rafael/0000-0002-8854-3776
FU NASA's Science Mission Directorate; Deutsche Forschungsgemeinschaft
(DFG) [UY 52/1-1]; Spanish National Plan of RD [AYA2010-17803];
AstroMadrid [CAM S2009/ESP-1496]; MNiSW [NN 203 405139, NN 203 302635];
Austrian Fonds zur Forderung der wissenschaftlichen Forschung
[P20526-N16]; UNAM [PAPIIT IN114309]; Hungarian Academy of Sciences;
Hungarian OTKA [K83790, MB08C 81013]; Netherlands Organisation for
Scientific Research (NWO); Spanish [ESP2007-65475-C02-02, AYA
2010-21161-C02-02, CSD2006-00070]; European Community [269194]
FX We are grateful to Joanna Molenda-Zakowicz, James Nemec and the
anonymous referee for their suggestions and comments to improve this
paper. Funding for the Kepler mission is provided by NASA's Science
Mission Directorate. We thank the entire Kepler team for the development
and operations of this outstanding mission. K. U. acknowledges financial
support by the Deutsche Forschungsgemeinschaft (DFG) in the framework of
project UY 52/1-1, and by the Spanish National Plan of R&D for 2010,
project AYA2010-17803. A. M. acknowledges the funding of AstroMadrid
(CAM S2009/ESP-1496). E.N. and A. P. acknowledge the financial support
of the NN 203 405139 and NN 203 302635 grant, respectively, from the
MNiSW. The work by G. H. and V. A. was supported by the Austrian Fonds
zur Forderung der wissenschaftlichen Forschung under grant P20526-N16.
L. F. M. acknowledge financial support from the UNAM under grant PAPIIT
IN114309. R.Sz. and L. L. K. have been supported by the "Lendulet"
program of the Hungarian Academy of Sciences and the Hungarian OTKA
grants K83790 and MB08C 81013. RSz was supported by the Janos Bolyai
Research Scholarship of the Hungarian Academy of Sciences. SH
acknowledges financial support from the Netherlands Organisation for
Scientific Research (NWO). This research has been funded by the Spanish
grants ESP2007-65475-C02-02, AYA 2010-21161-C02-02 and CSD2006-00070.
The research leading to these results has received funding from the
European Community's Seventh Framework Programme (FP7/2007-2013) under
grant agreement No. 269194. This research has made use of the SIMBAD
database, operated at CDS, Strasbourg, France, and is partly based on
observations obtained at the Observatorio Astronomico Nacional-San Pedro
Martir (OAN-SPM), Baja California, Mexico, at the Observatoire de Haute
Provence, France, and at the Thuringer Landessternwarte Tautenburg,
Germany. We acknowledge with thanks the variable star observations from
the AAVSO International Database contributed by observers worldwide and
used in this research.
NR 159
TC 105
Z9 105
U1 0
U2 10
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 OCT
PY 2011
VL 534
AR A125
DI 10.1051/0004-6361/201117368
PG 70
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 841ZS
UT WOS:000296554800089
ER
PT J
AU Woitke, P
Riaz, B
Duchene, G
Pascucci, I
Lyo, AR
Dent, WRF
Phillips, N
Thi, WF
Menard, F
Herczeg, GJ
Bergin, E
Brown, A
Mora, A
Kamp, I
Aresu, G
Brittain, S
de Gregorio-Monsalvo, I
Sandell, G
AF Woitke, P.
Riaz, B.
Duchene, G.
Pascucci, I.
Lyo, A. -R.
Dent, W. R. F.
Phillips, N.
Thi, W. -F.
Menard, F.
Herczeg, G. J.
Bergin, E.
Brown, A.
Mora, A.
Kamp, I.
Aresu, G.
Brittain, S.
de Gregorio-Monsalvo, I.
Sandell, G.
TI The unusual protoplanetary disk around the T Tauri star ET Chamaeleontis
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: pre-main sequence; protoplanetary disks; astrochemistry;
radiative transfer; line: formation; stars: individual: ET Cha
ID MAIN-SEQUENCE STARS; INTERSTELLAR SILICATE MINERALOGY; RADIATION
THERMOCHEMICAL MODELS; DIRTY DUST GRAINS; ETA-CHAMAELEONTIS;
MOLECULAR-HYDROGEN; INFRARED-EMISSION; YOUNG STARS; GAS MASS;
PLANETARY-SYSTEMS
AB We present new continuum and line observations, along with modelling, of the faint (6-8) Myr old T Tauri star ET Cha belonging to the eta Chamaeleontis cluster. We have acquired Herschel/PACS photometric fluxes at 70 mu m and 160 mu m, as well as a detection of the [OI] 63 mu m fine-structure line in emission, and derived upper limits for some other far-IR OI, CII, CO and o-H2O lines. These observations were carried out in the frame of the open time key programme GASPS, where ETCha was selected as one of the science demonstration phase targets. The Herschel data is complemented by new simultaneous ANDICAM B-K photometry, new HST/COS and HST/STIS UV-observations, a non-detection of CO J = 3 -> 2 with APEX, re-analysis of a UCLES high-resolution optical spectrum showing forbidden emission lines like [OI] 6300 angstrom, [SII] 6731 angstrom and 6716 angstrom, and [NII] 6583 angstrom, and a compilation of existing broad-band photometric data. We used the thermo-chemical disk code ProDiMo and the Monte-Carlo radiative transfer code MCFOST to model the protoplanetary disk around ETCha. The paper also introduces a number of physical improvements to the ProDiMo disk modelling code concerning the treatment of PAH ionisation balance and heating, the heating by exothermic chemical reactions, and several non-thermal pumping mechanisms for selected gas emission lines. By applying an evolutionary strategy to minimise the deviations between model predictions and observations, we find a variety of united gas and dust models that simultaneously fit all observed line and continuum fluxes about equally well. Based on these models we can determine the disk dust mass with confidence, M-dust approximate to (2-5) x 10(-8) M-circle dot whereas the total disk gas mass is found to be only little constrained, M-gas approximate to (5 x 10(-5)-3 x 10(-3)) M-circle dot. Both mass estimates are substantially lower than previously reported. In the models, the disk extends from 0.022 AU (just outside of the co-rotation radius) to only about 10 AU, remarkably small for single stars, whereas larger disks are found to be inconsistent with the CO J = 3 -> 2 non-detection. The low velocity component of the [OI] 6300 angstrom emission line is centred on the stellar systematic velocity, and is consistent with being emitted from the inner disk. The model is also consistent with the line flux of H-2 v = 1 -> 0 S(1) at 2.122 mu m and with the [OI] 63 mu m line as seen with Herschel/PACS. An additional high-velocity component of the [OI] 6300 angstrom emission line, however, points to the existence of an additional jet/outflow of low velocity 40-65 km s(-1) with mass loss rate approximate to 10(-9) M-circle dot/yr. In relation to our low estimations of the disk mass, such a mass loss rate suggests a disk lifetime of only similar to 0.05-3 Myr, substantially shorter than the cluster age. If a generic gas/dust ratio of 100 was assumed, the disk lifetime would be even shorter, only similar to 3000 yrs. The evolutionary state of this unusual protoplanetary disk is discussed.
C1 [Woitke, P.] Univ Vienna, Dept Astron, A-1180 Vienna, Austria.
[Woitke, P.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Woitke, P.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Riaz, B.; Pascucci, I.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Duchene, G.; Thi, W. -F.; Menard, F.] UJF Grenoble 1, CNRS INSU, Inst Planetol & Astrophys IPAG, UMR 5274, F-38041 Grenoble, France.
[Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Kamp, I.; Aresu, G.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Lyo, A. -R.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Sandell, G.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA.
[Dent, W. R. F.; de Gregorio-Monsalvo, I.] ESO ALMA, Santiago, Chile.
[Brittain, S.] Clemson Univ, Clemson, SC USA.
[Mora, A.] ESA ESAC Gaia SOC, Madrid 28691, Spain.
[Phillips, N.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Herczeg, G. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Brown, A.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
RP Woitke, P (reprint author), Univ Vienna, Dept Astron, Turkenschanzstr 17, A-1180 Vienna, Austria.
EM ptw@roe.ac.uk
RI Brittain, Sean/K-9001-2012
OI Brittain, Sean/0000-0001-5638-1330
FU SUPA astrobiology fellowship; NASA/JPL; ANR [ANR-07-BLAN-0221]; PNPS;
CNES; Ministerio de Ciencia e Innovacion (Spain) [AYA 2008-06189-C03];
Consejeria de Innovacion y Ciencia y Empresa of Junta de Andalucia,
(Spain)
FX We thank Catherine Dougados for fruitful discussions about the
properties of disk outflows and the interpretation of optical emission
lines. W.-F. Thi acknowledges a SUPA astrobiology fellowship. I.
Pascucci and B. Riaz acknowledge NASA/JPL for funding support. The LAOG
group acknowledges PNPS, CNES and ANR (contract ANR-07-BLAN-0221) for
financial support. I. de Gregorio-Monsalvo is partially supported by
Ministerio de Ciencia e Innovacion (Spain), grant AYA 2008-06189-C03
(including FEDER funds), and by Consejeria de Innovacion y Ciencia y
Empresa of Junta de Andalucia, (Spain).
NR 96
TC 33
Z9 34
U1 0
U2 7
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2011
VL 534
AR A44
DI 10.1051/0004-6361/201116684
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 841ZS
UT WOS:000296554800021
ER
PT J
AU Lewis, WE
Im, E
Tanelli, S
Haddad, Z
Tripoli, GJ
Smith, EA
AF Lewis, William E.
Im, Eastwood
Tanelli, Simone
Haddad, Ziad
Tripoli, Gregory J.
Smith, Eric A.
TI Geostationary Doppler Radar and Tropical Cyclone Surveillance
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID SATELLITE IMAGERY; INTENSITY; ALGORITHM; SCHEME; WIND
AB The potential usefulness of spaceborne Doppler radar as a tropical cyclone observing tool is assessed by conducting a high-resolution simulation of an intense hurricane and generating synthetic observations of reflectivity and radial velocity. The ground-based velocity track display (GBVTD) technique is used to process the radial velocity observations and generate retrievals of meteorologically relevant metrics such as the maximum wind (MW), radius of maximum wind (RMW), and radius of 64-kt wind (R64). Results indicate that the performance of the retrieved metrics compares favorably with the current state-of-the-art satellite methods for intensity estimation and somewhat better than current methods for structure (i.e., wind radii).
C1 [Lewis, William E.] Univ Wisconsin, Ctr Space Sci & Engn, Dept Atmospher & Ocean Sci, Madison, WI 53706 USA.
[Im, Eastwood; Tanelli, Simone; Haddad, Ziad] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Smith, Eric A.] Ctr Res Changing Earth Syst, Clarksville, MD USA.
RP Lewis, WE (reprint author), Univ Wisconsin, Ctr Space Sci & Engn, Dept Atmospher & Ocean Sci, 1225 W Dayton St, Madison, WI 53706 USA.
EM welewis@wisc.edu
FU National Aeronautics and Space Administration [NNG04GA36G]
FX This research was supported by National Aeronautics and Space
Administration Grant NNG04GA36G. The contributions by Drs. Eastwood Im,
Simone Tanelli, and Ziad Haddad were performed at the Jet Propulsion
Laboratory, California Institute of Technology under contract with the
National Aeronautics and Space Administration. The authors thank two
anonymous reviewers whose comments led to significant improvements in
the final version of the manuscript.
NR 19
TC 1
Z9 1
U1 0
U2 3
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 OCT
PY 2011
VL 28
IS 10
BP 1185
EP 1191
DI 10.1175/JTECH-D-11-00060.1
PG 7
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 843FP
UT WOS:000296658000001
ER
PT J
AU Berkoff, TA
Sorokin, M
Stone, T
Eck, TF
Hoff, R
Welton, E
Holben, B
AF Berkoff, Timothy A.
Sorokin, Mikail
Stone, Tom
Eck, Thomas F.
Hoff, Raymond
Welton, Ellsworth
Holben, Brent
TI Nocturnal Aerosol Optical Depth Measurements with a Small-Aperture
Automated Photometer Using the Moon as a Light Source
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID MOUNTAIN SITE; CALIBRATION; VALIDATION; POLLUTION; AERONET; NETWORK;
SMOKE; DUST
AB A method is described that enables the use of lunar irradiance to obtain nighttime aerosol optical depth (AOD) measurements using a small-aperture photometer. In this approach, the U.S. Geological Survey lunar calibration system was utilized to provide high-precision lunar exoatmospheric spectral irradiance predictions for a ground-based sensor location, and when combined with ground measurement viewing geometry, provided the column optical transmittance for retrievals of AOD. Automated multiwavelength lunar measurements were obtained using an unmodified Cimel-318 sunphotometer sensor to assess existing capabilities and enhancements needed for day/night operation in NASA's Aerosol Robotic Network (AERONET). Results show that even existing photometers can provide the ability for retrievals of aerosol optical depths at night near full moon. With an additional photodetector signal-to-noise improvement of 10-100, routine use over the bright half of the lunar phase and a much wider range of wavelengths and conditions can be achieved. Although the lunar cycle is expected to limit the frequency of observations to 30%-40% compared to solar measurements, nevertheless this is an attractive extension of AERONET capabilities.
C1 [Berkoff, Timothy A.; Welton, Ellsworth; Holben, Brent] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Berkoff, Timothy A.; Eck, Thomas F.; Hoff, Raymond] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
[Sorokin, Mikail] Sigma Res Inc, Lanham, MD USA.
[Stone, Tom] US Geol Survey, Flagstaff, AZ 86001 USA.
RP Berkoff, TA (reprint author), NASA, Goddard Space Flight Ctr, Code 613-1, Greenbelt, MD 20771 USA.
EM berkoff@umbc.edu
RI Welton, Ellsworth/A-8362-2012; ECK, THOMAS/D-7407-2012
FU NASA; MPLNET; USGS ROLO; UMBC
FX The authors wish to acknowledge Marius Canini (Cimel Eletronique), Nader
Abuhassan (UMBC), and Joel Schafer (Sigma Research) for technical advice
and assistance, and Patricia Sawamura (UMBC), Daniel Orozco (UMBC), and
Alex Tran (Sigma Research) for photometer operational assistance. This
work was supported in part by the MPLNET, USGS ROLO, and UMBC
Measurement of Atmospheric Pollution (UMAP) Baltimore Air Quality
projects, funded by the NASA EOS and Radiation Sciences programs. Open
source software used in this work includes Python programming language
(http://www.python.org/) for instrumentation and data collection and
Open Office (http://www.openoffice.org/) productivity suite for the
preparation of figures and text. We thank the anonymous reviewers who
helped to significantly improve the original manuscript.
NR 33
TC 15
Z9 15
U1 2
U2 8
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 OCT
PY 2011
VL 28
IS 10
BP 1297
EP 1306
DI 10.1175/JTECH-D-10-05036.1
PG 10
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 843FP
UT WOS:000296658000010
ER
PT J
AU van Diedenhoven, B
Fridlind, AM
Ackerman, AS
AF van Diedenhoven, Bastiaan
Fridlind, Ann M.
Ackerman, Andrew S.
TI Influence of Humidified Aerosol on Lidar Depolarization Measurements
below Ice-Precipitating Arctic Stratus
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID SINGLE-SCATTERING PROPERTIES; GENERAL HYDRODYNAMIC THEORY; MIXED-PHASE
MICROPHYSICS; CIRRUS CLOUDS; PARTICLES; SHEBA; RADAR; CLASSIFICATION;
CLARIFICATION; SIMULATION
AB Lidar measurements obtained during the Surface Heat Budget of the Arctic Ocean (SHEBA) experiment under a mixed-phase stratus cloud that was lightly precipitating ice show a range of surprisingly low depolarization ratios (4%-23%), despite an absence of cloud droplets there. These depolarization ratios are much lower than the range of theoretical values obtained for various ice habits. The depolarization ratios correlate well with radar reflectivity, suggesting that the variation in depolarization ratios results from variations in ice water content, rather than variation in ice habits or orientation. By calculating lidar depolarization based on (i) large-eddy simulations and (ii) in situ ice size distribution measurements, it is shown that the presence of humidified aerosol particles in addition to the ice precipitation can explain the distribution and vertical profile of the observed depolarization ratios, although uncertainties related to the aerosol size distributions are substantial. These calculations show that humidified aerosol must be taken into account when interpreting lidar depolarization measurements for cloud and precipitation phase discrimination or ice habit classification, at least under conditions similar to those observed during SHEBA.
C1 [van Diedenhoven, Bastiaan] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Fridlind, Ann M.; Ackerman, Andrew S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP van Diedenhoven, B (reprint author), 2880 Broadway, New York, NY 10025 USA.
EM bvandiedenhoven@giss.nasa.gov
RI Ackerman, Andrew/D-4433-2012; Fridlind, Ann/E-1495-2012; van
Diedenhoven, Bastiaan/A-2002-2013;
OI Ackerman, Andrew/0000-0003-0254-6253; van Diedenhoven,
Bastiaan/0000-0001-5622-8619
FU National Aeronautics and Space Administration [06-EOS/06-100];
Department of Energy [DE-AI02-06ER64173]; U.S. Department of Energy,
Office of Science, Office of Biological and Environmental Research,
Environmental Sciences Division
FX This work was supported by the National Aeronautics and Space
Administration under Grant 06-EOS/06-100 issued through the Science
Mission Directorate, Earth Science Division, and by the Department of
Energy under Interagency Agreement DE-AI02-06ER64173 issued through the
Office of Science, Office of Biological and Environmental Research. MMCR
data were obtained from the Atmospheric Radiation Measurement (ARM)
Program sponsored by the U.S. Department of Energy, Office of Science,
Office of Biological and Environmental Research, Environmental Sciences
Division. We thank Paquita Zuidema and Hugh Morisson for their help in
obtaining the DABUL data and the in situ ice and aerosol size
distribution data. Computational resources were provided by the DOE
National Energy Research Scientific Computing Center, and by the NASA
Advanced Supercomputing Division through the NASA High-End Computing
Program. We thank two anonymous reviewers for their helpful comments and
suggestions.
NR 41
TC 2
Z9 2
U1 0
U2 6
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 OCT
PY 2011
VL 50
IS 10
BP 2184
EP 2192
DI 10.1175/JAMC-D-11-037.1
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 838CK
UT WOS:000296264100014
ER
PT J
AU Merten, J
Coe, D
Dupke, R
Massey, R
Zitrin, A
Cypriano, ES
Okabe, N
Frye, B
Braglia, FG
Jimenez-Teja, Y
Benitez, N
Broadhurst, T
Rhodes, J
Meneghetti, M
Moustakas, LA
Sodre, L
Krick, J
Bregman, JN
AF Merten, J.
Coe, D.
Dupke, R.
Massey, R.
Zitrin, A.
Cypriano, E. S.
Okabe, N.
Frye, B.
Braglia, F. G.
Jimenez-Teja, Y.
Benitez, N.
Broadhurst, T.
Rhodes, J.
Meneghetti, M.
Moustakas, L. A.
Sodre, L., Jr.
Krick, J.
Bregman, J. N.
TI Creation of cosmic structure in the complex galaxy cluster merger Abell
2744
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: strong; gravitational lensing: weak; galaxies:
clusters: individual: Abell 2744; dark matter; large-scale structure of
Universe; X-rays: individual: Abell 2744
ID HUBBLE-SPACE-TELESCOPE; STRONG-LENSING ANALYSIS; CHARGE-TRANSFER
INEFFICIENCY; INTERACTION CROSS-SECTION; POINT-SPREAD FUNCTION;
X-RAY-CLUSTERS; DARK-MATTER; ADVANCED CAMERA; BULLET CLUSTER; XMM-NEWTON
AB We present a detailed strong-lensing, weak-lensing and X-ray analysis of Abell 2744 (z = 0.308), one of the most actively merging galaxy clusters known. It appears to have unleashed 'dark', 'ghost', 'bullet' and 'stripped' substructures, each similar to 10(14) M-circle dot. The phenomenology is complex and will present a challenge for numerical simulations to reproduce. With new, multiband Hubble Space Telescope (HST) imaging, we identify 34 strongly lensed images of 11 galaxies around the massive Southern 'core'. Combining this with weak-lensing data from HST, VLT and Subaru, we produce the most detailed mass map of this cluster to date. We also perform an independent analysis of archival Chandra X-ray imaging. Our analyses support a recent claim that the Southern core and Northwestern substructure are post-merger and exhibit morphology similar to the Bullet Cluster viewed from an angle. From the separation between X-ray emitting gas and lensing mass in the Southern core, we derive a new and independent constraint on the self-interaction cross-section of dark matter particles sigma/m < 3 +/- 1 cm(2) g(-1). In the Northwestern substructure, the gas, dark matter and galaxy components have become separated by much larger distances. Most curiously, the 'ghost' clump (primarily gas) leads the 'dark' clump (primarily dark matter) by more than 150 kpc. We propose an enhanced 'ram-pressure slingshot' scenario which may have yielded this reversal of components with such a large separation, but needs further confirmation by follow-up observations and numerical simulations. A secondary merger involves a second 'bullet' clump in the North and an extremely 'stripped' clump to the West. The latter appears to exhibit the largest separation between dark matter and X-ray emitting baryons detected to date in our sky.
C1 [Merten, J.] Heidelberg Univ, Inst Theoret Astrophys, ZAH, D-69120 Heidelberg, Germany.
[Merten, J.; Meneghetti, M.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Coe, D.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Dupke, R.] Eureka Sci, Oakland, CA 94602 USA.
[Dupke, R.; Bregman, J. N.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Dupke, R.] Observ Nacl, BR-20921400 Rio De Janeiro, Brazil.
[Massey, R.] Univ Edinburgh, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Zitrin, A.] Tel Aviv Univ, Sch Phys & Astron, Raymond & Beverly Sackler Fac Exact Sci, IL-69978 Tel Aviv, Israel.
[Cypriano, E. S.; Sodre, L., Jr.] Univ Sao Paulo IAG USP, Inst Astron Geofis & Ciencias Almosfer, BR-05508090 Sao Paulo, Brazil.
[Okabe, N.] ASIAA, Taipei 10617, Taiwan.
[Frye, B.] Univ San Francisco, Dept Phys & Astron, San Francisco, CA 94117 USA.
[Braglia, F. G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Jimenez-Teja, Y.; Benitez, N.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain.
[Broadhurst, T.] Univ Basque Country UPV EHU, Dept Theoret Phys, Leioa, Spain.
[Broadhurst, T.] Basque Fdn Sci, IKERBASQUE, Bilbao 48011, Spain.
[Rhodes, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Krick, J.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
RP Merten, J (reprint author), Heidelberg Univ, Inst Theoret Astrophys, ZAH, Albert Ueberle Str 2, D-69120 Heidelberg, Germany.
EM jmerten@ita.uni-heidelberg.de
RI Cypriano, Eduardo/C-7293-2012; 7, INCT/H-6207-2013; Astrofisica,
Inct/H-9455-2013; Jimenez-Teja, Yolanda/D-5933-2011; Meneghetti,
Massimo/O-8139-2015; Sodre, Laerte/P-6045-2016
OI Moustakas, Leonidas/0000-0003-3030-2360; Benitez,
Narciso/0000-0002-0403-7455; Meneghetti, Massimo/0000-0003-1225-7084;
Sodre, Laerte/0000-0002-3876-268X
FU Heidelberg Graduate School of Fundamental Physics (HGSFP);
Baden-Wurrtemberg Stiftung; NASA [NNH10CD19C]; STFC [PP/E006450/1]; ERC
[MIRG-CT-208994]; FAPESP [2009/07154]; CNPq; Spanish MICINN
[AYA2010-22111-C03-00]; Junta de Andalucia Proyecto de Excelencia; ASI
[I/064/08/0, I/009/10/0]; PRIN INAF; [HST-GO-11689.09-A]
FX The authors thank Matt Owers, Catherine Grant and Matthias Bartelmann
for useful discussions. We are particularly grateful to Douglas Clowe,
the referee of this work, for his thorough reading of the manuscript.
His competent comments and suggestions improved the quality of this work
substantially. JM acknowledges financial support from the Heidelberg
Graduate School of Fundamental Physics (HGSFP) and by contract research
Galaxy Clusters of the Baden-Wurrtemberg Stiftung. All runtime-expensive
calculations were performed on dedicated GPU-machines at the
Osservatorio Astronomico di Bologna. DC and RD acknowledge partial
financial support from grant HST-GO-11689.09-A. RD also acknowledges
support from NASA Grant NNH10CD19C. RM is supported by STFC Advanced
Fellowship #PP/E006450/1 and ERC grant MIRG-CT-208994. ESC and LSJ
acknowledge support from FAPESP (process ID 2009/07154) and CNPq. NB and
YJ-T acknowledge support from the Spanish MICINN grant
AYA2010-22111-C03-00 and from the Junta de Andalucia Proyecto de
Excelencia NBL2003. MM and JM acknowledge financial support from ASI
(contracts I/064/08/0, I/009/10/0 and EUCLID-IC) and from PRIN INAF
2009. This research was carried out in part at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
NASA.
NR 102
TC 104
Z9 104
U1 1
U2 7
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2011
VL 417
IS 1
BP 333
EP 347
DI 10.1111/j.1365-2966.2011.19266.x
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 838GV
UT WOS:000296276300043
ER
PT J
AU Steffen, JH
Quinn, SN
Borucki, WJ
Brugamyer, E
Bryson, ST
Buchhave, LA
Cochran, WD
Endl, M
Fabrycky, DC
Ford, EB
Holman, MJ
Jenkins, J
Koch, D
Latham, DW
MacQueen, P
Mullally, F
Prsa, A
Ragozzine, D
Rowe, JF
Sanderfer, DT
Seader, SE
Short, D
Shporer, A
Thompson, SE
Torres, G
Twicken, JD
Welsh, WF
Windmiller, G
AF Steffen, J. H.
Quinn, S. N.
Borucki, W. J.
Brugamyer, E.
Bryson, S. T.
Buchhave, L. A.
Cochran, W. D.
Endl, M.
Fabrycky, D. C.
Ford, E. B.
Holman, M. J.
Jenkins, J.
Koch, D.
Latham, D. W.
MacQueen, P.
Mullally, F.
Prsa, A.
Ragozzine, D.
Rowe, J. F.
Sanderfer, D. T.
Seader, S. E.
Short, D.
Shporer, A.
Thompson, S. E.
Torres, G.
Twicken, J. D.
Welsh, W. F.
Windmiller, G.
TI The architecture of the hierarchical triple star KOI 928 from eclipse
timing variations seen in Kepler photometry
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: eclipsing
ID LIGHT CURVES; LOW-MASS; PLANETS; SYSTEM; GIANT
AB We present a hierarchical triple star system (KIC 9140402) where a low-mass eclipsing binary orbits a more massive third star. The orbital period of the binary (4.988 29 d) is determined by the eclipse times seen in photometry from NASA's Kepler spacecraft. The periodically changing tidal field, due to the eccentric orbit of the binary about the tertiary, causes a change in the orbital period of the binary. The resulting eclipse timing variations provide insight into the dynamics and architecture of this system and allow the inference of the total mass of the binary (0.424 +/- 0.017M(circle dot)) and the orbital parameters of the binary about the central star.
C1 [Steffen, J. H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Quinn, S. N.; Holman, M. J.; Latham, D. W.; Ragozzine, D.; Torres, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Borucki, W. J.; Bryson, S. T.; Jenkins, J.; Koch, D.; Mullally, F.; Rowe, J. F.; Sanderfer, D. T.; Seader, S. E.; Thompson, S. E.; Twicken, J. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Brugamyer, E.; Cochran, W. D.; Endl, M.; MacQueen, P.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Fabrycky, D. C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Ford, E. B.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.
[Jenkins, J.; Mullally, F.; Seader, S. E.; Thompson, S. E.; Twicken, J. D.] SETI Inst, Mountain View, CA 94043 USA.
[Prsa, A.] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA.
[Short, D.; Welsh, W. F.; Windmiller, G.] San Diego State Univ, San Diego, CA 92182 USA.
[Shporer, A.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
RP Steffen, JH (reprint author), Fermilab Ctr Particle Astrophys, POB 500, Batavia, IL 60510 USA.
EM jsteffen@fnal.gov
RI Steffen, Jason/A-4320-2013; Ragozzine, Darin/C-4926-2013;
OI Buchhave, Lars A./0000-0003-1605-5666; Fabrycky,
Daniel/0000-0003-3750-0183
FU NASA's Science Mission Directorate; NASA [HF-51272.01-A, HF-51267.01-A];
STScI; AURA [NAS 5-26555]
FX Kepler is NASA's 10th Discovery mission with funding provided by NASA's
Science Mission Directorate. DCF acknowledges NASA support through
Hubble Fellowship grants #HF-51272.01-A and #HF-51267.01-A awarded by
STScI and operated by AURA under contract NAS 5-26555.
NR 22
TC 15
Z9 15
U1 0
U2 0
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 OCT
PY 2011
VL 417
IS 1
BP L31
EP L35
DI 10.1111/j.1745-3933.2011.01114.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 838GV
UT WOS:000296276300007
ER
PT J
AU Grindlay, J
Hong, J
Allen, B
Barthelmy, S
Baker, R
AF Grindlay, J.
Hong, J.
Allen, B.
Barthelmy, S.
Baker, R.
TI Development of tiled imaging CZT detectors for sensitive wide-field hard
X-ray surveys to EXIST
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article
DE CZT detectors; Pixellated CZT; Coded aperture telescopes; Black holes;
Wide-field surveys
ID BURST
AB Motivated by the proposed EXIST mission, a "medium-class" space observatory to survey black holes and the Early Universe proposed to the 2010 NAS/NRC Astronomy and Astrophysics Decadal Survey, we have developed the first "large" area 256 cm(2) close-tiled (0.6 mm gaps) hard X-ray (20-600 key) imaging detector employing pixelated (2.5 mm) CdZnTe (CZT) detectors, each 2 x 2 x 0.5 cm(3). We summarize the design, development and operation of this detector array (8 x 8 CZTs) and its performance as the imager for a coded aperture telescope on a high altitude (40 km) balloon flight in October, 2009, as the ProtoEXIST1 payload. We then outline our current development of a second-generation imager, ProtoEXIST2, with 0.6 mm pixels on a 32 x 32 array on each CZT, and how it will lead to the ultimate imaging system needed for EXIST. Other applications of this technology will also be mentioned. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Grindlay, J.; Hong, J.; Allen, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Barthelmy, S.; Baker, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Grindlay, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM josh@head.cfa.harvard.edu
RI Barthelmy, Scott/D-2943-2012
FU NASA [NNG06WC12G, NN09AD76G]
FX This work is supported in part by NASA APRA Grants NNG06WC12G and
NN09AD76G.
NR 7
TC 6
Z9 6
U1 2
U2 10
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 OCT 1
PY 2011
VL 652
IS 1
BP 671
EP 673
DI 10.1016/j.nima.2010.09.160
PG 3
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 831XS
UT WOS:000295765000162
ER
PT J
AU Parsons, A
Bodnarik, J
Evans, L
Floyd, S
Lim, L
McClanahan, T
Namkung, M
Nowicki, S
Schweitzer, J
Starr, R
Trombka, J
AF Parsons, A.
Bodnarik, J.
Evans, L.
Floyd, S.
Lim, L.
McClanahan, T.
Namkung, M.
Nowicki, S.
Schweitzer, J.
Starr, R.
Trombka, J.
TI Active neutron and gamma-ray instrumentation for in situ planetary
science applications
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article
DE Gamma ray; Neutron generator; Space applications
AB We describe the development of an instrument capable of detailed in situ bulk geochemical analysis of the surface of planets, moons, asteroids, and comets. This instrument technology uses a pulsed neutron generator to excite the solid materials of a planet and measures the resulting neutron and gamma-ray emission with its detector system. These time-resolved neutron and gamma-ray data provide detailed information about the bulk elemental composition, chemical context, and density distribution of the soil within 50 cm of the surface. While active neutron scattering and neutron-induced gamma-ray techniques have been used extensively for terrestrial nuclear well logging applications, our goal is to apply these techniques to surface instruments for use on any solid solar system body. As described, experiments at NASA Goddard Space Flight Center use a prototype neutron-induced gamma-ray instrument and the resulting data presented show the promise of this technique for becoming a versatile, robust, workhorse technology for planetary science, and exploration of any of the solid bodies in the solar system. The detection of neutrons at the surface also provides useful information about the material. This paper focuses on the data provided by the gamma-ray detector. Published by Elsevier B.V.
C1 [Parsons, A.; Bodnarik, J.; Evans, L.; Floyd, S.; Lim, L.; McClanahan, T.; Namkung, M.; Nowicki, S.; Starr, R.; Trombka, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bodnarik, J.] Vanderbilt Univ, Nashville, TN USA.
[Evans, L.] Comp Sci Corp, Cincinnati, OH 45202 USA.
[Nowicki, S.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Schweitzer, J.] Univ Connecticut, Storrs, CT 06269 USA.
[Starr, R.] Catholic Univ Amer, Washington, DC 20064 USA.
[Trombka, J.] Univ Maryland, College Pk, MD 20742 USA.
RP Parsons, A (reprint author), NASA, Goddard Space Flight Ctr, Code 691, Greenbelt, MD 20771 USA.
EM Ann.M.Parsons@nasa.gov
RI McClanahan, Timothy/C-8164-2012; Lim, Lucy/C-9557-2012; Namkung,
Min/E-1533-2012; Parsons, Ann/I-6604-2012
OI Lim, Lucy/0000-0002-9696-9654;
NR 10
TC 23
Z9 23
U1 0
U2 10
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 OCT 1
PY 2011
VL 652
IS 1
BP 674
EP 679
DI 10.1016/j.nima.2010.09.157
PG 6
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 831XS
UT WOS:000295765000163
ER
PT J
AU Serabyn, E
Wallace, JK
Mawet, D
AF Serabyn, Eugene
Wallace, J. Kent
Mawet, Dimitri
TI Speckle-phase measurement in a tandem-vortex coronagraph
SO APPLIED OPTICS
LA English
DT Article
ID MASK CORONAGRAPH; PLANET DETECTION; DYNAMIC-RANGE; SPACE
AB A tandem-vortex coronagraph can in theory enable high-contrast imaging behind a classical on-axis telescope. Here we point out that a tandem-vortex coronagraph configuration can also directly enable the measurement of the phases of focal-plane speckles, thereby allowing for their suppression in the resultant high-contrast image. (C) 2011 Optical Society of America
C1 [Serabyn, Eugene; Wallace, J. Kent; Mawet, Dimitri] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Serabyn, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM gene.serabyn@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA)
FX This work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration (NASA).
NR 21
TC 9
Z9 9
U1 0
U2 3
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD OCT 1
PY 2011
VL 50
IS 28
BP 5453
EP 5456
DI 10.1364/AO.50.005453
PG 4
WC Optics
SC Optics
GA 832XA
UT WOS:000295842600033
PM 22016212
ER
PT J
AU Rezac, L
Kutepov, AA
Feofilov, AG
Russell, JM
AF Rezac, L.
Kutepov, A. A.
Feofilov, A. G.
Russell, J. M., III
TI On limb radiance calculations and convergence of relaxation type
retrieval algorithms
SO APPLIED OPTICS
LA English
DT Article
ID PLANETARY-ATMOSPHERES; LINE TRANSFER; TEMPERATURE; GAS
AB Several approaches to the solution of the radiative transfer equation assume either Curtis-Godson average or linear change of the source function across grid segments. When such solutions are used for calculating limb radiances, the peak radiance response to the source function perturbation at tangent point i is displaced down to the tangent point i + 1. This effect is explained through a geometric argument. Temperature profile retrievals performed by applying the ratio of signals at level i + 1 for correcting temperature at level i demonstrate dramatic convergence acceleration of the iterative relaxation scheme. (C) 2011 Optical Society of America
C1 [Rezac, L.; Russell, J. M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Kutepov, A. A.; Feofilov, A. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kutepov, A. A.; Feofilov, A. G.] Catholic Univ Amer, Washington, DC 20064 USA.
RP Rezac, L (reprint author), Hampton Univ, Ctr Atmospher Sci, 23 Tyler St, Hampton, VA 23668 USA.
EM ladislav.rezac@hamptonu.edu
RI Feofilov, Artem/A-2271-2015
OI Feofilov, Artem/0000-0001-9924-4846
NR 15
TC 2
Z9 2
U1 0
U2 3
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD OCT 1
PY 2011
VL 50
IS 28
BP 5499
EP 5502
DI 10.1364/AO.50.005499
PG 4
WC Optics
SC Optics
GA 832XA
UT WOS:000295842600038
PM 22016217
ER
PT J
AU Haghighipour, N
Kirste, S
AF Haghighipour, Nader
Kirste, Sabrina
TI On the detection of (habitable) super-Earths around low-mass stars using
Kepler and transit timing variation method
SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY
LA English
DT Article
DE Planetary systems: Detection; Detection techniques; Methods: Numerical
simulations; TTV; Resonant orbits
ID CARNEGIE EXOPLANET SURVEY; GIANT PLANET MIGRATION; EXTRA-SOLAR PLANETS;
M-CIRCLE-PLUS; HOT-JUPITER SYSTEMS; SUN-LIKE STAR; TERRESTRIAL PLANETS;
HARPS SEARCH; CIRCUMBINARY PLANETS; BINARY-SYSTEMS
AB We present the results of an extensive study of the detectability of Earth-sized planets and super-Earths in the habitable zones of cool and low-mass stars using transit timing variation method. We have considered a system consisting of a star, a transiting giant planet, and a terrestrial-class perturber, and calculated TTVs for different values of the parameters of the system. To identify ranges of the parameters for which these variations would be detectable by Kepler, we considered the analysis presented by Ford et al. (Transit timing observations from Kepler: I. Statistical analysis of the first four months. ArXiv:1102.0544, 2011) and assumed that a peak-to-peak variation of 20 s would be within the range of the photometric sensitivity of this telescope. We carried out simulations for resonant and non-resonant orbits, and identified ranges of the semimajor axes and eccentricities of the transiting and perturbing bodies for which an Earth-sized planet or a super-Earth in the habitable zone of a low-mass star would produce such TTVs. Results of our simulations indicate that in general, outer perturbers near first-and second-order resonances show a higher prospect for detection. Inner perturbers are potentially detectable only when near 1: 2 and 1: 3 mean-motion resonances. For a typical M star with a Jupiter-mass transiting planet, for instance, an Earth-mass perturber in the habitable zone can produce detectable TTVs when the orbit of the transiting planet is between 15 and 80 days. We present the details of our simulations and discuss the implication of the results for the detection of terrestrial planets around different low-mass stars.
C1 [Haghighipour, Nader] Univ Hawaii, Inst Astron, Honolulu, HI 96825 USA.
[Haghighipour, Nader] Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96825 USA.
[Kirste, Sabrina] Tech Univ Berlin, ZAA, D-10623 Berlin, Germany.
RP Haghighipour, N (reprint author), Univ Hawaii, Inst Astron, Honolulu, HI 96825 USA.
EM nader@ifa.hawaii.edu
FU NASA Astrobiology Institute (NAI) at the Institute for Astronomy (IfA),
University of Hawaii (UH) [NNA04CC08A]; NASA [NNX09AN05G]
FX Support is acknowledged for NH from NASA Astrobiology Institute (NAI)
under Cooperative Agreement NNA04CC08A at the Institute for Astronomy
(IfA), University of Hawaii (UH), and NASA EXOB grant NNX09AN05G. SK is
thankful to the IfA and UH/NAI for their great hospitality during the
course of this project, and to NAI central for travel support. We are
especially thankful to the referee, Eric Agol, for his critically
reading of our manuscript and for his insightful comments that greatly
enhanced this article.
NR 66
TC 5
Z9 5
U1 0
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0923-2958
J9 CELEST MECH DYN ASTR
JI Celest. Mech. Dyn. Astron.
PD OCT
PY 2011
VL 111
IS 1-2
SI SI
BP 267
EP 284
DI 10.1007/s10569-011-9363-1
PG 18
WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications
SC Astronomy & Astrophysics; Mathematics
GA 836DO
UT WOS:000296089500012
ER
PT J
AU Newman, JC
Yamada, Y
James, MA
AF Newman, J. C., Jr.
Yamada, Y.
James, M. A.
TI Back-face strain compliance relation for compact specimens for wide
range in crack lengths
SO ENGINEERING FRACTURE MECHANICS
LA English
DT Article
DE Cracks; Compact; Back-face strain; Elasticity
AB A back-face strain (BFS) compliance relation has been developed for the standard compact C(T) specimen for a very wide range in crack-length-to-width (a/W) ratios. Both finite-element and boundary-element methods were used to develop the BFS relation for a/W ratios from 0.2 to 0.95. In addition, experimentally determined compliance values on four metallic materials compared well with the new relation over nearly the complete a/W range. The new relation can be used to monitor crack-length-against-cycles using computerized crack-monitoring systems that are currently used with the crack-mouth-opening-displacement (CMOD) gage method, and the relation has been cast in a standard form compatible with existing compliance crack length monitoring systems. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Newman, J. C., Jr.] Mississippi State Univ, Dept Aerosp Engn, Mississippi State, MS 39762 USA.
[Yamada, Y.] NASA, Ohio Aerosp Inst, Glenn Res Ctr, Cleveland, OH 44135 USA.
[James, M. A.] Alcoa Tech Ctr, Alcoa Ctr, PA 15069 USA.
RP Newman, JC (reprint author), Mississippi State Univ, Dept Aerosp Engn, Mississippi State, MS 39762 USA.
EM j.c.newman.jr@ae.msstate.edu
NR 12
TC 5
Z9 5
U1 0
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0013-7944
J9 ENG FRACT MECH
JI Eng. Fract. Mech.
PD OCT
PY 2011
VL 78
IS 15
BP 2707
EP 2711
DI 10.1016/j.engfracmech.2011.07.001
PG 5
WC Mechanics
SC Mechanics
GA 838DN
UT WOS:000296267100006
ER
PT J
AU Edmonds, LD
AF Edmonds, Larry D.
TI A Theoretical Analysis of the Role of Ambipolar Diffusion in
Charge-Carrier Transport in a Quasi-Neutral Region Under High Injection
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article
DE Ambipolar diffusion; ambipolar region (AR); charge collection;
drift-diffusion; high-resistance region (HRR); quasi-neutral region
(QNR); regional partitioning
AB A recent theoretical analysis considered charge collection from an ionization source in a p-n junction silicon diode under steady-state conditions, i.e., carrier liberation is at a quasi-constant rate, and concluded that the quasi-neutral region partitions into distinct sub-regions. A later empirical investigation (via TCAD simulations) found that this partitioning also applies under transient conditions, but a theoretical explanation was not given for the transient problem. The theoretical analysis given here provides that explanation, and also explains why a charge-collection model derived under steady-state conditions gives correct predictions for the transient problem.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Edmonds, LD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM larry.d.edmonds@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX Manuscript received January 07, 2011; revised April 15, 2011; accepted
July 06, 2011. Date of publication August 12, 2011; date of current
version October 12, 2011. The research in this paper was carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with the National Aeronautics and Space Administration.
Reference herein to any specific commercial product, process, or service
by trade name, manufacturer, or otherwise, does not constitute or imply
its endorsement by the U.S. Government or the Jet Propulsion Laboratory,
California Institute of Technology.
NR 4
TC 5
Z9 5
U1 0
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD OCT
PY 2011
VL 58
IS 5
BP 2459
EP 2469
DI 10.1109/TNS.2011.2161884
PN 2
PG 11
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA 832CH
UT WOS:000295778000021
ER
PT J
AU Irom, F
Nguyen, DN
Harboe-Sorensen, R
Virtanen, A
AF Irom, Farokh
Nguyen, Duc N.
Harboe-Sorensen, Reno
Virtanen, Ari
TI Evaluation of Mechanisms in TID Degradation and SEE Susceptibility of
Single- and Multi-Level High Density NAND Flash Memories
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article
DE Floating gate; gamma rays; NAND flash; nonvolatile memory; single event
effects; single event upset; total ionizing dose; x-ray
ID FLOATING-GATE MEMORIES; CHARGE LOSS; HEAVY-IONS; CELLS; DEPENDENCE
AB Heavy ion single-event measurements and total ionizing dose (TID) response for 8 Gb commercial NAND flash memories are reported. Radiation results of multi-level flash technology are compared with results from single-level flash technology. The single-level devices are less sensitive to single event upsets (SEUs) than multi-level devices. In general, these commercial high density memories exhibit less TID degradation compared to older generations of flash memories.
C1 [Irom, Farokh; Nguyen, Duc N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Harboe-Sorensen, Reno] European Space Agcy, NL-2200 AG Noordwijk, Netherlands.
[Virtanen, Ari] Univ Jyvaskyla, Dept Phys, Accelerator Lab, FIN-40351 Jyvaskyla, Finland.
RP Irom, F (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM farokh.irom@jpl.nasa.gov; duc.n.nguyen@jpl.nasa.gov;
reno.harboe.sorensen@esa.int; ari.virtanen@phys.jyu.fi
OI Virtanen, Ari/0000-0002-6591-6787
FU National Aeronautics and Space Administration (NASA)
FX Manuscript received February 04, 2011; revised April 07, 2011; accepted
June 01, 2011. Date of publication August 18, 2011; date of current
version October 12, 2011. The research in this paper was carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration (NASA),
under the NASA Electronic Parts and Packaging Program.
NR 24
TC 13
Z9 13
U1 0
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD OCT
PY 2011
VL 58
IS 5
BP 2477
EP 2482
DI 10.1109/TNS.2011.2161885
PN 2
PG 6
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA 832CH
UT WOS:000295778000023
ER
PT J
AU Thiruppathiraja, C
Saroja, V
Kamatchiammal, S
Adaikkappan, P
Alagar, M
AF Thiruppathiraja, Chinnasamy
Saroja, Veerappan
Kamatchiammal, Senthilkumar
Adaikkappan, Periyakaruppan
Alagar, Muthukaruppan
TI Development of electrochemical based sandwich enzyme linked immunosensor
for Cryptosporidium parvum detection in drinking water
SO JOURNAL OF ENVIRONMENTAL MONITORING
LA English
DT Article
ID REAL-TIME DETECTION; DNA; NANOPARTICLES; BIOSENSOR; BIOMARKER; OOCYSTS;
ASSAY; AMPLIFICATION; IMMUNOASSAY; SEQUENCES
AB Cryptosporidium parvum is one of the most important biological contaminants in drinking water and generates significant risks to public health. Due to low infectious dose of C. parvum, remarkably sensitive detection methods are required for water and food industry analysis. This present study describes a simple, sensitive, enzyme amplified sandwich form of an electrochemical immunosensor using dual labeled gold nanoparticles (alkaline phosphatase and anti-oocysts monoclonal antibody) in indium tin oxide (ITO) as an electrode to detect C. parvum. The biosensor was fabricated by immobilizing the anti-oocysts McAb on a gold nanoparticle functionalized ITO electrode, followed by the corresponding capture of analytes and dual labeled gold nanoparticle probe to detect the C. parvum target. The outcome shows the sensitivity of electrochemical immune sensor enhanced by gold nanoparticles with a limit of detection of 3 oocysts/mL in a minimal processing period. Our results demonstrated the sensitivity of the new approach compared to the customary method and the immunosensors showed acceptable precision, reproducibility, stability, and could be readily applied to multi analyte determination for environmental monitoring.
C1 [Thiruppathiraja, Chinnasamy; Alagar, Muthukaruppan] Anna Univ, Dept Chem Engn, Nanocomposites Res Grp, Madras 600025, Tamil Nadu, India.
[Saroja, Veerappan; Kamatchiammal, Senthilkumar] Natl Environm Engn Res Inst, Chennai Zonal Lab, Madras 600113, Tamil Nadu, India.
[Adaikkappan, Periyakaruppan] NASA, Ames Res Ctr, Ctr Nanosci & Nanotechnol, Moffett Field, CA 94035 USA.
RP Alagar, M (reprint author), Anna Univ, Dept Chem Engn, Nanocomposites Res Grp, Madras 600025, Tamil Nadu, India.
EM mkalagar@yahoo.com
RI Periyakaruppan, Adaikkappan/B-7398-2013
OI Periyakaruppan, Adaikkappan/0000-0002-0395-6564
FU Council of Scientific and Industrial Research, New Delhi, India
FX Authors thank the Supra Institutional Project, Council of Scientific and
Industrial Research, New Delhi, India for funding to execute this study
successfully.
NR 42
TC 11
Z9 11
U1 1
U2 21
PU ROYAL SOC CHEMISTRY
PI CAMBRIDGE
PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS,
ENGLAND
SN 1464-0325
EI 1464-0333
J9 J ENVIRON MONITOR
JI J. Environ. Monit.
PD OCT
PY 2011
VL 13
IS 10
BP 2782
EP 2787
DI 10.1039/c1em10372e
PG 6
WC Chemistry, Analytical; Environmental Sciences
SC Chemistry; Environmental Sciences & Ecology
GA 829KN
UT WOS:000295579000014
PM 21897977
ER
PT J
AU Liu, Q
Reichle, RH
Bindlish, R
Cosh, MH
Crow, WT
de Jeu, R
De Lannoy, GJM
Huffman, GJ
Jackson, TJ
AF Liu, Qing
Reichle, Rolf H.
Bindlish, Rajat
Cosh, Michael H.
Crow, Wade T.
de Jeu, Richard
De Lannoy, Gabrielle J. M.
Huffman, George J.
Jackson, Thomas J.
TI The Contributions of Precipitation and Soil Moisture Observations to the
Skill of Soil Moisture Estimates in a Land Data Assimilation System
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID ENSEMBLE KALMAN FILTER; SOUTHERN UNITED-STATES; GLOBAL PRECIPITATION;
PASSIVE MICROWAVE; SURFACE MODELS; TEMPERATURE OBSERVATIONS; GAUGE
OBSERVATIONS; ERS SCATTEROMETER; AMSR-E; SIMULATIONS
AB The contributions of precipitation and soil moisture observations to soil moisture skill in a land data assimilation system are assessed. Relative to baseline estimates from the Modern Era Retrospective-analysis for Research and Applications (MERRA), the study investigates soil moisture skill derived from (i) model forcing corrections based on large-scale, gauge- and satellite-based precipitation observations and (ii) assimilation of surface soil moisture retrievals from the Advanced Microwave Scanning Radiometer for Earth Observing System (AMSR-E). Soil moisture skill (defined as the anomaly time series correlation coefficient R) is assessed using in situ observations in the continental United States at 37 single-profile sites within the Soil Climate Analysis Network (SCAN) for which skillful AMSR-E retrievals are available and at 4 USDA Agricultural Research Service ("Cal Val") watersheds with high-quality distributed sensor networks that measure soil moisture at the scale of land model and satellite estimates. The average skill of AMSR-E retrievals is R = 0.42 versus SCAN and R = 0.55 versus CalVal measurements. The skill of MERRA surface and root-zone soil moisture is R = 0.43 and R = 0.47, respectively, versus SCAN measurements. MERRA surface moisture skill is R = 0.56 versus CalVal measurements. Adding information from precipitation observations increases (surface and root zone) soil moisture skills by Delta R similar to 0.06. Assimilating AMSR-E retrievals increases soil moisture skills by Delta R similar to 0.08. Adding information from both sources increases soil moisture skills by Delta R similar to 0.13, which demonstrates that precipitation corrections and assimilation of satellite soil moisture retrievals contribute important and largely independent amounts of information.
C1 [Liu, Qing; Reichle, Rolf H.; De Lannoy, Gabrielle J. M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Liu, Qing] Sci Applicat Int Corp, Beltsville, MD USA.
[Bindlish, Rajat; Cosh, Michael H.; Crow, Wade T.; Jackson, Thomas J.] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD USA.
[Bindlish, Rajat; Huffman, George J.] Sci Syst & Applicat Inc, Lanham, MD USA.
[de Jeu, Richard] Vrije Univ Amsterdam, Fac Earth & Life Sci, Dept Hydrol & GeoEnvironm Sci, Amsterdam, Netherlands.
[De Lannoy, Gabrielle J. M.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[De Lannoy, Gabrielle J. M.] Univ Ghent, Lab Hydrol & Water Management, B-9000 Ghent, Belgium.
[Huffman, George J.] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Branch, Greenbelt, MD 20771 USA.
RP Liu, Q (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA.
EM qing.liu@nasa.gov
RI Reichle, Rolf/E-1419-2012; Huffman, George/F-4494-2014; Cosh,
MIchael/A-8858-2015
OI Huffman, George/0000-0003-3858-8308; Cosh, MIchael/0000-0003-4776-1918
FU NASA; Terra; Aqua; ACRIMSAT; Research Foundation Flanders (FWO),
Belgium; USDA/ARS; NASA GSFC; NOAA/CPC; Deutscher Wetterdienst; NSIDC;
VU Amsterdam
FX Funding for this work was provided by the NASA Earth System Science
Research using Data and Products from the Terra, Aqua, and ACRIMSAT
Satellites program and the NASA Soil Moisture Active Passive mission
project. Gabrielle De Lannoy is a postdoctoral research fellow supported
by the Research Foundation Flanders (FWO), Belgium. Computing was
supported by the NASA High End Computing Program. We are grateful for
access to the many datasets that supported this work and highly
appreciate the personnel at USDA/ARS, NASA GSFC, NOAA/CPC, Deutscher
Wetterdienst, NSIDC, and VU Amsterdam who made them possible. Helpful
comments were provided by Pingping Xie and three anonymous reviewers.
NR 56
TC 54
Z9 54
U1 2
U2 18
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD OCT
PY 2011
VL 12
IS 5
BP 750
EP 765
DI 10.1175/JHM-D-10-05000.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 835ID
UT WOS:000296029000003
ER
PT J
AU Santanello, JA
Peters-Lidard, CD
Kumar, SV
AF Santanello, Joseph A., Jr.
Peters-Lidard, Christa D.
Kumar, Sujay V.
TI Diagnosing the Sensitivity of Local Land-Atmosphere Coupling via the
Soil Moisture-Boundary Layer Interaction
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID DIURNAL TIME SCALES; EQUILIBRIUM EVAPORATION; SURFACE EVAPORATION;
VERTICAL DIFFUSION; BUDGET METHODS; GLOBAL-MODELS; FEEDBACK;
ENTRAINMENT; TRANSPIRATION; PRECIPITATION
AB The inherent coupled nature of earth's energy and water cycles places significant importance on the proper representation and diagnosis of land atmosphere (LA) interactions in hydrometeorological prediction models. However, the precise nature of the soil moisture precipitation relationship at the local scale is largely determined by a series of nonlinear processes and feedbacks that are difficult to quantify. To quantify the strength of the local LA coupling (LoCo), this process chain must be considered both in full and as individual components through their relationships and sensitivities. To address this, recent modeling and diagnostic studies have been extended to I) quantify the processes governing LoCo utilizing the thermodynamic properties of mixing diagrams, and 2) diagnose the sensitivity of coupled systems, including clouds and moist processes, to perturbations in soil moisture. This work employs NASA's Land Information System (LIS) coupled to the Weather Research and Forecasting (WRF) mesoscale model and simulations performed over the U.S. Southern Great Plains. The behavior of different planetary boundary layers (PBL) and land surface scheme couplings in LIS WRF are examined in the context of the evolution of thermodynamic quantities that link the surface soil moisture condition to the PBL regime, clouds, and precipitation. Specifically, the tendency toward saturation in the PBL is quantified by the lifting condensation level (LCL) deficit and addressed as a function of time and space. The sensitivity of the LCL deficit to the soil moisture condition is indicative of the strength of LoCo, where both positive and negative feedbacks can be identified. Overall, this methodology can be applied to any model or observations and is a crucial step toward improved evaluation and quantification of LoCo within models, particularly given the advent of next-generation satellite measurements of PBL and land surface properties along with advances in data assimilation schemes.
C1 [Santanello, Joseph A., Jr.; Peters-Lidard, Christa D.; Kumar, Sujay V.] NASA GSFC, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
[Kumar, Sujay V.] Sci Applicat Int Corp, Mclean, VA 22102 USA.
RP Santanello, JA (reprint author), NASA GSFC, Hydrol Sci Branch, Code 614-3,Bldg 33,Room G220, Greenbelt, MD 20771 USA.
EM Joseph.A.Santanello@nasa.gov
RI Santanello, Joseph/D-4438-2012; Kumar, Sujay/B-8142-2015; Peters-Lidard,
Christa/E-1429-2012
OI Santanello, Joseph/0000-0002-0807-6590; Peters-Lidard,
Christa/0000-0003-1255-2876
FU NASA Energy and Water Cycle Study (NEWS)
FX This work was supported by the NASA Energy and Water Cycle Study (NEWS;
PI: C. Peters-Lidard). In particular, Jim Geiger was instrumental in
providing support related to LIS-WRF coupling and testing. We also
appreciate the past and ongoing collaboration with the LoCo community
that has stimulated this work, in particular Michael Ek, Cor Jacobs,
Obbe Tuinenburg, Bert Holtslag, Chiel van Heerwaarden. Bart van den
Hurk, and Martin Best.
NR 60
TC 74
Z9 74
U1 1
U2 44
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD OCT
PY 2011
VL 12
IS 5
BP 766
EP 786
DI 10.1175/JHM-D-10-05014.1
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 835ID
UT WOS:000296029000004
ER
PT J
AU Koster, RD
Mahanama, SPP
Yamada, TJ
Balsamo, G
Berg, AA
Boisserie, M
Dirmeyer, PA
Doblas-Reyes, FJ
Drewitt, G
Gordon, CT
Guo, Z
Jeong, JH
Lee, WS
Li, Z
Luo, L
Malyshev, S
Merryfield, WJ
Seneviratne, SI
Stanelle, T
van den Hurk, BJJM
Vitart, F
Wood, EF
AF Koster, R. D.
Mahanama, S. P. P.
Yamada, T. J.
Balsamo, Gianpaolo
Berg, A. A.
Boisserie, M.
Dirmeyer, P. A.
Doblas-Reyes, F. J.
Drewitt, G.
Gordon, C. T.
Guo, Z.
Jeong, J. -H.
Lee, W. -S.
Li, Z.
Luo, L.
Malyshev, S.
Merryfield, W. J.
Seneviratne, S. I.
Stanelle, T.
van den Hurk, B. J. J. M.
Vitart, F.
Wood, E. F.
TI The Second Phase of the Global Land-Atmosphere Coupling Experiment: Soil
Moisture Contributions to Subseasonal Forecast Skill
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID SURFACE AIR-TEMPERATURE; PART I; MINIMUM TEMPERATURES; AFRICAN MONSOONS;
MONTHLY RAINFALL; CLIMATE MODELS; DATA SET; PRECIPITATION; SIMULATION;
IMPACT
AB The second phase of the Global Land Atmosphere Coupling Experiment (GLACE-2) is a multi-institutional numerical modeling experiment focused on quantifying, for boreal summer, the subseasonal (out to two months) forecast skill for precipitation and air temperature that can be derived from the realistic initialization of land surface states, notably soil moisture. An overview of the experiment and model behavior at the global scale is described here, along with a determination and characterization of multimodel "consensus" skill. The models show modest but significant skill in predicting air temperatures, especially where the rain gauge network is dense. Given that precipitation is the chief driver of soil moisture, and thereby assuming that rain gauge density is a reasonable proxy for the adequacy of the observational network contributing to soil moisture initialization, this result indeed highlights the potential contribution of enhanced observations to prediction. Land-derived precipitation forecast skill is much weaker than that for air temperature. The skill for predicting air temperature, and to some extent precipitation, increases with the magnitude of the initial soil moisture anomaly. GLACE-2 results are examined further to provide insight into the asymmetric impacts of wet and dry soil moisture initialization on skill.
C1 [Koster, R. D.; Mahanama, S. P. P.; Yamada, T. J.; Li, Z.] NASA GSFC, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Mahanama, S. P. P.; Yamada, T. J.] UMBC GEST, Baltimore, MD USA.
[Mahanama, S. P. P.; Li, Z.; Vitart, F.] SAIC, Beltsville, MD USA.
[Yamada, T. J.] Hokkaido Univ, Div Field Engn Environm, Sapporo, Hokkaido, Japan.
[Balsamo, Gianpaolo] ECMWF, Reading, Berks, England.
[Berg, A. A.; Drewitt, G.] Univ Guelph, Dept Geog, Guelph, ON N1G 2W1, Canada.
[Boisserie, M.] Florida State Univ, Ctr Ocean Atmospher Predict Studies, Tallahassee, FL 32306 USA.
[Boisserie, M.] Meteo France, Toulouse, France.
[Dirmeyer, P. A.; Guo, Z.] Ctr Ocean Land Atmosphere Steudies, Calverton, MD USA.
[Doblas-Reyes, F. J.] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain.
[Doblas-Reyes, F. J.] Inst Catala Ciencies Clima IC3, Barcelona, Spain.
[Gordon, C. T.] NOAA GFDL, Princeton, NJ USA.
[Jeong, J. -H.] Univ Gothenburg, Dept Earth Sci, Gothenburg, Sweden.
[Lee, W. -S.; Merryfield, W. J.] Environm Canada, CCCMA, Victoria, BC, Canada.
[Luo, L.] Michigan State Univ, Dept Geog, E Lansing, MI 48824 USA.
[Luo, L.; Malyshev, S.; Wood, E. F.] Princeton Univ, Princeton, NJ 08544 USA.
[Seneviratne, S. I.; Stanelle, T.] ETH, Inst Atmospher & Climate Sci, Zurich, Switzerland.
[van den Hurk, B. J. J. M.] KNMI, De Bilt, Netherlands.
RP Koster, RD (reprint author), NASA GSFC, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA.
EM randal.d.koster@nasa.gov
RI Seneviratne, Sonia/G-8761-2011; Koster, Randal/F-5881-2012; Balsamo,
Gianpaolo/I-3362-2013; Jeong, Jee-Hoon/A-4286-2010; Dirmeyer,
Paul/B-6553-2016; Doblas-Reyes, Francisco/C-1228-2016
OI Seneviratne, Sonia/0000-0001-9528-2917; Koster,
Randal/0000-0001-6418-6383; Balsamo, Gianpaolo/0000-0002-1745-3634;
Jeong, Jee-Hoon/0000-0002-3358-3949; Dirmeyer, Paul/0000-0003-3158-1752;
Doblas-Reyes, Francisco/0000-0002-6622-4280
FU NOAA; NASA
FX Coordinators of the GLACE-2 project gratefully acknowledge financial
support from NOAA's Climate Prediction Program for the Americas and
NASA's Terrestrial Hydrology program. The various participants in the
project (see Table 1) were able to perform the GLACE-2 simulations
thanks to financial and computational support from their home
institutions and/or from the institutions hosting the numerical
prediction systems. We thank George Huffmann and David Bolvin for
valuable discussions on the precipitation gauge network, and we thank
WCRP's GEWEX and CLIVAR projects for their sponsorship of this project.
One of the authors (Tony Gordon) passed away during the review process
for this manuscript. His contributions to the project were particularly
significant, and we dedicate this paper to his memory.
NR 65
TC 112
Z9 114
U1 3
U2 39
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD OCT
PY 2011
VL 12
IS 5
BP 805
EP 822
DI 10.1175/2011JHM1365.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 835ID
UT WOS:000296029000006
ER
PT J
AU Ramos, M
Drouin, BJ
AF Ramos, Marlon
Drouin, Brian J.
TI Submillimeter spectrum of methyl bromide (CH3Br)
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE CH3Br; Methyl halides; Atmospheric spectra; Methyl bromide
ID ROTATIONAL SPECTRA; GROUND-STATE; MILLIMETER; SPECTROSCOPY;
SPECTROMETER; POTENTIALS; VIBRATION; CONSTANTS; BANDS; BRO
AB Methyl bromide is a ubiquitous component of the atmosphere, but has yet to be remotely detected in the upper atmosphere. Due to the strong ozone depletion capability of the activated bromine species, the total atmospheric bromine load needs to be carefully monitored. Combined analysis of precise measurements and cataloging of the rotational spectrum of methyl bromide may enable its concentration to be monitored with future remote sensing instrumentation. In an effort to extend and improve previous work for this molecule, the spectrum of CH3Br has been measured at JPL. Using an isotopically enriched (CH3Br)-C-13 (90%) sample, spectra have been recorded from 750 to 1200 GHz. Quantum number assignments cover the (CH3Br)-Br-78, (CH3Br)-Br-81, (CH3Br)-C-13-Br-79 and (CH3Br)-C-13-Br-81 isotopologues with J < 66 and K < 17 for the ground and v(3) vibrational states. The dataset for the C-12 isotopologues is more precise than previous THz measurements resulting in reductions of rotational and distortion parameter uncertainties by factors of 2-15. Parameters of the v(3) state of the C-12 isotopologues are improved by 2-105. The spectra of the C-13 isotopologues are the first reported beyond J = 2. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Ramos, Marlon; Drouin, Brian J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Drouin, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM brian.j.drouin@jpl.nasa.gov
FU Jet Propulsion Laboratory, California Institute of Technology; NASA
FX This paper presents research carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
NASA Undergraduate Student Research Program (USRP). Any opinions,
findings, and conclusions or recommendations expressed in this material
are those of the author(s) and do not necessarily reflect the views of
NASA. Copyright 2011 California Institute of Technology. Government
sponsorship acknowledged.
NR 34
TC 2
Z9 2
U1 1
U2 6
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD OCT
PY 2011
VL 269
IS 2
BP 187
EP 192
DI 10.1016/j.jms.2011.07.001
PG 6
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 833VE
UT WOS:000295912200006
ER
PT J
AU Drouin, BJ
Yu, SS
AF Drouin, Brian J.
Yu, Shanshan
TI Acetylene spectra near 2.6 THz
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Rotational spectroscopy; Terahertz spectroscopy; Atmospheric species;
Astrophysical species
AB We present high precision frequency measurements of acetylene in the 2.5-2.7 THz range obtained with our most recent multiplier technology. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Drouin, Brian J.; Yu, Shanshan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Drouin, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM brian.j.drouin@jpl.nasa.gov
RI Yu, Shanshan/D-8733-2016
FU Jet Propulsion Laboratory, California Institute of Technology; National
Aeronautics and Space Administration; California Institute of
Technology. Government
FX This paper presents research carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under Contract with the
National Aeronautics and Space Administration. 2011 California Institute
of Technology. Government sponsorship acknowledged.
NR 6
TC 2
Z9 2
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 0022-2852
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD OCT
PY 2011
VL 269
IS 2
BP 254
EP 256
DI 10.1016/j.jms.2011.06.004
PG 3
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 833VE
UT WOS:000295912200015
ER
PT J
AU Lawson, JW
Bauschlicher, CW
Daw, MS
AF Lawson, John W.
Bauschlicher, Charles W., Jr.
Daw, Murray S.
TI Ab Initio Computations of Electronic, Mechanical, and Thermal Properties
of ZrB2 and HfB2
SO JOURNAL OF THE AMERICAN CERAMIC SOCIETY
LA English
DT Article
ID TRANSITION-METAL DIBORIDES; TOTAL-ENERGY CALCULATIONS; WAVE BASIS-SET;
DENSITY; LOCALIZATION; ZIRCONIUM
AB A comprehensive ab initio analysis of the ultra high temperature ceramics ZrB2 and HfB2 is presented. Density functional theory (DFT) computations were performed for the electronic, mechanical, thermal, and point defect properties of these materials. Lattice constants and elastic constants were determined. Computations of the electronic density of states, band structure, electron localization function, etc. show the diverse bonding types that exist in these materials. They also suggest the connection between the electronic structure and the superior mechanical properties. Lattice dynamical effects were considered, including phonon dispersions, vibrational densities of states, and specific heat curves. Point defect (vacancies and antisites) structures and energetics are also presented.
C1 [Lawson, John W.] NASA, Thermal Protect Mat Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Bauschlicher, Charles W., Jr.] NASA, Entry Syst & Technol Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Daw, Murray S.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29631 USA.
RP Lawson, JW (reprint author), NASA, Thermal Protect Mat Branch, Ames Res Ctr, Mail Stop 234-1, Moffett Field, CA 94035 USA.
EM john.w.lawson@nasa.gov
FU NASA
FX J.W.L. and C.W.B are civil servants in the Entry Systems and Technology
Division. M.S.D was supported under a NASA prime contract to ELORET
Corporation.
NR 24
TC 23
Z9 23
U1 3
U2 36
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-7820
J9 J AM CERAM SOC
JI J. Am. Ceram. Soc.
PD OCT
PY 2011
VL 94
IS 10
BP 3494
EP 3499
DI 10.1111/j.1551-2916.2011.04649.x
PG 6
WC Materials Science, Ceramics
SC Materials Science
GA 828SY
UT WOS:000295524300061
ER
PT J
AU Lang, SE
Tao, WK
Zeng, XP
Li, YP
AF Lang, Stephen E.
Tao, Wei-Kuo
Zeng, Xiping
Li, Yaping
TI Reducing the Biases in Simulated Radar Reflectivities from a Bulk
Microphysics Scheme: Tropical Convective Systems
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID CLOUD-RESOLVING MODEL; LATENT HEATING PROFILES; TRMM PR DATA; ADVECTION
TRANSPORT ALGORITHM; SMALL IMPLICIT DIFFUSION; 2001 IMPROVE-2 EVENT;
PART I; SQUALL LINE; TOGA-COARE; NUMERICAL-SIMULATION
AB A well-known bias common to many bulk microphysics schemes currently being used in cloud-resolving models is the tendency to produce excessively large reflectivity values (e.g., 40 dBZ) in the middle and upper troposphere in simulated convective systems. The Rutledge and Hobbs-based bulk microphysics scheme in the Goddard Cumulus Ensemble model is modified to reduce this bias and improve realistic aspects. Modifications include lowering the efficiencies for snow/graupel riming and snow accreting cloud ice; converting less rimed snow to graupel; allowing snow/graupel sublimation; adding rime splintering, immersion freezing, and contact nucleation; replacing the Fletcher formulation for activated ice nuclei with that of Meyers et al.; allowing for ice supersaturation in the saturation adjustment; accounting for ambient RH in the growth of cloud ice to snow; and adding/accounting for cloud ice fall speeds. In addition, size-mapping schemes for snow/graupel were added as functions of temperature and mixing ratio, lowering particle sizes at colder temperatures but allowing larger particles near the melting level and at higher mixing ratios. The modifications were applied to a weakly organized continental case and an oceanic mesoscale convective system (MCS). Strong echoes in the middle and upper troposphere were reduced in both cases. Peak reflectivities agreed well with radar for the weaker land case but, despite improvement, remained too high for the MCS. Reflectivity distributions versus height were much improved versus radar for the less organized land case but not for the MCS despite fewer excessively strong echoes aloft due to a bias toward weaker echoes at storm top.
C1 [Lang, Stephen E.] NASA GSFC, Mesoscale Atmospher Proc Branch, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Lang, Stephen E.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Zeng, Xiping] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Li, Yaping] NOAA NESDIS STAR, IMSG, Camp Springs, MD USA.
RP Lang, SE (reprint author), NASA GSFC, Mesoscale Atmospher Proc Branch, Atmospheres Lab, Code 613-1, Greenbelt, MD 20771 USA.
EM stephen.e.lang@nasa.gov
FU NASA
FX This research was supported by the NASA Precipitation Measuring Mission
(PMM) and the NASA Modeling, Analysis, and Prediction (MAP) Program. The
authors are grateful to Drs. Ramesh Kakar, Don Anderson, and David B.
Considine at NASA headquarters for their support of this research; to
Drs. Andrew Heymsfield and Derek Posselt and Prof. J.-P. Chen for their
useful suggestions; to Dr. Robert Cifelli for providing the LBA radar
data; and to Dr. Jiundar Chern for carefully checking the code.
Acknowledgment is also made to the NASA Goddard Space Flight Center and
NASA Ames Research Center computing facilities and to Dr. Tsengdar Lee
at NASA HQ for the computational resources used in this research. We
would also like to thank three anonymous reviewers for their
constructive comments that improved this paper.
NR 96
TC 33
Z9 34
U1 1
U2 4
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 OCT
PY 2011
VL 68
IS 10
BP 2306
EP 2320
DI 10.1175/JAS-D-10-05000.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 835KG
UT WOS:000296034700009
ER
PT J
AU Witek, ML
Teixeira, J
Matheou, G
AF Witek, Marcin L.
Teixeira, Joao
Matheou, Georgios
TI An Eddy Diffusivity-Mass Flux Approach to the Vertical Transport of
Turbulent Kinetic Energy in Convective Boundary Layers
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID SHALLOW CUMULUS CONVECTION; INCOMPRESSIBLE-FLOW; CLOSURE SCHEMES; MODEL;
SIMULATION; PARAMETERIZATION; DRY; STRATOCUMULUS; ATMOSPHERE; FRAMEWORK
AB In this study a new approach to the vertical transport of the turbulent kinetic energy (TKE) is proposed. The principal idea behind the new parameterization is that organized updrafts or convective plumes play an important role in transferring TKE vertically within convectively driven boundary layers. The parameterization is derived by applying an updraft environment decomposition to the vertical velocity triple correlation term in the TKE prognostic equation. The additional mass flux (MF) term that results from this decomposition closely resembles the features of the TKE transport diagnosed from the large-eddy simulation (LES) and accounts for 97% of the LES-diagnosed transport when the updraft fraction is set to 0.13. Another advantage of the MF term is that it is a function of the updraft vertical velocity and can be readily calculated using already existing parameterization. The new MF approach, combined with several eddy diffusivity (ED) formulations, is implemented into a simplified 1D TKE prognostic model. The ID model results, compared against LES simulations of dry convective boundary layers, show substantial improvement in representing the vertical structure of TKE. The new combined ED MF parameterization, as well as the MF term alone, surpasses in accuracy the ED parameterizations. The proposed TKE transport parameterization shows large potential of improving TKE simulations in mesoscale and global circulation models.
C1 [Witek, Marcin L.; Teixeira, Joao; Matheou, Georgios] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Witek, ML (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM marcin.l.witek@jpl.nasa.gov
RI Witek, Marcin/G-9440-2016
FU National Aeronautics and Space Administration; NASA Advanced
Super-computing Division at Ames Research Center; NSF MRI [EIA-0079871];
AFOSR [FA9550-07-1-0091]; Office of Naval Research [N0001408IP20064];
NASA MAP
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. Resources supporting this work
were provided by the NASA High-End Computing Program through the NASA
Advanced Super-computing Division at Ames Research Center. Simulations
were also performed on the Shared Heterogeneous Cluster at the Center
for Advanced Computing Research at the California Institute of
Technology developed with cofunding by NSF MRI Grant EIA-0079871 and
AFOSR Grant FA9550-07-1-0091 as part of a larger research effort on
turbulent mixing. The authors also acknowledge the support provided by
the Office of Naval Research, Marine Meteorology Program under Award
N0001408IP20064 and the NASA MAP Program.
NR 37
TC 4
Z9 4
U1 2
U2 10
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 OCT
PY 2011
VL 68
IS 10
BP 2385
EP 2394
DI 10.1175/JAS-D-11-06.1
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 835KG
UT WOS:000296034700013
ER
PT J
AU Pearson, JC
Drouin, BJ
Yu, SS
Gupta, H
AF Pearson, John C.
Drouin, Brian J.
Yu, Shanshan
Gupta, Harshal
TI Microwave spectroscopy of methanol between 2.48 and 2.77 THz
SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA B-OPTICAL PHYSICS
LA English
DT Article
ID MOLECULAR-SPECTROSCOPY; INTERNAL-ROTATION; ASYMMETRIC-TOP; WAVE;
SPECTRUM; DATABASE; MASERS; LASER; TOOL
AB Methanol is the prototypical intermediate C(3V) barrier to the internal rotation molecule. It is also one of the primary sources of line confusion in the interstellar medium where it is observed in a variety of regions with temperatures approaching room temperature in the more extreme cases. Recently, a fairly comprehensive rotational study of methanol was performed that analyzed the available data to J = 30 in the first three torsional states with a rho axis method (RAM) Hamiltonian. The availability of a new frequency source covering 2.48 to 2.77 THz offered a unique opportunity to rigorously test the ability of the RAM Hamiltonian model in extrapolation in both J and K quantum numbers and an opportunity to confirm a number of newly assigned methanol levels. It also facilitated a unique opportunity for a direct comparison of results obtained with a frequency multiplier, Fourier transform infrared, laser sideband, tunable far infrared, and quantum cascade lasers at terahertz frequencies. The spectrum of methanol is presented and assigned for the 2.48-2.77 THz band. Lines in the first four torsional states are identified and compared to predictions of the RAM model for the first three torsional states and available energy levels for the nu(t) = 3 state. A number of previously unidentified subbands are assigned for the first time, providing some unique insight into the difficulties of extrapolating with a rho axis C(3V) internal rotation Hamiltonian. (C) 2011 Optical Society of America
C1 [Pearson, John C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Pearson, JC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM John.C.Pearson@jpl.nasa.gov
RI Yu, Shanshan/D-8733-2016
FU National Aeronautics and Space Administration (NASA); NASA Astrophysics
Research and Analysis
FX This research was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration (NASA). Funding from two NASA Astrophysics
Research and Analysis grants is gratefully acknowledged-one for the
construction of the source and the other for the collection and analysis
of the spectra of astrophysical weeds, such as methanol, both being
essential in the present result. Thanks go to Dr. G. Moruzzi for
providing the FTIR methanol spectrum and to Dr. H.-W. Hubers for
providing the QCL methanol spectrum.
NR 27
TC 10
Z9 11
U1 2
U2 20
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 OCT
PY 2011
VL 28
IS 10
BP 2549
EP 2577
PG 29
WC Optics
SC Optics
GA 835OJ
UT WOS:000296045400035
ER
PT J
AU Wade, GA
Howarth, ID
Townsend, RHD
Grunhut, JH
Shultz, M
Bouret, JC
Fullerton, A
Marcolino, W
Martins, F
Naze, Y
Doula, AU
Walborn, NR
Donati, JF
AF Wade, G. A.
Howarth, I. D.
Townsend, R. H. D.
Grunhut, J. H.
Shultz, M.
Bouret, J. -C.
Fullerton, A.
Marcolino, W.
Martins, F.
Naze, Y.
Doula, A. Ud
Walborn, N. R.
Donati, J. -F.
CA MiMeS Collaboration
TI Confirmation of the magnetic oblique rotator model for the Of?p star HD
191612
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: individual: HD 191612; stars: magnetic field; stars: massive;
stars: rotation
ID DRIVEN STELLAR WINDS; DYNAMICAL SIMULATIONS; BP STARS; FIELD; HD-191612;
AP; SPECTROSCOPY; FLOW
AB This paper reports high-precision Stokes V spectra of HD 191612 acquired using the ESPaDOnS spectropolarimeter at the Canada-France-Hawaii Telescope, in the context of the Magnetism in Massive Stars (MiMeS) Project. Using measurements of the equivalent width of the Ha line and radial velocities of various metallic lines, we have updated both the spectroscopic and orbital ephemerides of this star. We confirm the presence of a strong magnetic field in the photosphere of HD 191612, and detect its variability. We establish that the longitudinal field varies in a manner consistent with the spectroscopic period of 537.6d, in an approximately sinusoidal fashion. The phases of minimum and maximum longitudinal field are, respectively, coincident with the phases of maximum and minimum Ha equivalent width and Hp magnitude. This demonstrates a firm connection between the magnetic field and the processes responsible for the line and continuum variability. Interpreting the variation of the longitudinal magnetic field within the context of the dipole oblique rotator model, and adopting an inclination i = 30 degrees obtained assuming alignment of the orbital and rotational angular momenta, we obtain a best-fitting surface magnetic field model with obliquity beta = 67 degrees +/- 5 degrees and polar strength B-d = 2450 +/- 400 G. The inferred magnetic field strength implies an equatorial wind magnetic confinement parameter eta* similar or equal to 50, supporting a picture in which the H alpha emission and photometric variability have their origin in an oblique, rigidly rotating magnetospheric structure resulting from a magnetically channelled wind. This interpretation is supported by our successful Monte Carlo radiative transfer modelling of the photometric variation, which assumes the enhanced plasma densities in the magnetic equatorial plane above the star implied by such a picture, according to a geometry that is consistent with that derived from the magnetic field. Predictions of the continuum linear polarization resulting from Thompson scattering from the magnetospheric material indicate that the Stokes Q and U variations are highly sensitive to the magnetospheric geometry, and that expected amplitudes are in the range of current instrumentation.
C1 [Wade, G. A.; Grunhut, J. H.; Shultz, M.] Royal Mil Coll Canada, Dept Phys, Stn Forces, Kingston, ON K7K 7B4, Canada.
[Howarth, I. D.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Townsend, R. H. D.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Grunhut, J. H.; Shultz, M.] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada.
[Bouret, J. -C.] CNRS, LAM UMR 6110, F-13388 Marseille 13, France.
[Bouret, J. -C.] Univ Aix Marseille 1, F-13388 Marseille 13, France.
[Bouret, J. -C.] NASA, GSFC, Greenbelt, MD 20771 USA.
[Fullerton, A.; Walborn, N. R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Marcolino, W.] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio De Janeiro, Brazil.
[Martins, F.] CNRS, LUPM UMR5299, F-34095 Montpellier, France.
[Martins, F.] Univ Montpellier 2, F-34095 Montpellier, France.
[Naze, Y.] Univ Liege, FNRS Inst Astrophys & Geophys, Liege, Belgium.
[Doula, A. Ud] Penn State Worthington Scranton, Dunmore, PA 18512 USA.
[Donati, J. -F.] Observ Midi Pyrenees, F-31400 Toulouse, France.
RP Wade, GA (reprint author), Royal Mil Coll Canada, Dept Phys, Stn Forces, POB 17000, Kingston, ON K7K 7B4, Canada.
EM wade-g@rmc.ca
RI 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013; Marcolino,
Wagner/M-7428-2014;
OI Naze, Yael/0000-0003-4071-9346
FU Natural Science and Engineering Research Council of Canada (NSERC); NASA
[NAS5-26555]; Fonds National de la Recherche Scientifique (Belgium);
PRODEX XMM; Integral; 'Action de Recherche Concertee' (CFWB-Academie
Wallonie Europe)
FX GAW acknowledges support from the Natural Science and Engineering
Research Council of Canada (NSERC). STScI is operated by AURA, Inc.,
under NASA contract NAS5-26555. YN acknowledges support from the Fonds
National de la Recherche Scientifique (Belgium), the PRODEX XMM and
Integral contracts and the 'Action de Recherche Concertee'
(CFWB-Academie Wallonie Europe).
NR 34
TC 37
Z9 38
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2011
VL 416
IS 4
BP 3160
EP 3169
DI 10.1111/j.1365-2966.2011.19265.x
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 829OJ
UT WOS:000295592600059
ER
PT J
AU Mader, TH
Gibson, CR
Pass, AF
Kramer, LA
Lee, AG
Fogarty, J
Tarver, WJ
Dervay, JP
Hamilton, DR
Sargsyan, A
Phillips, JL
Tran, D
Lipsky, W
Choi, J
Stern, C
Kuyumjian, R
Polk, JD
AF Mader, Thomas H.
Gibson, C. Robert
Pass, Anastas F.
Kramer, Larry A.
Lee, Andrew G.
Fogarty, Jennifer
Tarver, William J.
Dervay, Joseph P.
Hamilton, Douglas R.
Sargsyan, Ashot
Phillips, John L.
Duc Tran
Lipsky, William
Choi, Jung
Stern, Claudia
Kuyumjian, Raffi
Polk, James D.
TI Optic Disc Edema, Globe Flattening, Choroidal Folds, and Hyperopic
Shifts Observed in Astronauts after Long-duration Space Flight
SO OPHTHALMOLOGY
LA English
DT Article
ID HEAD-DOWN TILT; IDIOPATHIC INTRACRANIAL HYPERTENSION;
CEREBROSPINAL-FLUID OUTFLOW; COTTON-WOOL SPOTS; ACQUIRED HYPEROPIA;
INTRAOCULAR-PRESSURE; REFRACTIVE CHANGES; RADIAL KERATOTOMY;
HIGH-ALTITUDE; NERVE
AB Purpose: To describe the history, clinical findings, and possible etiologies of ophthalmic findings discovered in 7 astronauts after long-duration space flight, and document vision changes in approximately 300 additional astronauts.
Design: Retrospective, observational examination of ophthalmic findings in 7 astronauts and analysis of postflight questionnaires regarding in-flight vision changes in approximately 300 additional astronauts.
Participants: Seven astronauts with ophthalmic anomalies upon return from long-duration space missions to the International Space Station and 300 additional astronauts who completed postflight questionnaires regarding in-flight vision changes.
Methods: Before and after long-duration space flight, all 7 subjects underwent complete eye examinations, including cycloplegic and/or manifest refraction and fundus photography. Six underwent postmission optical coherence tomography (OCT) and magnetic resonance imaging (MRI); 4 had lumbar punctures (LP). Approximately 300 astronauts were queried regarding visual changes during space missions.
Main Outcome Measures: Refractive change, fundus photograph examination, retina OCT, orbital MRI, LP opening pressures, and examination of visual acuity data.
Results: After 6 months of space flight, 7 astronauts had ophthalmic findings, consisting of disc edema in 5, globe flattening in 5, choroidal folds in 5, cotton wool spots (CWS) in 3, nerve fiber layer thickening by OCT in 6, and decreased near vision in 6 astronauts. Five of 7 with near vision complaints had a hyperopic shift >= + 0.50 diopters (D) between pre/postmission spherical equivalent refraction in 1 or both eyes (range, +0.50 to +1.75 D). These 5 showed globe flattening on MRI. Lumbar punctures performed in the 4 with disc edema documented opening pressures of 22, 21, 28, and 28.5 cm H(2)O performed 60, 19, 12, and 57 days postmission, respectively. The 300 postflight questionnaires documented that approximately 29% and 60% of astronauts on short and long-duration missions, respectively, experienced a degradation in distant and near visual acuity. Some of these vision changes remain unresolved years after flight.
Conclusions: We hypothesize that the optic nerve and ocular changes we describe may result from cephalad fluid shifts brought about by prolonged microgravity exposure. The findings we report may represent parts of a spectrum of ocular and cerebral responses to extended microgravity exposure.
Financial Disclosure(s): The authors have no proprietary or commercial interest in any of the materials discussed in this article. Ophthalmology 2011; 118: 2058-2069 (C) 2011 by the American Academy of Ophthalmology.
C1 [Mader, Thomas H.] Alaska Native Med Ctr, Dept Ophthalmol, Anchorage, AK 99508 USA.
[Gibson, C. Robert; Duc Tran; Lipsky, William; Choi, Jung] Coastal Eye Associates, Webster, TX USA.
[Pass, Anastas F.] Univ Houston, Univ Eye Inst, Houston, TX USA.
[Kramer, Larry A.] Univ Texas Hlth Sci Ctr, Dept Diagnost Imaging & Intervent, Houston, TX USA.
[Lee, Andrew G.] Methodist Hosp, Dept Ophthalmol, Houston, TX 77030 USA.
[Fogarty, Jennifer; Tarver, William J.; Dervay, Joseph P.; Phillips, John L.; Polk, James D.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Hamilton, Douglas R.; Sargsyan, Ashot] Wyle Integrated Sci & Engn, Houston, TX USA.
[Stern, Claudia] German Aerosp Ctr, Cologne, Germany.
[Kuyumjian, Raffi] European Space Agcy, Crew Med Support Off, Cologne, Germany.
RP Mader, TH (reprint author), Alaska Native Med Ctr, Dept Ophthalmol, 4315 Diplomacy Dr, Anchorage, AK 99508 USA.
EM tmader@acsalaska.net
NR 56
TC 114
Z9 120
U1 4
U2 33
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0161-6420
J9 OPHTHALMOLOGY
JI Ophthalmology
PD OCT
PY 2011
VL 118
IS 10
BP 2058
EP 2069
DI 10.1016/j.ophtha.2011.06.021
PG 12
WC Ophthalmology
SC Ophthalmology
GA 835WG
UT WOS:000296066900026
PM 21849212
ER
PT J
AU Liu, R
Wang, TJ
Lee, J
Stenborg, G
Liu, C
Park, SH
Wang, HM
AF Liu, Rui
Wang, Tong-Jiang
Lee, Jeongwoo
Stenborg, Guillermo
Liu, Chang
Park, Sung-Hong
Wang, Hai-Min
TI Observing the reconnection region in a transequatorial loop system
SO RESEARCH IN ASTRONOMY AND ASTROPHYSICS
LA English
DT Article
DE Sun: coronal mass ejections; Sun: flares; Sun: corona
ID CORONAL MASS EJECTIONS; X-RAY SOURCE; MAGNETIC RECONNECTION;
SOLAR-FLARE; CURRENT SHEET; CHROMOSPHERIC EVAPORATION;
PARTICLE-ACCELERATION; ACTIVE-REGION; FIELD; PLASMA
AB A vertical current sheet is a crucial element in many flare/coronal mass ejection (CME) models. For the first time, Liu et al. reported a vertical current sheet directly imaged during the flare rising phase with the EUV Imaging Telescope (EIT) onboard the Solar and Heliospheric Observatory (SOHO). As a follow-up study, here we present the comprehensive analysis and detailed physical interpretation of the observation. The current sheet formed due to the gradual rise of a transequatorial loop system. As the loop legs approached each other, plasma flew at similar to 6 km s(-1) into a local area where a cusp-shaped flare loop subsequently formed and the current sheet was seen as a bright, collimated structure of global length (>= 0.25 R-circle dot) and macroscopic width ((5-10) x 10(3) km), extending from 50 Mm above the flaring loop to the border of the BIT field of view (FOV). The reconnection rate in terms of the Alfven Mach number is estimated to be only 0.005-0.009, albeit a halo CME was accelerated from similar to 400 km s(-1) to similar to 1300 km s(-1) within the coronagraph FOV. Drifting pulsating structures at metric frequencies were recorded during the impulsive phase, implying tearing of the current sheet in the high corona. A radio Type III burst occurred when the current sheet was clearly seen in EUV, indicative of accelerated electrons beaming upward from the upper tip of the current sheet. A cusp-shaped dimming region was observed to be located above the post-flare arcade during the decay phase in EIT; both the arcade and the dimming expanded with time. With the Coronal Diagnostic Spectrometer (CDS) aboard SOHO, a clear signature of chromospheric evaporation was seen during the decay phase, i.e., the cusp-shaped dimming region was associated with plasma upflows detected with EUV hot emission lines, while the post-flare loop was associated with downflows detected with cold lines. This event provides a comprehensive view of the reconnection geometry and dynamics in the solar corona.
C1 [Liu, Rui; Liu, Chang; Park, Sung-Hong; Wang, Hai-Min] New Jersey Inst Technol, Ctr Solar Terr Res, Space Weather Res Lab, Newark, NJ 07102 USA.
[Wang, Tong-Jiang] Catholic Univ Amer, Greenbelt, MD 20771 USA.
[Wang, Tong-Jiang] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lee, Jeongwoo] New Jersey Inst Technol, Dept Phys, Newark, NJ 07102 USA.
[Stenborg, Guillermo] Interferometrics Inc, Herndon, VA 20171 USA.
[Park, Sung-Hong] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
RP Liu, R (reprint author), New Jersey Inst Technol, Ctr Solar Terr Res, Space Weather Res Lab, Newark, NJ 07102 USA.
EM rui.liu@njit.edu
RI Liu, Rui/B-4107-2012; Park, Sung-Hong/K-1578-2014
OI Liu, Chang/0000-0002-6178-7471; Liu, Rui/0000-0003-4618-4979; Park,
Sung-Hong/0000-0001-9149-6547
FU NASA [NNX08-AJ23G, NNX08-AQ90G, NNX08AP88G, NNX09AG10G]; NSF
[ATM-0849453, AST-0908344]
FX SOHO is a project of international cooperation between ESA and NASA.
R.L., C.L., S.P. and H.W. were supported by NASA grants NNX08-AJ23G and
NNX08-AQ90G and by NSF grant ATM-0849453. T.W. was supported by NASA
grants NNX08AP88G and NNX09AG10G. J.L. was supported by NSF grant
AST-0908344.
NR 84
TC 6
Z9 7
U1 3
U2 8
PU NATL ASTRONOMICAL OBSERVATORIES, CHIN ACAD SCIENCES
PI BEIJING
PA 20A DATUN RD, CHAOYANG, BEIJING, 100012, PEOPLES R CHINA
SN 1674-4527
J9 RES ASTRON ASTROPHYS
JI Res. Astron. Astrophys.
PD OCT
PY 2011
VL 11
IS 10
BP 1209
EP 1228
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 836RC
UT WOS:000296127800009
ER
PT J
AU Schultz, CJ
Petersen, WA
Carey, LD
AF Schultz, Christopher J.
Petersen, Walter A.
Carey, Lawrence D.
TI Lightning and Severe Weather: A Comparison between Total and
Cloud-to-Ground Lightning Trends
SO WEATHER AND FORECASTING
LA English
DT Article
ID INTENSE CONVECTIVE STORMS; UNITED-STATES; MAPPING ARRAY; THUNDERSTORM
ELECTRIFICATION; TORNADIC SUPERCELL; DETECTION NETWORK; PRECIPITATION;
EVOLUTION; RADAR; ALGORITHMS
AB Many studies over the past several decades have attempted to correlate trends in lightning (e.g., rates, polarity) to severe weather occurrence. These studies mainly used cloud-to-ground (CG) lightning information due to the ease of data availability, high detection efficiency, and broad coverage across the United States, with somewhat inconclusive results. Conversely, it has been demonstrated that trends in total lightning are more robustly correlated to severe weather occurrence, with rapid increases in total lightning observed 10s of minutes prior to the onset of severe weather. Unfortunately, total lightning observations are not as numerous, or available over the same areal coverage domain, as provided by CG networks. Relatively few studies have examined concurrent trends in both total and CG lightning within the same severe thunderstorm, or even large sets of thunderstorms using an objective lightning jump algorithm. Multiple studies have shown that the total flash rate rapidly increases prior to the onset of severe weather. What is untested within the same framework is the use of CG information to perform the same task. Herein, total and CG lightning trends for 711 thunderstorms occurring in four regions of the country were examined to demonstrate the increased utility that total lightning provides over CG lightning, specifically within the framework of developing a useful lightning-based severe weather warning decision support tool. Results indicate that while both lightning datasets demonstrate the presence of increased lightning activity prior to the onset of severe weather, the use of total lightning trends was more effective than CG trends [probability of detection (POD), 79% versus 66%; false alarm rate (FAR), 36% versus 53%; critical success index (CSI), 55% versus 38%; Heidke skill score (HSS), 0.71 versus 0.55]. Moreover, 40% of false alarms associated with total lightning, and 16% of false alarms with CG lightning trends, occurred when a lightning jump associated with a severe weather "warning" was already in effect. If these false alarms are removed, the FAR drops from 36% to 22% for total lightning and from 53% to 44% for CG lightning. Importantly, average lead times prior to severe weather occurrence were higher using total lightning as compared with CG lightning (20.65 versus 13.54 min). The ultimate goal of this study was to demonstrate the increased utility of total lightning information that the Geostationary Lightning Mapper (GLM) will provide to operational meteorology in anticipation of severe convective weather on a hemispheric scale once Geostationary Operational Environmental Satellite-R (GOES-R) is deployed in the next decade.
C1 [Schultz, Christopher J.] Univ Alabama, Dept Atmospher Sci, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
[Petersen, Walter A.] NASA Marshall Space Flight Ctr, Huntsville, AL USA.
[Carey, Lawrence D.] Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35805 USA.
RP Schultz, CJ (reprint author), Univ Alabama, Dept Atmospher Sci, Natl Space Sci & Technol Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM schultz@nsstc.uah.edu
FU GOES-R Risk Reduction effort under the Space Act Agreement
[NA07AANEG0284]; NOAA/NWS [NA08NWS4680034]; NOAA, UAH/NSSTC Tornado and
Hurricane Observations Research Center (THOR)
FX This work was funded by the GOES-R Risk Reduction effort under the Space
Act Agreement (NA07AANEG0284). Larry Carey also gratefully acknowledges
partial support for this research under an award from the NOAA/NWS CSTAR
program (NA08NWS4680034). Walt Petersen and Larry Carey acknowledge
partial funding of this research via NOAA's support of the UAH/NSSTC
Tornado and Hurricane Observations Research Center (THOR). A special
thank you goes out to Dr. Timothy Lang of Colorado State University,
Mrs. Stephanie Weiss of the University of Oklahoma, and Dr. Eric Bruning
of Texas Tech University for their support of this study by providing
lightning mapping array data from the STEPS field project and the OK-LMA
network, as well as valuable discussions about the datasets. The authors
would also like to acknowledge John Hall and Jeff Bailey for their
continued support through maintenance of the NALMA and DCLMA, as well
as, Hugh Christian and William Koshak of NASA MSFC for their continued
support and advice throughout this study. Finally, the authors would
like to acknowledge three anonymous reviewers for helping to improve the
quality of this manuscript.
NR 60
TC 54
Z9 56
U1 3
U2 28
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 OCT
PY 2011
VL 26
IS 5
BP 744
EP 755
DI 10.1175/WAF-D-10-05026.1
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 834FI
UT WOS:000295944400011
ER
PT J
AU Hall, JL
Yavrouian, AH
Kerzhanovich, VV
Fredrickson, T
Sandy, C
Pauken, MT
Kulczycki, EA
Walsh, GJ
Said, M
Day, S
AF Hall, J. L.
Yavrouian, A. H.
Kerzhanovich, V. V.
Fredrickson, T.
Sandy, C.
Pauken, Michael T.
Kulczycki, E. A.
Walsh, G. J.
Said, M.
Day, S.
TI Technology development for a long duration, mid-cloud level Venus
balloon
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Aerobot; Balloon; Venus; Mobility; Deployment; Inflation
ID SYSTEM
AB This paper describes the results of ongoing technology development activities for a Venus spherical superpressure balloon capable of flying for long durations (30 days) in the middle cloud layer at an altitude of 55.5 km. Data is presented from a successful aerial deployment and inflation flight experiment on a 5.5 m diameter prototype balloon conducted at a 2.5 km altitude above the Earth. Although the balloon in that test was not released for free flight, all other steps in the deployment and inflation process were successfully executed. Experimental and computational results are also presented from an investigation of the stress concentration phenomenon at the junction of the metal end fitting and fabric end cap of the prototype Venus balloon. Good agreement was found between the simulation and experimental results and a stress concentration factor of 1.55 determined for this end cap design compared to the expectations of thin membrane theory. Finally, results are presented for a new, second-generation Venus balloon material utilizing Actin' film instead of Teflon. Optical property and sulfuric acid tolerance data are presented for this material based on laboratory testing of samples. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Hall, J. L.; Yavrouian, A. H.; Kerzhanovich, V. V.; Pauken, Michael T.; Kulczycki, E. A.; Walsh, G. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Fredrickson, T.; Sandy, C.] ILC Dover Inc, Frederica, DE 19946 USA.
[Said, M.] NASA, Wallops Flight Facil, Wallops Isl, VA USA.
[Day, S.] Struct Integrity Associates Inc, San Jose, CA 95118 USA.
RP Hall, JL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jlhall@mail.jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The research described in this paper was performed by the Jet Propulsion
Laboratory, California Institute of Technology and ILC Dover Inc., under
a contract with the National Aeronautics and Space Administration. The
authors would like to thank the following people for this assistance
with various parts of the research reported herein: Alan Hirsch and Phil
Faria of Lamart Corp.; Jody Ware and Jeff Roushey of ILC Dover Inc.; Joe
Melko, Alexis Benz, Mark Anderson and Bill Haney of JPL.
NR 4
TC 1
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U1 0
U2 4
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD OCT 1
PY 2011
VL 48
IS 7
BP 1238
EP 1247
DI 10.1016/j.asr.2011.05.034
PG 10
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 828JV
UT WOS:000295498200008
ER
PT J
AU Gordon, KD
Meixner, M
Meade, MR
Whitney, B
Engelbracht, C
Bot, C
Boyer, ML
Lawton, B
Sewilo, M
Babler, B
Bernard, JP
Bracker, S
Block, M
Blum, R
Bolatto, A
Bonanos, A
Harris, J
Hora, JL
Indebetouw, R
Misselt, K
Reach, W
Shiao, B
Tielens, X
Carlson, L
Churchwell, E
Clayton, GC
Chen, CHR
Cohen, M
Fukui, Y
Gorjian, V
Hony, S
Israel, FP
Kawamura, A
Kemper, F
Leroy, A
Li, A
Madden, S
Marble, AR
McDonald, I
Mizuno, A
Mizuno, N
Muller, E
Oliveira, JM
Olsen, K
Onishi, T
Paladini, R
Paradis, D
Points, S
Robitaille, T
Rubin, D
Sandstrom, K
Sato, S
Shibai, H
Simon, JD
Smith, LJ
Srinivasan, S
Vijh, U
Van Dyk, S
van Loon, JT
Zaritsky, D
AF Gordon, K. D.
Meixner, M.
Meade, M. R.
Whitney, B.
Engelbracht, C.
Bot, C.
Boyer, M. L.
Lawton, B.
Sewilo, M.
Babler, B.
Bernard, J. -P.
Bracker, S.
Block, M.
Blum, R.
Bolatto, A.
Bonanos, A.
Harris, J.
Hora, J. L.
Indebetouw, R.
Misselt, K.
Reach, W.
Shiao, B.
Tielens, X.
Carlson, L.
Churchwell, E.
Clayton, G. C.
Chen, C. -H. R.
Cohen, M.
Fukui, Y.
Gorjian, V.
Hony, S.
Israel, F. P.
Kawamura, A.
Kemper, F.
Leroy, A.
Li, A.
Madden, S.
Marble, A. R.
McDonald, I.
Mizuno, A.
Mizuno, N.
Muller, E.
Oliveira, J. M.
Olsen, K.
Onishi, T.
Paladini, R.
Paradis, D.
Points, S.
Robitaille, T.
Rubin, D.
Sandstrom, K.
Sato, S.
Shibai, H.
Simon, J. D.
Smith, L. J.
Srinivasan, S.
Vijh, U.
Van Dyk, S.
van Loon, J. Th
Zaritsky, D.
TI SURVEYING THE AGENTS OF GALAXY EVOLUTION IN THE TIDALLY STRIPPED, LOW
METALLICITY SMALL MAGELLANIC CLOUD (SAGE-SMC). I. OVERVIEW
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: individual (SMC)
ID SPITZER-SPACE-TELESCOPE; MULTIBAND IMAGING PHOTOMETER; INFRARED ARRAY
CAMERA; MASS-LOSS RETURN; SPECTRAL IRRADIANCE CALIBRATION; YOUNG STELLAR
OBJECTS; GIANT BRANCH STARS; 24 MU-M; ABSOLUTE CALIBRATION; EVOLVED
STARS
AB The Small Magellanic Cloud (SMC) provides a unique laboratory for the study of the lifecycle of dust given its low metallicity (similar to 1/5 solar) and relative proximity (similar to 60 kpc). This motivated the SAGE-SMC (Surveying the Agents of Galaxy Evolution in the Tidally Stripped, Low Metallicity Small Magellanic Cloud) Spitzer Legacy program with the specific goals of studying the amount and type of dust in the present interstellar medium, the sources of dust in the winds of evolved stars, and how much dust is consumed in star formation. This program mapped the full SMC (30 deg(2)) including the body, wing, and tail in seven bands from 3.6 to 160 mu m using IRAC and MIPS on the Spitzer Space Telescope. The data were reduced and mosaicked, and the point sources were measured using customized routines specific for large surveys. We have made the resulting mosaics and point-source catalogs available to the community. The infrared colors of the SMC are compared to those of other nearby galaxies and the 8 mu m/24 mu m ratio is somewhat lower than the average and the 70 mu m/160 mu m ratio is somewhat higher than the average. The global infrared spectral energy distribution (SED) shows that the SMC has approximately 1/3 the aromatic emission/polycyclic aromatic hydrocarbon abundance of most nearby galaxies. Infrared color-magnitude diagrams are given illustrating the distribution of different asymptotic giant branch stars and the locations of young stellar objects. Finally, the average SED of H II/star formation regions is compared to the equivalent Large Magellanic Cloud average H II/star formation region SED. These preliminary results will be expanded in detail in subsequent papers.
C1 [Gordon, K. D.; Meixner, M.; Boyer, M. L.; Lawton, B.; Shiao, B.; Smith, L. J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Meade, M. R.; Whitney, B.; Babler, B.; Bracker, S.; Churchwell, E.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Whitney, B.] Space Sci Inst, Boulder, CO 80301 USA.
[Engelbracht, C.; Block, M.; Misselt, K.; Marble, A. R.; Zaritsky, D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Bot, C.] Univ Strasbourg, Ctr Donnees Astron Strasbourg CDS, UMR 7550, F-67000 Strasbourg, France.
[Sewilo, M.; Carlson, L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Bernard, J. -P.] Univ Toulouse, UPS, CESR, F-31028 Toulouse 4, France.
[Blum, R.; Harris, J.; Olsen, K.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Bolatto, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Bonanos, A.] Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece.
[Hora, J. L.; Robitaille, T.] Harvard Smithsonian, CfA, Cambridge, MA 02138 USA.
[Indebetouw, R.; Reach, W.; Paladini, R.; Paradis, D.; Van Dyk, S.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Indebetouw, R.; Leroy, A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Tielens, X.; Israel, F. P.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands.
[Clayton, G. C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
[Chen, C. -H. R.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Cohen, M.] Monterey Inst Res Astron, Marina, CA 93933 USA.
[Fukui, Y.; Kawamura, A.; Mizuno, A.; Mizuno, N.; Muller, E.; Onishi, T.; Sato, S.; Shibai, H.] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Gorjian, V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hony, S.; Madden, S.; Rubin, D.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Kawamura, A.; Muller, E.] Natl Astron Observ Japan, ALMA J Project Off, Tokyo 1818588, Japan.
[Kemper, F.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Kemper, F.; van Loon, J. Th] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Li, A.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA.
[Marble, A. R.] Natl Solar Observ, Tucson, AZ 85719 USA.
[McDonald, I.; Oliveira, J. M.] Univ Keele, Astrophys Grp, Lennard Jones Labs, Keele ST5 5BG, Staffs, England.
[Points, S.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, La Serena, Chile.
[Sandstrom, K.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Simon, J. D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Smith, L. J.] European Space Agcy, Res & Sci Support Dept, Baltimore, MD 21218 USA.
[Srinivasan, S.] Inst Astrophys, F-75014 Paris, France.
[Vijh, U.] Univ Toledo, Ritter Astrophys Res Ctr, Toledo, OH 43606 USA.
RP Gordon, KD (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
RI Kemper, Francisca/D-8688-2011; Bonanos, Alceste/K-5392-2013;
OI Kemper, Francisca/0000-0003-2743-8240; Bonanos,
Alceste/0000-0003-2851-1905; Bot, Caroline/0000-0001-6118-2985; Babler,
Brian/0000-0002-6984-5752; Hora, Joseph/0000-0002-5599-4650; Reach,
William/0000-0001-8362-4094; Robitaille, Thomas/0000-0002-8642-1329; Van
Dyk, Schuyler/0000-0001-9038-9950
FU NASA [1340964, 1407]
FX This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under NASA contract 1407. Support for
this work was provided by NASA through Contract Number 1340964 issued by
JPL/Caltech.
NR 94
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD OCT
PY 2011
VL 142
IS 4
AR 102
DI 10.1088/0004-6256/142/4/102
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 822JY
UT WOS:000295042500006
ER
PT J
AU Koay, JY
Macquart, JP
Rickett, BJ
Bignall, HE
Lovell, JEJ
Reynolds, C
Jauncey, DL
Pursimo, T
Kedziora-Chudczer, L
Ojha, R
AF Koay, J. Y.
Macquart, J. -P.
Rickett, B. J.
Bignall, H. E.
Lovell, J. E. J.
Reynolds, C.
Jauncey, D. L.
Pursimo, T.
Kedziora-Chudczer, L.
Ojha, R.
TI DUAL-FREQUENCY OBSERVATIONS OF 140 COMPACT, FLAT-SPECTRUM ACTIVE
GALACTIC NUCLEI FOR SCINTILLATION-INDUCED VARIABILITY
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: active; intergalactic medium; ISM: structure; methods: data
analysis; quasars: general; radio continuum: ISM
ID EXTRAGALACTIC RADIO-SOURCES; PHASE CALIBRATION SOURCES; INTERSTELLAR
SCINTILLATION; INTRADAY VARIABILITY; QUASAR J1819+3845; ANNUAL
MODULATION; ANNUAL CYCLES; SKY SURVEY; BARYONS; SCATTERING
AB The 4.9 GHz Micro-Arcsecond Scintillation-Induced Variability (MASIV) Survey detected a drop in interstellar scintillation (ISS) for sources at redshifts z greater than or similar to 2, indicating an apparent increase in angular diameter or a decrease in flux density of the most compact components of these sources relative to their extended emission. This can result from intrinsic source size effects or scatter broadening in the intergalactic medium (IGM) in excess of the expected (1 + z)(1/2) angular diameter scaling of brightness temperature limited sources resulting from cosmological expansion. We report here 4.9 GHz and 8.4 GHz observations and data analysis for a sample of 140 compact, flat-spectrum sources which may allow us to determine the origin of this angular diameter-redshift relation by exploiting their different wavelength dependences. In addition to using ISS as a cosmological probe, the observations provide additional insight into source morphologies and the characteristics of ISS. As in the MASIV Survey, the variability of the sources is found to be significantly correlated with line-of-sight H alpha intensities, confirming its link with ISS. For 25 sources, time delays of about 0.15-3 days are observed between the scintillation patterns at both frequencies, interpreted as being caused by a shift in core positions when probed at different optical depths. Significant correlation is found between ISS amplitudes and source spectral index; in particular, a large drop in ISS amplitudes is observed at alpha < -0.4 confirming that steep spectrum sources scintillate less. We detect a weakened redshift dependence of ISS at 8.4 GHz over that at 4.9 GHz, with the mean variance at four-day timescales reduced by a factor of 1.8 in the z > 2 sources relative to the z < 2 sources, as opposed to the factor of three decrease observed at 4.9 GHz. This suggests scatter broadening in the IGM, but the interpretation is complicated by subtle selection effects that will be explored further in a follow-up paper.
C1 [Koay, J. Y.; Macquart, J. -P.; Bignall, H. E.; Reynolds, C.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia.
[Rickett, B. J.] Univ Calif San Diego, Dept Elect & Comp Engn, La Jolla, CA 92093 USA.
[Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
[Jauncey, D. L.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Jauncey, D. L.] Mt Stromlo & Siding Spring Observ, Weston, ACT 2611, Australia.
[Pursimo, T.] Nord Opt Telescope, Santa Cruz De La Palma 38700, Spain.
[Kedziora-Chudczer, L.] Univ New S Wales, Sch Phys & Astrophys, Sydney, NSW 2052, Australia.
[Ojha, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ojha, R.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
RP Koay, JY (reprint author), Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia.
EM kevin.koay@icrar.org
RI Macquart, Jean-Pierre/B-5306-2013; Reynolds, Cormac/B-5635-2013;
Bignall, Hayley/B-2867-2013; Koay, Jun Yi /E-4952-2015
OI Reynolds, Cormac/0000-0002-8978-0626; Bignall,
Hayley/0000-0001-6247-3071; Koay, Jun Yi /0000-0002-7029-6658
FU Curtin University; National Science Foundation (NSF) [AST-0507713]; NASA
FX J. Y. Koay is supported by the Curtin Strategic International Research
Scholarship (CSIRS) provided by Curtin University, and thanks Professor
Ron Ekers of CSIRO and Greg Taylor of the University of New Mexico for
helpful discussions. B. J. Rickett thanks the National Science
Foundation (NSF) for partial support under grant AST-0507713. R. Ojha is
supported by an appointment to the NASA Postdoctoral Program at the
Goddard Space Flight Center, administered by Oak Ridge Associated
Universities through a contract with NASA. We all thank the operators
and scientific staff at the Very Large Array; in particular, we thank
Vivek Dhawan for his extensive advice and help during our long sequence
of observations. The VLA is part of the National Radio Astronomy
Observatory (NRAO), which is a facility of the NSF operated under
cooperative agreement by Associated Universities, Inc. This study made
use of data from the Wisconsin H-Alpha Mapper (WHAM) survey, which is
funded by the NSF. Data were also obtained from the NASA/IPAC
Extragalactic Database (NED), which is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD OCT
PY 2011
VL 142
IS 4
AR 108
DI 10.1088/0004-6256/142/4/108
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 822JY
UT WOS:000295042500012
ER
PT J
AU Petrov, L
AF Petrov, L.
TI THE CATALOG OF POSITIONS OF OPTICALLY BRIGHT EXTRAGALACTIC RADIO SOURCES
OBRS-1
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE astrometry; catalogs; surveys
ID VLBA CALIBRATOR SURVEY; CELESTIAL REFERENCE FRAME; INTERFEROMETRY;
POLARIMETRY; ALIGNMENT; OPACITY; NUCLEI; JETS; SKY
AB It is expected that the European Space Agency mission Gaia will make it possible to determine coordinates in the optical domain of more than 500,000 quasars. In 2006, a radio astrometry project was launched with the overall goal of making comparisons between coordinate systems derived from future space-born astrometry instruments and the coordinate system constructed from analysis of global very long baseline interferometry (VLBI) more robust. Investigation of the rotation, zonal errors, and non-alignment of the radio and optical positions caused by both radio and optical structures is needed to validate both techniques. In order to support these studies, the densification of the list of compact extragalactic objects that are bright in both radio and optical ranges is desirable. A set of 105 objects from the list of 398 compact extragalactic radio sources with decl. > -10 degrees was observed with the Very Long Baseline Array and European VLBI Network (EVN) with the primary goal of producing images with milliarcsecond resolution. These sources are brighter than 18 mag in the V band, and they were previously detected by the EVN. In this paper, coordinates of observed sources have been derived with milliarcsecond accuracies from analysis of these VLBI observations using an absolute astrometry method. The catalog of positions for 105 target sources is presented. The accuracies of source coordinates are in the range of 0.3-7 mas, with a median of 1.1 mas.
C1 NASA, ADNET Syst Inc, GSFC, Greenbelt, MD 20771 USA.
RP Petrov, L (reprint author), NASA, ADNET Syst Inc, GSFC, Greenbelt, MD 20771 USA.
EM Leonid.Petrov@lpetrov.net
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD OCT
PY 2011
VL 142
IS 4
AR 105
DI 10.1088/0004-6256/142/4/105
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 822JY
UT WOS:000295042500009
ER
PT J
AU Xie, Y
Zhang, Y
Xiong, XX
Qu, JJ
Che, HZ
AF Xie, Yong
Zhang, Yan
Xiong, Xiaoxiong
Qu, John J.
Che, Huizheng
TI Validation of MODIS aerosol optical depth product over China using
CARSNET measurements
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE MODIS; CARSNET; Aerosol optical depth; Validation; China
ID SPECTRAL RADIANCES; LAND; EOS
AB This study evaluates Moderate Resolution Imaging Spectroradiometer (MODIS) Aerosol Optical Depth (ACID) retrievals with ground measurements collected by the China Aerosol Remote Sensing NETwork (CARSNET). In current stage, the MODIS Collection 5 (C5) AODs are retrieved by two distinct algorithms: the Dark Target (DT) and the Deep Blue (DB). The CARSNET AODs are derived with measurements of Cimel Electronique CE-318, the same instrument deployed by the AEROsol Robotic Network (AEROENT). The collocation is performed by matching each MODIS ADD pixel (10 x 10 km(2)) to CARSNET AOD mean within 7.5 min of satellite overpass. Four-year comparisons (2005-2008) of MODIS/CARSNET at ten sites show the performance of MODIS AOD retrieval is highly dependent on the underlying land surface. The MODIS DT AODs are on average lower than the CARSNET AODs by 6-30% over forest and grassland areas, but can be higher by up to 54% over urban area and 95% over desert-like area. More than 50% of the MODIS DT AODs fall within the expected error envelope over forest and grassland areas. The MODIS DT tends to overestimate for small ADD at urban area. At high vegetated area it underestimates for small ADD and overestimates for large ADD. Generally, its quality reduces with the decreasing ADD value. The MODIS DB is capable of retrieving ADD over desert but with a significant underestimation at CARSNET sites. The best retrieval of the MODIS DB is over grassland area with about 70% retrievals within the expected error. The uncertainties of MODIS ADD retrieval from spatial temporal collocation and instrument calibration are discussed briefly. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Che, Huizheng] Chinese Acad Meteorol Sci, Key Lab Atmospher Chem, Beijing 100081, Peoples R China.
[Xie, Yong; Qu, John J.] George Mason Univ, Environm Sci & Technol Ctr, Fairfax, VA 22030 USA.
[Zhang, Yan] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21250 USA.
[Zhang, Yan] NASA GSFC, Climate & Radiat Branch, Greenbelt, MD 20771 USA.
[Xiong, Xiaoxiong] NASA GSFC 614 4, Biospher Sci Branch, Greenbelt, MD 20771 USA.
RP Che, HZ (reprint author), Chinese Acad Meteorol Sci, Key Lab Atmospher Chem, Beijing 100081, Peoples R China.
EM chehz@cams.cma.gov.cn
RI Zhang, Yan/C-4792-2012; che, Huizheng/B-1354-2014
OI che, Huizheng/0000-0002-9458-3387
FU National Key Project of Basic Research [2011CB403401]; NSFC [41005086];
CAMS Basis Research Project [2008Y02, 2010Z002, 2009Z001]
FX The paper is partially supported by the National Key Project of Basic
Research (2011CB403401), Project (41005086) supported by NSFC, and the
CAMS Basis Research Project (2008Y02 &2010Z002 & 2009Z001). The authors
would like to thank the instrument managers and staffs of CARSNET sites
for the instrument maintenance. The authors would like to thank the two
anonymous reviewers for their constructive suggestions and comments.
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD OCT
PY 2011
VL 45
IS 33
BP 5970
EP 5978
DI 10.1016/j.atmosenv.2011.08.002
PG 9
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 831UT
UT WOS:000295757300002
ER
PT J
AU Kuang, S
Newchurch, MJ
Burris, J
Wang, LH
Buckley, PI
Johnson, S
Knupp, K
Huang, GY
Phillips, D
Cantrell, W
AF Kuang, Shi
Newchurch, M. J.
Burris, John
Wang, Lihua
Buckley, Patrick I.
Johnson, Steve
Knupp, Kevin
Huang, Guanyu
Phillips, Dustin
Cantrell, Wesley
TI Nocturnal ozone enhancement in the lower troposphere observed by lidar
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Air quality; Atmospheric chemistry; DIAL; Huntsville; Nocturnal boundary
layer; Residual layer
ID SOUTHEASTERN UNITED-STATES; BOUNDARY-LAYER; NORTH-AMERICA; TRANSPORT;
TENNESSEE; NASHVILLE; FIELD; CLIMATOLOGY; VARIABILITY; PROFILES
AB An ozone enhancement in the nocturnal residual layer was observed by the Huntsville ozone lidar from the late evening to midnight on 4 October 2008. The well-correlated ozone, aerosol, water vapor, and wind structures suggest a low-level jet is responsible for this ozone enhancement. HYSPLIT backward trajectories support this conclusion with southerly transport suggesting Birmingham, AL as the source. Correspondingly, the higher increasing rate of surface ozone observed in the morning of 5 October can be explained by the entrainment into the mixed layer of higher ozone aloft on this day as compared with 4 October. This case study demonstrates the importance of continuous high-resolution lidar profiling for capturing short-duration ozone variations in the lower troposphere. Published by Elsevier Ltd.
C1 [Kuang, Shi; Newchurch, M. J.; Wang, Lihua; Buckley, Patrick I.; Knupp, Kevin; Huang, Guanyu; Phillips, Dustin; Cantrell, Wesley] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA.
[Burris, John] NASA, Goddard Space Flight Ctr, Code 694, Greenbelt, MD 20771 USA.
[Johnson, Steve] NASA, George C Marshall Space Flight Ctr, Off Code VP61, Huntsville, AL 35812 USA.
RP Newchurch, MJ (reprint author), Univ Alabama, Dept Atmospher Sci, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM mike@nsstc.uah.edu
OI Buckley, Patrick/0000-0002-0806-3917; Kuang, Shi/0000-0003-2423-6088;
Huang, Guanyu/0000-0001-7314-8485
FU NASA's Science Mission Directorate; NOAA's National Environmental
Satellite, Data, and Information Service (NESDIS)
FX This work was supported by NASA's Science Mission Directorate and NOAA's
National Environmental Satellite, Data, and Information Service
(NESDIS).
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PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD OCT
PY 2011
VL 45
IS 33
BP 6078
EP 6084
DI 10.1016/j.atmosenv.2011.07.038
PG 7
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 831UT
UT WOS:000295757300014
ER
PT J
AU Hutcheson, FV
Brooks, TF
Humphreys, WM
AF Hutcheson, Florence V.
Brooks, Thomas F.
Humphreys, William M., Jr.
TI Noise radiation from a continuous mold-line link flap configuration
SO INTERNATIONAL JOURNAL OF AEROACOUSTICS
LA English
DT Article
ID AIRFRAME NOISE
AB The results of an experimental study of the noise from a Continuous Mold-Line Link (CML) flap are presented. Acoustic and unsteady surface pressure measurements were performed on a main element wing section with a half-span CML flap in NASA Langley's Quiet Flow Facility. The acoustic data were acquired with a medium aperture directional array (MADA) of microphones. The Deconvolution Approach for the Mapping of Acoustic Sources (DAMAS) method is applied to determine the spatial distribution and strength of the noise sources over the surface of the test model. A Coherent Output Power (COP) method which relates the output from unsteady surface pressure sensors to the output of the MADA is also used to obtain more detailed characteristics of the noise source distribution in the trailing edge region of the CML. These results are compared to those obtained for a blunt flap to quantify the level of noise benefit that is achieved with the CML flap. The results indicate that the noise from the CML region of the flap is 5 to 17 dB lower (depending on flap deflection and Mach number) than the noise from the side edge region of the blunt flap. Lower noise levels are obtained for all frequencies. Spectral analysis of the noise from the cove region of the CML and blunt flap models also reveal a spectral peak in the high frequency range that is related to noise scattering at the trailing edge of the main element. The peaks in the CML and blunt flap cove noise spectra are close in level and often exceed blunt side edge noise. Applying a strip of serrated tape to the trailing edge of the CML flap model main airfoil reduced the peak but increased other noise somewhat. Directivity measurements show that the CML flap can be more directional than the blunt flap.
C1 [Hutcheson, Florence V.; Brooks, Thomas F.; Humphreys, William M., Jr.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Hutcheson, FV (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM florence.v.hutcheson@nasa.gov
NR 33
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Z9 1
U1 2
U2 5
PU MULTI-SCIENCE PUBL CO LTD
PI BRENTWOOD
PA 5 WATES WAY, BRENTWOOD CM15 9TB, ESSEX, ENGLAND
SN 1475-472X
J9 INT J AEROACOUST
JI Int. J. Aeroacoust.
PD OCT-DEC
PY 2011
VL 10
IS 5-6
BP 565
EP 588
DI 10.1260/1475-472X.10.5-6.565
PG 24
WC Acoustics; Engineering, Aerospace; Mechanics
SC Acoustics; Engineering; Mechanics
GA 834TZ
UT WOS:000295988300003
ER
PT J
AU Zaman, KBMQ
Bridges, JE
Huff, DL
AF Zaman, K. B. M. Q.
Bridges, J. E.
Huff, D. L.
TI Evolution from 'tabs' to 'chevron technology' - a review
SO INTERNATIONAL JOURNAL OF AEROACOUSTICS
LA English
DT Article
ID MIXING ENHANCEMENT; NOZZLE MECHANISMS; ROUND JET; NOISE; DISTORTION;
EXIT
AB 'Chevrons', a sawtooth pattern on the trailing edge of exhaust nozzles, are being implemented on modern jet engines. The technology reduces jet noise for 'separate-flow' nozzles used on newer jet aircraft engines. The purpose of this paper is to describe the development of this technology, starting with studies of 'tabs' in the 1980' s and 1990' s. The tabs, essentially chevrons with more aggressive penetration, were studied in those early years with a focus on mixing enhancement in jets. Observations from experimentalists in connection with mixing enhancement and plume signature reduction suggested that there might also be a noise benefit. In the mid-nineties, these devices, with mild penetration to minimize thrust loss, were first seriously explored for aircraft engine noise reduction purposes. Prompted by a strong need for jet noise reduction, the study became a joint NASA/industry effort that ultimately matured the chevron technology to production by mid-2000' s. The process is an example of how fundamental studies over decades eventually migrate to application but often take a concerted effort.
C1 [Zaman, K. B. M. Q.; Bridges, J. E.; Huff, D. L.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Zaman, KBMQ (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
EM khairul.b.zaman@nasa.gov
FU Subsonic Fixed Wing; Supersonic Projects under the Fundamental
Aeronautics Program
FX Thanks are due to Jeffrey Berton, Mary Jo Long-Davis and Edmane Envia of
GRC, Charlotte Whitfield of LaRC and Naseem Saiyed of NASA headquarters
for providing comments on the manuscript, and to Steven Miller of LaRC,
Donald Weir of Honeywell Engines and Kevin Mikkelson of ASE FluiDyne for
providing helpful information. Support from the Subsonic Fixed Wing and
the Supersonic Projects under the Fundamental Aeronautics Program is
gratefully acknowledged.
NR 67
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U1 0
U2 15
PU SAGE PUBLICATIONS INC
PI THOUSAND OAKS
PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA
SN 1475-472X
EI 2048-4003
J9 INT J AEROACOUST
JI Int. J. Aeroacoust.
PD OCT-DEC
PY 2011
VL 10
IS 5-6
BP 685
EP 709
DI 10.1260/1475-472X.10.5-6.685
PG 25
WC Acoustics; Engineering, Aerospace; Mechanics
SC Acoustics; Engineering; Mechanics
GA 834TZ
UT WOS:000295988300008
ER
PT J
AU Cook, BI
Seager, R
Miller, RL
AF Cook, Benjamin I.
Seager, Richard
Miller, Ron L.
TI On the Causes and Dynamics of the Early Twentieth-Century North American
Pluvial
SO JOURNAL OF CLIMATE
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; ATLANTIC MULTIDECADAL OSCILLATION; PACIFIC
DECADAL OSCILLATION; WESTERN UNITED-STATES; COLORADO-RIVER; SST
ANOMALIES; GEOPOTENTIAL HEIGHT; REANALYSIS PROJECT; DROUGHT; CLIMATE
AB The early twentieth-century North American pluvial (1905-17) was one of the most extreme wet periods of the last 500 yr and directly led to overly generous water allotments in the water-limited American west. Here, the causes and dynamics of the pluvial event are examined using a combination of observation-based datasets and general circulation model (GCM) experiments. The character of the moisture surpluses during the pluvial differed by region, alternately driven by increased precipitation (the Southwest), low evaporation from cool temperatures (the central plains), or a combination of the two (the Pacific Northwest). Cool temperature anomalies covered much of the West and persisted through most months, part of a globally extensive period of cooler land and sea surface temperatures (SST). Circulation during boreal winter favored increased moisture import and precipitation in the Southwest, while other regions and seasons were characterized by near-normal or reduced precipitation. Anomalies in the mean circulation, precipitation, and SST fields are partially consistent with the relatively weak El Nino forcing during the pluvial and, also, reflect the impacts of positive departures in the Arctic Oscillation that occurred in 10 of the 13 pluvial winters. Differences between the reanalysis dataset, an independent statistical drought model, and GCM simulations highlight some of the remaining uncertainties in understanding the full extent of SST forcing of North American hydroclimatic variability.
C1 [Cook, Benjamin I.; Miller, Ron L.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Seager, Richard] Lamont Doherty Earth Observ, Palisades, NY USA.
RP Cook, BI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM bc9z@ldeo.columbia.edu
RI Miller, Ron/E-1902-2012; Cook, Benjamin/H-2265-2012
FU National Oceanic and Atmospheric Administration [NA08OAR4320912,
NA10OAR4310137]; NSF [ATM-06-20066, ATMO9-02716]; NASA
FX The authors thank three anonymous reviews for comments that
significantly improved the quality of this manuscript. Twentieth Century
Reanalysis V2 data were provided by the NOAA/OAR/ESRL PSD, Boulder,
Colorado, from their Web site (http://www.esrl.noaa.gov/psd/). Support
for the Twentieth Century Reanalysis Project dataset is provided by the
U.S. Department of Energy, Office of Science Innovative and Novel
Computational Impact on Theory and Experiment (DOE INCITE) program, and
the Office of Biological and Environmental Research (BER), and by the
National Oceanic and Atmospheric Administration Climate Program Office.
The authors gratefully acknowledge support from the NSF Grant
ATM-06-20066 and the NASA Atmospheric Composition Program, as well as
NSF Grant ATMO9-02716, NOAA Award NA08OAR4320912, and NOAA Grant
NA10OAR4310137.
NR 66
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U1 1
U2 10
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 OCT 1
PY 2011
VL 24
IS 19
BP 5043
EP 5060
DI 10.1175/2011JCLI4201.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 833SO
UT WOS:000295905400006
ER
PT J
AU Haynes, JM
Jakob, C
Rossow, WB
Tselioudis, G
Brown, J
AF Haynes, John M.
Jakob, Christian
Rossow, William B.
Tselioudis, George
Brown, Josephine
TI Major Characteristics of Southern Ocean Cloud Regimes and Their Effects
on the Energy Budget
SO JOURNAL OF CLIMATE
LA English
DT Article
ID TROPICAL WESTERN PACIFIC; HIGH-LEVEL CLOUDS; RADIATIVE FLUXES; CLIMATE
MODEL; ACE 1; ISCCP; MULTIMODEL; REANALYSIS; RADAR
AB Clouds over the Southern Ocean are often poorly represented by climate models, but they make a significant contribution to the top-of-atmosphere (TOA) radiation balance, particularly in the shortwave portion of the energy spectrum. This study seeks to better quantify the organization and structure of Southern Hemisphere midlatitude clouds by combining measurements from active and passive satellite-based datasets. Geostationary and polar-orbiter satellite data from the International Satellite Cloud Climatology Project (ISCCP) are used to quantify large-scale, recurring modes of cloudiness, and active observations from CloudSat and Cloud Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) are used to examine vertical structure, radiative heating rates, and precipitation associated with these clouds. It is found that cloud systems are organized into eight distinct regimes and that ISCCP overestimates the midlevel cloudiness of these regimes. All regimes contain a relatively high occurrence of low cloud, with 79% of all cloud layers observed having tops below 3 km, but multiple-layered clouds systems are present in approximately 34% of observed cloud profiles. The spatial distribution of regimes varies according to season, with cloud systems being geometrically thicker, on average, during the austral winter. Those regimes found to be most closely associated with midlatitude cyclones produce precipitation the most frequently, although drizzle is extremely common in low-cloud regimes. The regimes associated with cyclones have the highest in-regime shortwave cloud radiative effect at the TOA, but the low-cloud regimes, by virtue of their high frequency of occurrence over the oceans, dominate both TOA and surface shortwave effects in this region as a whole.
C1 [Haynes, John M.; Jakob, Christian] Monash Univ, Clayton, Vic, Australia.
[Rossow, William B.] CUNY City Coll, New York, NY 10031 USA.
[Tselioudis, George] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Brown, Josephine] Bur Meteorol, Docklands, Vic, Australia.
RP Haynes, JM (reprint author), Colorado State Univ, CIRA, Ft Collins, CO 80523 USA.
EM haynes@cira.colostate.edu
RI Rossow, William/F-3138-2015; Jakob, Christian/A-1082-2010;
OI Jakob, Christian/0000-0002-5012-3207; Brown,
Josephine/0000-0002-1100-7457
FU Australian Research Council [LP0883961]
FX The research in this study is supported by the Australian Research
Council's Linkage Project Scheme (LP0883961).
NR 53
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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 OCT 1
PY 2011
VL 24
IS 19
BP 5061
EP 5080
DI 10.1175/2011JCLI4052.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 833SO
UT WOS:000295905400007
ER
PT J
AU Jiang, XN
Waliser, DE
Olson, WS
Tao, WK
L'Ecuyer, TS
Li, KF
Yung, YL
Shige, S
Lang, S
Takayabu, YN
AF Jiang, Xianan
Waliser, Duane E.
Olson, William S.
Tao, Wei-Kuo
L'Ecuyer, Tristan S.
Li, King-Fai
Yung, Yuk L.
Shige, Shoichi
Lang, Stephen
Takayabu, Yukari N.
TI Vertical Diabatic Heating Structure of the MJO: Intercomparison between
Recent Reanalyses and TRMM Estimates
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID MADDEN-JULIAN OSCILLATION; TROPICAL INTRASEASONAL OSCILLATION; MOIST
THERMODYNAMIC STRUCTURE; SPECTRAL RETRIEVAL; LIFE-CYCLE; PR DATA; PART
I; TRIMODAL CHARACTERISTICS; RADAR OBSERVATIONS; CLIMATE MODELS
AB Capitalizing on recently released reanalysis datasets and diabatic heating estimates based on Tropical Rainfall Measuring Mission (TRMM), the authors have conducted a composite analysis of vertical anomalous heating structures associated with the Madden-Julian oscillation (MJO). Because diabatic heating lies at the heart of prevailing MJO theories, the intention of this effort is to provide new insights into the fundamental physics of the MJO. However, some discrepancies in the composite vertical MJO heating profiles are noted among the datasets, particularly between three reanalyses and three TRMM estimates. A westward tilting with altitude in the vertical heating structure of the MJO is clearly evident during its eastward propagation based on three reanalysis datasets, which is particularly pronounced when the MJO migrates from the equatorial eastern Indian Ocean (EEIO) to the western Pacific (WP). In contrast, this vertical tilt in heating structure is not readily seen in the three TRMM products. Moreover, a transition from a shallow to deep heating structure associated with the MJO is clearly evident in a pressure-time plot over both the EEIO and WP in three reanalysis datasets. Although this vertical heating structure transition is detectable over the WP in two TRMM products, it is weakly defined in another dataset over the WP and in all three TRMM datasets over the EEIO.
The vertical structures of radiative heating Q(R) associated with the MJO are also analyzed based on TRMM and two reanalysis datasets. A westward vertical tilt in Q(R) is apparent in all these datasets: that is, the low-level Q(R) is largely in phase of convection, whereas Q(R) in the upper troposphere lags the maximum convection. The results also suggest a potentially important role of radiative heating for the MJO, particularly over the Indian Ocean. Caveats in heating estimates based on both the reanalysis datasets and TRMM are briefly discussed.
C1 [Jiang, Xianan; Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Jiang, Xianan] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Olson, William S.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Tao, Wei-Kuo; Lang, Stephen] NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
[L'Ecuyer, Tristan S.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Li, King-Fai; Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91109 USA.
[Shige, Shoichi] Kyoto Univ, Grad Sch Sci, Kyoto, Japan.
[Takayabu, Yukari N.] Univ Tokyo, Atmosphere & Ocean Res Inst, Tokyo, Japan.
RP Jiang, XN (reprint author), CALTECH, Jet Prop Lab, MS 183-501,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM xianan@jifresse.ucla.edu
RI Jiang, Xianan/A-2283-2012; L'Ecuyer, Tristan/E-5607-2012; L'Ecuyer,
Tristan/C-7040-2013; PMM, JAXA/K-8537-2016;
OI L'Ecuyer, Tristan/0000-0002-7584-4836; Li, King-Fai/0000-0003-0150-2910
FU NSF Climate and Large-Scale Dynamics [ATM-0934285]; NOAA
[NA09OAR4310191]; NASA
FX We thank anonymous reviewers for their constructive comments on an
earlier version of this manuscript. Thanks also to Terry Kubar for his
comments and editorial assistance. The first author (Xi) acknowledges
support by NSF Climate and Large-Scale Dynamics under Award ATM-0934285
and NOAA CPPA program under Award NA09OAR4310191. W. Olson and T.
L'Ecuyer acknowledge support by NASA NEWS program. The Wheeler-Hendon
MJO index was down-loaded from the Australian BMRC website. We also
thank Prof. B. Wang for insightful discussion. Part of this research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 73
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U1 0
U2 10
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 OCT
PY 2011
VL 139
IS 10
BP 3208
EP 3223
DI 10.1175/2011MWR3636.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 833AP
UT WOS:000295854300007
ER
PT J
AU Kwok, R
Untersteiner, N
AF Kwok, Ron
Untersteiner, Norbert
TI Flying over thin ice Reply
SO PHYSICS TODAY
LA English
DT Letter
C1 [Kwok, Ron] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Untersteiner, Norbert] Univ Washington, Seattle, WA 98195 USA.
RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM ronald.kwok@jpl.nasa.gov
RI Kwok, Ron/A-9762-2008
OI Kwok, Ron/0000-0003-4051-5896
NR 1
TC 0
Z9 0
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 0031-9228
J9 PHYS TODAY
JI Phys. Today
PD OCT
PY 2011
VL 64
IS 10
BP 10
EP 10
PG 1
WC Physics, Multidisciplinary
SC Physics
GA 833PS
UT WOS:000295898000005
ER
PT J
AU Giuranna, M
Roush, TL
Duxbury, T
Hogan, RC
Carli, C
Geminale, A
Formisano, V
AF Giuranna, M.
Roush, T. L.
Duxbury, T.
Hogan, R. C.
Carli, C.
Geminale, A.
Formisano, V.
TI Compositional interpretation of PFS/MEx and TES/MGS thermal infrared
spectra of Phobos
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Phobos; Composition; Mineralogy; Mars; Satellite
ID REFLECTANCE SPECTRA; MU-M; EMISSION SPECTROMETER; WAVELENGTH CHANNEL;
SILICATE MIXTURES; ASTEROID SURFACES; IGNEOUS ROCKS; SOLAR-SYSTEM;
MERCURY; MISSION
AB The origin of the Martian satellites presents a puzzle of long standing. Addressing the composition of Phobos will help constrain theories of its formation. Visible and near-infrared spectra of Phobos lack deep absorption features, making the compositional interpretation a tricky task. PFS/MEx and TES/MGS observations in the thermal infrared show several spectral features that can be used to investigate the composition of the surface. Our results show that the majority of the spectra are consistent with the presence of phyllosilicates, particularly in the area northeast of Stickney. This area corresponds to the "blue" region as defined by Murchie et al. (1999). Analysis of PFS and TES observations in the "red" region defined by Murchie et al. (1999) are consistent with tectosilicates, especially feldspars/feldspathoids. We discuss several physical and chemical mechanisms that can act to eliminate or reduce the strength of bands in the VIS/NIR spectra, with possibly little or no effect in the mid-IR. Comparison of the TES and PFS data to the meteorites shows that no class of chondritic meteorites provide significant agreement with the spectral features observed. The lack of consistency of the PFS and TES spectra to analogs of ultraprimitive materials (organic residues) suggests that an origin via capture of a transneptunian object is not supported by these observations, although it cannot be completely ruled out. Derived surface temperatures from PFS and TES data are in very good agreement with brightness temperatures derived from Viking orbiter measurements. Earth-based observations, and values predicted by numerical models. Our results show that the surface temperature of Phobos varies with solar incidence angle and heliocentric distance, reconciling the different results.
We collect and summarize the compositional clues for the origin of Phobos discussed in this paper, including our results. Currently, the most likely scenario is the in-situ formation of Phobos, although a capture of achrondrite-like meteorites is not ruled out. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Giuranna, M.; Geminale, A.] Ist Fis Spazio Interplanetario INAF IFSI, I-00133 Rome, Italy.
[Roush, T. L.; Formisano, V.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Duxbury, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hogan, R. C.] Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Carli, C.] Isituto Astrofis Spaziale & Fis Cosm INAF IASF, I-00133 Rome, Italy.
RP Giuranna, M (reprint author), Ist Fis Spazio Interplanetario INAF IFSI, Via Fosso del Cavaliere 100, I-00133 Rome, Italy.
EM marco.giuranna@ifsi-roma.inaf.it
OI GIURANNA, Marco/0000-0001-8967-9184; carli, cristian/0000-0002-4674-1029
FU Italian Space Agency (ASI); NASA
FX The PFS experiment has been built at the Istituto di Fisica dello Spazio
Interplanetario (IFSI) of Istituto Nazionale di Astrofisica (INAF), and
has been funded by the Italian Space Agency (ASI) in the context of the
Italian participation to the Mars Express mission of ESA. The
participation of TLR was enabled via support from NASA's Planetary
Geology and Geophysics Program. This manuscript was improved through the
constructive reviews, suggestions and comments of Dr. P. Vernazza and an
anonymous referee. The authors wish to thank Pascal Rosenblatt for
providing helpful discussions.
NR 90
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U1 0
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD OCT
PY 2011
VL 59
IS 13
BP 1308
EP 1325
DI 10.1016/j.pss.2011.01.019
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 833OI
UT WOS:000295894400003
ER
PT J
AU Weider, SZ
Swinyard, BM
Kellett, BJ
Howe, CJ
Joy, KH
Crawford, IA
Gow, J
Smith, DR
AF Weider, Shoshana Z.
Swinyard, Bruce M.
Kellett, Barry J.
Howe, Chris J.
Joy, Katherine H.
Crawford, Ian A.
Gow, Jason
Smith, David R.
TI Planetary X-ray fluorescence analogue laboratory experiments and an
elemental abundance algorithm for C1XS
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE X-ray fluorescence (XRF) spectroscopy; Planetary analogues; Moon,
Mercury, asteroids-surface; Regolith; Chandrayaan-1
ID SWEPT CHARGE DEVICE; REGOLITH BRECCIAS; LUNAR REGOLITH; SURFACE;
SPECTROMETER; CHANDRAYAAN-1; MOON; SPECTROSCOPY; INSTRUMENT; PARAMETERS
AB We have conducted laboratory experiments as an analogue to planetary XRF (X-ray fluorescence) missions in order to investigate the role of changing incidence (and phase) angle geometry and sample grain-size on the intensity of XRF from regolith-like samples. Our data provide evidence of a grain-size effect, where XRF line intensity decreases with increasing sample grain-size, as well as an almost ubiquitous increase in XRF line intensity above incidence angles of similar to 60 degrees. Data from a lunar regolith simulant are also used to test the accuracy of an XRF abundance algorithm developed at the Rutherford Appleton Laboratory (RAL), which is used to estimate the major element abundance of the lunar surface from Chandrayaan-1 X-ray Spectrometer (C1XS) XRF data. In ideal situations (i.e., when the input spectrum is well defined and the XRF spectrum has a sufficient signal to noise ratio) the algorithm can recover a known rock composition to within 1.0 elemental wt% (1 sigma). (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Weider, Shoshana Z.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Weider, Shoshana Z.; Joy, Katherine H.; Crawford, Ian A.] Birkbeck Coll, Dept Earth & Planetary Sci, London WC1E 7HX, England.
[Weider, Shoshana Z.; Joy, Katherine H.; Crawford, Ian A.] UCL Birkbeck, Ctr Planetary Sci, Dept Earth Sci, London WC1E 6BT, England.
[Weider, Shoshana Z.; Swinyard, Bruce M.; Kellett, Barry J.; Howe, Chris J.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England.
[Swinyard, Bruce M.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Joy, Katherine H.] USRA, Lunar & Planetary Inst, Ctr Lunar Sci & Explorat, Houston, TX 77058 USA.
[Joy, Katherine H.] NASA, Lunar Sci Inst, Washington, DC USA.
[Gow, Jason] Open Univ, PSSRI, Ctr Elect Imaging E2v, Milton Keynes MK7 6AA, Bucks, England.
[Smith, David R.] Brunel Univ, Sch Engn & Design, Ctr Sensors & Instrumentat, Uxbridge UB8 3PH, Middx, England.
RP Weider, SZ (reprint author), Carnegie Inst Washington, Dept Terr Magnetism, 5241 Broad Branch Rd, Washington, DC 20015 USA.
EM sweider@ciw.edu
RI Crawford, Ian/H-7510-2012;
OI Crawford, Ian/0000-0001-5661-7403; Gow, Jason/0000-0002-5208-7924;
Weider, Shoshana/0000-0003-1034-909X; Smith, David/0000-0003-3658-4506;
Joy, Katherine/0000-0003-4992-8750
FU UK Science and Technology Facilities Council (STFC); Leverhulme Trust
FX We acknowledge the useful comments of three anonymous reviewers, which
have significantly improved this paper. S.Z.W. thanks the UK Science and
Technology Facilities Council (STFC) for the award of a post-graduate
studentship. I.A.C and K.H.J. thank the Leverhulme Trust for financial
support. We thank Jim Davy for help acquiring the SEM images, James
Carpenter for help preparing the JSC-1A pressed pellet sample (material
donated by NASA), as well as Brian Maddison and Mattias Wallner for all
their help improving the RESIK laboratory setup at RAL. This is LPI
Contribution Number 1619.
NR 48
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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 OCT
PY 2011
VL 59
IS 13
BP 1393
EP 1407
DI 10.1016/j.pss.2011.05.005
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 833OI
UT WOS:000295894400007
ER
PT J
AU Flandes, A
Kruger, H
Hamilton, DP
Valdes-Galicia, JF
Spilker, L
Caballero, R
AF Flandes, Alberto
Krueger, Harald
Hamilton, Douglas P.
Francisco Valdes-Galicia, J.
Spilker, Linda
Caballero, Rogelio
TI Magnetic field modulated dust streams from Jupiter in interplanetary
space
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Interplanetary dust; Solar wind; Jupiter; Io
ID ULYSSES; MAGNETOSPHERE; IO; IDENTIFICATION; PARTICLES; EJECTION;
IMPACTS; MISSION; GRAINS; SATURN
AB High speed dust streams emanating from near Jupiter were first discovered by the Ulysses spacecraft in 1992. Since then the phenomenon has been re-observed by Galileo in 1995, Cassini in 2000, and Ulysses in 2004. The dust grains are expected to be charged to a potential of similar to 5 V. which is sufficient to allow the planet's magnetic field to accelerate them away from the planet, where they are subsequently influenced by the interplanetary Magnetic field (IMF). A similar phenomenon was observed near Saturn by Cassini. Here, we report and analyze simultaneous dust, IMF and solar wind data for all dust streams from the two Ulysses Jupiter flybys. We find that compression regions (CRs) in the IMF - regions of enhanced magnetic field - precede most dust streams. Furthermore, the duration of a dust stream is roughly comparable with that of the precedent CR, and the occurrence of a dust stream and the occurrence of the previous CR are separated by a time interval that depends on the distance to Jupiter. The intensity of the dust streams and their precedent CRs are also correlated, but this correlation is only evident at distances from the planet no greater than 2 AU. Combining these observations, we argue that CRs strongly affect dust streams, probably by deflecting dust grain trajectories, so that they can reach the spacecraft and be detected by its dust sensor. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Flandes, Alberto; Francisco Valdes-Galicia, J.; Caballero, Rogelio] Univ Nacl Autonoma Mexico, Ciencias Espaciales Inst Geofis, Mexico City 04510, DF, Mexico.
[Krueger, Harald] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Krueger, Harald] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Hamilton, Douglas P.] Univ Maryland, College Pk, MD 20742 USA.
[Spilker, Linda] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Flandes, A (reprint author), Univ Nacl Autonoma Mexico, Ciencias Espaciales Inst Geofis, Ciudad Univ, Mexico City 04510, DF, Mexico.
EM flandes@geofisica.unam.mx
OI Caballero, Rogelio/0000-0001-8954-1927
FU NASA; [DGAPA IN111207]
FX Part of this work was carried out at the Jet Propulsion Laboratory under
contract with NASA. Part of this work was also carried out at the
Max-Planck-Institut fur Sonnensystemforschung in Katlenburg-Lindau
during a research stay. The authors thank Reiner Schwenn for his support
in the CIRs and CMEs identification. A. Flandes thanks D. Maravilla and
her support through the project DGAPA IN111207. The authors thank A.
Craps and S. Kempf for thorough reviews.
NR 27
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U1 0
U2 2
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 OCT
PY 2011
VL 59
IS 13
BP 1455
EP 1471
DI 10.1016/j.pss.2011.05.014
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 833OI
UT WOS:000295894400012
ER
PT J
AU Du, AM
Sun, W
Tsurutani, BT
Boroyev, RN
Moiseyev, AV
AF Du, A. M.
Sun, W.
Tsurutani, B. T.
Boroyev, R. N.
Moiseyev, A. V.
TI Observations of dawn-dusk aligned polar cap aurora during the substorms
of January 21, 2005
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Substorm; Planetary shock; Polar cap Aurora; Reconnection
ID GEOMAGNETIC-ACTIVITY; IMAGE SPACECRAFT; DOUBLE OVAL; BOUNDARY; DYNAMICS;
ARCS; RECONNECTION; EVENTS; SHOCKS; FIELD
AB A new type of polar cap aurora, dawn-dusk aligned polar cap aurora (DDAPCA), was detected during the exceptionally intense January 21, 2005 substorm (AE(max)=3504 nT). The DDAPCA was located at very high latitude (> 85 degrees MLAT) in the polar cap region. As the interplanetary magnetic field (IMF) GSM By component rotated from a positive to a negative value, the DDAPCA tilt angle relative to the dawn-dusk direction rotated anticlockwise and reached similar to 45 degrees. It is speculated that the DDAPCA arises from the formation of an X-line in the distant (> 80R(E)) tail due to polar cap magnetic field reconnection under unusually high solar wind compression conditions. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Du, A. M.] Chinese Acad Sci, Inst Geol & Geophys, Beijing 100029, Peoples R China.
[Sun, W.] Univ Alaska, Inst Geophys, Fairbanks, AK 99775 USA.
[Tsurutani, B. T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Boroyev, R. N.; Moiseyev, A. V.] Yu G Shafer Inst Cosmophys Res & Aeron, Yakutsk, Russia.
RP Du, AM (reprint author), Chinese Acad Sci, Inst Geol & Geophys, Beijing 100029, Peoples R China.
EM amdu@mail.iggcas.ac.cn
FU NSFC [40890163, 41031066]; State Oceanic Administration People's
Republic of China [201005017]; RFBR [09-05-98546, 11-05-00908]; SB RAS
[69]
FX We especially thank S.B. Mende and Harald Frey for the use of IMAGE FUV
WIC data. The AE data are provided by the World Data Center for
Geomagnetism at Kyoto University. Portion of this research were
performed at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with NASA. This work was supported by NSFC
Grants (40890163, 41031066) and Ocean Public Welfare Scientific Research
Project, State Oceanic Administration People's Republic of China (No.
201005017). This work was partially supported by RFBR grant nos.
09-05-98546, 11-05-00908 and by SB RAS project no. 69.
NR 37
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U1 0
U2 7
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 OCT
PY 2011
VL 59
IS 13
BP 1551
EP 1558
DI 10.1016/j.pss.2011.06.021
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 833OI
UT WOS:000295894400022
ER
PT J
AU Stubbs, TJ
Glenar, DA
Farrell, WM
Vondrak, RR
Collier, MR
Halekas, JS
Delory, GT
AF Stubbs, T. J.
Glenar, D. A.
Farrell, W. M.
Vondrak, R. R.
Collier, M. R.
Halekas, J. S.
Delory, G. T.
TI On the role of dust in the lunar ionosphere
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Moon; Lunar ionosphere; Radio occultation; Dust-electrons; Luna 19;
Apollo 15; Horizon glow
ID ATMOSPHERE; SURFACES; SPACE
AB Radio occultation measurements from the Soviet Luna 19 mission suggest that electron concentrations above the sunlit lunar surface can be significantly higher than that expected from either the photoionization of exospheric neutrals or any other well-known process. These measurements were used to infer the electron column concentrations above the lunar limb as a function of tangent height, which surprisingly indicated peak concentrations of similar to 10(3) cm(-3) at similar to 5 km altitude. It has been speculated that electrically charged exospheric dust could contribute to such electron populations. This possibility is examined here using the exospheric dust abundances inferred from Apollo 15 coronal photographs to estimate the concentration of electrons produced by photo- and secondary emission from dust. These estimates far exceed the electron concentrations predicted by any other suggested mechanism, and are within a factor of approximate to 20 of those inferred from the Luna 19 measurements. It is possible that this discrepancy is due to an under-estimate in dust grain capacitances and/or the presence of much higher exospheric dust abundances during the Luna 19 measurements. These results suggest that electrons emitted from exospheric dust could be responsible for the Luna 19 measurements, and that this process could dominate the formation and evolution of the lunar ionosphere. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Stubbs, T. J.; Glenar, D. A.; Farrell, W. M.; Vondrak, R. R.; Collier, M. R.; Halekas, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stubbs, T. J.] Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21228 USA.
[Glenar, D. A.] New Mexico State Univ, Las Cruces, NM 88003 USA.
[Delory, G. T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Stubbs, T. J.; Glenar, D. A.; Farrell, W. M.; Vondrak, R. R.; Collier, M. R.; Halekas, J. S.; Delory, G. T.] NASA Ames Res Ctr, NASA Lunar Sci Inst, Moffett Field, CA USA.
RP Stubbs, TJ (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 695, Greenbelt, MD 20771 USA.
EM Timothy.J.Stubbs@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
FU NASA [NNX08AM76G, NNX07AG10G, NNX08BA32G, NNX09AG78A]
FX Research was funded by NASA Grants: NNX08AM76G, NNX07AG10G, NNX08BA32G,
and NNX09AG78A. We benefitted from access to NASA/OMNIWeb, as well as
from useful discussions with J.K. Burchill and helpful suggestions from
the reviewers.
NR 24
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Z9 22
U1 0
U2 11
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 OCT
PY 2011
VL 59
IS 13
BP 1659
EP 1664
DI 10.1016/j.pss.2011.05.011
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 833OI
UT WOS:000295894400030
ER
PT J
AU Raga, AC
Noriega-Crespo, A
Rodriguez-Ramirez, JC
Lora, V
Stapelfeldt, KR
Carey, SJ
AF Raga, A. C.
Noriega-Crespo, A.
Rodriguez-Ramirez, J. C.
Lora, V.
Stapelfeldt, K. R.
Carey, S. J.
TI AN INTEPRETIVE BALLISTIC MODEL FOR QUASI-SYMMETRIC BIPOLAR JET SYSTEMS
SO REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA
LA English
DT Article
DE Herbig-Haro objects; infrared: ISM; ISM: individual objects (HH 34, HR
111); ISM: jets and outflows; stars: formation
ID HUBBLE-SPACE-TELESCOPE; PROPER MOTIONS; ORION-NEBULA; OUTFLOW;
EXCITATION; SIGNATURES; EMISSION; VELOCITY; COMPLEX; ORIGIN
AB We present an analytic, ballistic model for quasi-symmetric jet/counterjet systems, considering both the non-relativistic and the relativistic cases. The model considers the presence of ejection time and velocity asymmetries, which produce offsets between the positions of the knots in jet/counterjet pairs. A fit of the non-relativistic model predictions to observations of two quasi-symmetric HH outflows (HH 34 and HH 111) allows us to obtain the magnitudes of the ejection time and velocity asymmetries of these systems.
C1 [Raga, A. C.; Rodriguez-Ramirez, J. C.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico.
[Noriega-Crespo, A.; Carey, S. J.] CALTECH, SPITZER Sci Ctr, Pasadena, CA 91125 USA.
[Lora, V.] Univ Heidelberg, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany.
[Stapelfeldt, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Raga, AC (reprint author), Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Apdo Postal 70-543, Mexico City 04510, DF, Mexico.
EM raga@nucleares.unam.mx; alberto@ipac.caltech.edu;
juan.rodriguez@nucleares.unam.mx; vlora@ari.uni-heidelberg.de;
krs@exoplanet.jpl.nasa.gov; carey@ipac.caltech.edu
RI Stapelfeldt, Karl/D-2721-2012
FU Conacyt [61547, 101356, 101975]
FX This work was supported by the Conacyt grants 61547, 101356 and 101975.
NR 31
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U1 0
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 OCT
PY 2011
VL 47
IS 2
BP 289
EP 295
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 830NM
UT WOS:000295663700008
ER
PT J
AU Cook, BI
Puma, MJ
Krakauer, NY
AF Cook, Benjamin I.
Puma, Michael J.
Krakauer, Nir Y.
TI Irrigation induced surface cooling in the context of modern and
increased greenhouse gas forcing
SO CLIMATE DYNAMICS
LA English
DT Article
ID LAND-COVER CHANGE; GISS MODELE; HIGH-PLAINS; CLIMATE; PRECIPITATION;
SIMULATIONS; TEMPERATURE; SATELLITE; HYDROLOGY; REGIONS
AB There is evidence that expected warming trends from increased greenhouse gas (GHG) forcing have been locally 'masked' by irrigation induced cooling, and it is uncertain how the magnitude of this irrigation masking effect will change in the future. Using an irrigation dataset integrated into a global general circulation model, we investigate the equilibrium magnitude of irrigation induced cooling under modern (Year 2000) and increased (A1B Scenario, Year 2050) GHG forcing, using modern irrigation rates in both scenarios. For the modern scenario, the cooling is largest over North America, India, the Middle East, and East Asia. Under increased GHG forcing, this cooling effect largely disappears over North America, remains relatively unchanged over India, and intensifies over parts of China and the Middle East. For North America, irrigation significantly increases precipitation under modern GHG forcing; this precipitation enhancement largely disappears under A1B forcing, reducing total latent heat fluxes and the overall irrigation cooling effect. Over India, irrigation rates are high enough to keep pace with increased evaporative demand from the increased GHG forcing and the magnitude of the cooling is maintained. Over China, GHG forcing reduces precipitation and shifts the region to a drier evaporative regime, leading to a relatively increased impact of additional water from irrigation on the surface energy balance. Irrigation enhances precipitation in the Middle East under increased GHG forcing, increasing total latent heat fluxes and enhancing the irrigation cooling effect. Ultimately, the extent to which irrigation will continue to compensate for the warming from increased GHG forcing will primarily depend on changes in the background evaporative regime, secondary irrigation effects (e.g. clouds, precipitation), and the ability of societies to maintain (or increase) current irrigation rates.
C1 [Cook, Benjamin I.; Puma, Michael J.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Krakauer, Nir Y.] CUNY City Coll, New York, NY 10031 USA.
RP Cook, BI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM bc9z@ldeo.columbia.edu
RI Cook, Benjamin/H-2265-2012;
OI Puma, Michael/0000-0002-4255-8454
FU National Oceanic and Atmospheric Administration (NOAA) [NA06OAR4810162];
NASA [NNX08AJ75A]
FX The authors wish to thank the anonymous reviewers who greatly improved
the quality of this manuscript. NY Krakauer acknowledges the support of
the National Oceanic and Atmospheric Administration (NOAA), under Grant
Number NA06OAR4810162. MJ Puma gratefully acknowledges funding for
Interdisciplinary Global Change Research under NASA Cooperative
Agreement NNX08AJ75A supported by the NASA Climate and Earth Observing
Program. Lamont contribution number #7407.
NR 40
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U1 3
U2 20
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD OCT
PY 2011
VL 37
IS 7-8
BP 1587
EP 1600
DI 10.1007/s00382-010-0932-x
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 828SI
UT WOS:000295522600019
ER
PT J
AU Lutz, R
AF Lutz, Robyn
TI Software Engineering for Space Exploration
SO COMPUTER
LA English
DT Article
AB Software engineering offers tools and techniques that improve the odds spacecraft will survive long missions, contributing to their resilience to new environmental challenges and to their adaptability to updated mission requirements.
C1 [Lutz, Robyn] Iowa State Univ, Ames, IA 50011 USA.
[Lutz, Robyn] CALTECH, Jet Prop Lab, Software Syst Engn Grp, Pasadena, CA 91125 USA.
RP Lutz, R (reprint author), Iowa State Univ, Ames, IA 50011 USA.
EM rlutz@iastate.edu
FU National Science Foundation [0916275]; American Recovery and
Reinvestment Act of 2009
FX Thanks to Margaret Smith, Martin Feather, and Scott Morgan for
additional examples. This work was supported in part by National Science
Foundation grant 0916275 with funds from the American Recovery and
Reinvestment Act of 2009.
NR 11
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Z9 0
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 0018-9162
J9 COMPUTER
JI Computer
PD OCT
PY 2011
VL 44
IS 10
BP 40
EP 45
PG 6
WC Computer Science, Hardware & Architecture; Computer Science, Software
Engineering
SC Computer Science
GA 829VL
UT WOS:000295612700012
ER
PT J
AU Rappold, AG
Stone, SL
Cascio, WE
Neas, LM
Kilaru, VJ
Carraway, MS
Szykman, JJ
Ising, A
Cleve, WE
Meredith, JT
Vaughan-Batten, H
Deyneka, L
Devlin, RB
AF Rappold, Ana G.
Stone, Susan L.
Cascio, Wayne E.
Neas, Lucas M.
Kilaru, Vasu J.
Carraway, Martha Sue
Szykman, James J.
Ising, Amy
Cleve, William E.
Meredith, John T.
Vaughan-Batten, Heather
Deyneka, Lana
Devlin, Robert B.
TI Peat Bog Wildfire Smoke Exposure in Rural North Carolina Is Associated
with Cardiopulmonary Emergency Department Visits Assessed through
Syndromic Surveillance
SO ENVIRONMENTAL HEALTH PERSPECTIVES
LA English
DT Article
DE cardiopulmonary health effects; satellite data; syndromic surveillance;
wildfire smoke exposure
ID PARTICULATE AIR-POLLUTION; SOUTHERN CALIFORNIA WILDFIRES;
CONGESTIVE-HEART-FAILURE; FOREST-FIRES; HOSPITAL ADMISSIONS;
UNITED-STATES; ROOM VISITS; URBAN AREA; QUALITY; MORTALITY
AB BACKGROUND: In June 2008, burning peat deposits produced haze and air pollution far in excess of National Ambient Air Quality Standards, encroaching on rural communities of eastern North Carolina. Although the association of mortality and morbidity with exposure to urban air pollution is well established, the health effects associated with exposure to wildfire emissions are less well understood.
OBJECTIVE: We investigated the effects of exposure on cardiorespiratory outcomes in the population affected by the fire.
METHODS: We performed a population-based study using emergency department (ED) visits reported through the syndromic surveillance program NC DETECT (North Carolina Disease Event Tracking and Epidemiologic Collection Tool). We used aerosol optical depth measured by a satellite to determine a high-exposure window and distinguish counties most impacted by the dense smoke plume from surrounding referent counties. Poisson log-linear regression with a 5-day distributed lag was used to estimate changes in the cumulative relative risk (RR).
RESULTS: In the exposed counties, significant increases in cumulative RR for asthma [1.65 (95% confidence interval, 1.25-2.1)], chronic obstructive pulmonary disease [1.73 (1.06-2.83)], and pneumonia and acute bronchitis [1.59 (1.07-2.34)] were observed. ED visits associated with cardiopulmonary symptoms [1.23 (1.06-1.43)] and heart failure [1.37 (1.01-1.85)] were also significantly increased.
CONCLUSIONS: Satellite data and syndromic surveillance were combined to assess the health impacts of wildfire smoke in rural counties with sparse air-quality monitoring. This is the first study to demonstrate both respiratory and cardiac effects after brief exposure to peat wildfire smoke.
C1 [Rappold, Ana G.; Stone, Susan L.; Cascio, Wayne E.; Neas, Lucas M.; Carraway, Martha Sue; Devlin, Robert B.] US EPA, Environm Publ Hlth Div, Natl Hlth & Environm Effects Res Lab, Res Triangle Pk, NC 27711 USA.
[Kilaru, Vasu J.] US EPA, Natl Exposure Res Lab, Res Triangle Pk, NC 27711 USA.
[Szykman, James J.] US EPA, Environm Sci Div, Natl Exposure Res Lab, NASA Langley Res Ctr, Hampton, VA USA.
[Ising, Amy] Univ N Carolina, Sch Med, Dept Emergency Med, Chapel Hill, NC USA.
[Cleve, William E.] Pitt Cty Mem Hosp, Greenville, NC USA.
[Meredith, John T.] E Carolina Univ, Brody Sch Med, Dept Cardiovasc Sci, Greenville, NC USA.
[Meredith, John T.] E Carolina Heart Inst, Greenville, NC USA.
[Vaughan-Batten, Heather; Deyneka, Lana] N Carolina Dept Hlth & Human Serv, N Carolina Div Publ Hlth, Raleigh, NC USA.
[Rappold, Ana G.; Stone, Susan L.; Cascio, Wayne E.; Neas, Lucas M.; Carraway, Martha Sue; Devlin, Robert B.] US EPA, Environm Publ Hlth Div, Natl Hlth & Environm Effects Res Lab, Res Triangle Pk, NC 27711 USA.
RP Rappold, AG (reprint author), US EPA, Environm Publ Hlth Div, Natl Hlth & Environm Effects Res Lab, MD 58B,109 TW Alexander Dr, Res Triangle Pk, NC 27711 USA.
EM rappold.ana@epa.gov
RI Neas, Lucas/J-9378-2012; Xiongfei, Zhao/G-7690-2015
FU U.S. Environmental Protection Agency (EPA)
FX This work was supported by internal funding by the U.S. Environmental
Protection Agency (EPA).
NR 39
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U1 3
U2 44
PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE
PI RES TRIANGLE PK
PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233,
RES TRIANGLE PK, NC 27709-2233 USA
SN 0091-6765
EI 1552-9924
J9 ENVIRON HEALTH PERSP
JI Environ. Health Perspect.
PD OCT
PY 2011
VL 119
IS 10
BP 1415
EP 1420
DI 10.1289/ehp.1003206
PG 6
WC Environmental Sciences; Public, Environmental & Occupational Health;
Toxicology
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Toxicology
GA 827CA
UT WOS:000295402400026
PM 21705297
ER
PT J
AU Han, SC
Mazarico, E
Rowlands, D
Lemoine, F
Goossens, S
AF Han, Shin-Chan
Mazarico, Erwan
Rowlands, David
Lemoine, Frank
Goossens, Sander
TI New analysis of Lunar Prospector radio tracking data brings the nearside
gravity field of the Moon with an unprecedented resolution
SO ICARUS
LA English
DT Article
DE Radio observations; Celestial mechanics; Geophysics; Moon, Surface
AB A new analysis of the Doppler tracking data from the Lunar Prospector mission in 1999 revealed a number of previously-unseen gravity anomalies at spatial scales as small as 27 km over the nearside. The tracking data at low altitudes (50 km or below) were better analyzed to resolve the nearside features without dampening from a power law constraint, by partitioning the gravity parameters concentrated on either the nearside or farside. The resulting model presents gravity anomalies correlated with topography with a correlation coefficient of 0.7 or higher from degree 50 to 150, the widest bandwidth yet. The gravity-topography admittance of similar to 70 mGal/km is found from numerous craters of which diameters are 60 km or less. In addition, the new model produces orbits that fit to independent radio tracking data from the Lunar Reconnaissance Orbiter and Kaguya (SELENE) better than previous gravity models. This high-resolution model can be of immediate use to geophysical analysis of small craters. Our technique could be applied to an upcoming mission, the Gravity Recovery And Interior Laboratory and useful to extract short wavelength signals from the MESSENGER Doppler data. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Han, Shin-Chan; Mazarico, Erwan; Rowlands, David; Lemoine, Frank] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Han, Shin-Chan] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Catonsville, MD 21228 USA.
[Goossens, Sander] Natl Inst Nat Sci, Natl Astron Observ Japan, RISE Project, Oshu City, Iwate 0230861, Japan.
RP Han, SC (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698, Greenbelt, MD 20771 USA.
EM shin-chan.han@nasa.gov
RI Rowlands, David/D-2751-2012; Lemoine, Frank/D-1215-2013; Han,
Shin-Chan/A-2022-2009; Mazarico, Erwan/N-6034-2014; Goossens,
Sander/K-2526-2015
OI Mazarico, Erwan/0000-0003-3456-427X; Goossens,
Sander/0000-0002-7707-1128
FU NASA; GRACE
FX This work was supported by NASA's programs in Lunar Advanced Science and
Exploration Research, Mars Data Analysis, and GRACE projects. We
acknowledge NASA GSFC's LRO project. We thank Noriyuki Namiki and the
RISE Project team for the use of the Kaguya extended mission data and
two anonymous reviewers for constructive comments. LPE200 model
coefficients and formal errors are available from the journal as
supplementary data and from PDS Geosciences Node. The full covariance
matrix of the gravity solution (similar to 7 GB) is available by
contacting the corresponding author.
NR 13
TC 16
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 OCT
PY 2011
VL 215
IS 2
BP 455
EP 459
DI 10.1016/j.icarus.2011.07.020
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 827MK
UT WOS:000295432400001
ER
PT J
AU Schinder, PJ
Flasar, FM
Marouf, EA
French, RG
McGhee, CA
Kliore, AJ
Rappaport, NJ
Barbinis, E
Fleischman, D
Anabtawi, A
AF Schinder, Paul J.
Flasar, F. Michael
Marouf, Essam A.
French, Richard G.
McGhee, Colleen A.
Kliore, Arvydas J.
Rappaport, Nicole J.
Barbinis, Elias
Fleischman, Don
Anabtawi, Aseel
TI The structure of Titan's atmosphere from Cassini radio occultations
SO ICARUS
LA English
DT Article
DE Titan; Atmospheres, Structure
ID COMPOSITE INFRARED SPECTROMETER; PLANETARY ATMOSPHERES; VENUS;
TEMPERATURES; DYNAMICS; SYSTEM; REFRACTIVITY; ABSORPTION; VOYAGER-2;
PROFILES
AB We present results from the two radio occultations of the Cassini spacecraft by Titan in 2006, which probed mid-southern latitudes. Three of the ingress and egress soundings occurred within a narrow latitude range, 31-34 degrees S near the surface, and the fourth at 52.8 degrees S. Temperature-altitude profiles for all four occultation soundings are presented, and compared with the results of the Voyager 1 radio occultation (Lindal, C.F., Wood, G.E., Hotz, I-LB., Sweetnam, ON., Eshleman, V.R., Tyler, G.L. [1983]. Icarus 53, 348-363). the HASI instrument on the Huygens descent probe (Fulchignoni, M. et al. [2005]. Nature 438, 785-791), and Cassini CIRS results (Flasar. F.M. et al. [2005]. Science 308, 975-978; Achterberg, R.K., Conrath, B.J., Gierasch, P.J., Flasar, F.M., Nixon, CA. [2008b]. Icarus 194, 263-277). Sources of error in the retrieved temperature-altitude profiles are also discussed, and a major contribution is from spacecraft velocity errors in the reconstructed ephemeris. These can be reduced by using CIRS data at 300 km to make along-track adjustments of the spacecraft timing. The occultation soundings indicate that the temperatures just above the surface at 31-34 degrees S are about 93K, while that at 53 degrees S is about 1 K colder. At the tropopause, the temperatures at the lower latitudes are all about 70 K, while the 53 degrees S profile is again 1 K colder. The temperature lapse rate in the lowest 2 km for the two ingress (dawn) profiles at 31 and 33 degrees S lie along a dry adiabat except within similar to 200 m of the surface, where a small stable inversion occurs. This could be explained by turbulent mixing with low viscosity near the surface. The egress profile near 34 degrees S shows a more complex structure in the lowest 2 km, while the egress profile at 53 S is more stable. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Schinder, Paul J.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Flasar, F. Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
[Marouf, Essam A.] San Jose State Univ, Dept Elect Engn, San Jose, CA 95193 USA.
[French, Richard G.; McGhee, Colleen A.] Wellesley Coll, Dept Astron, Wellesley, MA 02481 USA.
[Kliore, Arvydas J.; Rappaport, Nicole J.; Barbinis, Elias; Fleischman, Don; Anabtawi, Aseel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Schinder, PJ (reprint author), Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
EM schinder@astro.cornell.edu; f.m.flasar@nasa.gov; emarouf@email.sjsu.edu;
rfrench@wellesley.edu; cmcghee@firstclass.wellesley.edu;
akliore@jpl.nasa.gov; Nicole.J.Rappaport@jpl.nasa.gov;
elias.barbinis@jpl.nasa.gov; don.u.fleischman@jpl.nasa.gov;
Aseel.Anabtawi@jpl.nasa.gov
RI Flasar, F Michael/C-8509-2012;
OI Schinder, Paul/0000-0002-4571-7895
NR 47
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U1 0
U2 7
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD OCT
PY 2011
VL 215
IS 2
BP 460
EP 474
DI 10.1016/j.icarus.2011.07.030
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 827MK
UT WOS:000295432400002
ER
PT J
AU Sonnett, S
Kleyna, J
Jedicke, R
Masiero, J
AF Sonnett, Sarah
Kleyna, Jan
Jedicke, Robert
Masiero, Joseph
TI Limits on the size and orbit distribution of main belt comets
SO ICARUS
LA English
DT Article
DE Asteroids; Astrobiology; Comets
ID TELESCOPE LEGACY SURVEY; ASTEROID P/2010 A2; DIGITAL SKY SURVEY; SNOW
LINE; THERMAL EVOLUTION; WATER; 133P/ELST-PIZARRO; POPULATION; SEARCH;
ORIGIN
AB The first of a new class of objects now known as main belt comets (MBCs) or "activated asteroids" was identified in 1996. The seven known members of this class have orbital characteristics of main belt asteroids yet exhibit dust ejection like comets. In order to constrain their physical and orbital properties we searched the Thousand Asteroid Light Curve Survey (TALCS; Masiero, JR., Jedicke, R., Durech, J., Gwyn, S., Denneau, L, Larsen, J. [2009]. Icarus 204, 145-171) for additional candidates using two diagnostics: tail and coma detection. This was the most sensitive MBC survey effort to date, extending the search from MBCs with H similar to 18 (D similar to 1 km) to MBCs as small as H similar to 21 (D similar to 150 m).
We fit each of the 924 objects detected by TALCS to a PSF model incorporating both a coma and nuclear component to measure the fractional contribution of the coma to the total surface brightness. We determined the significance of the coma detection using the same algorithm on a sample of null detections of comparable magnitude and rate of motion. We did not identify any MBC candidates with this technique to a sensitivity limit on the order of cometary mass loss rate of about 0.1 kg/s.
Our tail detection algorithm relied on identifying statistically significant flux in a segmented annulus around the candidate object. We show that the technique can detect tail activity throughout the asteroid belt to the level of the currently known MBCs. Although we did not identify any MBC candidates with this technique, we find a statistically significant detection of faint activity in the entire ensemble of TALCS asteroids. This suggests that many main belt asteroids are active at very low levels.
Our null detection of MBCs allows us to set 90% upper confidence limits on the number distribution of MBCs as a function of absolute magnitude, semi-major axis, eccentricity, and inclination. There are less than or similar to 400,000 MBCs in the main belt brighter than H-V = 21 (similar to 150-m in diameter) and the MBC:MBA ratio is less than or similar to 1:400.
We further comment on the ability of observations to meaningfully constrain the snow line's location. Under some reasonable and simple assumptions we claim 85% confidence that the contemporary snow line lies beyond 2.5 AU. Published by Elsevier Inc.
C1 [Sonnett, Sarah; Kleyna, Jan; Jedicke, Robert] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Masiero, Joseph] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sonnett, S (reprint author), Univ Hawaii Manoa, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
EM sonnett@ifa.hawaii.edu
OI Masiero, Joseph/0000-0003-2638-720X
FU NASA [NNG06GI46G]; NSF [1011059]; NASA through the NASA Astrobiology
Institute [NNA09DA77A]
FX This work was made possible with NASA PAST Grant NNG06GI46G and NSF
Grant 1011059, and was based on observations obtained with
MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the
Canada-France-Hawaii Telescope (CFHT) which is operated by the National
Research Council (NRC) of Canada, the Institut National des Science de
l'Univers of the Centre National de la Recherche Scientifique (CNRS) of
France, and the University of Hawaii. This work was partly supported by
NASA through the NASA Astrobiology Institute under Cooperative Agreement
NNA09DA77A issued through the Office of Space Science. We thank the
people of Hawaii for use of their sacred space atop Mauna Kea.
NR 54
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD OCT
PY 2011
VL 215
IS 2
BP 534
EP 546
DI 10.1016/j.icarus.2011.08.001
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 827MK
UT WOS:000295432400010
ER
PT J
AU Shepard, MK
Harris, AW
Taylor, PA
Clark, BE
Ockert-Bell, M
Nolan, MC
Howell, ES
Magri, C
Giorgini, JD
Benner, LAM
AF Shepard, Michael K.
Harris, Alan W.
Taylor, Patrick A.
Clark, Beth Ellen
Ockert-Bell, Maureen
Nolan, Michael C.
Howell, Ellen S.
Magri, Christopher
Giorgini, Jon D.
Benner, Lance A. M.
TI Radar observations of Asteroids 64 Angelina and 69 Hesperia
SO ICARUS
LA English
DT Article
DE Asteroids; Asteroids, Composition; Radar observations
ID POLARIZATION; 64-ANGELINA; METEORITE; 44-NYSA; BODIES; SHAPE
AB We report new radar observations of E-class Asteroid 64 Angelina and M-class Asteroid 69 Hesperia obtained with the Arecibo Observatory S-band radar (2480 MHz, 12.6 cm). Our measurements of Angelina's radar bandwidth are consistent with reported diameters and poles. We find Angelina's circular polarization ratio to be 0.8 +/- 0.1, tied with 434 Hungaria for the highest value observed for main-belt asteroids and consistent with the high values observed for all E-class asteroids (Benner, LAM., Ostro, S.J., Magri, C., Nolan, MC., Howell, ES., Giorgini, J.D., Jurgens, R.F., Margot, J.L Taylor, P.A., Busch, MW., Shepard, M.K. [2008]. Icarus 198, 294-304; Shepard, MM., Kressler, KM., Clark, B.E., Ockert-Bell, ME., Nolan, MC., Howell, E.S., Magri, C., Giorgini, J.D., Benner, L.A.M., Ostro, S.J. [200813]. Icarus 195, 220-225). Our radar observations of 69 Hesperia, combined with lightcurve-based shape models, lead to a diameter estimate, D(eff) = 110 +/- 15 km, approximately 20% smaller than the reported IRAS value. We estimate Hesperia to have a radar albedo of (sigma) over cap (OC) 0.45 +/- 0.12, consistent with a high-metal content. We therefore add 69 Hesperia to the Mm-class (high metal M) (Shepard, M.K., Clark, BE., Ockert-Bell, M., Nolan, M.C., Howell, ES., Magri, C., Giorgini, J.D., Benner, LAM., Ostro, S.J., Harris, A.W., Warner, B.D., Stephens, R.D., Mueller, M. [2010]. Icarus 208, 221-237), bringing the total number of Mm-class objects to eight; this is 40% of all M-class asteroids observed by radar to date. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Shepard, Michael K.] Bloomsburg Univ, Bloomsburg, PA 17815 USA.
[Harris, Alan W.] Space Sci Inst, La Canada Flintridge, CA 91011 USA.
[Taylor, Patrick A.; Nolan, Michael C.; Howell, Ellen S.] NAIC Arecibo Observ, Arecibo, PR 00612 USA.
[Clark, Beth Ellen; Ockert-Bell, Maureen] Ithaca Coll, Ithaca, NY 14853 USA.
[Magri, Christopher] Univ Maine, Farmington, ME 04938 USA.
[Giorgini, Jon D.; Benner, Lance A. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Shepard, MK (reprint author), Bloomsburg Univ, 400 E 2nd St, Bloomsburg, PA 17815 USA.
EM mshepard@bloomu.edu
RI Nolan, Michael/H-4980-2012
OI Nolan, Michael/0000-0001-8316-0680
FU NSF [AST 0908098, 0908217]; National Science Foundation; National
Aeronautics and Space Administration (NASA) under the Science Mission
Directorate Research
FX MKS and BEC gratefully acknowledge funding from NSF AST 0908098 and
0908217. The Arecibo Observatory is part of the National Astronomy and
Ionosphere Center, which is operated by Cornell University under a
cooperative agreement with the National Science Foundation. We thank the
technical staff at the observatory for help with observations. Some of
this work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration. This material is based in part upon work
supported by the National Aeronautics and Space Administration (NASA)
under the Science Mission Directorate Research and Analysis Programs.
NR 40
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PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD OCT
PY 2011
VL 215
IS 2
BP 547
EP 551
DI 10.1016/j.icarus.2011.07.027
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 827MK
UT WOS:000295432400011
ER
PT J
AU Strycker, PD
Chanover, NJ
Simon-Miller, AA
Banfield, D
Gierasch, PJ
AF Strycker, Paul D.
Chanover, Nancy J.
Simon-Miller, Amy A.
Banfield, Don
Gierasch, Peter J.
TI Jovian chromophore characteristics from multispectral HST images
SO ICARUS
LA English
DT Article
DE Jupiter; Jupiter, Atmosphere; Atmospheres, Composition; Atmospheres,
Structure
ID JUPITERS CLOUD STRUCTURE; GALILEO PROBE; ATMOSPHERE; COLOR;
SPECTROPHOTOMETRY; AEROSOLS; RED
AB The chromophores responsible for coloring the jovian atmosphere are embedded within Jupiter's vertical aerosol structure. Sunlight propagates through this vertical distribution of aerosol particles, whose colors are defined by pi(0)(gimel)(2), and we remotely observe the culmination of the radiative transfer as I/F(gimel). In this study, we employed a radiative transfer code to retrieve pi(0)(gimel) for particles in Jupiter's tropospheric haze at seven wavelengths in the near-UV and visible regimes. The data consisted of images of the 2008 passage of Oval BA to the south of the Great Red Spot obtained by the Wide Field Planetary Camera 2 on-board the Hubble Space Telescope. We present derived particle colors for locations that were selected from 14 weather regions, which spanned a large range of observed colors. All pi(0)(gimel) curves were absorbing in the blue, and pi(0)(gimel) increased monotonically to approximately unity as wavelength increased. We found accurate fits to all pi(0)(gimel) curves using an empirically derived functional form: pi(0)(gimel) = 1 A exp(-B gimel).). The best-fit parameters for the mean pi(0)(gimel) curve were A= 25.4 and B = 0.0149 for gimel in units of nm. We performed a principal component analysis (PCA) on our pi(0)(gimel) results and found that one or two independent chromophores were sufficient to produce the variations in moo).). A PCA of I/F(gimel) for the same jovian locations resulted in principal components (PCs) with roughly the same variances as the pi(0)(gimel) PCA, but they did not result in a one-to-one mapping of PC amplitudes between the pi(0)(gimel) PCA and I/F(gimel) PCA. We suggest that statistical analyses performed on I/F(.) image cubes have limited applicability to the characterization of chromophores in the jovian atmosphere due to the sensitivity of If F(gimel) to horizontal variations in the vertical aerosol distribution. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Strycker, Paul D.; Chanover, Nancy J.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Simon-Miller, Amy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Banfield, Don; Gierasch, Peter J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
RP Strycker, PD (reprint author), Univ Wisconsin, Dept Chem & Engn Phys, 1 Univ Plaza, Platteville, WI 53818 USA.
EM stryckerp@uwplatt.edu
RI Simon, Amy/C-8020-2012;
OI Simon, Amy/0000-0003-4641-6186; Banfield, Don/0000-0003-2664-0164
FU NASA [NNX08AF53A, NAS 5-26555]
FX The authors would like to thank two anonymous reviewers for constructive
feedback, which greatly enhanced this work. We also wish to acknowledge
Michael Roman for contributions to the radiative transfer code. This
work was supported by NASA's Planetary Atmospheres Program through Grant
Number NNX08AF53A. This work is based on observations made with the
NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy. Inc., under NASA Contract NAS 5-26555. These
observations are associated with program #GO/DD11498.
NR 37
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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 OCT
PY 2011
VL 215
IS 2
BP 552
EP 583
DI 10.1016/j.icarus.2011.08.004
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 827MK
UT WOS:000295432400012
ER
PT J
AU Castillo-Rogez, JC
AF Castillo-Rogez, Julie C.
TI Ceres - Neither a porous nor salty ball
SO ICARUS
LA English
DT Article
DE Asteroids; Geophysics; Cosmochemistry
ID THERMAL-CONDUCTIVITY; 2 PALLAS; ASTEROIDS; SHAPE; ICE; DIFFERENTIATION;
SURFACE
AB This study explores the geophysical implications of two compositional models recently proposed for Ceres, which assume that the dwarf planet is a homogeneous mixture of chondritic material devoid with free water. In order to reproduce Ceres' density, the rock density has to be offset by the presence of porosity and/or an abundance of hydrated salts resulting from the extensive hydration and oxidation of the chondritic material. Thermal modeling shows that a mixture of hydrated minerals is bound to compact and partly dehydrate as a consequence of long-lived radioisotope decay heat. The resulting interior structure is differentiated in a silicate-rich core and water-rich shell, with little porosity. Hence, this study confirms previous suggestion that Ceres contains a large fraction of free water. (C) 2011 Elsevier Inc. All rights reserved.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Castillo-Rogez, JC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Julie.C.Castillo@jpl.nasa.gov
FU National Aeronautics and Space Administration; California Institute of
Technology. Government
FX This research was conducted at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. Copyright 2011 California Institute of
Technology. Government sponsorship acknowledged. The author appreciated
very much the thorough reviews sent by Jeff Kargel and an anonymous
referee who helped improve this manuscript. The author is also grateful
to Dennis Matson for reviewing this manuscript prior to submission. She
acknowledges discussions with M. Zolotov during a 2010 Workshop hosted
at the Bear Fight Center by T. McCord. This work has made use of NASA's
Astrophysics Data System.
NR 37
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PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD OCT
PY 2011
VL 215
IS 2
BP 599
EP 602
DI 10.1016/j.icarus.2011.08.007
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 827MK
UT WOS:000295432400015
ER
PT J
AU Anderson, RB
Morris, RV
Clegg, SM
Bell, JF
Wiens, RC
Humphries, SD
Mertzman, SA
Graff, TG
McInroy, R
AF Anderson, Ryan B.
Morris, Richard V.
Clegg, Samuel M.
Bell, James F., III
Wiens, Roger C.
Humphries, Seth D.
Mertzman, Stanley A.
Graff, Trevor G.
McInroy, Rhonda
TI The influence of multivariate analysis methods and target grain size on
the accuracy of remote quantitative chemical analysis of rocks using
laser induced breakdown spectroscopy
SO ICARUS
LA English
DT Article
DE Mars; Spectroscopy; Data reduction techniques; Mars, Surface;
Experimental techniques
ID ARTIFICIAL NEURAL-NETWORKS; GENETIC ALGORITHM; FEATURE-SELECTION;
OPTIMIZATION; CALIBRATION; MARS; PLS
AB Laser-induced breakdown spectroscopy (LIBS) was used to quantitatively analyze 195 rock slab samples with known bulk chemical compositions, 90 pressed-powder samples derived from a subset of those rocks, and 31 pressed-powder geostandards under conditions that simulate the ChemCam instrument on the Mars Science Laboratory Rover (MSL), Curiosity. The low-volatile (<2 wt.%) silicate samples (90 rock slabs, corresponding powders, and 22 geostandards) were split into training, validation, and test sets. The LIBS spectra and chemical compositions of the training set were used with three multivariate methods to predict the chemical compositions of the test set. The methods were partial least squares (PLS), multilayer perceptron artificial neural networks (MLP ANNs) and cascade correlation (CC) ANNs. Both the full LIBS spectrum and the intensity at five pre-selected spectral channels per major element (feature selection) were used as input data for the multivariate calculations. The training spectra were supplied to the algorithms without averaging (i.e. five spectra per target) and with averaging (i.e. all spectra from the same target averaged and treated as one spectrum). In most cases neural networks did not perform better than PLS for our samples. PLS2 without spectral averaging outperformed all other procedures on the basis of lowest quadrature root mean squared error (RMSE) for both the full test set and the igneous rocks test set. The RMSE for PLS2 using the igneous rock slab test set is: 3.07 wt.% SiO2, 0.87 wt.% TiO2, 2.36 wt.% Al2O3, 2.20 wt.% Fe2O3, 0.08 wt.% MnO, 1.74 wt.% MgO, 1.14 wt.% CaO, 0.85 wt.% Na2O, 0.81 wt.% K2O. PLS1 with feature selection and averaging had a higher quadrature RMSE than PLS2, but merits further investigation as a method of reducing data volume and computation time and potentially improving prediction accuracy, particularly for samples that differ significantly from the training set. Precision and accuracy were influenced by the ratio of laser beam diameter (similar to 490 mu m) to grain size, with coarse-grained rocks often resulting in lower accuracy and precision than analyses of fine-grained rocks and powders. The number of analysis spots that were normally required to produce a chemical analysis within one standard deviation of the true bulk composition ranged from 10 for fine-grained rocks to >20 for some coarse-grained rocks. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Anderson, Ryan B.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Morris, Richard V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Clegg, Samuel M.; Wiens, Roger C.; Humphries, Seth D.; McInroy, Rhonda] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Bell, James F., III] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Mertzman, Stanley A.] Franklin & Marshall Coll, Dept Earth & Environm, Lancaster, PA 17604 USA.
[Graff, Trevor G.] ESCG, Houston, TX 77058 USA.
RP Anderson, RB (reprint author), Cornell Univ, Dept Astron, 406 Space Sci Bldg, Ithaca, NY 14853 USA.
EM randerson@astro.cornell.edu; richard.v.morris@nasa.gov; sclegg@lanl.gov;
Jim.Bell@asu.edu; nwiens@lanl.gov; sethdh@lanl.gov;
stan.mertzman@fandm.edu; trevor.g.graff@nasa.gov; rhondam@lanl.gov
OI Clegg, Sam/0000-0002-0338-0948
FU NASA; Mars Program Office through MSL; NASA Johnson Space Center
FX This work was supported by the NASA Graduate Student Researchers
Program, by the Mars Program Office through MSL, and by the NASA Johnson
Space Center. We thank Suniti Karunatil-lake for helpful discussions of
statistical significance testing and Roger Jarvis for assistance with
the PYCHEM software.
NR 51
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD OCT
PY 2011
VL 215
IS 2
BP 608
EP 627
DI 10.1016/j.icarus.2011.07.034
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 827MK
UT WOS:000295432400017
ER
PT J
AU Wolkenberg, P
Smith, MD
Formisano, V
Sindoni, G
AF Wolkenberg, Paulina
Smith, Michael D.
Formisano, Vittorio
Sindoni, Giuseppe
TI Comparison of PFS and TES observations of temperature and water vapor in
the martian atmosphere
SO ICARUS
LA English
DT Article
DE Atmospheres Structure; Mars, Atmosphere
ID THERMAL EMISSION SPECTROMETER; PLANETARY FOURIER SPECTROMETER; MARS
GLOBAL SURVEYOR; WAVELENGTH CHANNEL; EXPRESS MISSION; SURFACE; AEROSOL;
DUST; CALIBRATION; ENVIRONMENT
AB The interval from L(s) = 330 degrees in Mars Year (MY) 26 until L(s) = 84 degrees in MY 27 has been used to compare and validate measurements from the Mars Global Surveyor Thermal Emission Spectrometer (TES) and the Mars Express Planetary Fourier Spectrometer (PFS). We studied differences between atmospheric temperatures observed by the two instruments. The best agreement between atmospheric temperatures was found at 50 Pa between 40 degrees S and 40 degrees N latitude, where differences were within +/- 5 K. For other atmospheric levels, differences as large as similar to 25 K were observed between the two instruments at some locations. The largest temperature differences occurred mainly over the Hellas Planitia, Argyre Planitia, Tharsis and Valles Marineris regions.
On this basis we report on the variability of the martian atmosphere during the 5.5 martian years of Mars climatology obtained by combining the two data sets from TES and PFS. Atmospheric temperatures at 50 Pa responded to the global-scale dust storms of MY 25 and in MY 28 raising temperatures from similar to 220 K to similar to 250 K during the daytime. An atmospheric temperature of similar to 140 K at 50 Pa was observed poleward of 70 degrees N during northern winter and poleward of 60 degrees S during southern winter each year in both the PFS and TES results. Water vapor observed by the two spectrometers showed consistent seasonal and latitudinal variations. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Wolkenberg, Paulina] NASA, CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Smith, Michael D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Formisano, Vittorio; Sindoni, Giuseppe] INAF, IFSI, I-00133 Rome, Italy.
RP Wolkenberg, P (reprint author), NASA, CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM pwolkenberg@gmail.com
RI Smith, Michael/C-8875-2012
FU National Aeronautics and Space Administration
FX We thank Daniel J. McCleese for many helpful prompts and discussions
about the analysis presented in this manuscript. We are also grateful to
James H. Shirley for discussion. The research described in this paper
was carried out at the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with the National Aeronautics and Space
Administration.
NR 35
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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 OCT
PY 2011
VL 215
IS 2
BP 628
EP 638
DI 10.1016/j.icarus.2011.07.032
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 827MK
UT WOS:000295432400018
ER
PT J
AU Vahidinia, S
Cuzzi, JN
Hedman, M
Draine, B
Clark, RN
Roush, T
Filacchione, G
Nicholson, PD
Brown, RH
Buratti, B
Sotin, C
AF Vahidinia, Sanaz
Cuzzi, Jeffrey N.
Hedman, Matt
Draine, Bruce
Clark, Roger N.
Roush, Ted
Filacchione, Gianrico
Nicholson, Philip D.
Brown, Robert H.
Buratti, Bonnie
Sotin, Christophe
TI Saturn's F ring grains: Aggregates made of crystalline water ice
SO ICARUS
LA English
DT Article
DE Planetary rings; Saturn, Rings; Ices, IR spectroscopy; Radiative
transfer
ID OPTICAL-CONSTANTS; CASSINI-VIMS; MU-M; PARTICLE SIZES; SCATTERING;
OCCULTATION; ABSORPTION; SPECTRA; VOYAGER-2; MOONLETS
AB We present models of the near-infrared (1-5 mu m) spectra of Saturn's F ring obtained by Cassini's Visual and Infrared Mapping Spectrometer (VIMS) at ultra-high phase angles (177.4-178.5 degrees). Modeling this spectrum constrains the size distribution, composition, and structure of F ring particles in the 0.1-100 mu m size range. These spectra are very different from those obtained at lower phase angles; they lack the familiar 1.5 and 2 mu n absorption bands, and the expected 3 mu m water ice primary absorption appears as an unusually narrow dip at 2.87 mu m. We have modeled these data using multiple approaches. First, we use a simple Mie scattering model to constrain the size distribution and composition of the particles. The Mie model allows us to understand the overall shapes of the spectra in terms of dominance by diffraction at these ultra-high phase angles, and also to demonstrate that the 2.87 mu m dip is associated with the Christiansen frequency of water ice (where the real refractive index passes unity). Second, we use a combination of Mie scattering with Effective Medium Theory to probe the effect of porous (but structureless) particles on the overall shape of the spectrum and depth of the 2.87 mu m band. Such simple models are not able to capture the shape of this absorption feature well. Finally, we model each particle as an aggregate of discrete monomers, using the Discrete Dipole Approximation (DDA) model, and find a better fit for the depth of the 2.87 mu m feature. The DDA models imply a slightly different overall size distribution. We present a simple heuristic model which explains the differences between the Mie and DDA model results. We conclude that the F ring contains aggregate particles with a size distribution that is distinctly narrower than a typical power law, and that the particles are predominantly crystalline water ice. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Vahidinia, Sanaz; Cuzzi, Jeffrey N.; Hedman, Matt; Draine, Bruce; Clark, Roger N.; Roush, Ted; Filacchione, Gianrico; Nicholson, Philip D.; Brown, Robert H.; Buratti, Bonnie; Sotin, Christophe] NASA, Ames Res Ctr, Post Doctoral Program, Div Space Sci, Nasa Moffett Field, CA 94035 USA.
RP Vahidinia, S (reprint author), NASA, Ames Res Ctr, Post Doctoral Program, Div Space Sci, Mail Stop 245-3, Nasa Moffett Field, CA 94035 USA.
EM svahidinia@yahoo.com
OI Filacchione, Gianrico/0000-0001-9567-0055; Draine,
Bruce/0000-0002-0846-936X
FU Cassini project; NASA
FX We are very grateful to Kathy Rages for providing her Mie scattering
code and for assistance fixing problems it developed with the unusual
set of refractive indices we were using. We have profited greatly from
generous allocations of cpu time on the NASA High-End Computing (HEC)
machines at Ames. In addition to raw cycles, expert consultants have
provided invaluable help in parallelization and optimization. We'd like
to thank Terry Nelson, Piyush Mehrotra, and especially Art Lazanoff for
help getting the optimizing done, Denis Richard for his help testing the
code, Rachel Mastrapa for providing data in advance of publication and
several helpful conversations, observation designers on the VIMS team,
Essam Marouf and Frank Bridges for insightful conversations. The
research was partially supported by the Cassini project and partially by
a grant to JNC from NASA's Planetary Geology and Geophysics program.
NR 51
TC 8
Z9 8
U1 0
U2 1
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD OCT
PY 2011
VL 215
IS 2
BP 682
EP 694
DI 10.1016/j.icarus.2011.04.011
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 827MK
UT WOS:000295432400022
ER
PT J
AU Hedman, MM
Nicholson, PD
Showalter, MR
Brown, RH
Buratti, BJ
Clark, RN
Baines, K
Sotin, C
AF Hedman, M. M.
Nicholson, P. D.
Showalter, M. R.
Brown, R. H.
Buratti, B. J.
Clark, R. N.
Baines, K.
Sotin, C.
TI The Christiansen Effect in Saturn's narrow dusty rings and the spectral
identification of clumps in the F ring
SO ICARUS
LA English
DT Article
DE Planetary rings; Saturn, Rings; Spectroscopy
ID STELLAR OCCULTATION; PARTICLE SIZES; MOONLETS; VIMS
AB Stellar occultations by Saturn's rings observed with the Visual and Infrared Mapping Spectrometer (VIMS) onboard the Cassini spacecraft reveal that dusty features such as the F ring and the ringlets in the Encke and the Laplace Gaps have distinctive infrared transmission spectra. These spectra show a narrow optical depth minimum at wavelengths around 2.87 mu m. This minimum is likely due to the Christiansen Effect, a reduction in the extinction of small particles when their (complex) refractive index is close to that of the surrounding medium. Simple Mie-scattering models demonstrate that the strength of this opacity dip is sensitive to the size distribution of particles between 1 and 100 mu m across. Furthermore, the spatial resolution of the occultation data is sufficient to reveal variations in the transmission spectra within and among these rings. In both the Encke Gap ringlets and F ring, the opacity dip weakens with increasing local optical depth, which is consistent with the larger particles being concentrated near the cores of these rings. The Encke Gap ringlets also show systematically weaker opacity dips than the F ring and Laplace Gap ringlet, implying that the former has a smaller fraction of grains less than similar to 30 mu m across. However, the strength of the opacity dip varies most dramatically within the F ring; certain compact regions of enhanced optical depth lack an opacity dip and therefore appear to have a greatly reduced fraction of grains in the few-micron size range. Such spectrally-identifiable structures probably represent a subset of the compact optically-thick clumps observed by other Cassini instruments. These variations in the ring's particle size distribution can provide new insights into the processes of grain aggregation, disruption and transport within dusty rings. For example, the unusual spectral properties of the F-ring clumps could perhaps be ascribed to small grains adhering onto the surface of larger particles in regions of anomalously low velocity dispersion. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Hedman, M. M.; Nicholson, P. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Showalter, M. R.] SETI Inst, Mountain View, CA 94043 USA.
[Brown, R. H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Buratti, B. J.; Baines, K.; Sotin, C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Clark, R. N.] US Geol Survey, Fed Ctr, Denver, CO 80225 USA.
RP Hedman, MM (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
EM mmhedman@astro.cornell.edu
FU Cassini Data Analysis Program [NNX09AE74G]
FX We wish to acknowledge NASA, the Cassini project and the VIMS team for
providing the data that made this analysis possible. We also thank H.
Throop and J.N. Cuzzi for their detailed and insightful reviews of this
manuscript, and L. Esposito and C. Murray for the useful discussions.
This work was supported in part by a Cassini Data Analysis Program Grant
NNX09AE74G.
NR 31
TC 15
Z9 15
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 OCT
PY 2011
VL 215
IS 2
BP 695
EP 711
DI 10.1016/j.icarus.2011.02.025
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 827MK
UT WOS:000295432400023
ER
PT J
AU Lee, S
von Allmen, P
Kamp, L
Gulkis, S
Davidsson, B
AF Lee, Seungwon
von Allmen, Paul
Kamp, Lucas
Gulkis, Samuel
Davidsson, Bjorn
TI Non-LTE radiative transfer for sub-millimeter water lines in Comet
67P/Churyumov-Gerasimenko
SO ICARUS
LA English
DT Article
DE Comets, Coma; Comets, Composition; Spectroscopy
ID RADIO TELESCOPES; VAPOR; EXCITATION; FLUORESCENCE; TEMPERATURES;
INSTRUMENT; MODEL; ODIN
AB The European Space Agency (ESA) Rosetta spacecraft (Schulz, R., Alexander, C., Boehnhardt, H., Glassmeier, K.H. (Eds.) [2009]. "ROSETTA - ESA") will encounter Comet 67P/Churyumov-Gerasimenko in 2014 and spend the next 18 months in the vicinity of the comet, permitting very high spatial and spectral resolution observations of the coma and nucleus. During this time, the heliocentric distance of the comet will change from similar to 3.5 AU to similar to 1.3 AU, accompanied by an increasing temperature of the nucleus and the development of the coma. The Microwave Instrument for the Rosetta Orbiter (MIRO) will observe the ground-state rotational transition (1(10)-1(01)) of H(2) (16)O at 556.936 GHz, the two isotopologues H(2)(17)O and H(2) (18)O and other molecular transitions in the coma during this time (Gulkis, S. et al., [2007]. MIRO: Microwave Instrument for Rosetta Orbiter. Space Sci. Rev, 128, 561-597). The aim of this study is to simulate the water line spectra that could be obtained with the MIRO instrument and to understand how the observed line spectra with various viewing geometries can be used to study the physical conditions of the coma and the water excitation processes throughout the coma. We applied an accelerated Monte Carlo method to compute the excitations of the seven lowest rotational levels (1(01), 1(10), 2(12), 2(21), 3(03), 3(12), and 3(21)) of ortho-water using a comet model with spherically symmetric water outgassing, density, temperature and expansion velocity at three different heliocentric distances 1.3 AU, 2.5 AU, and 3.5 AU. Mechanisms for the water excitation include water-water collisions, water-electron collisions, and infrared pumping by solar radiation. Synthetic line spectra are calculated at various observational locations and directions using the MIRO instrument parameters. We show that observations at varying viewing distances from the nucleus and directions have the potential to give diagnostic information on the continuum temperature and water outgassing rates at the surface of the nucleus, and the gas density, expansion velocity, and temperature of the coma as a function of distance from the nucleus. The gas expansion velocity and temperature affect the spectral line width and frequency shift of the line from the rest frequency, while the gas density (which is directly related to the outgassing rate) and the line excitation temperature determine the antenna temperature of the absorption and emission signal in the line profile. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Lee, Seungwon; von Allmen, Paul; Kamp, Lucas; Gulkis, Samuel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Davidsson, Bjorn] Uppsala Univ, Dept Phys & Astron, SE-75120 Uppsala, Sweden.
RP Lee, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Seungwon.Lee@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This research was carried out at the Jet Propulsion Laboratory (JPL),
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. This work was funded by the
NASA-Rosetta project. We thank the reviewers of this paper for their
constructive comments, which helped us clarify and improve the
interpretation of some of the results.
NR 29
TC 8
Z9 8
U1 0
U2 1
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD OCT
PY 2011
VL 215
IS 2
BP 721
EP 731
DI 10.1016/j.icarus.2011.07.007
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 827MK
UT WOS:000295432400025
ER
PT J
AU Soldani, D
Sajal
Hassan, M
Hassan, JA
Mandyam, GD
AF Soldani, David
Das, Sajal K.
Hassan, Mahbub
Hassan, Jahan A.
Mandyam, Giridhar D.
TI TRAFFIC MANAGEMENT FOR MOBILE BROADBAND NETWORKS
SO IEEE COMMUNICATIONS MAGAZINE
LA English
DT Editorial Material
C1 [Soldani, David] Nokia Siemens Networks NSN, Customer Networks & Solut, Munich, Germany.
[Soldani, David] Nokia Siemens Networks NSN, Solut & Serv Innovat funct, Munich, Germany.
[Soldani, David] Nokia Siemens Networks NSN, Res Technol & Platforms RTP, Munich, Germany.
[Soldani, David] Italian Mil Navy, Livorno, Italy.
[Soldani, David] European Network Solut R&D Huawei, Munich, Germany.
[Das, Sajal K.] Univ Texas Arlington, Ctr Res Wireless Mobil & Networking CReWMaN, Arlington, TX USA.
[Hassan, Mahbub; Hassan, Jahan A.] Univ New S Wales, Sch Comp Sci & Engn, Sydney, NSW 2052, Australia.
[Hassan, Mahbub] Univ Nantes, F-44035 Nantes, France.
[Hassan, Mahbub] IEEE ICON Wireless Workshop, Sydney, NSW, Australia.
[Hassan, Jahan A.] Univ Sydney, Sch Informat Technol, Sydney, NSW 2006, Australia.
[Mandyam, Giridhar D.] Qualcomm Internet Serv, San Diego, CA USA.
[Mandyam, Giridhar D.] NASA, UNM, Washington, DC USA.
RP Soldani, D (reprint author), European Res Ctr, Munich, Germany.
EM david.soldani@huawei.com; mahbub@cse.unsw.edu.au; jahan@cse.unw.edu.au
NR 0
TC 1
Z9 1
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0163-6804
J9 IEEE COMMUN MAG
JI IEEE Commun. Mag.
PD OCT
PY 2011
VL 49
IS 10
BP 98
EP 100
PG 3
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA 831LA
UT WOS:000295731000009
ER
PT J
AU Seo, M
Urteaga, M
Hacker, J
Young, A
Griffith, Z
Jain, V
Pierson, R
Rowell, P
Skalare, A
Peralta, A
Lin, R
Pukala, D
Rodwell, M
AF Seo, Munkyo
Urteaga, Miguel
Hacker, Jonathan
Young, Adam
Griffith, Zach
Jain, Vibhor
Pierson, Richard
Rowell, Petra
Skalare, Anders
Peralta, Alejandro
Lin, Robert
Pukala, David
Rodwell, Mark
TI InP HBT IC Technology for Terahertz Frequencies: Fundamental Oscillators
Up to 0.57 THz
SO IEEE JOURNAL OF SOLID-STATE CIRCUITS
LA English
DT Article; Proceedings Paper
CT 2010 IEEE Compound Semiconductor Integrated Circuit Symposium (CSICS)
CY OCT 03-06, 2010
CL Monterey, CA
SP IEEE
DE InP HBT; millimeter-wave oscillators; MMIC oscillators; terahertz;
TMICs; voltage-controlled oscillators
ID GHZ
AB We report on the development of a 0.25-mu m InP HBT IC technology for lower end of the THz frequency band (0.3-3 THz). Transistors demonstrate an extrapolated f(max) of > 800 GHz while maintaining a common-emitter breakdown voltage (BVCEO) > 4 V. The transistors have been integrated in a full IC process that includes three-levels of interconnects, and backside processing. The technology has been utilized for key circuit building blocks (amplifiers, oscillators, frequency dividers, PLL, etc), all operating at >= 300 GHz.
Next, we report a series of fundamental oscillators operating up to 0.57 THz fabricated in a 0.25-mu m InP HBT technology. Oscillator designs are based on a differential series-tuned topology followed by a common-base buffer, in a fixed-frequency or varactor-tuned scheme. For >= 400 GHz designs, a subharmonic down-conversion mixer is integrated to facilitate spectrum measurement. At optimum bias, the measured output power was -6.2, -5.6, and -19.2 dBm, for 310.2-, 412.9-, and 573.1-GHz designs, respectively, with P-DC <= 115 mW. Varactor-tuned designs demonstrated 10.6-12.3 GHz of tuning bandwidth up to 300 GHz.
C1 [Seo, Munkyo; Urteaga, Miguel; Hacker, Jonathan; Young, Adam; Griffith, Zach; Pierson, Richard; Rowell, Petra] Teledyne Sci Co, Thousand Oaks, CA 91360 USA.
[Jain, Vibhor; Rodwell, Mark] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA.
[Skalare, Anders; Peralta, Alejandro; Lin, Robert; Pukala, David] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Seo, M (reprint author), Teledyne Sci Co, Thousand Oaks, CA 91360 USA.
EM mkseo@ieee.org
FU Defense Advanced Research Projects Agency [HR0011-09-060]; Teledyne
Scientific Imaging
FX Manuscript received March 14, 2011; revised June 07, 2011; accepted June
13, 2011. Date of publication September 06, 2011; date of current
version September 30, 2011. This work was supported by the Defense
Advanced Research Projects Agency under the THz Electronics Program
under Contract HR0011-09-060. Program support provided by Dr. A. Hung
(Program Manager, Army Research Lab) and Dr. J. Albrecht (Program
Manger, DARPA). Part of this work was carried out by the Jet Propulsion
Laboratory, California Institute of Technology, as part of a DARPA
study, under subcontract from Teledyne Scientific & Imaging. The views,
opinions and/or findings contained in this article are those of the
authors and should not be interpreted as representing the official
policies, either expressed or implied, of the Defense Advanced Research
Projects Agency, or the Department of Defense. This paper was presented
in part at the 2010 IEEE Compound Semiconductor Integrated Circuit
Symposium and the 2010 IEEE MTT-S International Microwave Symposium.
This paper was approved by Guest Editor Gabriel Rebeiz.
NR 30
TC 57
Z9 60
U1 0
U2 9
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9200
EI 1558-173X
J9 IEEE J SOLID-ST CIRC
JI IEEE J. Solid-State Circuit
PD OCT
PY 2011
VL 46
IS 10
BP 2203
EP 2214
DI 10.1109/JSSC.2011.2163213
PG 12
WC Engineering, Electrical & Electronic
SC Engineering
GA 828OC
UT WOS:000295510500003
ER
PT J
AU Rumsey, CL
Nishino, T
AF Rumsey, Christopher L.
Nishino, Takafumi
TI Numerical study comparing RANS and LES approaches on a circulation
control airfoil
SO INTERNATIONAL JOURNAL OF HEAT AND FLUID FLOW
LA English
DT Article
DE Flow control; Circulation control; Turbulence
ID TURBULENCE MODELS; ONE-EQUATION; FLOWS
AB A numerical study over a nominally two-dimensional circulation control airfoil is performed using a large-eddy simulation code and two Reynolds-averaged Navier-Stokes codes. Different Coanda jet blowing conditions are investigated. In addition to investigating the influence of grid density, a comparison is made between incompressible and compressible flow solvers. The incompressible equations are found to yield negligible differences from the compressible equations up to at least a jet exit Mach number of 0.64. The effects of different turbulence models are also studied. Models that do not account for streamline curvature effects tend to predict jet separation from the Coanda surface too late, and can produce non-physical solutions at high blowing rates. Three different turbulence models that account for streamline curvature are compared with each other and with large eddy simulation solutions. All three models are found to predict the Coanda jet separation location reasonably well, but one of the models predicts specific flow field details near the Coanda surface prior to separation much better than the other two. All Reynolds-averaged Navier-Stokes computations produce higher circulation than large eddy simulation computations, with different stagnation point location and greater flow acceleration around the nose onto the upper surface. The precise reasons for the higher circulation are not clear, although it is not solely a function of predicting the jet separation location correctly. Published by Elsevier Inc.
C1 [Rumsey, Christopher L.] NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
[Nishino, Takafumi] NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA.
RP Rumsey, CL (reprint author), NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
EM c.l.rumsey@nasa.gov
RI Nishino, Takafumi/A-2685-2012
OI Nishino, Takafumi/0000-0001-6306-7702
FU Subsonic Fixed Wing Project of the Fundamental Aerodynamics Program
FX The first author would like to thank Ms. Shelly Jiang, who served as an
intern at NASA Langley during summer 2009 and helped to implement and
test the SSTRC model. The second author would like to thank Dr.
Seonghyeon Hahn of Stanford University for providing the LES code. This
work was funded by the Subsonic Fixed Wing Project of the Fundamental
Aerodynamics Program.
NR 34
TC 8
Z9 9
U1 2
U2 13
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0142-727X
J9 INT J HEAT FLUID FL
JI Int. J. Heat Fluid Flow
PD OCT
PY 2011
VL 32
IS 5
BP 847
EP 864
DI 10.1016/j.ijheatfluidflow.2011.06.011
PG 18
WC Thermodynamics; Engineering, Mechanical; Mechanics
SC Thermodynamics; Engineering; Mechanics
GA 829HM
UT WOS:000295569200001
ER
PT J
AU Fairen, AG
Davila, AF
Gago-Duport, L
Haqq-Misra, JD
Gil, C
McKay, CP
Kasting, JF
AF Fairen, Alberto G.
Davila, Alfonso F.
Gago-Duport, Luis
Haqq-Misra, Jacob D.
Gil, Carolina
McKay, Christopher P.
Kasting, James F.
TI Cold glacial oceans would have inhibited phyllosilicate sedimentation on
early Mars
SO NATURE GEOSCIENCE
LA English
DT Article
ID CARBONATE; IDENTIFICATION; OUTCROPS; FJORDS; ROCKS
AB Phyllosilicate minerals are commonly found in marine sediments on Earth(1,2). Accordingly, the presence of an ocean in the northern lowlands of Mars during the Noachian period would be expected to lead to the presence of abundant phyllosilicates in crust of the same age. However, mineralogical data from orbiting spectrometers show that phyllosilicates are rare in the Noachian-aged crust that is exposed in impact craters in the northern lowlands(3). In contrast, phyllosilicate minerals are abundant in the equatorial and tropical highlands(4,5), raising doubts about the presence of an ocean. Here we use climatic and geochemical model calculations and palaeohydrological reconstructions to assess the factors that control phyllosilicate synthesis and sedimentation on early Mars. Our model results show that temperatures in an ocean confined to latitudes poleward of 30 degrees N would have been near freezing, which would have hindered the formation of phyllosilicate minerals in the ocean basin. In addition, the presence of cold-based glaciers surrounding the ocean would have limited the delivery of phyllosilicates from the highlands to the ocean basin. We therefore suggest that the presence of a cold, Noachian ocean could explain the paucity of phyllosilicates in the Noachian-aged crust of the northern lowlands.
C1 [Fairen, Alberto G.; Davila, Alfonso F.] SETI Inst, Mountain View, CA 94043 USA.
[Fairen, Alberto G.; Davila, Alfonso F.; McKay, Christopher P.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Gago-Duport, Luis; Gil, Carolina] Univ Vigo, Dept Geociencias Marinas, Vigo 36200, Spain.
[Haqq-Misra, Jacob D.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Kasting, James F.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
RP Fairen, AG (reprint author), SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
EM alberto.g.fairen@nasa.gov
RI Davila, Alfonso/A-2198-2013; Gil Lozano, Carolina/L-5687-2015;
OI Davila, Alfonso/0000-0002-0977-9909; Gil Lozano,
Carolina/0000-0003-3500-2850; Haqq-Misra, Jacob/0000-0003-4346-2611
NR 30
TC 11
Z9 12
U1 0
U2 3
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 OCT
PY 2011
VL 4
IS 10
BP 667
EP 670
DI 10.1038/NGEO1243
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 827CN
UT WOS:000295403900010
ER
PT J
AU Jelliffe, R
Neely, M
Schumitzky, A
Bayard, D
Van Guilder, M
Botnen, A
Bustad, A
Laing, D
Yamada, W
Bartroff, J
Tatarinova, T
AF Jelliffe, Roger
Neely, Michael
Schumitzky, Alan
Bayard, David
Van Guilder, Michael
Botnen, Andreas
Bustad, Aida
Laing, Derek
Yamada, Walter
Bartroff, Jay
Tatarinova, Tatiana
TI Nonparametric population modeling and Bayesian analysis
SO PHARMACOLOGICAL RESEARCH
LA English
DT Letter
C1 [Jelliffe, Roger; Neely, Michael; Van Guilder, Michael; Botnen, Andreas; Bustad, Aida; Laing, Derek; Yamada, Walter] Univ So Calif, Keck Sch Med, Lab Appl Pharmacokinet, Los Angeles, CA 90033 USA.
[Bayard, David] Jet Prop Labs, Pasadena, CA USA.
[Tatarinova, Tatiana] Univ Glamorgan, Div Math & Stat, Pontypridd CF37 1DL, M Glam, Wales.
RP Jelliffe, R (reprint author), Univ So Calif, Keck Sch Med, Lab Appl Pharmacokinet, Los Angeles, CA 90033 USA.
EM JELLIFFE@USC.EDU
RI Tatarinova, Tatiana/K-3445-2016
OI Tatarinova, Tatiana/0000-0003-1787-1112
NR 3
TC 3
Z9 3
U1 0
U2 7
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 1043-6618
J9 PHARMACOL RES
JI Pharmacol. Res.
PD OCT
PY 2011
VL 64
IS 4
BP 426
EP 426
DI 10.1016/j.phrs.2011.04.008
PG 1
WC Pharmacology & Pharmacy
SC Pharmacology & Pharmacy
GA 831YO
UT WOS:000295767200024
PM 21699981
ER
PT J
AU Lewis, WS
Antiochos, SK
Drake, JF
AF Lewis, W. S.
Antiochos, S. K.
Drake, J. F.
TI Magnetic Reconnection: Theoretical and Observational Perspectives
Preface
SO SPACE SCIENCE REVIEWS
LA English
DT Editorial Material
C1 [Lewis, W. S.] SW Res Inst, San Antonio, TX USA.
[Antiochos, S. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Drake, J. F.] Univ Maryland, College Pk, MD 20742 USA.
RP Lewis, WS (reprint author), SW Res Inst, San Antonio, TX USA.
EM wlewis@swri.edu
RI Antiochos, Spiro/D-4668-2012
OI Antiochos, Spiro/0000-0003-0176-4312
NR 0
TC 0
Z9 0
U1 1
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 OCT
PY 2011
VL 160
IS 1-4
BP 1
EP 2
DI 10.1007/s11214-011-9822-8
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 831NO
UT WOS:000295738600001
ER
PT J
AU Hesse, M
Neukirch, T
Schindler, K
Kuznetsova, M
Zenitani, S
AF Hesse, Michael
Neukirch, Thomas
Schindler, Karl
Kuznetsova, Masha
Zenitani, Seiji
TI The Diffusion Region in Collisionless Magnetic Reconnection
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Magnetic reconnection; Numerical simulations; Solar physics;
Magnetospheric physics
ID 3-DIMENSIONAL PARTICLE SIMULATIONS; THIN CURRENT SHEETS; HYBRID
SIMULATIONS; EARTHS MAGNETOPAUSE; MAGNETOTAIL RECONNECTION; ELECTRON
ACCELERATION; KINK INSTABILITY; FIELD; PLASMA; DISSIPATION
AB A review of present understanding of the dissipation region in magnetic reconnection is presented. The review focuses on results of the thermal inertia-based dissipation mechanism but alternative mechanisms are mentioned as well. For the former process, a combination of analytical theory and numerical modeling is presented. Furthermore, a new relation between the electric field expressions for anti-parallel and guide field reconnection is developed.
C1 [Hesse, Michael; Kuznetsova, Masha; Zenitani, Seiji] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Neukirch, Thomas] Univ St Andrews, St Andrews, Fife, Scotland.
[Schindler, Karl] Ruhr Univ Bochum, Bochum, Germany.
RP Hesse, M (reprint author), NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM michael.hesse@nasa.gov
RI Hesse, Michael/D-2031-2012; Kuznetsova, Maria/F-6840-2012; Zenitani,
Seiji/D-7988-2013; NASA MMS, Science Team/J-5393-2013
OI Zenitani, Seiji/0000-0002-0945-1815; NASA MMS, Science
Team/0000-0002-9504-5214
FU NASA's MMS/SMART mission
FX This research was supported by NASA's MMS/SMART mission.
NR 73
TC 42
Z9 43
U1 3
U2 12
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD OCT
PY 2011
VL 160
IS 1-4
BP 3
EP 23
DI 10.1007/s11214-010-9740-1
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 831NO
UT WOS:000295738600002
ER
PT J
AU Moore, RL
Sterling, AC
Gary, GA
Cirtain, JW
Falconer, DA
AF Moore, Ronald L.
Sterling, Alphonse C.
Gary, G. Allen
Cirtain, Jonathan W.
Falconer, David A.
TI Observed Aspects of Reconnection in Solar Eruptions
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Sun: flares; Sun: coronal mass ejections (CMEs); Sun: magnetic
reconnection; Sun: magnetic topology
ID CORONAL MASS EJECTIONS; INTERNAL RECONNECTION; MODEL; JETS; FLARES;
EVOLUTION; TELESCOPE
AB The observed magnetic field configuration and signatures of reconnection in the large solar magnetic eruptions that make major flares and coronal mass ejections and in the much smaller magnetic eruptions that make X-ray jets are illustrated with cartoons and representative observed eruptions. The main reconnection signatures considered are the imaged bright emission from the heated plasma on reconnected field lines. In any of these eruptions, large or small, the magnetic field that drives the eruption and/or that drives the buildup to the eruption is initially a closed bipolar arcade. From the form and configuration of the magnetic field in and around the driving arcade and from the development of the reconnection signatures in coordination with the eruption, we infer that (1) at the onset of reconnection the reconnection current sheet is small compared to the driving arcade, and (2) the current sheet can grow to the size of the driving arcade only after reconnection starts and the unleashed erupting field dynamically forces the current sheet to grow much larger, building it up faster than the reconnection can tear it down. We conjecture that the fundamental reason the quasi-static pre-eruption field is prohibited from having a large current sheet is that the magnetic pressure is much greater than the plasma pressure in the chromosphere and low corona in eruptive solar magnetic fields.
C1 [Moore, Ronald L.; Sterling, Alphonse C.; Gary, G. Allen; Cirtain, Jonathan W.; Falconer, David A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Moore, RL (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM ron.moore@nasa.gov
FU NASA's Science Mission Directorate; Solar and Heliospheric Physics
Supporting Research and Technology Program; Hinode Project; Living With
a Star Targeted Research and Technology Program
FX This work was funded by NASA's Science Mission Directorate through the
Heliophysics Guest Investigators Program, the Solar and Heliospheric
Physics Supporting Research and Technology Program, the Hinode Project,
and the Living With a Star Targeted Research and Technology Program.
NR 40
TC 8
Z9 8
U1 1
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 OCT
PY 2011
VL 160
IS 1-4
BP 73
EP 94
DI 10.1007/s11214-011-9758-z
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 831NO
UT WOS:000295738600005
ER
PT J
AU Matthaeus, WH
Velli, M
AF Matthaeus, W. H.
Velli, M.
TI Who Needs Turbulence? A Review of Turbulence Effects in the Heliosphere
and on the Fundamental Process of Reconnection
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Magnetic reconnection; Turbulence; Solar wind; Corona
ID 3-DIMENSIONAL MAGNETOHYDRODYNAMIC TURBULENCE; SOLAR-WIND TURBULENCE;
MEAN MAGNETIC-FIELD; ALFVEN WAVES; RADIAL EVOLUTION; INTERPLANETARY
TURBULENCE; OBSERVATIONAL CONSTRAINTS; HYDROMAGNETIC TURBULENCE;
STATISTICAL PROPERTIES; ISOTROPIC TURBULENCE
AB The significant influences of turbulence in neutral fluid hydrodynamics are well accepted but the potential for analogous effects in space and astrophysical plasmas is less widely recognized. This situation sometimes gives rise to the question posed in the title; "Who need turbulence?" After a brief overview of turbulence effects in hydrodynamics, some likely effects of turbulence in solar and heliospheric plasma physics are reviewed here, with the goal of providing at least a partial answer to the posed question.
C1 [Matthaeus, W. H.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Velli, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Matthaeus, WH (reprint author), Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
EM whm@udel.edu
FU NASA [NNX08AI47G, NNX08AM48G]; MMS project theory and modeling program
[NNX08AI47G]; Solar Probe Plus project; NSF [NNX08AM48G]
FX This research has been supported in part by the NASA Heliospheric Theory
Program NNX08AI47G, the MMS project theory and modeling program
NNX08AI47G, the Solar Probe Plus project, the NASA Geospace program
NNX08AM48G, and the NSF SHINE program NNX08AM48G. 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. We thank W.J. Matthaeus for
comments on the manuscript.
NR 142
TC 62
Z9 62
U1 1
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD OCT
PY 2011
VL 160
IS 1-4
BP 145
EP 168
DI 10.1007/s11214-011-9793-9
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 831NO
UT WOS:000295738600008
ER
PT J
AU Bishop, JL
Schelble, RT
McKay, CP
Brown, AJ
Perry, KA
AF Bishop, Janice L.
Schelble, Rachel T.
McKay, Christopher P.
Brown, Adrian J.
Perry, Kaysea A.
TI Carbonate rocks in the Mojave Desert as an analogue for Martian
carbonates
SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY
LA English
DT Article
DE Mars; spectroscopy; Mojave Desert; carbonate; 'life in extreme
environments'
ID COMMON GEOLOGIC MINERALS; THERMAL EMISSION-SPECTRA; SPIRIT ROVER; GUSEV
CRATER; REFLECTANCE SPECTROSCOPY; GEOCHEMICAL ANALYSES; MICROBIAL MATS;
MARS; IDENTIFICATION; CALIFORNIA
AB Carbonate rocks in the Mojave Desert are presented as potential analogues for the carbonates on Mars. Rocks collected from the Little Red Hill site contain iron oxide-bearing coatings that greatly suppress the spectral features due to carbonate of the underlying material and impart a spectral slope. The Mojave Desert was formerly a lush pedogenic soil environment that, over time, transformed into the current arid climate with abundant rock varnish. One niche for microbes in the current desolate environment is inside and underneath the rocks where the microbes profit from solar protection by the iron oxide rock coatings. Carbonates were long predicted to be present on Mars and have recently been detected by instruments on Phoenix and MER and using hyperspectral orbiters such as the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM), the Planetary Fourier Spectrometer (PFS) and the Thermal Emission Spectrometer (TES). We describe here the results of a study of carbonate rocks from the Little Red Hill site of the Mojave Desert that includes X-ray diffraction (XRD), chemistry and visible-infrared reflectance spectroscopy. Coatings on the carbonate rocks greatly reduced the strength of the carbonate bands and caused changes in the shape of some bands. We compare these data with a carbonate outcrop at Nili Fossae, Mars. If microbes once inhabited Mars, similar carbonate rocks with iron oxide coatings could have provided a UV-protected niche there as well. Thus, analysis of carbonate-bearing regions on Mars by future landers would be useful sites to search for biosignatures. Received 8 April 2011, accepted 11 May 2011, first published online 1 July 2011
C1 [Bishop, Janice L.; Brown, Adrian J.; Perry, Kaysea A.] SETI Inst, Mountain View, CA 94043 USA.
[Bishop, Janice L.; McKay, Christopher P.; Brown, Adrian J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Schelble, Rachel T.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA.
RP Bishop, JL (reprint author), SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
EM jbishop@seti.org
FU NASA [NNG06GJ31G]; NSF; NAI; ASTEP program
FX RELAB is operated as an open multi-user facility under NASA grant
NNG06GJ31G. Funding is appreciated from NSF and the NAI for the SETI
Institute REU program that supported KAP and from the ASTEP program for
field work.
NR 69
TC 11
Z9 11
U1 1
U2 21
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 OCT
PY 2011
VL 10
IS 4
BP 349
EP 358
DI 10.1017/S1473550411000206
PG 10
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 825ZT
UT WOS:000295321600006
ER
PT J
AU Kassemi, M
Brock, R
Nemeth, N
AF Kassemi, Mohammad
Brock, Robert
Nemeth, Noel
TI A combined transport-kinetics model for the growth of renal calculi
SO JOURNAL OF CRYSTAL GROWTH
LA English
DT Article
DE Convection; Diffusion; Growth models; Mass transfer; Growth from
solutions; Biological substances
ID CALCIUM-OXALATE MONOHYDRATE; URINARY STONE FORMATION; CRYSTAL-GROWTH;
CONSTANT COMPOSITION; IN-VITRO; CRYSTALLIZATION; INHIBITION; CITRATE;
NUCLEATION; DISEASE
AB Renal stone disease is not only a concern on the Earth but could conceivably pose a serious risk to the astronauts' health and safety in Space. In this study, a combined transport-kinetics model for the growth of calcium oxalate (CaOx) crystals is presented. The model is used to parametrically investigate the growth of renal calculi in urine with a focus on the coupled effects of transport and surface reaction on the ionic concentrations at the surface of the crystal and their impact on the resulting growth rates. It is shown that under nominal conditions of low solution supersaturation and low Damkohler number that typically exist on the Earth, the surface concentrations of calcium and oxalate approach their bulk solution values in the urine and the growth rate is most likely limited by the surface reaction kinetics. But for higher solution supersaturations and large Damkohler numbers that may be prevalent in the microgravity environment of Space, the calcium and oxalate surface concentrations tend to shift more towards their equilibrium or saturation values and thus the growth process may be limited by the transport through the medium. Furthermore, it is shown that as the crystal size increases a shift towards a transport-limited growth process is likely. In this situation beyond a critical radius that is a function of the physiochemical parameters of the renal environment, the growth rate will not be independent of the radius as in a reaction-limited situation but will decrease as the crystal size increases. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Kassemi, Mohammad] NASA, Glenn Res Ctr, NCSER, Cleveland, OH 44135 USA.
[Brock, Robert] ZIN Technol Inc, Cleveland, OH 44130 USA.
[Nemeth, Noel] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
RP Kassemi, M (reprint author), NASA, Glenn Res Ctr, NCSER, 21000 Brookpk Rd,Mailstop 110-3, Cleveland, OH 44135 USA.
EM Mohammad.Kassemi@nasa.gov
FU NASA
FX The support of NASA's Human Research Program (HRP) for this work is
gratefully acknowledged. We are also indebted to Dr. Ilana Iskovitz and
Dr. Suleyman Gokoglu, Glenn Research Center, for their time and effort
in reviewing this article and providing helpful comments and
suggestions.
NR 36
TC 3
Z9 3
U1 0
U2 3
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 OCT 1
PY 2011
VL 332
IS 1
BP 48
EP 57
DI 10.1016/j.jcrysgro.2011.07.009
PG 10
WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied
SC Crystallography; Materials Science; Physics
GA 825TE
UT WOS:000295304200010
ER
PT J
AU Schwerdt, HN
Xu, WC
Shekhar, S
Abbaspour-Tamijani, A
Towe, BC
Miranda, FA
Chae, J
AF Schwerdt, Helen N.
Xu, Wencheng
Shekhar, Sameer
Abbaspour-Tamijani, Abbas
Towe, Bruce C.
Miranda, Felix A.
Chae, Junseok
TI A Fully Passive Wireless Microsystem for Recording of Neuropotentials
Using RF Backscattering Methods
SO JOURNAL OF MICROELECTROMECHANICAL SYSTEMS
LA English
DT Article
DE Backscattering; biomicroelectromechanical systems; neural recording;
neural telemetry; radio frequency (RF) identification (RFID)
ID POWER INTEGRATED-CIRCUIT; SYSTEM
AB The ability to safely monitor neuropotentials is essential in establishing methods to study the brain. Current research focuses on the wireless telemetry aspect of implantable sensors in order to make these devices ubiquitous and safe. Chronic implants necessitate superior reliability and durability of the integrated electronics. The power consumption of implanted electronics must also be limited to within several milliwatts to microwatts to minimize heat trauma in the human body. In order to address these severe requirements, we developed an entirely passive and wireless microsystem for recording neuropotentials. An external interrogator supplies a fundamental microwave carrier to the microsystem. The microsystem comprises varactors that perform nonlinear mixing of neuropotential and fundamental carrier signals. The varactors generate third-order mixing products that are wirelessly backscattered to the external interrogator where the original neuropotential signals are recovered. Performance of the neurorecording microsystem was demonstrated by wireless recording of emulated and in vivo neuropotentials. The obtained results were wireless recovery of neuropotentials as low as approximately 500 microvolts peak-to-peak (mu V(pp)) with a bandwidth of 10 Hz to 3 kHz (for emulated signals) and with 128 epoch signal averaging of repetitive signals (for in vivo signals). [2010-0338]
C1 [Schwerdt, Helen N.; Xu, Wencheng; Chae, Junseok] Arizona State Univ, Sch Elect Comp & Energy Engn, Tempe, AZ 85287 USA.
[Towe, Bruce C.] Arizona State Univ, Sch Biol & Hlth Syst Engn, Tempe, AZ 85287 USA.
[Miranda, Felix A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Schwerdt, HN (reprint author), Arizona State Univ, Sch Elect Comp & Energy Engn, Tempe, AZ 85287 USA.
EM hschwerd@asu.edu; wencheng.xu@asu.edu; Sameer.Shekhar@asu.edu;
abbas.a.tamijani@asu.edu; felix.a.miranda@nasa.gov; Junseok.Chae@asu.edu
RI Chae, Junseok/E-5984-2010
FU U.S. National Science Foundation [ECCS-0702227]; National Institutes of
Health [5R21NS059815-02]; National Aeronautics and Space Administration
[NNX09AK93H]
FX This work was supported in part by the U.S. National Science Foundation
under Grant ECCS-0702227, in part by the National Institutes of Health
under Grant 5R21NS059815-02, and in part by the National Aeronautics and
Space Administration Graduate Student Research Program fellowship
NNX09AK93H.
NR 42
TC 22
Z9 22
U1 3
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1057-7157
J9 J MICROELECTROMECH S
JI J. Microelectromech. Syst.
PD OCT
PY 2011
VL 20
IS 5
BP 1119
EP 1130
DI 10.1109/JMEMS.2011.2162487
PG 12
WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology;
Instruments & Instrumentation; Physics, Applied
SC Engineering; Science & Technology - Other Topics; Instruments &
Instrumentation; Physics
GA 828UT
UT WOS:000295529500009
PM 22267898
ER
PT J
AU Okojie, RS
Chang, CW
Evans, LJ
AF Okojie, Robert S.
Chang, Carl W.
Evans, Laura J.
TI Reducing DRIE-Induced Trench Effects in SiC Pressure Sensors Using FEA
Prediction
SO JOURNAL OF MICROELECTROMECHANICAL SYSTEMS
LA English
DT Article
DE Burst force; etch trench; finite-element (FE) analyses (FEAs); fracture
strength; pressure sensors; silicon carbide
ID SILICON-CARBIDE MICROSPECIMENS; SINGLE-CRYSTAL SILICON; FRACTURE
STRENGTH; MIXTURES; DYNAMICS; BEHAVIOR; RATIO
AB Burst force of several 4H-SiC pressure sensor diaphragms fabricated by reactive ion etching (RIE) is measured and coupled with finite-element (FE) analyses to extract a fracture strength of 786 +/- 0.3 MPa. The result, which was in relative agreement with previously published values, was applied in various failure prediction models for RIE-induced trench defects that were responsible for the premature failures observed in SiC pressure sensors. The FE model associated with trench-free diaphragms was experimentally validated to prevent such failure, thereby resulting in the expansion of the sensor pressure handling capacity by more than twofold. The RIE fabrication process conditions for this model have been successfully implemented as a standard process. This result was extended further into developing failure prediction models for other observed RIE-induced etch characteristics. [2010-0246]
C1 [Okojie, Robert S.; Chang, Carl W.] NASA, Glenn Res Ctr, ASRC Aerosp Corp, Cleveland, OH 44135 USA.
RP Okojie, RS (reprint author), NASA, Glenn Res Ctr, ASRC Aerosp Corp, Cleveland, OH 44135 USA.
EM robert.s.okojie@nasa.gov; carl.w.chang@nasa.gov; laura.j.evans@nasa.gov
FU National Aeronautics and Space Administration
FX This work was supported in part by the Supersonic, Subsonic Fixed Wing,
and Subsonic Rotary Wing Projects of the National Aeronautics and Space
Administration Fundamental Aeronautics Program.
NR 40
TC 6
Z9 6
U1 0
U2 15
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1057-7157
J9 J MICROELECTROMECH S
JI J. Microelectromech. Syst.
PD OCT
PY 2011
VL 20
IS 5
BP 1174
EP 1183
DI 10.1109/JMEMS.2011.2163298
PG 10
WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology;
Instruments & Instrumentation; Physics, Applied
SC Engineering; Science & Technology - Other Topics; Instruments &
Instrumentation; Physics
GA 828UT
UT WOS:000295529500014
ER
PT J
AU Kabashnikov, VP
Chaikovsky, AP
Kucsera, TL
Metelskaya, NS
AF Kabashnikov, Vitaliy P.
Chaikovsky, Anatoli P.
Kucsera, Tom L.
Metelskaya, Natalia S.
TI Estimated accuracy of three common trajectory statistical methods
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Trajectory statistical method; Back trajectories; Source reconstruction;
Atmospheric trace substance
ID SOURCE-RECEPTOR RELATIONSHIPS; SOURCE APPORTIONMENT; ARTIFICIAL SOURCES;
CARBON-DIOXIDE; AIR-POLLUTANTS; SOURCE REGIONS; GRAND-CANYON; TRANSPORT;
IDENTIFICATION; PRECIPITATION
AB Three well-known trajectory statistical methods (TSMs), namely concentration field (CF), concentration weighted trajectory (CWT), and potential source contribution function (PSCF) methods were tested using known sources and artificially generated data sets to determine the ability of TSMs to reproduce spatial distribution of the sources. In the works by other authors, the accuracy of the trajectory statistical methods was estimated for particular species and at specified receptor locations. We have obtained a more general statistical estimation of the accuracy of source reconstruction and have found optimum conditions to reconstruct source distributions of atmospheric trace substances. Only virtual pollutants of the primary type were considered.
In real world experiments, TSMs are intended for application to a priori unknown sources. Therefore, the accuracy of TSMs has to be tested with all possible spatial distributions of sources. An ensemble of geographical distributions of virtual sources was generated. Spearman's rank order correlation coefficient between spatial distributions of the known virtual and the reconstructed sources was taken to be a quantitative measure of the accuracy. Statistical estimates of the mean correlation coefficient and a range of the most probable values of correlation coefficients were obtained. All the TSMs that were considered here showed similar close results.
The maximum of the ratio of the mean correlation to the width of the correlation interval containing the most probable correlation values determines the optimum conditions for reconstruction. An optimal geographical domain roughly coincides with the area supplying most of the substance to the receptor. The optimal domain's size is dependent on the substance decay time. Under optimum reconstruction conditions, the mean correlation coefficients can reach 0.70-0.75. The boundaries of the interval with the most probable correlation values are 0.6-0.9 for the decay time of 240 h and 0.5-0.95 for the decay time of 12 h. The best results of source reconstruction can be expected for the trace substances with a decay time on the order of several days.
Although the methods considered in this paper do not guarantee high accuracy they are computationally simple and fast. Using the TSMs in optimum conditions and taking into account the range of uncertainties, one can obtain a first hint on potential source areas. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Kabashnikov, Vitaliy P.; Chaikovsky, Anatoli P.; Metelskaya, Natalia S.] Natl Acad Sci Belarus, BI Stepanov Phys Inst, Minsk 220072, Byelarus.
[Kucsera, Tom L.] NASA, Goddard Space Flight Ctr, USRA, GESTAR, Greenbelt, MD 20771 USA.
RP Kabashnikov, VP (reprint author), Natl Acad Sci Belarus, BI Stepanov Phys Inst, Nezavisimosti Ave 68, Minsk 220072, Byelarus.
EM v.kabashnikov@dragon.bas-net.by
FU Belarusian Republican Foundation for Fundamental Research
FX We would like to thank the Belarusian Republican Foundation for
Fundamental Research for financial support.
NR 31
TC 17
Z9 17
U1 2
U2 23
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 OCT
PY 2011
VL 45
IS 31
BP 5425
EP 5430
DI 10.1016/j.atmosenv.2011.07.006
PG 6
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 822SQ
UT WOS:000295070300003
ER
PT J
AU Liang, MTC
Navidi, M
Cleek, TM
Arnaud, SB
AF Liang, Michael T. C.
Navidi, Meena
Cleek, Tammy M.
Arnaud, Sara B.
TI Dietary Salt, Bone Strength, and Mineral Content in Unloaded Rat Femurs
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Article
DE hind limb suspension; BMC; torsional strength; mature rats; calcium
ID URINARY CALCIUM EXCRETION; SPACE-FLIGHT; SODIUM; MODEL; OSTEOPOROSIS;
METABOLISM
AB LIANG MTC, NAVIDI M, CLEEK TM, ARNAUD SB. Dietary salt, bone strength, and mineral content in unloaded rat femurs. Aviat Space Environ Med 2011; 82:941-5.
Introduction: Reduced bone mineral and ultimate strength are regular consequences of unloading bone. The aim of this study was to determine if high dietary salt intake would reduce the bone density and strength to a greater extent in rats with unloaded bones compared to ambulatory control rats fed the same dietary calcium and phosphorus. Methods: Mature male Sprague-Dawley rats were divided into four groups: two exposed to a spaceflight mode. that unloaded the hind limbs (HU) and two controls (C) with normal ambulation. Half the HU and C rats were fed normal dietary salt (0.26%, NNa) and half high dietary salt (8%, HNa). The calcium (Ca) and phosphorus (P) content of the diets was normal (Ca 0.5% and P 0.6%) in all four groups. After 4 wk of hind limb unloading, the bone mineral content (BMC) of excised femurs was measured by the ash weight and the ultimate torsional strength was determined by a torsional strength test device. Results: Femoral BMC (mg) was lower in HUNNa than C rats fed normal salt diets. Femurs from HU rats fed normal salt diets showed lower (20-26%) torsional strength (Nmm), compared to all other groups. Discussion: It appears that high salt diets with normal amounts of calcium and phosphorus may prevent the decrease in bone torsional strength and BMC induced by unloading the femurs in 6-mo-old rats.
C1 [Liang, Michael T. C.; Navidi, Meena; Cleek, Tammy M.; Arnaud, Sara B.] NASA, Div Life Sci, Ames Res Ctr, Moffett Field, CA USA.
RP Liang, MTC (reprint author), Calif State Polytech Univ Pomona, Dept Kinesiol & Hlth Promot, Room 43-108,3801 W Temple Ave, Pomona, CA 91768 USA.
EM mtcliang@csupomona.edu
FU NASA [199-26-02]; NASA-Stanford-ASEE
FX This study was supported by NASA Grant 199-26-02 and NASA-Stanford-ASEE
Summer Faculty Fellowship Program for 1997 and 1998. We thank Dr. Robert
Whalen for technical assistance with the torsional testing machine and
Mrs. Claire Angissora for assisting with manuscript preparation.
NR 24
TC 0
Z9 2
U1 2
U2 7
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD OCT
PY 2011
VL 82
IS 10
BP 941
EP 945
DI 10.3357/ASEM.2967.2011
PG 5
WC Public, Environmental & Occupational Health; Medicine, General &
Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
Medicine; Sport Sciences
GA 824FE
UT WOS:000295187000002
PM 21961397
ER
PT J
AU Rundle, JB
Holliday, JR
Yoder, M
Sachs, MK
Donnellan, A
Turcotte, DL
Tiampo, KF
Klein, W
Kellogg, LH
AF Rundle, John B.
Holliday, James R.
Yoder, Mark
Sachs, Michael K.
Donnellan, Andrea
Turcotte, Donald L.
Tiampo, Kristy F.
Klein, William
Kellogg, Louise H.
TI Earthquake precursors: activation or quiescence?
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Time series analysis; Persistence; memory; correlations; clustering;
Probablistic forecasting
ID FORECAST VERIFICATION; PROBABILITY FORECASTS; SEISMIC QUIESCENCE;
CRITICAL-POINT; SKILL SCORES; CHI-CHI; MODEL; CRITICALITY; NUCLEATION;
INDICATOR
AB We discuss the long-standing question of whether the probability for large earthquake occurrence (magnitudes m > 6.0) is highest during time periods of smaller event activation, or highest during time periods of smaller event quiescence. The physics of the activation model are based on an idea from the theory of nucleation, that a small magnitude earthquake has a finite probability of growing into a large earthquake. The physics of the quiescence model is based on the idea that the occurrence of smaller earthquakes (here considered as magnitudes m > 3.5) may be due to a mechanism such as critical slowing down, in which fluctuations in systems with long-range interactions tend to be suppressed prior to large nucleation events. To illuminate this question, we construct two end-member forecast models illustrating, respectively, activation and quiescence. The activation model assumes only that activation can occur, either via aftershock nucleation or triggering, but expresses no choice as to which mechanism is preferred. Both of these models are in fact a means of filtering the seismicity time-series to compute probabilities. Using 25 yr of data from the California-Nevada catalogue of earthquakes, we show that of the two models, activation and quiescence, the latter appears to be the better model, as judged by backtesting (by a slight but not significant margin). We then examine simulation data from a topologically realistic earthquake model for California seismicity, Virtual California. This model includes not only earthquakes produced from increases in stress on the fault system, but also background and off-fault seismicity produced by a BASS-ETAS driving mechanism. Applying the activation and quiescence forecast models to the simulated data, we come to the opposite conclusion. Here, the activation forecast model is preferred to the quiescence model, presumably due to the fact that the BASS component of the model is essentially a model for activated seismicity. These results lead to the (weak) conclusion that California seismicity may be characterized more by quiescence than by activation, and that BASS-ETAS models may not be robustly applicable to the real data.
C1 [Rundle, John B.; Holliday, James R.; Yoder, Mark; Sachs, Michael K.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Rundle, John B.; Turcotte, Donald L.; Kellogg, Louise H.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA.
[Rundle, John B.] Santa Fe Inst, Santa Fe, NM 87501 USA.
[Donnellan, Andrea] CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA.
[Tiampo, Kristy F.] Univ Western Ontario, Dept Earth Sci, London, ON N6A 3K7, Canada.
[Klein, William] Boston Univ, Dept Phys, Boston, MA 02215 USA.
RP Rundle, JB (reprint author), Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
EM yoder@physics.ucdavis.edu
RI Kellogg, Louise/J-2171-2012; Tiampo, Kristy/I-1355-2015
OI Kellogg, Louise/0000-0001-5874-0472; Tiampo, Kristy/0000-0002-5500-7600
FU NASA [NNX08AF69G]; JPL [1291967]
FX Research by JBR and JRH was supported by NASA grant NNX08AF69G to UC
Davis. Research by MY and MKS was supported by a contract from JPL to UC
Davis # 1291967.
NR 58
TC 11
Z9 11
U1 0
U2 7
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0956-540X
J9 GEOPHYS J INT
JI Geophys. J. Int.
PD OCT
PY 2011
VL 187
IS 1
BP 225
EP 236
DI 10.1111/j.1365-246X.2011.05134.x
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 822AH
UT WOS:000295015100016
ER
PT J
AU Cros, E
Roux, P
Vandemeulebrouck, J
Kedar, S
AF Cros, E.
Roux, P.
Vandemeulebrouck, J.
Kedar, S.
TI Locating hydrothermal acoustic sources at Old Faithful Geyser using
Matched Field Processing
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Hydrothermal systems; Volcano seismology; Wave propagation; North
America
ID YELLOWSTONE VOLCANIC FIELD; LONG-PERIOD EVENTS; RELATIVE RELOCATION;
SEISMIC AMPLITUDES; KILAUEA VOLCANO; NATIONAL-PARK; NEW-ZEALAND; TREMOR;
NOISE; LOCALIZATION
AB In 1992, a large and dense array of geophones was placed around the geyser vent of Old Faithful, in the Yellowstone National Park, to determine the origin of the seismic hydrothermal noise recorded at the surface of the geyser and to understand its dynamics. Old Faithful Geyser (OFG) is a small-scale hydrothermal system where a two-phase flow mixture erupts every 40 to 100 min in a high continuous vertical jet. Using Matched Field Processing (MFP) techniques on 10-min-long signal, we localize the source of the seismic pulses recorded at the surface of the geyser. Several MFP approaches are compared in this study, the frequency-incoherent and frequency-coherent approach, as well as the linear Bartlett processing and the non-linear Minimum Variance Distorsionless Response (MVDR) processing. The different MFP techniques used give the same source position with better focalization in the case of the MVDR processing. The retrieved source position corresponds to the geyser conduit at a depth of 12 m and the localization is in good agreement with in situ measurements made at Old Faithful in past studies.
C1 [Cros, E.; Vandemeulebrouck, J.] Univ Savoie, CNRS, UMR5275, ISTerre, F-73376 Le Bourget Du Lac, France.
[Roux, P.] Univ Grenoble 1, CNRS, UMR5275, ISTerre, F-38041 Grenoble 9, France.
[Kedar, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Cros, E (reprint author), Univ Savoie, CNRS, UMR5275, ISTerre, Campus Sci, F-73376 Le Bourget Du Lac, France.
EM estelle.cros@univ-savoie.fr
RI roux, philippe/B-8538-2014
FU National Science Foundation under NSF [0930731, 0930643]; National
Science Foundation [EAR-0350028, EAR-0732947]
FX Most of the computations presented in this paper were performed at the
Service Commun de Calcul Intensif de l'Observatoire de Grenoble (SCCI).
The Digital Elevation Model used in this study is based on data services
provided by the OpenTopography Facility with support from the National
Science Foundation under NSF Award Numbers 0930731 and 0930643 and is
based on services provided by the Plate Boundary Observatory operated by
UNAVCO for EarthScope (http://www.earthscope.org) and supported by the
National Science Foundation (No. EAR-0350028 and EAR-0732947). We would
like to thank Shaul Hurwitz and Robert Clayton for their help.
NR 29
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U1 0
U2 13
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0956-540X
J9 GEOPHYS J INT
JI Geophys. J. Int.
PD OCT
PY 2011
VL 187
IS 1
BP 385
EP 393
DI 10.1111/j.1365-246X.2011.05147.x
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 822AH
UT WOS:000295015100026
ER
PT J
AU Mojib, N
Nasti, TH
Andersen, DT
Attigada, VR
Hoover, RB
Yusuf, N
Bej, AK
AF Mojib, Nazia
Nasti, Tahseen H.
Andersen, Dale T.
Attigada, Venkatram R.
Hoover, Richard B.
Yusuf, Nabiha
Bej, Asim K.
TI The antiproliferative function of violacein-like purple violet pigment
(PVP) from an Antarctic Janthinobacterium sp Ant5-2 in UV-induced 2237
fibrosarcoma
SO INTERNATIONAL JOURNAL OF DERMATOLOGY
LA English
DT Article
ID SKIN-CANCER; CHROMOBACTERIUM-VIOLACEUM; MUTANT P53; APOPTOSIS; TUMORS;
CARCINOGENESIS; ANGIOGENESIS; PREVENTION; CELLS; MICE
AB Background In this study, we have investigated the chemotherapeutic potential of a purple violet pigment (PVP), which was isolated from a previously undescribed Antarctic Janthinobacterium sp. (Ant5-2), against murine UV-induced 2237 fibrosarcoma and B16F10 melanoma cells.
Methods The 2237, B16F10, C50, and NIH3T3 cells were treated with PVP at different doses and for different times, and their proliferation and viability were detected by 3-[4,5-dimethylthiazol-2-yl]-2,5-diphenyltetrazolium bromide (MTT) assay. Cell cycle arrest induced by PVP in 2237 fibrosarcoma cells was assessed by flow cytometry and expression analysis of cell cycle regulatory proteins were done by Western blot. Apoptosis induced by PVP in 2237 cells was observed by annexin-V/propidium iodide double staining flow cytometry assay and fluorescence microscopy. To further determine the molecular mechanism of apoptosis induced by PVP, the changes in expression of Bcl-2, Bax and cytochrome c were detected by Western blot. The loss of mitochondrial membrane potential in PVP treated 2237 cells was assessed by staining with JC-1 dye following flow cytometry. Caspase-3, Caspase-9 and PARP cleavage were analyzed by Western blot and Caspase-3 and -9 activities were measured by colorimetric assays.
Results In vitro treatment of murine 2237 cells with the PVP resulted in decreased cell viability (13-79%) in a time (24-72 h) and dose (0.1-1 mu M)-dependent manner. The PVP-induced growth inhibition in 2237 cells was associated with both G0/G1 and G2/M phase arrest accompanied with decrease in the expression of cyclin dependent kinases (Cdks) and simultaneous increase in the expression of cyclin dependent kinase inhibitors (Cdki) - Cip1/p21 and Kip1/p27. Further, we observed a significant increase in the apoptosis of the 2237 fibrosarcoma cells which was associated with an increased expression of pro-apoptotic protein Bax, decreased expression of anti-apoptotic proteins Bcl-2, disruption of mitochondrial membrane potential, cytochrome c release, activation of caspase-3, caspase-9 and poly-ADP-ribose-polymerase (PARP) cleavage.
Conclusions We describe the anti-cancer mechanism of the PVP for the first time from an Antarctic bacterium and suggest that the PVP could be used as a potent chemotherapeutic agent against nonmelanoma skin cancers.
C1 [Mojib, Nazia; Bej, Asim K.] Univ Alabama, Dept Biol, Birmingham, AL 35294 USA.
[Nasti, Tahseen H.; Yusuf, Nabiha] Univ Alabama, Dept Dermatol, Birmingham, AL 35294 USA.
[Attigada, Venkatram R.] Univ Alabama, Dept Chem, Birmingham, AL 35294 USA.
[Andersen, Dale T.] SETI Inst, Mountain View, CA USA.
[Hoover, Richard B.] NASA Marshall Space Flight Ctr, Huntsville, AL USA.
RP Bej, AK (reprint author), Univ Alabama Birmingham Biol, Dept Biol, 1300 Univ Blvd,CH464, Birmingham, AL 35294 USA.
EM abej@uab.edu
OI MOJIB, NAZIA/0000-0003-4924-5538
FU NIH UAB Skin Disease Research Center [P30AR050948]
FX We are grateful to Colonel (IL) J.N. Pritzker IL ARNG (Ret) (Tawani
Foundation), Rasik Ravindra (NCAOR, India) and Marty Kress
(NSSTC/VCSI/NASA) for their support in the Tawani International
Antarctic Scientific Expedition; 2008-2009 NASA's Exobiology Grant
program (Dale T. Andersen); logistics support provided by the Antarctic
Russian Novolazarevskaya and Indian Maitri stations. We thank Keela Dodd
for providing us some of the antibodies. We thank Marion Spell at the
UAB core facility of the Center for the AIDS Research (CFAR) for flow
cytometry study. This study was supported in part by Pilot & Feasibility
Study awarded to Dr. Nabiha Yusuf from NIH funded UAB Skin Disease
Research Center grant P30AR050948 (August 2008-July 2009) and an
internal support to Dr. Asim K. Bej from the Department of Biology
(UAB). The isolation, identification and characterization of the
Janthinobacterium (Ant 5-2) strain was conducted in A. Bej's lab; the
purification and chemical analysis of the PVP were conducted in V. R.
Attigada and A. Bej's labs; the cell culture, treatment of PVP on murine
UV-induced 2237 skin cancer cells and some of the analysis of the
treated cells were conducted in N. Yusuf's lab; and most of the western
blot study were conducted in A. Bej's lab.
NR 22
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U1 0
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PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0011-9059
J9 INT J DERMATOL
JI Int. J. Dermatol.
PD OCT
PY 2011
VL 50
IS 10
BP 1223
EP 1233
DI 10.1111/j.1365-4632.2010.04825.x
PG 11
WC Dermatology
SC Dermatology
GA 824BY
UT WOS:000295176300005
PM 21790550
ER
PT J
AU Basu-Zych, AR
Hornschemeier, AE
Hoversten, EA
Lehmer, B
Gronwall, C
AF Basu-Zych, Antara R.
Hornschemeier, Ann E.
Hoversten, Erik A.
Lehmer, Bret
Gronwall, Caryl
TI A SEARCH FOR LYMAN BREAK GALAXIES IN THE CHANDRA DEEP FIELD SOUTH USING
SWIFT ULTRAVIOLET/OPTICAL TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: starburst; methods: analytical;
ultraviolet: galaxies
ID HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES; LARGE-SCALE STRUCTURES;
LUMINOSITY FUNCTION; FORMATION HISTORY; QSO FIELDS; PHOTOMETRIC
REDSHIFTS; INFRARED PROPERTIES; STARBURST GALAXIES; NUMBER COUNTS
AB While the Swift satellite is primarily designed to study gamma-ray bursts, its ultraviolet and optical imaging and spectroscopy capabilities are also being used for a variety of scientific programs. In this study, we use the UV/Optical Telescope (UVOT) instrument on board Swift to discover 0.5 < z < 2 Lyman break galaxies (LBGs). UVOT has covered similar to 266 arcmin(2) at >60 ks exposure time, achieving a limiting magnitude of u < 24.5, in the Chandra Deep Field South (CDF-S). Applying UVOT near-ultraviolet color selection, we select 50 UV-dropouts from this UVOT CDF-S data. We match the selected sources with available multiwavelength data from Great Observatories Origins Deep Survey (GOODS) South, Multiwavelength Survey by Yale-Chile, and COMBO-17 to characterize the spectral energy distributions for these galaxies and determine stellar masses, star formation rates (SFRs), and dust attenuations. We compare these properties for LBGs selected in this paper versus z similar to 3 LBGs and other CDF-S galaxies in the same redshift range (0.5 < z < 2), identified using photometric redshift techniques. The z similar to 1 LBGs have stellar masses of < logM(*)/M-circle dot > = 9.4 +/- 0.6, which is slightly lower than z similar to 3 LBGs < logM(*)/M-circle dot > = 10.2 +/- 0.4) and slightly higher compared with the z similar to 1 CDF-S galaxies (< logM(*)/M-circle dot > = 8.7 +/- 0.7). Similarly, our sample of z similar to 1 LBGs has SFRs (derived using both ultraviolet and infrared data, where available) of < logSFR/(M-circle dot yr(-1))> = 0.7 +/- 0.6, nearly an order of magnitude lower than z similar to 3 LBGs (< logSFR/(M-circle dot yr(-1)> = 1.5 +/- 0.4), but slightly higher than the comparison z similar to 1 sample of CDF-S galaxies (< logSFR/(M-circle dot yr(-1)> = 0.2 +/- 0.7). We find that our z similar to 1 UV-dropouts have < A(FUV)> = 2.0 +/- 1.0, which is higher than z similar to 3 LBGs (< A(FUV)> = 1.0 +/- 0.5), but similar to the distribution of dust attenuations in the other CDF-S galaxies (< A(FUV)> similar to 2.8 +/- 1.5). Using the GOODS-South multiwavelength catalog of galaxies, we simulate a larger and fainter sample of LBGs to compare their properties with those of the UVOT-selected LBG sample. We conclude that UVOT can be useful for finding and studying the bright end of 0.5 < z < 2.0 LBGs.
C1 [Basu-Zych, Antara R.; Hornschemeier, Ann E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hoversten, Erik A.; Gronwall, Caryl] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Lehmer, Bret] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Basu-Zych, AR (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
EM antara.r.basu-zych@nasa.gov; Ann.Hornschemeier@nasa.gov;
hoversten@astro.psu.edu; blehmer@pha.jhu.edu; caryl@astro.psu.edu
FU NASA [NNX09AC87G, NAS5-00136]
FX This research was supported by an appointment to the NASA Postdoctoral
Program at the Goddard Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA. We acknowledge
support from NASA Astrophysics Data Analysis grant NNX09AC87G. This
research is sponsored at PSU by NASA contract NAS5-00136. We appreciate
and acknowledge the members of the Swift instrument and science team for
their efforts, particularly Dean Hinshaw and Scott Koch for their work
on the UVOT catalog and images. Finally, we offer our gratitude to the
anonymous referee whose thoughtful feedback and comments greatly
improved this work.
NR 80
TC 10
Z9 10
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2011
VL 739
IS 2
AR 98
DI 10.1088/0004-637X/739/2/98
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821IZ
UT WOS:000294969800043
ER
PT J
AU Koss, M
Mushotzky, R
Veilleux, S
Winter, LM
Baumgartner, W
Tueller, J
Gehrels, N
Valencic, L
AF Koss, Michael
Mushotzky, Richard
Veilleux, Sylvain
Winter, Lisa M.
Baumgartner, Wayne
Tueller, Jack
Gehrels, Neil
Valencic, Lynne
TI HOST GALAXY PROPERTIES OF THE SWIFT BAT ULTRA HARD X-RAY SELECTED ACTIVE
GALACTIC NUCLEUS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: interactions; X-rays: galaxies
ID SPECTRAL ENERGY-DISTRIBUTIONS; PALOMAR-GREEN QUASARS; BAND IMAGING
SURVEY; SEYFERT 2 GALAXIES; DIGITAL-SKY-SURVEY; INFRARED GALAXIES; ULIRG
EVOLUTION; SPITZER QUASAR; AGN ACTIVITY; BLACK-HOLES
AB We have assembled the largest sample of ultra hard X-ray selected (14-195 keV) active galactic nucleus (AGN) with host galaxy optical data to date, with 185 nearby (z < 0.05), moderate luminosity AGNs from the Swift BAT sample. The BAT AGN host galaxies have intermediate optical colors (u - r and g - r) that are bluer than a comparison sample of inactive galaxies and optically selected AGNs from the Sloan Digital Sky Survey (SDSS) which are chosen to have the same stellar mass. Based on morphological classifications from the RC3 and the Galaxy Zoo, the bluer colors of BAT AGNs are mainly due to a higher fraction of mergers and massive spirals than in the comparison samples. BAT AGNs in massive galaxies (log M(*) > 10.5) have a 5-10 times higher rate of spiral morphologies than in SDSS AGNs or inactive galaxies. We also see enhanced far-infrared emission in BAT AGN suggestive of higher levels of star formation compared to the comparison samples. BAT AGNs are preferentially found in the most massive host galaxies with high concentration indexes indicative of large bulge-to-disk ratios and large supermassive black holes. The narrow-line (NL) BAT AGNs have similar intrinsic luminosities as the SDSS NL Seyferts based on measurements of [OIII] lambda 5007. There is also a correlation between the stellar mass and X-ray emission. The BAT AGNs in mergers have bluer colors and greater ultra hard X-ray emission compared to the BAT sample as a whole. In agreement with the unified model of AGNs, and the relatively unbiased nature of the BAT sources, the host galaxy colors and morphologies are independent of measures of obscuration such as X-ray column density or Seyfert type. The high fraction of massive spiral galaxies and galaxy mergers in BAT AGNs suggest that host galaxy morphology is related to the activation and fueling of local AGN.
C1 [Koss, Michael; Mushotzky, Richard; Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Koss, Michael; Baumgartner, Wayne; Tueller, Jack; Gehrels, Neil; Valencic, Lynne] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Koss, Michael] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Winter, Lisa M.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
RP Koss, M (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM mkoss@astro.umd.edu
RI Gehrels, Neil/D-2971-2012; Tueller, Jack/D-5334-2012; Koss,
Michael/B-1585-2015;
OI Koss, Michael/0000-0002-7998-9581; Winter, Lisa/0000-0002-3983-020X
FU Japanese Society for the Promotion of Science; Maryland Senatorial
Scholarship; NASA [NAG5-7385, NAG5-7067]; Space Telescope Science
Institute; Alexander von Humboldt Foundation; University of Maryland
[0417, 0393, 0339]; National Science Foundation; PPARC
FX We thank the anonymous referee for helpful comments that improved the
presentation of this work. We acknowledge the work that the Swift BAT
team has done to make this work possible. We are grateful to Meg Urry
for useful discussions and suggestions. M. K. also acknowledges support
through a Japanese Society for the Promotion of Science Fellowship, a
Maryland Senatorial Scholarship, and a NASA graduate fellowship. L. W.
acknowledges support through a Hubble Fellowship from the Space
Telescope Science Institute. S. V. acknowledges support from a Senior
Award from the Alexander von Humboldt Foundation and thanks the host
institution, MPE Garching, where some of this work was performed. The
Kitt Peak National Observatory observations were obtained using MD-TAC
time as part of the thesis of M. K. at the University of Maryland
(programs 0417, 0393, and 0339). Kitt Peak National Observatory,
National Optical Astronomy Observatory, is operated by the Association
of Universities for Research in Astronomy (AURA), Inc., under
cooperative agreement with the National Science Foundation. Based on
observations from Akari, a JAXA project with the participation of ESA.
This research used the Tartarus database, created by Paul O'Neill and
Kirpal Nandra at Imperial College London, and Jane Turner at NASA/GSFC.
Tartarus is supported by funding from PPARC, and NASA grants NAG5-7385
and NAG5-7067. Finally, this research used the NASA/IPAC Extragalactic
Database (NED) which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the NASA.
NR 71
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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 OCT 1
PY 2011
VL 739
IS 2
AR 57
DI 10.1088/0004-637X/739/2/57
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821IZ
UT WOS:000294969800002
ER
PT J
AU Lin, L
Kouveliotou, C
Baring, MG
van der Horst, AJ
Guiriec, S
Woods, PM
Gogus, E
Kaneko, Y
Scargle, J
Granot, J
Preece, R
von Kienlin, A
Chaplin, V
Watts, AL
Wijers, RAMJ
Zhang, SN
Bhat, N
Finger, MH
Gehrels, N
Harding, A
Kaper, L
Kaspi, V
Mcenery, J
Meegan, CA
Paciesas, WS
Pe'er, A
Ramirez-Ruiz, E
van der Klis, M
Wachter, S
Wilson-Hodge, C
AF Lin, Lin
Kouveliotou, Chryssa
Baring, Matthew G.
van der Horst, Alexander J.
Guiriec, Sylvain
Woods, Peter M.
Gogus, Ersin
Kaneko, Yuki
Scargle, Jeffrey
Granot, Jonathan
Preece, Robert
von Kienlin, Andreas
Chaplin, Vandiver
Watts, Anna L.
Wijers, Ralph A. M. J.
Zhang, Shuang Nan
Bhat, Narayan
Finger, Mark H.
Gehrels, Neil
Harding, Alice
Kaper, Lex
Kaspi, Victoria
Mcenery, Julie
Meegan, Charles A.
Paciesas, William S.
Pe'er, Asaf
Ramirez-Ruiz, Enrico
van der Klis, Michiel
Wachter, Stefanie
Wilson-Hodge, Colleen
TI Fermi/GAMMA-RAY BURST MONITOR OBSERVATIONS OF SGR J0501+4516 BURSTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (SGR J0501+4516); X-rays: bursts
ID SOFT GAMMA-REPEATERS; RESONANT CYCLOTRON SCATTERING; 1E 1547.0-5408;
MAGNETAR; EMISSION; SGR-1900+14; SPECTRA; TIME;
SOFT-GAMMA-REPEATER-1806-20; SPECTROSCOPY
AB We present our temporal and spectral analyses of 29 bursts from SGR J0501+4516, detected with the gamma-ray burst monitor on board the Fermi Gamma-ray Space Telescope during 13 days of the source's activation in 2008 (August 22-September 3). We find that the T-90 durations of the bursts can be fit with a log-normal distribution with a mean value of similar to 123 ms. We also estimate for the first time event durations of soft gamma repeater (SGR) bursts in photon space (i.e., using their deconvolved spectra) and find that these are very similar to the T-90 values estimated in count space (following a log-normal distribution with a mean value of similar to 124 ms). We fit the time-integrated spectra for each burst and the time-resolved spectra of the five brightest bursts with several models. We find that a single power law with an exponential cutoff model fits all 29 bursts well, while 18 of the events can also be fit with two blackbody functions. We expand on the physical interpretation of these two models and we compare their parameters and discuss their evolution. We show that the time-integrated and time-resolved spectra reveal that E-peak decreases with energy flux (and fluence) to a minimum of similar to 30 keV at F = 8.7 x 10(-6) erg cm(-2) s(-1), increasing steadily afterward. Two more sources exhibit a similar trend: SGRs J1550-5418 and 1806-20. The isotropic luminosity, L-iso, corresponding to these flux values is roughly similar for all sources (0.4-1.5 x 10(40) erg s(-1)).
C1 [Lin, Lin; Zhang, Shuang Nan] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Lin, Lin; Guiriec, Sylvain; Preece, Robert; Chaplin, Vandiver; Bhat, Narayan; Paciesas, William S.] Univ Alabama, CSPAR, Huntsville, AL 35805 USA.
[Kouveliotou, Chryssa; Wilson-Hodge, Colleen] NASA, Space Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Baring, Matthew G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA.
[van der Horst, Alexander J.; Finger, Mark H.; Meegan, Charles A.] Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA.
[Woods, Peter M.] Corvid Technol, Huntsville, AL 35806 USA.
[Gogus, Ersin; Kaneko, Yuki] Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey.
[Scargle, Jeffrey] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Granot, Jonathan] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[von Kienlin, Andreas] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Watts, Anna L.; Wijers, Ralph A. M. J.; Kaper, Lex; van der Klis, Michiel] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Zhang, Shuang Nan] Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, Beijing 100049, Peoples R China.
[Gehrels, Neil; Harding, Alice; Mcenery, Julie] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kaspi, Victoria] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Pe'er, Asaf] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ramirez-Ruiz, Enrico] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Wachter, Stefanie] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
RP Lin, L (reprint author), Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
EM lin.lin@uah.edu
RI Gehrels, Neil/D-2971-2012; Harding, Alice/D-3160-2012; McEnery,
Julie/D-6612-2012;
OI Wijers, Ralph/0000-0002-3101-1808; Preece, Robert/0000-0003-1626-7335
FU NASA [NNH07ZDA001-GLAST, NNX10AC59A]; Scientific and Technological
Research Council of Turkey (TUBITAK) [109T755]; Bundesministeriums fur
Wirtschaft und Technologie (BMWi) [50 OG 1101]; Netherlands Organization
for Scientific Research (NWO); European Research Council [247295]
FX This publication is part of the GBM/Magnetar Key Project (NASA grant
NNH07ZDA001-GLAST, PI: C. Kouveliotou). M. G. B. acknowledges support
from NASA through grant NNX10AC59A. E.G. and Y.K. acknowledge the
support from the Scientific and Technological Research Council of Turkey
(TUBITAK) through grant 109T755. A. v. K. was supported by the
Bundesministeriums fur Wirtschaft und Technologie (BMWi) through DLR
grant 50 OG 1101. A. L. W. acknowledges support from a Netherlands
Organization for Scientific Research (NWO) Vidi Grant. R.A.M.J.W.
acknowledges support from the European Research Council via Advanced
Investigator Grant No. 247295.
NR 48
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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 OCT 1
PY 2011
VL 739
IS 2
AR 87
DI 10.1088/0004-637X/739/2/87
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821IZ
UT WOS:000294969800032
ER
PT J
AU Mazzuca, LM
Swaters, RA
Knapen, JH
Veilleux, S
AF Mazzuca, Lisa M.
Swaters, Robert A.
Knapen, Johan H.
Veilleux, Sylvain
TI NUCLEAR RINGS IN GALAXIES-A KINEMATIC PERSPECTIVE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: kinematics and dynamics; galaxies: nuclei; galaxies: spiral;
galaxies: structure
ID MASSIVE STAR-FORMATION; DISK GALAXIES; BARRED GALAXIES; SPIRAL GALAXIES;
CENTRAL REGION; MOLECULAR GAS; GALACTIC BARS; STELLAR BARS; DUST LANES;
M100
AB We combine DensePak integral field unit and TAURUS Fabry-Perot observations of 13 nuclear rings to show an interconnection between the kinematic properties of the rings and their resonant origin. The nuclear rings have regular and symmetric kinematics, and lack strong non-circular motions. This symmetry, coupled with a direct relationship between the position angles and ellipticities of the rings and those of their host galaxies, indicates that the rings are in the same plane as the disk and are circular. From the rotation curves derived, we have estimated the compactness (v(2)/r) up to the turnover radius, which is where the nuclear rings reside. We find that there is evidence of a correlation between compactness and ring width and size. Radially wide rings are less compact, and thus have lower mass concentration. The compactness increases as the ring width decreases. We also find that the nuclear ring size is dependent on the bar strength, with weaker bars allowing rings of any size to form.
C1 [Mazzuca, Lisa M.] NASA, Goddard Space Flight Ctr, Mission Validat & Operat Branch, Greenbelt, MD 20771 USA.
[Swaters, Robert A.; Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Knapen, Johan H.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.
[Knapen, Johan H.] Univ La Laguna, Dept Astrofis, E-38205 San Cristobal la Laguna, Spain.
RP Mazzuca, LM (reprint author), NASA, Goddard Space Flight Ctr, Mission Validat & Operat Branch, Code 584, Greenbelt, MD 20771 USA.
NR 38
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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 OCT 1
PY 2011
VL 739
IS 2
AR 104
DI 10.1088/0004-637X/739/2/104
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821IZ
UT WOS:000294969800049
ER
PT J
AU Nissanke, S
Sievers, J
Dalal, N
Holz, D
AF Nissanke, Samaya
Sievers, Jonathan
Dalal, Neal
Holz, Daniel
TI LOCALIZING COMPACT BINARY INSPIRALS ON THE SKY USING GROUND-BASED
GRAVITATIONAL WAVE INTERFEROMETERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general; gravitational waves; stars: neutron; surveys
ID RADIATION; BURSTS
AB The inspirals and mergers of compact binaries are among the most promising events for ground-based gravitational-wave (GW) observatories. The detection of electromagnetic (EM) signals from these sources would provide complementary information to the GW signal. It is therefore important to determine the ability of GW detectors to localize compact binaries on the sky, so that they can be matched to their EM counterparts. We use Markov Chain Monte Carlo techniques to study sky localization using networks of ground-based interferometers. Using a coherent-network analysis, we find that the Laser Interferometer Gravitational Wave Observatory (LIGO)-Virgo network can localize 50% of their detected neutron star binaries to better than 50 deg(2) with a 95% confidence interval. The addition of the Large Scale Cryogenic Gravitational Wave Telescope (LCGT) and LIGO-Australia improves this to 12 deg(2). Using a more conservative coincident detection threshold, we find that 50% of detected neutron star binaries are localized to 13 deg(2) using the LIGO-Virgo network, and to 3 deg(2) using the LIGO-Virgo-LCGT-LIGO-Australia network. Our findings suggest that the coordination of GW observatories and EM facilities offers great promise.
C1 [Nissanke, Samaya] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Nissanke, Samaya] CALTECH, Pasadena, CA 91125 USA.
[Sievers, Jonathan; Dalal, Neal] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada.
[Dalal, Neal] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Holz, Daniel] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA.
[Holz, Daniel] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Holz, Daniel] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA.
RP Nissanke, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
OI Sievers, Jonathan/0000-0001-6903-5074
FU NSERC; CIAR; National Aeronautics and Space Administration
FX We are grateful to Josh Bloom, Scott Hughes, Sterl Phinney, Bangalore
Sathyaprakash, and Michele Vallisneri for suggestions in the early
development of the work. We thank Chad Galley, Mansi Kasliwal, Ilya
Mandel, and Eran Ofek for careful reading of the manuscript, and Yanbei
Chen, Curt Cutler, Wen-Fai Fong, Chris Hirata, Tom Prince, Bernard
Schutz, Kip Thorne, Linqing Wen, and Stan Whitcomb for helpful
discussions. Simulations were performed using the Sunnyvale cluster at
CITA, which is funded by NSERC and CIAR. S.M.N.'s research was carried
out at the Jet Propulsion Laboratory, California Institute of Technology
under a contract with National Aeronautics and Space Administration.
NR 34
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2011
VL 739
IS 2
AR 99
DI 10.1088/0004-637X/739/2/99
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821IZ
UT WOS:000294969800044
ER
PT J
AU Perlman, ES
Georganopoulos, M
Marshall, HL
Schwartz, DA
Padgett, CA
Gelbord, J
Lovell, JEJ
Worrall, DM
Birkinshaw, M
Murphy, DW
Jauncey, DL
AF Perlman, Eric S.
Georganopoulos, Markos
Marshall, Herman L.
Schwartz, Daniel A.
Padgett, C. A.
Gelbord, Jonathan
Lovell, J. E. J.
Worrall, Diana M.
Birkinshaw, Mark
Murphy, David W.
Jauncey, David L.
TI DEEP MULTIWAVEBAND OBSERVATIONS OF THE JETS OF 0208-512 AND 1202-262
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: jets; quasars: individual (PKS0208-512,
PKS1202-262); radio continuum: galaxies; X-rays: galaxies
ID X-RAY JETS; SPACE-TELESCOPE OBSERVATIONS; SPECTRUM RADIO QUASARS;
INVERSE-COMPTON MODEL; EXTRAGALACTIC JETS; SOUTHERN-HEMISPHERE; PKS
0637-752; CHANDRA; EMISSION; SYNCHROTRON
AB We present deep Hubble Space Telescope, Chandra, Very Large Array, and Australia Telescope Compact Array images of the jets of PKS 0208-512 and PKS 1202-262, which were found in a Chandra survey of a flux-limited sample of flat-spectrum radio quasars with jets. We discuss in detail their X-ray morphologies and spectra. We find optical emission from one knot in the jet of PKS 1202-262 and two regions in the jet of PKS 0208-512. The X-ray emission of both jets is most consistent with external Comptonization of cosmic microwave background photons by particles within the jet, while the optical emission is most consistent with the synchrotron process. We model the emission from the jet in this context and discuss implications for jet emission models, including magnetic field and beaming parameters.
C1 [Perlman, Eric S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
[Perlman, Eric S.; Georganopoulos, Markos] Univ Maryland Baltimore Cty, Dept Phys, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
[Georganopoulos, Markos; Padgett, C. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Marshall, Herman L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Schwartz, Daniel A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Gelbord, Jonathan] Univ Durham, Dept Phys, Sci Labs, Durham DH1 3LE, England.
[Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
[Lovell, J. E. J.; Jauncey, David L.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Worrall, Diana M.; Birkinshaw, Mark] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England.
[Murphy, David W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Perlman, ES (reprint author), Florida Inst Technol, Dept Phys & Space Sci, 150 W Univ Blvd, Melbourne, FL 32901 USA.
EM eperlman@fit.edu; georgano@umbc.edu; hermanm@space.mit.edu;
das@head-cfa.harvard.edu; j.m.gelbord@durham.ac.uk;
Jim.Lovell@utas.edu.au; d.worrall@bristol.ac.uk;
mark.birkinshaw@bristol.ac.uk; dwm@sgra.jpl.nasa.gov;
david.jauncey@csiro.au
OI Perlman, Eric/0000-0002-3099-1664
FU Chandra GO [G02-3151D, G04- 5107X]; HST [STGO-10002.01]; NASA
[NAG5-9997, NNG05-GD63DG, SAO SV1-61010, NAS8-39073, NAS8-03060]; UMBC
[NNX07-AM17G]; CXC [GO2-3151A, G02-3151C]
FX E. S. P., C. A. P., and M. G. acknowledge support from Chandra GO grants
G02-3151D and G04- 5107X), HST (grant STGO-10002.01), and NASA (LTSA
grants NAG5-9997 and NNG05-GD63DG at UMBC and NNX07-AM17G at FIT). H. L.
M. was supported under NASA contract SAO SV1-61010 for the Chandra X-Ray
Center (CXC). J.M.G. was supported under Chandra grant GO2-3151A to MIT
from the CXC. D. A. S. was partially supported by Chandra grant
G02-3151C to SAO from the CXC, and by NASA contracts NAS8-39073 and
NAS8-03060 to the CXC.
NR 53
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U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2011
VL 739
IS 2
AR 65
DI 10.1088/0004-637X/739/2/65
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821IZ
UT WOS:000294969800010
ER
PT J
AU Schmidt, JM
Ofman, L
AF Schmidt, J. M.
Ofman, L.
TI SLOW MAGNETOACOUSTIC WAVE OSCILLATION OF AN EXPANDING CORONAL LOOP
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic fields; magnetohydrodynamics (MHD); methods: numerical; solar
wind; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: photosphere
ID DOPPLER-SHIFT OSCILLATIONS; BRAGG CRYSTAL SPECTROMETER; TOTAL SOLAR
ECLIPSE; MAGNETIC-FIELD; STANDING WAVES; TRANSVERSE OSCILLATIONS;
THERMAL CONDUCTION; SUMER; WIND; STREAMER
AB We simulated an expanding loop or slow coronal mass ejection (CME) in the solar corona dimensioned with size parameters taken from real coronal expanding loops observed with the STEREO spacecraft. We find that the loop expands to Sun's size within about one hour, consistent with slow CME observations. At the top of the loop, plasma is being blown off the loop, enabled with the reconnection between the loop's flux rope magnetic field and the radial magnetic field of the Sun, thus yielding feeding material for the formation of the slow solar wind. This mechanism is in accordance with the observed blob formation of the slow solar wind. We find wave packets traveling with local sound speed downward toward the footpoints of the loop, already seen in coronal seismology observations and simulations of stationary coronal loops. Here, we generalize these results for an expanding medium. We also find a reflection of the wave packets, identified as slow magnetoacoustic waves, at the footpoints of the loop. This confirms the formation of standing waves within the coronal loop. In particular, the reflected waves can partly escape the loop top and contribute to the heating of the solar wind. The present study improves our understanding on how loop material can emerge to form blobs, major ingredients of slow CMEs, and how the release of the wave energy stored in slow magnetoacoustic waves, and transported away from the Sun within expanding loops, contributes to the acceleration and formation of the slow solar wind.
C1 [Schmidt, J. M.; Ofman, L.] Catholic Univ Amer, Greenbelt, MD 20771 USA.
[Schmidt, J. M.; Ofman, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Schmidt, J. M.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
RP Schmidt, JM (reprint author), Catholic Univ Amer, Code 671,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Joachim.M.Schmidt@nasa.gov
OI Schmidt, Joachim/0000-0002-7927-0665
FU NASA ESS; NASA ESTO-CT; NSF KDI; DoD MURI; NASA [NNX09AG10G, NNX08AV88G]
FX CME simulation results were obtained using the Space Weather Modeling
Framework, developed by the Center for Space Environment Modeling, at
the University of Michigan with funding support from NASA ESS, NASA
ESTO-CT, NSF KDI, and DoD MURI. The authors acknowledge support by NASA
grant NNX09AG10G and NNX08AV88G. Also, we thank NASA NAS for the use of
computational resources.
NR 67
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U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2011
VL 739
IS 2
AR 75
DI 10.1088/0004-637X/739/2/75
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821IZ
UT WOS:000294969800020
ER
PT J
AU Woods, TN
Hock, R
Eparvier, F
Jones, AR
Chamberlin, PC
Klimchuk, JA
Didkovsky, L
Judge, D
Mariska, J
Warren, H
Schrijver, CJ
Webb, DF
Bailey, S
Tobiska, WK
AF Woods, Thomas N.
Hock, Rachel
Eparvier, Frank
Jones, Andrew R.
Chamberlin, Phillip C.
Klimchuk, James A.
Didkovsky, Leonid
Judge, Darrell
Mariska, John
Warren, Harry
Schrijver, Carolus J.
Webb, David F.
Bailey, Scott
Tobiska, W. Kent
TI NEW SOLAR EXTREME-ULTRAVIOLET IRRADIANCE OBSERVATIONS DURING FLARES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: flares; Sun: transition region; Sun: UV radiation
ID CORONAL MASS EJECTIONS; X-RAY; MODEL; EUV; DISTURBANCES; EMISSION;
RHESSI
AB New solar extreme-ultraviolet (EUV) irradiance observations from the NASA Solar Dynamics Observatory (SDO) EUV Variability Experiment provide full coverage in the EUV range from 0.1 to 106 nm and continuously at a cadence of 10 s for spectra at 0.1 nm resolution and even faster, 0.25 s, for six EUV bands. These observations can be decomposed into four distinct characteristics during flares. First, the emissions that dominate during the flare's impulsive phase are the transition region emissions, such as the He II 30.4 nm. Second, the hot coronal emissions above 5 MK dominate during the gradual phase and are highly correlated with the GOES X-ray. A third flare characteristic in the EUV is coronal dimming, seen best in the cool corona, such as the Fe IX 17.1 nm. As the post-flare loops reconnect and cool, many of the EUV coronal emissions peak a few minutes after the GOES X-ray peak. One interesting variation of the post-eruptive loop reconnection is that warm coronal emissions (e. g., Fe XVI 33.5 nm) sometimes exhibit a second large peak separated from the primary flare event by many minutes to hours, with EUV emission originating not from the original flare site and its immediate vicinity, but rather from a volume of higher loops. We refer to this second peak as the EUV late phase. The characterization of many flares during the SDO mission is provided, including quantification of the spectral irradiance from the EUV late phase that cannot be inferred from GOES X-ray diagnostics.
C1 [Woods, Thomas N.; Hock, Rachel; Eparvier, Frank; Jones, Andrew R.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA.
[Chamberlin, Phillip C.; Klimchuk, James A.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Didkovsky, Leonid; Judge, Darrell] Univ So Calif, Ctr Space Sci, Los Angeles, CA 90089 USA.
[Mariska, John; Warren, Harry] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Schrijver, Carolus J.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Webb, David F.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02467 USA.
[Bailey, Scott] Virginia Tech, Dept Elect & Comp Engn, Blacksburg, VA 24061 USA.
[Tobiska, W. Kent] Space Environm Technol, Pacific Palisades, CA 90272 USA.
RP Woods, TN (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA.
EM tom.woods@lasp.colorado.edu
RI Chamberlin, Phillip/C-9531-2012; Klimchuk, James/D-1041-2012
OI Chamberlin, Phillip/0000-0003-4372-7405; Klimchuk,
James/0000-0003-2255-0305
FU NASA
FX The SDO mission and this research are supported by NASA. The authors
thank Vanessa George for her assistance with this manuscript.
NR 47
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U1 0
U2 9
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 OCT 1
PY 2011
VL 739
IS 2
AR 59
DI 10.1088/0004-637X/739/2/59
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821IZ
UT WOS:000294969800004
ER
PT J
AU Torok, T
Panasenco, O
Titov, VS
Mikic, Z
Reeves, KK
Velli, M
Linker, JA
De Toma, G
AF Toeroek, T.
Panasenco, O.
Titov, V. S.
Mikic, Z.
Reeves, K. K.
Velli, M.
Linker, J. A.
De Toma, G.
TI A MODEL FOR MAGNETICALLY COUPLED SYMPATHETIC ERUPTIONS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE methods: numerical; Sun: corona; Sun: coronal mass ejections (CMEs);
Sun: filaments, prominences; Sun: flares; Sun: magnetic topology
ID CORONAL MASS EJECTIONS; SOLAR CORONA; FLUX ROPES; FLARES; TOPOLOGY;
RECONNECTION; OSCILLATIONS; CONNECTION; FILAMENTS; LINKAGES
AB Sympathetic eruptions on the Sun have been observed for several decades, but the mechanisms by which one eruption can trigger another remain poorly understood. We present a three-dimensional MHD simulation that suggests two possible magnetic trigger mechanisms for sympathetic eruptions. We consider a configuration that contains two coronal flux ropes located within a pseudo-streamer and one rope located next to it. A sequence of eruptions is initiated by triggering the eruption of the flux rope next to the streamer. The expansion of the rope leads to two consecutive reconnection events, each of which triggers the eruption of a flux rope by removing a sufficient amount of overlying flux. The simulation qualitatively reproduces important aspects of the global sympathetic event on 2010 August 1 and provides a scenario for the so-called twin filament eruptions. The suggested mechanisms are also applicable for sympathetic eruptions occurring in other magnetic configurations.
C1 [Toeroek, T.; Titov, V. S.; Mikic, Z.; Linker, J. A.] Predict Sci Inc, San Diego, CA 92121 USA.
[Panasenco, O.] Helio Res, La Crescenta, CA 91214 USA.
[Reeves, K. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Velli, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[De Toma, G.] HAO NCAR, Boulder, CO 80307 USA.
RP Torok, T (reprint author), Predict Sci Inc, 9990 Mesa Rim Rd,Suite 170, San Diego, CA 92121 USA.
RI Reeves, Katharine/P-9163-2014
FU NASA [NNX09AG27G]; NASA/SHP [NNH09AK02I]; Lockheed-Martin [SP02H1701R];
International Space Science Institute via International Team 174 on
Solar Prominence Formation and Equilibrium
FX We thank P. Demoulin, B. Kliem, and K. Schrijver for stimulating
discussions. The contribution of T.T, V.S.T., Z.M., and J.A.L. was
supported by NASA's HTP, LWS, and SR&T programs, CISM (an NSF Science
and Technology Center), and a contract from Lockheed-Martin to
Predictive Science, Inc. O.P. was supported by NASA grant NNX09AG27G,
G.D.T. by NASA/SHP grant NNH09AK02I, and K. K. R. by contract SP02H1701R
from Lockheed-Martin to SAO. M.V's. contribution was carried out at JPL
(Caltech) under a contract with NASA. Computational resources were
provided by NSF TACC in Austin and by NASA NAS at the Ames Research
Center. This work was partially supported by the International Space
Science Institute via International Team 174 on Solar Prominence
Formation and Equilibrium.
NR 50
TC 57
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U1 1
U2 13
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 OCT 1
PY 2011
VL 739
IS 2
AR L63
DI 10.1088/2041-8205/739/2/L63
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821TP
UT WOS:000294997600029
ER
PT J
AU Karaca, HE
Saghaian, SM
Basaran, B
Bigelow, GS
Noebe, RD
Chumlyakov, YI
AF Karaca, H. E.
Saghaian, S. M.
Basaran, B.
Bigelow, G. S.
Noebe, R. D.
Chumlyakov, Y. I.
TI Compressive response of nickel-rich NiTiHf high-temperature shape memory
single crystals along the [111] orientation
SO SCRIPTA MATERIALIA
LA English
DT Article
DE Shape memory alloys; Martensitic phase transformation; Single crystals;
Transformation strain; NiTiHf
ID ALLOYS; MARTENSITE; BEHAVIOR
AB The shape memory properties of Ni-rich NiTiHf single crystals along the [1 1 1] orientation were investigated by thermal cycling under constant stress and stress cycling at constant temperature in compression. The single crystals demonstrate stable shape memory behavior under ultrahigh stress levels (1000 MPa) with about 3% transformation strain, a maximum work output of 30 J cm(-3) and nearly perfect pseudoelasticity at high temperatures (180-200 degrees C). (C) 2011 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Karaca, H. E.; Saghaian, S. M.; Basaran, B.] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
[Bigelow, G. S.; Noebe, R. D.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
[Chumlyakov, Y. I.] Siberian Phys Tech Inst, Tomsk 634050, Russia.
RP Karaca, HE (reprint author), Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
EM karaca@engr.uky.edu
RI yuriy, chumlyakov/C-6033-2009; Chumlyakov, Yuriy/R-6496-2016
FU KY NASA EPSCoR [N08R02B]; NASA, Dale Hopkins, API
FX This work was supported in part by the KY NASA EPSCoR (N08R02B) and NASA
Fundamental Aeronautics Program under the Supersonics Project, Dale
Hopkins, API.
NR 21
TC 26
Z9 28
U1 4
U2 22
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-6462
J9 SCRIPTA MATER
JI Scr. Mater.
PD OCT
PY 2011
VL 65
IS 7
BP 577
EP 580
DI 10.1016/j.scriptamat.2011.06.027
PG 4
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 820CG
UT WOS:000294882500004
ER
PT J
AU Horta, LG
Reaves, MC
Buehrle, RD
Templeton, JD
Lazor, DR
Gaspar, JL
Parks, RA
Bartolotta, PA
AF Horta, L. G.
Reaves, M. C.
Buehrle, R. D.
Templeton, J. D.
Lazor, D. R.
Gaspar, J. L.
Parks, R. A.
Bartolotta, P. A.
TI Finite Element Model Calibration for Ares I-X Flight Vehicle
SO EXPERIMENTAL MECHANICS
LA English
DT Article
DE Launch vehicle; Model calibration; Uncertainty quantification;
Correlation; Dynamics
ID GLOBAL SENSITIVITY-ANALYSIS; RADIAL BASIS FUNCTIONS
AB Ares I-X is a flight test vehicle developed by NASA to demonstrate a new class of crew launch vehicle. For this first flight test, the first stage was a four segment solid rocket booster with mass simulators used to represent the other sections of the Ares I vehicle. Although this vehicle is significantly simpler than the Ares I, model calibration was required for the finite element model used in loads analysis and flight control evaluations before its maiden flight. The process of calibrating models involves updating parameters and reconciling predictions with test data. This work presents a probabilistic approach to the calibration process. The approach uses Analysis of Variance (ANOVA) for parameter sensitivity, nonlinear optimization to minimize the error between test and analysis, and multiple FEM models to bound the system response and to assess the probability of finding a reconciling solution. To reduce the computational burden associated with ANOVA, response surface models are used in lieu of computationally intensive finite element solutions. Uncertainty in the parameters and their effect on the frequency response function is studied in terms of Principal Values of the frequency response functions. Uncertainty bounds of the principal values are established across multiple models to allow one to determine the probability of finding a solution that reconciles analysis with test results. Results from applying this model calibration process to the Ares I-X project are described. Findings presented in the paper confirmed that the baseline model used for pre-flight assessments was within the acceptable range established for guidance and control.
C1 [Horta, L. G.; Reaves, M. C.; Buehrle, R. D.; Templeton, J. D.; Gaspar, J. L.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Lazor, D. R.; Parks, R. A.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Bartolotta, P. A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Horta, LG (reprint author), NASA, Langley Res Ctr, MS 230, Hampton, VA 23681 USA.
EM lucas.g.horta@nasa.gov; mercedes.c.reaves@nasa.gov;
ralph.d.buehrle@nasa.gov; justin.d.templeton@nasa.gov;
daniel.r.lazor@nasa.gov; james.l.gaspar@nasa.gov;
russel.a.parks@nasa.gov; paul.a.bartolotta@nasa.gov
NR 27
TC 0
Z9 1
U1 2
U2 7
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0014-4851
J9 EXP MECH
JI Exp. Mech.
PD OCT
PY 2011
VL 51
IS 8
BP 1251
EP 1263
DI 10.1007/s11340-010-9456-x
PG 13
WC Materials Science, Multidisciplinary; Mechanics; Materials Science,
Characterization & Testing
SC Materials Science; Mechanics
GA 819BY
UT WOS:000294801600002
ER
PT J
AU Weitz, CM
Bishop, JL
Thollot, P
Mangold, N
Roach, LH
AF Weitz, Catherine M.
Bishop, Janice L.
Thollot, Patrick
Mangold, Nicolas
Roach, Leah H.
TI Diverse mineralogies in two troughs of Noctis Labyrinthus, Mars
SO GEOLOGY
LA English
DT Article
ID HISTORY; PLANUM
AB Two troughs in Noctis Labyrinthus display a diversity of mineral assemblages rarely seen spatially collocated on Mars. Minerals identified from Mars Reconnaissance Orbiter data within the troughs include polyhydrated and monohydrated sulfates, an Al clay (e. g., kaolinite or beidellite), Fe/Mg smectites, hydrated silica and/or opal, and a leached clay or jarosite mixture with a doublet absorption between 2.2 and 2.3 mu m. Units both pre-date and post-date smaller pits and depressions within the larger troughs, indicating that deposition was coeval with continued extension, collapse, and erosion in the Late Hesperian to Early Amazonian (2-3 Ga). The strata within each trough display a mineralogic diversity consistent with active aqueous processes and/or changing chemical conditions over time, perhaps due to hydrothermal alteration of volcanic ash, influxes of groundwater from nearby Tharsis volcanism, fumarole activity, and melting snow and/or ice. The superposition of younger Fe/Mg smectites over sulfates, Al clays, and hydrated silica and/or opal in both troughs indicates that this region is unique relative to most other locations on Mars, where the opposite progression is observed and the Fe/Mg smectites are Noachian (older than 3.6 Ga) in age. Consequently, these troughs may have been habitable regions on Mars at a time when drier conditions dominated the surface.
C1 [Weitz, Catherine M.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Bishop, Janice L.] SETI Search Extraterr Intelligence Inst, Mountain View, CA 94043 USA.
[Bishop, Janice L.] NASA, Ames Res Ctr, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[Thollot, Patrick; Mangold, Nicolas] CNRS Ctr Natl Rech Sci, Lab Planetol & Geodynam Nantes, F-44322 Nantes, France.
[Thollot, Patrick; Mangold, Nicolas] Univ Nantes, F-44322 Nantes, France.
[Roach, Leah H.] Frontier Technol, Beverly, MA 01915 USA.
RP Weitz, CM (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA.
NR 23
TC 28
Z9 28
U1 0
U2 5
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0091-7613
EI 1943-2682
J9 GEOLOGY
JI Geology
PD OCT
PY 2011
VL 39
IS 10
BP 899
EP 902
DI 10.1130/G32045.1
PG 4
WC Geology
SC Geology
GA 819IN
UT WOS:000294818700001
ER
PT J
AU Yi, BQ
Hsu, CN
Yang, P
Tsay, SC
AF Yi, Bingqi
Hsu, Christine N.
Yang, Ping
Tsay, Si-Chee
TI Radiative transfer simulation of dust-like aerosols: Uncertainties from
particle shape and refractive index
SO JOURNAL OF AEROSOL SCIENCE
LA English
DT Article
DE Non-spherical dust aerosol; Radiance and flux; Radiative transfer;
Broadband
ID SPHEROIDAL MODEL PARTICLES; TROPOSPHERIC AEROSOLS; SCATTERING MATRICES;
LIGHT-SCATTERING; MINERAL AEROSOLS; ERROR SOURCE; NONSPHERICITY;
RADIANCE; NM
AB The composition, particle shape, number concentration, size distribution, and spatial and temporal distributions of dust aerosols cause significant uncertainties in relevant radiative transfer simulations. The spherical particle approximation has been generally recognized to introduce errors in radiative transfer calculations involving dust aerosols. Although previous studies have attempted to quantify the effect of non-spherical particles, no consensus has been reached as to the significance of the dust aerosols non-spherical effect on flux calculations. For this study, we utilize a newly developed ultra-violet-to-far-infrared spectral database of the single-scattering properties of tri-axial ellipsoidal, mineral dust-like aerosols to study the non-spherical effect on radiative forcing. The radiance and flux differences between the spherical and ellipsoidal models are obtained for various refractive indices and particle size distributions. The errors originating from using the spherical model and the uncertainties in the refractive indices are quantified at both the top and bottom of the atmosphere. The dust non-spherical effect on the net flux and heating rate profile is obtained over the entire range of the solar spectrum. The particle shape effect is found to be related to the dust optical depth and the surface albedo and can be an important uncertainty source in radiative transfer simulation. The particle shape effect is largest over water surfaces and can cause up to a 30% difference in dust forcing at the top of the atmosphere. Published by Elsevier Ltd.
C1 [Hsu, Christine N.; Tsay, Si-Chee] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yi, Bingqi; Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77845 USA.
RP Hsu, CN (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 613-2, Greenbelt, MD 20771 USA.
EM Christina.Hsu@nasa.gov
RI Yang, Ping/B-4590-2011; Yi, Bingqi/E-4076-2012; Hsu, N.
Christina/H-3420-2013; Tsay, Si-Chee/J-1147-2014
OI Yi, Bingqi/0000-0002-1437-8376;
NR 36
TC 17
Z9 17
U1 1
U2 13
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0021-8502
EI 1879-1964
J9 J AEROSOL SCI
JI J. Aerosol. Sci.
PD OCT
PY 2011
VL 42
IS 10
BP 631
EP 644
DI 10.1016/j.jaerosci.2011.06.008
PG 14
WC Engineering, Chemical; Engineering, Mechanical; Environmental Sciences;
Meteorology & Atmospheric Sciences
SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric
Sciences
GA 816BB
UT WOS:000294572600002
ER
PT J
AU Gherlone, M
Tessler, A
Di Sciuva, M
AF Gherlone, Marco
Tessler, Alexander
Di Sciuva, Marco
TI C-0 beam elements based on the Refined Zigzag Theory for multilayered
composite and sandwich laminates
SO COMPOSITE STRUCTURES
LA English
DT Article
DE Refined Zigzag Theory; Timoshenko beam theory; Finite beam element;
Shear locking; Composite beam; Sandwich beam
ID SHALLOW SHELL ELEMENT; NONLINEAR-ANALYSIS; TRANSVERSE-SHEAR;
FINITE-ELEMENTS; PLATE ELEMENT; EFFICIENT; LOCKING; THIN
AB The paper deals with the development and computational assessment of three- and two-node beam finite elements based on the Refined Zigzag Theory (RZT) for the analysis of multilayered composite and sandwich beams. RZT is a recently proposed structural theory that accounts for the stretching, bending, and transverse shear deformations, and which provides substantial improvements over previously developed zigzag and higher-order theories. This new theory is analytically rigorous, variationally consistent, and computationally attractive. The theory is not affected by anomalies of most previous zigzag and higher-order theories, such as the vanishing of transverse shear stress and force at clamped boundaries. In contrast to Timoshenko theory, RZT does not employ shear correction factors to yield accurate results. From the computational mechanics perspective RZT requires C-0-continuous shape functions and thus enables the development of efficient displacement-type finite elements. The focus of this paper is to explore several low-order beam finite elements that offer the best compromise between computational efficiency and accuracy. The initial attention is on the choice of shape functions that do not admit shear locking effects in slender beams. For this purpose, anisoparametric (aka interdependent) interpolations are adapted to approximate the four independent kinematic variables that are necessary to model the planar beam deformations. To achieve simple two-node elements, several types of constraint conditions are examined and corresponding deflection shape-functions are derived. It is recognized that the constraint condition requiring a constant variation of the transverse shear force gives rise to a remarkably accurate two-node beam element. The proposed elements and their predictive capabilities are assessed using several elastostatic example problems, where simply supported and cantilevered beams are analyzed over a range of lamination sequences, heterogeneous material properties, and slenderness ratios. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Gherlone, Marco; Di Sciuva, Marco] Politecn Torino, Dept Aeronaut & Space Engn, I-10129 Turin, Italy.
[Tessler, Alexander] NASA, Struct Mech & Concepts Branch, Langley Res Ctr, Hampton, VA 23681 USA.
RP Gherlone, M (reprint author), Politecn Torino, Dept Aeronaut & Space Engn, Corso Duca Abruzzi 24, I-10129 Turin, Italy.
EM marco.gherlone@polito.it
OI Gherlone, Marco/0000-0002-5711-0046
NR 41
TC 28
Z9 29
U1 2
U2 6
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0263-8223
J9 COMPOS STRUCT
JI Compos. Struct.
PD OCT
PY 2011
VL 93
IS 11
BP 2882
EP 2894
DI 10.1016/j.compstruct.2011.05.015
PG 13
WC Materials Science, Composites
SC Materials Science
GA 813MO
UT WOS:000294371800024
ER
PT J
AU Williford, KH
Van Kranendonk, MJ
Ushikubo, T
Kozdon, R
Valley, JW
AF Williford, Kenneth H.
Van Kranendonk, Martin J.
Ushikubo, Takayuki
Kozdon, Reinhard
Valley, John W.
TI Constraining atmospheric oxygen and seawater sulfate concentrations
during Paleoproterozoic glaciation: In situ sulfur three-isotope
microanalysis of pyrite from the Turee Creek Group, Western Australia
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID GREAT OXIDATION EVENT; MASS-INDEPENDENT FRACTIONATION; SOUTH-AFRICA;
HAMERSLEY PROVINCE; ISOTOPIC EVIDENCE; ARCHEAN ATMOSPHERE; NIPISSING
DIABASE; SUPERIOR PROVINCE; GRIQUALAND WEST; SNOWBALL EARTH
AB Previous efforts to constrain the timing of Paleoproterozoic atmospheric oxygenation have documented the disappearance of large, mass-independent sulfur isotope fractionation and an increase in mass-dependent sulfur isotope fractionation associated with multiple glaciations. At least one of these glacial events is preserved in diamictites of the similar to 2.4 Ga Meteorite Bore Member of the Kungarra Formation, Turee Creek Group, Western Australia. Outcrop exposures of this unit show the transition from the Boolgeeda Iron Formation of the upper Hamersley Group into clastic, glaciomarine sedimentary rocks of the Turee Creek Group. Here we report in situ multiple sulfur isotope and elemental abundance measurements of sedimentary pyrite at high spatial resolution, as well as the occurrence of detrital pyrite in the Meteorite Bore Member. The 15.3 parts per thousand range of Delta(33)S in one sample containing detrital pyrite (-3.6 parts per thousand to 11.7 parts per thousand) is larger than previously reported worldwide, and there is evidence for mass-independent sulfur isotope fractionation in authigenic pyrite throughout the section (Delta(33)S from -0.8 parts per thousand to 1.0 parts per thousand). The 90 parts per thousand range in delta(34)S observed (-45.5 parts per thousand to 46.4 parts per thousand) strongly suggests microbial sulfate reduction under non-sulfate limiting conditions, indicating significant oxidative weathering of sulfides on the continents. Multiple generations of pyrite are preserved, typically represented by primary cores with low delta(34)S (<-20 parts per thousand) overgrown by euhedral rims with higher Delta(34)S (4-7 parts per thousand) and enrichments in As, Ni, and Co. The preservation of extremely sharp sulfur isotope gradients (30 parts per thousand/<4 mu m) implies limited sulfur diffusion and provides time and temperature constraints on the metamorphic history of the Meteorite Bore Member. Together, these results suggest that the Meteorite Bore Member was deposited during the final stages of the "Great Oxidation Event," when pO(2) first became sufficiently high to permit pervasive oxidative weathering of continental sulfides, yet remained low enough to permit the production and preservation of mass-independent sulfur isotope fractionation. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Williford, Kenneth H.; Ushikubo, Takayuki; Kozdon, Reinhard; Valley, John W.] Univ Wisconsin, NASA Astrobiol Inst, Astrobiol Res Consortium, WiscSIMS,Dept Geosci, Madison, WI 53706 USA.
[Van Kranendonk, Martin J.] Geol Survey Western Australia, Perth, WA 6004, Australia.
[Van Kranendonk, Martin J.] Univ Western Australia, Sch Earth & Environm, Crawley, WA 6009, Australia.
RP Williford, KH (reprint author), Univ Wisconsin, NASA Astrobiol Inst, Astrobiol Res Consortium, WiscSIMS,Dept Geosci, 1215 W Dayton St, Madison, WI 53706 USA.
EM kwilliford@geology.wisc.edu
RI Van Kranendonk, Martin/J-8755-2012; Kozdon, Reinhard/J-9468-2014;
Valley, John/B-3466-2011
OI Kozdon, Reinhard/0000-0001-6347-456X; Valley, John/0000-0003-3530-2722
FU NASA Astrobiology Institute; NSF-EAR [0319230, 0516725, 0744079]
FX We thank Noriko Kita and Jim Kern for assistance and training with the
ion microprobe, Brian Hess for sample preparation, John Fournelle for
assistance in the operation of the SEM and electron microprobe, Jason
Huberty for assistance with the SEM, and Clark Johnson, Brian Beard, and
Andy Czaja for helpful discussions. Funding was provided by the NASA
Astrobiology Institute. The WiscSIMS Lab is partially funded by NSF-EAR
(0319230, 0516725, 0744079). We thank Associate Editor James Farquhar
and reviewers David Johnston, Shuhei Ono, and Dominic Papineau for their
constructive comments that improved the quality of this manuscript.
NR 96
TC 39
Z9 41
U1 4
U2 37
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD OCT 1
PY 2011
VL 75
IS 19
BP 5686
EP 5705
DI 10.1016/j.gca.2011.07.010
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 814TK
UT WOS:000294479900019
ER
PT J
AU Fensholt, R
Anyamba, A
Huber, S
Proud, SR
Tucker, CJ
Small, J
Pak, E
Rasmussen, MO
Sandholt, I
Shisanya, C
AF Fensholt, R.
Anyamba, A.
Huber, S.
Proud, S. R.
Tucker, C. J.
Small, J.
Pak, E.
Rasmussen, M. O.
Sandholt, I.
Shisanya, C.
TI Analysing the advantages of high temporal resolution geostationary MSG
SEVIRI data compared to Polar Operational Environmental Satellite data
for land surface monitoring in Africa
SO INTERNATIONAL JOURNAL OF APPLIED EARTH OBSERVATION AND GEOINFORMATION
LA English
DT Article
DE Africa; Meteosat Second Generation; POES; Early warning systems; NDVI
ID VEGETATION INDEX; AVHRR DATA; NATURAL HAZARDS; WEST-AFRICA; NOAA-AVHRR;
MODIS; NDVI; PRODUCTS; TIME; EVAPOTRANSPIRATION
AB Since 1972, satellite remote sensing of the environment has been dominated by polar-orbiting sensors providing useful data for monitoring the earth's natural resources. However their observation and monitoring capacity are inhibited by daily to monthly looks for any given ground surface which often is obscured by frequent and persistent cloud cover creating large gaps in time series measurements. The launch of the Meteosat Second Generation (MSG) satellite into geostationary orbit has opened new opportunities for land surface monitoring. The Spinning Enhanced Visible and Infrared Imager (SEVIRI) instrument on-board MSG with an imaging capability every 15 min which is substantially greater than any temporal resolution that can be obtained from existing Polar Operational Environmental Satellite (POES) systems currently in use for environmental monitoring. Different areas of the African continent were affected by droughts and floods in 2008 caused by periods of abnormally low and high rainfall, respectively. Based on the effectiveness of monitoring these events from Earth Observation (EO) data the current analyses show that the new generation of geostationary remote sensing data can provide higher temporal resolution cloud-free (<5 days) measurements of the environment as compared to existing POES systems. SEVIRI MSG 5-day continental scale composites will enable rapid assessment of environmental conditions and improved early warning of disasters for the African continent such as flooding or droughts. The high temporal resolution geostationary data will complement existing higher spatial resolution polar-orbiting satellite data for various dynamic environmental and natural resource applications of terrestrial ecosystems. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Fensholt, R.; Huber, S.; Proud, S. R.; Rasmussen, M. O.; Sandholt, I.] Univ Copenhagen, Dept Geog & Geol, DK-1350 Copenhagen, Denmark.
[Anyamba, A.; Tucker, C. J.; Small, J.; Pak, E.] NASA, Goddard Space Flight Ctr, Biospher & Hydrol Sci Lab, Greenbelt, MD 20771 USA.
[Shisanya, C.] Kenyatta Univ, Dept Geog, Nairobi, Kenya.
RP Fensholt, R (reprint author), Univ Copenhagen, Dept Geog & Geol, Oster Voldgade 10, DK-1350 Copenhagen, Denmark.
EM rf@geo.ku.dk
RI Fensholt, Rasmus/L-7951-2014; Proud, Simon/A-4239-2015
OI Fensholt, Rasmus/0000-0003-3067-4527; Proud, Simon/0000-0003-3880-6774
NR 65
TC 14
Z9 14
U1 0
U2 14
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0303-2434
J9 INT J APPL EARTH OBS
JI Int. J. Appl. Earth Obs. Geoinf.
PD OCT
PY 2011
VL 13
IS 5
BP 721
EP 729
DI 10.1016/j.jag.2011.05.009
PG 9
WC Remote Sensing
SC Remote Sensing
GA 815NP
UT WOS:000294532600004
ER
PT J
AU Thiruppathiraja, C
Kamatchiammal, S
Adaikkappan, P
Santhosh, DJ
Alagar, M
AF Thiruppathiraja, Chinnasamy
Kamatchiammal, Senthilkumar
Adaikkappan, Periyakaruppan
Santhosh, Devakirubakaran Jayakar
Alagar, Muthukaruppan
TI Specific detection of Mycobacterium sp genomic DNA using dual labeled
gold nanoparticle based electrochemical biosensor
SO ANALYTICAL BIOCHEMISTRY
LA English
DT Article
DE Mycobacterium tuberculosis; Electrochemical biosensor; Genomic DNA; Gold
nanoparticles; Differential pulse voltammetry (DPV); Clinical
diagnostics
ID TUBERCULOSIS COMPLEX; SIGNAL AMPLIFICATION; SPECIMENS; ASSAY;
OLIGONUCLEOTIDE; IDENTIFICATION; ANTIBODIES; SAMPLES; SPUTUM; BEADS
AB The present study was aimed at the development and evaluation of a DNA electrochemical biosensor for Mycobacterium sp. genomic DNA detection in a clinical specimen using a signal amplifier as dual-labeled AuNPs. The DNA electrochemical biosensors were fabricated using a sandwich detection strategy involving two kinds of DNA probes specific to Mycobacterium sp. genomic DNA. The probes of enzyme ALP and the detector probe both conjugated on the AuNPs and subsequently hybridized with target DNA immobilized in a SAM/ITO electrode followed by characterization with CV, EIS, and DPV analysis using the electroactive species para-nitrophenol generated by ALP through hydrolysis of para-nitrophenol phosphate. The effect of enhanced sensitivity was obtained due to the AuNPs carrying numerous ALPs per hybridization and a detection limit of 1.25 ng/ml genomic DNA was determined under optimized conditions. The dual-labeled AuNP-facilitated electrochemical sensor was also evaluated by clinical sputum samples, showing a higher sensitivity and specificity and the outcome was in agreement with the PCR analysis. In conclusion, the developed electrochemical sensor demonstrated unique sensitivity and specificity for both genomic DNA and sputum samples and can be employed as a regular diagnostics tool for Mycobacterium sp. monitoring in clinical samples. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Thiruppathiraja, Chinnasamy; Alagar, Muthukaruppan] Anna Univ, Nanocomposites Res Grp, Dept Chem Engn, Madras 600025, TN, India.
[Kamatchiammal, Senthilkumar; Santhosh, Devakirubakaran Jayakar] Natl Environm Engn Res Inst, Chennai Zonal Lab, Madras 600113, TN, India.
[Adaikkappan, Periyakaruppan] NASA, Ames Res Ctr, Ctr Nanosci & Nanotechnol, Moffett Field, CA 94035 USA.
RP Alagar, M (reprint author), Anna Univ, Nanocomposites Res Grp, Dept Chem Engn, Madras 600025, TN, India.
EM mkalagar@yahoo.com
RI Periyakaruppan, Adaikkappan/B-7398-2013
OI Periyakaruppan, Adaikkappan/0000-0002-0395-6564
FU Indian Council for Medical Research (ICMR), New Delhi, India
FX The authors thank the Indian Council for Medical Research (ICMR), New
Delhi, India, for funding to execute this study successfully.
NR 25
TC 30
Z9 34
U1 1
U2 55
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0003-2697
J9 ANAL BIOCHEM
JI Anal. Biochem.
PD OCT 1
PY 2011
VL 417
IS 1
BP 73
EP 79
DI 10.1016/j.ab.2011.05.034
PG 7
WC Biochemical Research Methods; Biochemistry & Molecular Biology;
Chemistry, Analytical
SC Biochemistry & Molecular Biology; Chemistry
GA 802ZB
UT WOS:000293548400009
PM 21693099
ER
PT J
AU Jain, A
AF Jain, Abhinandan
TI Graph theoretic foundations of multibody dynamics
SO MULTIBODY SYSTEM DYNAMICS
LA English
DT Article
DE Multibody systems; Graph theory; Algorithms
ID RIGID BODY SYSTEMS; QUASI-VELOCITIES; FORMULATION; MANIPULATORS;
EQUATIONS; MATRIX; DESIGN
AB This is the first part of two papers that use concepts from graph theory to obtain a deeper understanding of the mathematical foundations of multibody dynamics. The key contribution is the development of a unifying framework that shows that key analytical results and computational algorithms in multibody dynamics are a direct consequence of structural properties and require minimal assumptions about the specific nature of the underlying multibody system. This first part focuses on identifying the abstract graph theoretic structural properties of spatial operator techniques in multibody dynamics. The second part paper exploits these structural properties to develop a broad spectrum of analytical results and computational algorithms.
Toward this end, we begin with the notion of graph adjacency matrices and generalize it to define block-weighted adjacency (BWA) matrices and their 1-resolvents. Previously developed spatial operators are shown to be special cases of such BWA matrices and their 1-resolvents. These properties are shown to hold broadly for serial and tree topology multibody systems. Specializations of the BWA and 1-resolvent matrices are referred to as spatial kernel operators (SKO) and spatial propagation operators (SPO). These operators and their special properties provide the foundation for the analytical and algorithmic techniques developed in the companion paper.
We also use the graph theory concepts to study the topology induced sparsity structure of these operators and the system mass matrix. Similarity transformations of these operators are also studied. While the detailed development is done for the case of rigid-link multibody systems, the extension of these techniques to a broader class of systems (e.g. deformable links) are illustrated.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Jain, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Abhi.Jain@jpl.nasa.gov
FU National Institute of Health [RO1GM082896-01A2]; National Aeronautics
and Space Administration
FX The research described in this paper was performed at the Jet Propulsion
Laboratory (JPL), California Institute of Technology, under contract
with the National Aeronautics and Space Administration.5 This
project was also supported in part by Grant Number RO1GM082896-01A2 from
the National Institute of Health.
NR 37
TC 11
Z9 11
U1 2
U2 6
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1384-5640
J9 MULTIBODY SYST DYN
JI Multibody Syst. Dyn.
PD OCT
PY 2011
VL 26
IS 3
BP 307
EP 333
DI 10.1007/s11044-011-9266-7
PG 27
WC Mechanics
SC Mechanics
GA 790CP
UT WOS:000292566400005
PM 22102790
ER
PT J
AU Jain, A
AF Jain, Abhinandan
TI Graph theoretic foundations of multibody dynamics
SO MULTIBODY SYSTEM DYNAMICS
LA English
DT Article
DE Multibody systems; Graph theory; Algorithms
ID SPATIAL OPERATOR ALGEBRA; FORMULATION; MATRIX
AB This second part of a two part paper uses concepts from graph theory to obtain a deeper understanding of the mathematical foundations of multibody dynamics. The first part (Jain in Graph theoretic foundations of multibody dynamics. Part I. Structural properties, 2010) established the block-weighted adjacency (BWA) matrix structure of spatial operators associated with serial- and tree-topology multibody system dynamics, and introduced the notions of spatial kernel operators (SKO) and spatial propagation operators (SPO). This paper builds upon these connections to show that key analytical results and computational algorithms are a direct consequence of these structural properties and require minimal assumptions about the specific nature of the underlying multibody system. We formalize this notion by introducing the notion of SKO models for general tree-topology multibody systems. We show that key analytical results, including mass-matrix factorization, inversion, and decomposition hold for all SKO models. It is also shown that key low-order scatter/gather recursive computational algorithms follow directly from these abstract-level analytical results. Application examples to illustrate the concrete application of these general results are provided. The paper also describes a general recipe for developing SKO models. The abstract nature of SKO models allows for the application of these techniques to a very broad class of multibody systems.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Jain, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Abhi.Jain@jpl.nasa.gov
FU National Aeronautics and Space Administration; National Institute of
Health [RO1GM082896-01A2]
FX The research described in this paper was performed at the Jet Propulsion
Laboratory (JPL), California Institute of Technology, under contract
with the National Aeronautics and Space Administration.4 This
project was also supported in part by Grant Number RO1GM082896-01A2 from
the National Institute of Health.
NR 20
TC 6
Z9 6
U1 1
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1384-5640
J9 MULTIBODY SYST DYN
JI Multibody Syst. Dyn.
PD OCT
PY 2011
VL 26
IS 3
BP 335
EP 365
DI 10.1007/s11044-011-9267-6
PG 31
WC Mechanics
SC Mechanics
GA 790CP
UT WOS:000292566400006
PM 22102791
ER
PT J
AU Sawicki, JT
Storozhev, DL
Lekki, JD
AF Sawicki, Jerzy T.
Storozhev, Dmitry L.
Lekki, John D.
TI Exploration of NDE Properties of AMB Supported Rotors for Structural
Damage Detection
SO JOURNAL OF ENGINEERING FOR GAS TURBINES AND POWER-TRANSACTIONS OF THE
ASME
LA English
DT Article
ID CRACK
AB This paper addresses self-diagnostic properties of active magnetic bearing (AMB) supported rotors for online detection of the transverse crack on a rotating shaft. In addition to pure levitation, the rotor supporting bearing also serves as an actuator that transforms current signals additionally injected into the control loop into the superimposed specially selected excitation forces into the suspended rotor. These additional excitations induce combination frequencies in the rotor response, providing unique signatures for the presence of crack. The background of theoretical modeling, experimental, and computer simulation results for the AMB supported cracked rotor with self-diagnostic excitation forces are presented and discussed. [DOI: 10.1115/1.4002908]
C1 [Sawicki, Jerzy T.; Storozhev, Dmitry L.] Cleveland State Univ, Fenn Coll Engn, Ctr Rotating Machinery Dynam & Control RoMaDyC, Cleveland, OH 44115 USA.
[Lekki, John D.] NASA, Glenn Res Ctr, Brookpark, OH 44135 USA.
RP Sawicki, JT (reprint author), Cleveland State Univ, Fenn Coll Engn, Ctr Rotating Machinery Dynam & Control RoMaDyC, Cleveland, OH 44115 USA.
EM j.sawicki@csuohio.edu; dmitry.storozhev@ge.com; john.d.lekki@nasa.gov
FU NASA [NNX08AC31A]
FX This research has been funded by NASA's "Research Opportunities in
Aeronautics," Grant No. NNX08AC31A.
NR 15
TC 9
Z9 9
U1 0
U2 4
PU ASME-AMER SOC MECHANICAL ENG
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0742-4795
J9 J ENG GAS TURB POWER
JI J. Eng. Gas. Turbines Power-Trans. ASME
PD OCT
PY 2011
VL 133
IS 10
AR 102501
DI 10.1115/1.4002908
PG 9
WC Engineering, Mechanical
SC Engineering
GA 760SI
UT WOS:000290343700009
ER
PT J
AU Yue, Q
Kahn, BH
Fetzer, EJ
Teixeira, J
AF Yue, Qing
Kahn, Brian H.
Fetzer, Eric J.
Teixeira, Joao
TI Relationship between marine boundary layer clouds and lower tropospheric
stability observed by AIRS, CloudSat, and CALIOP
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ATMOSPHERIC INFRARED SOUNDER; GENERAL-CIRCULATION MODELS; SURFACE
OBSERVATIONS; A-TRAIN; TEMPERATURE; FEEDBACK; RETRIEVAL; COVER;
PRECIPITATION; AIRS/AMSU/HSB
AB Thirteen months of matched temperature and water vapor profiles from the Atmospheric Infrared Sounder (AIRS), collocated European Centre for Medium-Range Weather Forecasts (ECMWF) model analyses, National Centers for Environmental Prediction-National Center for Atmospheric Research reanalysis, and cloud profiles from the CloudSat and Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) instruments are investigated to quantify aspects of maritime boundary layer (MBL) clouds and their thermodynamic environment. This study highlights the strengths and limitations of this multisensor A-Train approach. The AIRS retrieval yield (percentage of high-quality temperature and water vapor profiles to the surface) over the oceans between 40 degrees S and 40 degrees N within MBL clouds is between 61% and 71% globally and is greater than 80%-90% throughout most of the subtropics. The lower tropospheric stability (LTS) and estimated inversion strength (EIS) are derived from AIRS temperature and water vapor profiles over the global oceans as well as from collocated ECMWF model analysis data. Positive values of EIS derived from AIRS well represent MBL conditions, demonstrating that AIRS contains quantitatively useful information with regard to relative changes in dynamic range of temperature and water vapor in the MBL. The relative magnitude and seasonality of LTS and EIS from the collocated satellite data set in stratocumulus regions are very similar to spatially and temporally collocated ECMWF model analyses, but differences are found between different subsampling criteria of reanalysis data. For coincident vertical profiles, the MBL in AIRS data shows a more smoothed structure than that of ECMWF. This multisensor investigation establishes a basis for using A-train observations to quantify elements of low cloud-climate feedback.
C1 [Yue, Qing; Kahn, Brian H.; Fetzer, Eric J.; Teixeira, Joao] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Yue, Q (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop T1714-113, Pasadena, CA 91109 USA.
EM qing.yue@jpl.nasa.gov
RI Yue, Qing/A-5776-2013; Yue, Qing/F-4619-2017
OI Yue, Qing/0000-0002-3559-6508
FU National Aeronautics and Space Administration; JPL
FX The research described in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. During
this project, Qing Yue, Brian H. Kahn, and Eric J. Fetzer were supported
by NASA's Making Earth Science Data Records for Use in Research
Environments (MEaSUREs) program, and Joao Teixeira was supported by the
JPL Internal Research and Technology Development Program. We acknowledge
the support of the AIRS Project at JPL. AIRS data were obtained through
the Goddard Earth Services Data and Information Services Center
(http://daac.gsfc.nasa.gov/). CloudSat data were obtained through the
CloudSat Data Processing Center
(http://www.cloudsat.cira.colostate.edu/). CALIPSO data were obtained
through the Atmospheric Sciences Data Center (ASDC) at NASA Langley
Research Center (http://eosweb.larc.nasa.gov/). The authors would like
to thank Hsi-Yen Ma, Jun-Lin Li, and Tristan L'Ecuyer for useful
feedback; Brian Wilson and Gerald Manipon for developing the AIRS and
CloudSat collocated data product; and the anonymous reviewers for useful
comments and suggestions. NCEP reanalysis data were provided by the
NOAA/OAR/ESRL PSD, Boulder, Colorado, from their Web site
(http://www.esrl.noaa.gov/psd/).
NR 53
TC 15
Z9 15
U1 0
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 30
PY 2011
VL 116
AR D18212
DI 10.1029/2011JD016136
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 828XG
UT WOS:000295537000008
ER
PT J
AU Dymond, KF
Watts, C
Coker, C
Budzien, SA
Bernhardt, PA
Kassim, N
Lazio, TJ
Weiler, K
Crane, PC
Ray, PS
Cohen, A
Clarke, T
Rickard, LJ
Taylor, GB
Schinzel, F
Pihlstrom, Y
Kuniyoshi, M
Close, S
Colestock, P
Myers, S
Datta, A
AF Dymond, K. F.
Watts, C.
Coker, C.
Budzien, S. A.
Bernhardt, P. A.
Kassim, N.
Lazio, T. J.
Weiler, K.
Crane, P. C.
Ray, P. S.
Cohen, A.
Clarke, T.
Rickard, L. J.
Taylor, G. B.
Schinzel, F.
Pihlstrom, Y.
Kuniyoshi, M.
Close, S.
Colestock, P.
Myers, S.
Datta, A.
TI A medium-scale traveling ionospheric disturbance observed from the
ground and from space
SO RADIO SCIENCE
LA English
DT Article
ID ATMOSPHERIC GRAVITY-WAVES; ELECTRON-DENSITY; RADIO INTERFEROMETER; LARGE
ARRAY; RADIOTELESCOPE; IRREGULARITIES; OXYGEN
AB We report ultraviolet optical observations from space of a Medium-Scale Traveling Ionospheric Disturbance (MSTID) made during the Combined Radio Interferometry and COSMIC Experiment in Tomography Campaign (CRICKET) held on September 15, 2007 at similar to 8:30 UT. The experiment used a Constellation Observing System for Meteorology, Ionosphere, and Climate (COSMIC also known as FORMOSAT-3) satellite in conjunction with the Very Large Array (VLA) radio telescope, located near Socorro, NM, to study the ionosphere from the global scale down to the regional scale while the TIDs propagated through it. The COSMIC/FORMOSAT-3 satellite measured the F region electron density both horizontally and with altitude while the VLA measured the directions and speeds of the TIDs. These observations provide new information on this poorly understood class of TID and demonstrate the possibility of studying MSTIDs using space-based optical instruments.
C1 [Dymond, K. F.; Coker, C.; Budzien, S. A.; Ray, P. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Bernhardt, P. A.] USN, Res Lab, Div Plasma Phys, Washington, DC 20375 USA.
[Kassim, N.; Lazio, T. J.; Weiler, K.; Crane, P. C.; Cohen, A.; Clarke, T.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA.
[Close, S.] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA.
[Cohen, A.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Close, S.; Colestock, P.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Datta, A.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Schinzel, F.; Kuniyoshi, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Lazio, T. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Myers, S.; Datta, A.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Rickard, L. J.; Taylor, G. B.; Schinzel, F.; Pihlstrom, Y.; Kuniyoshi, M.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
[Watts, C.] ITER, Div Diagnost, F-13115 St Paul Les Durance, France.
[Watts, C.] Univ New Mexico, Dept Elect & Comp Engn, Albuquerque, NM 87131 USA.
RP Dymond, KF (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
EM kenneth.dymond@nrl.navy.mil
OI Ray, Paul/0000-0002-5297-5278
FU Office of Naval Research; NRAO [AM-909]
FX This work was supported in part by the Office of Naval Research. The
National Radio Astronomy Observatory (NRAO) is a facility of the
National Science Foundation operated under cooperative agreement by
Associated Universities, Inc. The VLA observations were funded under
NRAO proposal AM-909. We thank the NRAO staff at the VLA and the CF3
satellite operators in Taiwan for their assistance during the campaign.
The GOX and TIP data used in this study were provided by the University
Corporation for Atmospheric Research and the National Space Office
(NSPO) of the Republic of China (Taiwan).
NR 27
TC 6
Z9 6
U1 0
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0048-6604
EI 1944-799X
J9 RADIO SCI
JI Radio Sci.
PD SEP 30
PY 2011
VL 46
AR RS5010
DI 10.1029/2010RS004535
PG 7
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
GA 829UM
UT WOS:000295609800001
ER
PT J
AU LeGrande, AN
Schmidt, GA
AF LeGrande, Allegra N.
Schmidt, Gavin A.
TI Water isotopologues as a quantitative paleosalinity proxy
SO PALEOCEANOGRAPHY
LA English
DT Article
ID LAST GLACIAL MAXIMUM; OXYGEN ISOTOPES; SURFACE-TEMPERATURE; TROPICAL
PACIFIC; SALINITY; OCEAN; CIRCULATION; ATLANTIC; CLIMATE; PRECIPITATION
AB Paleosalinity reconstructions are a goal of paleoceanographic study because of their potential to provide insight into past ocean circulation. While temperature reconstructions have been assessed by using multiple independent proxies, the skill of existing salinity reconstructions remains poorly quantified. We examine the applicability of two different approaches using a set of coupled water isotope-enabled general circulation model experiments as a numerical analog for the real climate system. These simulations for the Holocene, at roughly 1000 year time steps, explicitly track variability in both the water isotopologues and salinity. Our simulations suggest that quantitative reconstructions of past salinity variability based solely on inferred delta O-18(sw) variability have very large errors and uncertainties. However, we find that paired delta O-18(sw) and delta D variability (from combining biomarker and calcite proxies) holds promise for providing better quantitative estimates of salinity variability.
C1 [LeGrande, Allegra N.; Schmidt, Gavin A.] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[LeGrande, Allegra N.; Schmidt, Gavin A.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
RP LeGrande, AN (reprint author), Columbia Univ, NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM legrande@giss.nasa.gov
RI Schmidt, Gavin/D-4427-2012; LeGrande, Allegra/D-8920-2012
OI Schmidt, Gavin/0000-0002-2258-0486; LeGrande,
Allegra/0000-0002-5295-0062
FU NSF [ATM 07-53868]; NOAA [NA10OAR4310126]
FX We would like to thank NASA Modeling, Analysis, and Prediction Program
for assistance with climate modeling and NASA GISS for institutional
support. A.N.L. was supported by NSF ATM 07-53868 and NOAA
NA10OAR4310126.
NR 40
TC 20
Z9 20
U1 3
U2 17
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0883-8305
EI 1944-9186
J9 PALEOCEANOGRAPHY
JI Paleoceanography
PD SEP 30
PY 2011
VL 26
AR PA3225
DI 10.1029/2010PA002043
PG 10
WC Geosciences, Multidisciplinary; Oceanography; Paleontology
SC Geology; Oceanography; Paleontology
GA 828TC
UT WOS:000295524700001
ER
PT J
AU Anderson, BJ
Johnson, CL
Korth, H
Purucker, ME
Winslow, RM
Slavin, JA
Solomon, SC
McNutt, RL
Raines, JM
Zurbuchen, TH
AF Anderson, Brian J.
Johnson, Catherine L.
Korth, Haje
Purucker, Michael E.
Winslow, Reka M.
Slavin, James A.
Solomon, Sean C.
McNutt, Ralph L., Jr.
Raines, Jim M.
Zurbuchen, Thomas H.
TI The Global Magnetic Field of Mercury from MESSENGER Orbital Observations
SO SCIENCE
LA English
DT Article
ID MISSION; DYNAMO
AB Magnetometer data acquired by the MESSENGER spacecraft in orbit about Mercury permit the separation of internal and external magnetic field contributions. The global planetary field is represented as a southward-directed, spin-aligned, offset dipole centered on the spin axis. Positions where the cylindrical radial magnetic field component vanishes were used to map the magnetic equator and reveal an offset of 484 +/- 11 kilometers northward of the geographic equator. The magnetic axis is tilted by less than 3 degrees from the rotation axis. A magnetopause and tail-current model was defined by using 332 magnetopause crossing locations. Residuals of the net external and offset-dipole fields from observations north of 30 degrees N yield a best-fit planetary moment of 195 +/- 10 nanotesla-R-M(3), where R-M is Mercury's mean radius.
C1 [Anderson, Brian J.; Korth, Haje; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Johnson, Catherine L.; Winslow, Reka M.] Univ British Columbia, Vancouver, BC V6T 1Z4, Canada.
[Johnson, Catherine L.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Purucker, Michael E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Slavin, James A.; Raines, Jim M.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
RP Anderson, BJ (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM brian.anderson@jhuapl.edu
RI Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; McNutt,
Ralph/E-8006-2010
OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166
FU NASA; MESSENGER Participating Scientist Program; Natural Sciences and
Engineering Research Council of Canada
FX We thank the MESSENGER operations and engineering teams. The MESSENGER
mission is supported by the NASA Discovery Program and the MESSENGER
Participating Scientist Program. C.L.J. and R. M. W. acknowledge support
from the Natural Sciences and Engineering Research Council of Canada.
NR 19
TC 108
Z9 108
U1 1
U2 23
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD SEP 30
PY 2011
VL 333
IS 6051
BP 1859
EP 1862
DI 10.1126/science.1211001
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 826PJ
UT WOS:000295365800047
PM 21960627
ER
PT J
AU Zurbuchen, TH
Raines, JM
Slavin, JA
Gershman, DJ
Gilbert, JA
Gloeckler, G
Anderson, BJ
Baker, DN
Korth, H
Krimigis, SM
Sarantos, M
Schriver, D
McNutt, RL
Solomon, SC
AF Zurbuchen, Thomas H.
Raines, Jim M.
Slavin, James A.
Gershman, Daniel J.
Gilbert, Jason A.
Gloeckler, George
Anderson, Brian J.
Baker, Daniel N.
Korth, Haje
Krimigis, Stamatios M.
Sarantos, Menelaos
Schriver, David
McNutt, Ralph L., Jr.
Solomon, Sean C.
TI MESSENGER Observations of the Spatial Distribution of Planetary Ions
Near Mercury
SO SCIENCE
LA English
DT Article
ID MAGNETOSPHERE; EXOSPHERE; PLASMA
AB Global measurements by MESSENGER of the fluxes of heavy ions at Mercury, particularly sodium (Na(+)) and oxygen (O(+)), exhibit distinct maxima in the northern magnetic-cusp region, indicating that polar regions are important sources of Mercury's ionized exosphere, presumably through solar-wind sputtering near the poles. The observed fluxes of helium (He(+)) are more evenly distributed, indicating a more uniform source such as that expected from evaporation from a helium-saturated surface. In some regions near Mercury, especially the nightside equatorial region, the Na(+) pressure can be a substantial fraction of the proton pressure.
C1 [Zurbuchen, Thomas H.; Raines, Jim M.; Slavin, James A.; Gershman, Daniel J.; Gilbert, Jason A.; Gloeckler, George] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Slavin, James A.; Sarantos, Menelaos] NASA Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Anderson, Brian J.; Korth, Haje; Krimigis, Stamatios M.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Baker, Daniel N.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA.
[Krimigis, Stamatios M.] Acad Athens, Off Space Res & Technol, Athens 11527, Greece.
[Sarantos, Menelaos] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
[Schriver, David] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
RP Zurbuchen, TH (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM thomasz@umich.edu
RI Anderson, Brian/I-8615-2012; Gilbert, Jason/I-9020-2012; Slavin,
James/H-3170-2012; Sarantos, Menelaos/H-8136-2013; McNutt,
Ralph/E-8006-2010
OI Gilbert, Jason/0000-0002-3182-7014; Slavin, James/0000-0002-9206-724X;
McNutt, Ralph/0000-0002-4722-9166
FU NASA [NAS5-97271, NASW-00002]
FX The MESSENGER project is supported by the NASA Discovery Program under
contracts NAS5-97271 to The Johns Hopkins University Applied Physics
Laboratory and NASW-00002 to the Carnegie Institution of Washington.
NR 17
TC 48
Z9 48
U1 2
U2 8
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 SEP 30
PY 2011
VL 333
IS 6051
BP 1862
EP 1865
DI 10.1126/science.1211302
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 826PJ
UT WOS:000295365800048
PM 21960628
ER
PT J
AU Ho, GC
Krimigis, SM
Gold, RE
Baker, DN
Slavin, JA
Anderson, BJ
Korth, H
Starr, RD
Lawrence, DJ
McNutt, RL
Solomon, SC
AF Ho, George C.
Krimigis, Stamatios M.
Gold, Robert E.
Baker, Daniel N.
Slavin, James A.
Anderson, Brian J.
Korth, Haje
Starr, Richard D.
Lawrence, David J.
McNutt, Ralph L., Jr.
Solomon, Sean C.
TI MESSENGER Observations of Transient Bursts of Energetic Electrons in
Mercury's Magnetosphere
SO SCIENCE
LA English
DT Article
ID MAGNETIC-FIELD; PARTICLE; SPACECRAFT
AB The MESSENGER spacecraft began detecting energetic electrons with energies greater than 30 kilo-electron volts (keV) shortly after its insertion into orbit about Mercury. In contrast, no energetic protons were observed. The energetic electrons arrive as bursts lasting from seconds to hours and are most intense close to the planet, distributed in latitude from the equator to the north pole, and present at most local times. Energies can exceed 200 keV but often exhibit cutoffs near 100 keV. Angular distributions of the electrons about the magnetic field suggest that they do not execute complete drift paths around the planet. This set of characteristics demonstrates that Mercury's weak magnetic field does not support Van Allen-type radiation belts, unlike all other planets in the solar system with internal magnetic fields.
C1 [Ho, George C.; Krimigis, Stamatios M.; Gold, Robert E.; Anderson, Brian J.; Korth, Haje; Lawrence, David J.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Krimigis, Stamatios M.] Acad Athens, Off Space Res & Technol, Athens 11527, Greece.
[Baker, Daniel N.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA.
[Slavin, James A.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Slavin, James A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
RP Ho, GC (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM george.ho@jhuapl.edu
RI Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; McNutt,
Ralph/E-8006-2010; Ho, George/G-3650-2015; Lawrence, David/E-7463-2015
OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166;
Ho, George/0000-0003-1093-2066; Lawrence, David/0000-0002-7696-6667
FU NASA [NAS5-97271, NASW-00002]
FX We thank the MESSENGER team for the development, cruise, orbit
insertion, and Mercury orbital operations of the MESSENGER spacecraft.
G. C. H. thanks M. Johnson, L. Brown, and J. Vandegriff for graphics
support. The NASA Discovery Program under contract NAS5-97271 to The
Johns Hopkins University Applied Physics Laboratory and contract
NASW-00002 to the Carnegie Institution of Washington supports the
MESSENGER mission to Mercury. MESSENGER data are available from NASA's
Planetary Data System archive.
NR 18
TC 17
Z9 17
U1 1
U2 6
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 SEP 30
PY 2011
VL 333
IS 6051
BP 1865
EP 1868
DI 10.1126/science.1211141
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 826PJ
UT WOS:000295365800049
PM 21960629
ER
PT J
AU Hardiman, SC
Butchart, N
Charlton-Perez, AJ
Shaw, TA
Akiyoshi, H
Baumgaertner, A
Bekki, S
Braesicke, P
Chipperfield, M
Dameris, M
Garcia, RR
Michou, M
Pawson, S
Rozanov, E
Shibata, K
AF Hardiman, Steven C.
Butchart, Neal
Charlton-Perez, Andrew J.
Shaw, Tiffany A.
Akiyoshi, Hideharu
Baumgaertner, Andreas
Bekki, Slimane
Braesicke, Peter
Chipperfield, Martyn
Dameris, Martin
Garcia, Rolando R.
Michou, Martine
Pawson, Steven
Rozanov, Eugene
Shibata, Kiyotaka
TI Improved predictability of the troposphere using stratospheric final
warmings
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID QUASI-BIENNIAL OSCILLATION; DATA ASSIMILATION SYSTEM; INTERANNUAL
VARIABILITY; DOWNWARD PROPAGATION; NORTHERN-HEMISPHERE; PLANETARY-WAVES;
CIRCULATION; REANALYSIS; WEATHER; EVENTS
AB The final warming of the stratospheric polar vortex at the end of northern hemisphere winter is examined in ECMWF ERA-Interim reanalysis data and an ensemble of chemistry climate models, using 20 years of data from each. In some years the final warming is found to occur first in the mid-stratosphere, and in others to occur first in the upper stratosphere. The strength of the winter stratospheric polar vortex, refraction of planetary waves, and the altitudes at which the planetary waves break in the northern extratropics lead to this difference in the vertical profile of the final warming. Years in which the final warming occurs first in the mid-stratosphere show, on average, a more negative NAO pattern in April mean sea level pressure than years in which the warming occurs first in the upper stratosphere. Thus, in the northern hemisphere, additional predictive skill of tropospheric climate in April can be gained from a knowledge of the vertical profile of the stratospheric final warming.
C1 [Hardiman, Steven C.; Butchart, Neal] Met Off Hadley Ctr, Exeter EX1 3PB, Devon, England.
[Akiyoshi, Hideharu] Natl Inst Environm Studies, Div Atmospher Environm, Tsukuba, Ibaraki 3058506, Japan.
[Baumgaertner, Andreas] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Bekki, Slimane] UPMC, UVSQ, LATMOS IPSL, CNRS INSU, F-75252 Paris 05, France.
[Braesicke, Peter] Univ Cambridge, Dept Chem, Natl Ctr Atmospher Sci, Cambridge CB2 1EW, England.
[Charlton-Perez, Andrew J.] Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England.
[Chipperfield, Martyn] Univ Leeds, Sch Earth & Environm, Inst Climate & Atmospher Sci, Leeds LS2 9JT, W Yorkshire, England.
[Dameris, Martin] Deutsch Zentrum Luft & Raumfahrt, Inst Atmospher Phys, Oberpfaffenhofen, Germany.
[Garcia, Rolando R.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA.
[Michou, Martine] CNRS, GAME CNRM, F-31057 Toulouse, France.
[Pawson, Steven] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Rozanov, Eugene] World Radiat Ctr, Phys Meteorol Observ Davos, CH-7260 Davos, Switzerland.
[Shaw, Tiffany A.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA.
[Shibata, Kiyotaka] Meteorol Res Inst, Atmospher Environm & Appl Meteorol Res Dept, Tsukuba, Ibaraki 3050052, Japan.
[Rozanov, Eugene] Swiss Fed Inst Technol, Zurich, Switzerland.
RP Hardiman, SC (reprint author), Met Off Hadley Ctr, Exeter EX1 3PB, Devon, England.
EM steven.hardiman@metoffice.gov.uk
RI Rozanov, Eugene/A-9857-2012; Baumgaertner, Andreas/C-4830-2011;
Chipperfield, Martyn/H-6359-2013; bekki, slimane/J-7221-2015; Braesicke,
Peter/D-8330-2016; Pawson, Steven/I-1865-2014
OI Rozanov, Eugene/0000-0003-0479-4488; Baumgaertner,
Andreas/0000-0002-4740-0701; Charlton-Perez, Andrew/0000-0001-8179-6220;
Chipperfield, Martyn/0000-0002-6803-4149; bekki,
slimane/0000-0002-5538-0800; Braesicke, Peter/0000-0003-1423-0619;
Pawson, Steven/0000-0003-0200-717X
FU Joint DECC/Defra Met Office Hadley Centre [GA01101]; Ministry of the
Environment of Japan [A-071]
FX The work of SCH and NB was supported by the Joint DECC/Defra Met Office
Hadley Centre Climate Programme (GA01101). The authors would like to
thank Steven Rumbold for several useful discussions during the course of
this work, and William Seviour for producing the planetary wave flux
diagnostics from ERA-Interim data. ECMWF ERA-Interim data used in this
study have been provided by ECMWF, ERA-40 data used in this study have
been obtained from the ECMWF data server, and NCEP Reanalysis data was
provided by the NOAA/OAR/ESRL PSD, Boulder, Colorado, USA, from their
Web site at http://www.esrl.noaa.gov/psd/. The authors also acknowledge
John Austin for providing the GFDL AMTRAC3 model data, the CCMVal
Activity for WCRP's SPARC (Stratospheric Processes and their Role in
Climate) project for organizing and coordinating the CCM data analysis
activity, and the British Atmospheric Data Center (BADC) for collecting
and archiving the CCMVal model output. The CCSRNIES simulations in the
CCMVal were completed with the super computer at CGER, NIES and
supported by the Global Environment Research Fund of the Ministry of the
Environment of Japan (A-071).
NR 34
TC 19
Z9 21
U1 1
U2 23
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 29
PY 2011
VL 116
AR D18113
DI 10.1029/2011JD015914
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 828XF
UT WOS:000295536900003
ER
PT J
AU Uritsky, VM
Slavin, JA
Khazanov, GV
Donovan, EF
Boardsen, SA
Anderson, BJ
Korth, H
AF Uritsky, V. M.
Slavin, J. A.
Khazanov, G. V.
Donovan, E. F.
Boardsen, S. A.
Anderson, B. J.
Korth, H.
TI Kinetic-scale magnetic turbulence and finite Larmor radius effects at
Mercury
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID SOLAR-WIND TURBULENCE; MESSENGERS 1ST FLYBY; PLASMA SHEET;
MAGNETOHYDRODYNAMIC TURBULENCE; HERMEAN MAGNETOSPHERE; ION FLOW;
RECONNECTION; MAGNETOTAIL; MODEL; WAVES
AB We use a nonstationary generalization of the higher-order structure function technique to investigate statistical properties of the magnetic field fluctuations recorded by MESSENGER spacecraft during its first flyby (01/14/2008) through the near-Mercury space environment, with the emphasis on key boundary regions participating in the solar wind - magnetosphere interaction. Our analysis shows, for the first time, that kinetic-scale fluctuations play a significant role in the Mercury's magnetosphere up to the largest resolvable timescale (similar to 20 s) imposed by the signal nonstationarity, suggesting that turbulence at this planet is largely controlled by finite Larmor radius effects. In particular, we report the presence of a highly turbulent and extended foreshock system filled with packets of ULF oscillations, broad-band intermittent fluctuations in the magnetosheath, ion-kinetic turbulence in the central plasma sheet of Mercury's magnetotail, and kinetic-scale fluctuations in the inner current sheet encountered at the outbound (dawn-side) magnetopause. Overall, our measurements indicate that the Hermean magnetosphere, as well as the surrounding region, are strongly affected by non-MHD effects introduced by finite sizes of cyclotron orbits of the constituting ion species. Physical mechanisms of these effects and their potentially critical impact on the structure and dynamics of Mercury's magnetic field remain to be understood.
C1 [Uritsky, V. M.; Donovan, E. F.] Univ Calgary, Dept Phys & Astron, Calgary, AB T3A 0P4, Canada.
[Uritsky, V. M.; Slavin, J. A.; Khazanov, G. V.; Boardsen, S. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Anderson, B. J.; Korth, H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Uritsky, VM (reprint author), Univ Calgary, Dept Phys & Astron, SB605,2500 Univ Dr NW, Calgary, AB T3A 0P4, Canada.
EM uritsky@ucalgary.ca
RI Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; feggans,
john/F-5370-2012;
OI Slavin, James/0000-0002-9206-724X; Donovan, Eric/0000-0002-8557-4155
NR 84
TC 19
Z9 19
U1 2
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP 29
PY 2011
VL 116
AR A09236
DI 10.1029/2011JA016744
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 828VO
UT WOS:000295532000002
ER
PT J
AU Antoci, V
Handler, G
Campante, TL
Thygesen, AO
Moya, A
Kallinger, T
Stello, D
Grigahcene, A
Kjeldsen, H
Bedding, TR
Luftinger, T
Christensen-Dalsgaard, J
Catanzaro, G
Frasca, A
De Cat, P
Uytterhoeven, K
Bruntt, H
Houdek, G
Kurtz, DW
Lenz, P
Kaiser, A
Van Cleve, J
Allen, C
Clarke, BD
AF Antoci, V.
Handler, G.
Campante, T. L.
Thygesen, A. O.
Moya, A.
Kallinger, T.
Stello, D.
Grigahcene, A.
Kjeldsen, H.
Bedding, T. R.
Lueftinger, T.
Christensen-Dalsgaard, J.
Catanzaro, G.
Frasca, A.
De Cat, P.
Uytterhoeven, K.
Bruntt, H.
Houdek, G.
Kurtz, D. W.
Lenz, P.
Kaiser, A.
Van Cleve, J.
Allen, C.
Clarke, B. D.
TI The excitation of solar-like oscillations in a delta Sct star by
efficient envelope convection
SO NATURE
LA English
DT Article
ID MAIN-SEQUENCE STARS; STELLAR OSCILLATIONS; KEPLER-MISSION; SCUTI STARS;
AM STARS; P MODES; ASTEROSEISMOLOGY; GRANULATION; AMPLITUDES; VARIABLES
AB Delta Scuti (delta Sct)(1) stars are opacity-driven pulsators with masses of 1.5-2.5 M(circle dot), their pulsations resulting from the varying ionization of helium. In less massive stars(2) such as the Sun, convection transports mass and energy through the outer 30 per cent of the star and excites a rich spectrum of resonant acoustic modes. Based on the solar example, with no firm theoretical basis, models predict that the convective envelope in delta Sct stars extends only about 1 per cent of the radius(3), but with sufficient energy to excite solar-like oscillations(4,5). This was not observed before the Kepler mission(6), so the presence of a convective envelope in the models has been questioned. Here we report the detection of solar-like oscillations in the delta Sct star HD187547, implying that surface convection operates efficiently in stars about twice as massive as the Sun, as the ad hoc models predicted.
C1 [Antoci, V.; Handler, G.; Kallinger, T.; Lueftinger, T.; Houdek, G.; Kaiser, A.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Handler, G.; Lenz, P.] Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Campante, T. L.; Grigahcene, A.] Univ Porto, Dept Fis Astron, Ctr Astrofis, Fac Ciencias, P-4150762 Oporto, Portugal.
[Campante, T. L.; Kjeldsen, H.; Christensen-Dalsgaard, J.; Bruntt, H.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Thygesen, A. O.] Nord Opt Telescope, E-38700 Santa Cruz De La Palma, Santa Cruz De T, Spain.
[Moya, A.] Consejo Super Invest Cient, Dept Astrofis, Ctr Astrobiol, Inst Nacl Tecn Aeroesp, E-28691 Madrid, Spain.
[Kallinger, T.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Kallinger, T.] Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Stello, D.; Bedding, T. R.] Univ Sydney, Sydney Inst Astron SIfA, Sch Phys, Sydney, NSW 2006, Australia.
[Catanzaro, G.; Frasca, A.] Osserv Astrofis Catania, Ist Nazl Astrofis, I-95123 Catania, Italy.
[De Cat, P.] Royal Observ Belgium, B-1180 Brussels, Belgium.
[Uytterhoeven, K.] Univ Paris Diderot, Ctr Etud Saclay, Inst Rech Lois Fondament,Commissariat Energia Ato, Serv Astrophys,CEA DSM CNRS,Lab AIM, F-79104 Gif Sur Yvette, France.
[Uytterhoeven, K.] Kiepenheuer Inst Sonnenphys, D-79104 Freiburg, Germany.
[Uytterhoeven, K.] Inst Astrofis Canarias, Tenerife 38200, Spain.
[Uytterhoeven, K.] Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain.
[Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Van Cleve, J.; Clarke, B. D.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Allen, C.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
RP Antoci, V (reprint author), Univ Vienna, Inst Astron, Turkenschanzstr 18, A-1180 Vienna, Austria.
EM victoria.antoci@univie.ac.at
OI Kallinger, Thomas/0000-0003-3627-2561; Catanzaro,
Giovanni/0000-0003-4337-8612
FU Austrian Fonds zur Forderung der wissenschaftlichen Forschung;
AstroMadrid; Spanish grants; Australian Reseach Council; Austrian Agency
for International Cooperation in Education and Research; Deutsche
Forschungsgemeinschaft; NASA's Science Mission Directorate
FX We thank the entire Kepler team, without whom these results would not be
possible. V. A., G. Ha. and G. Ho. were supported by the Austrian Fonds
zur Forderung der wissenschaftlichen Forschung. V. A. also thanks L.
Fossati for his help. A. M. acknowledges the funding of AstroMadrid, who
was also supported by Spanish grants. T. R. B. and D. S. acknowledge
support from the Australian Reseach Council. T. L was supported by the
Austrian Agency for International Cooperation in Education and Research.
K. U. acknowledges financial support from the Deutsche
Forschungsgemeinschaft. Funding for this Discovery mission is provided
by NASA's Science Mission Directorate.
NR 30
TC 34
Z9 34
U1 0
U2 10
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD SEP 29
PY 2011
VL 477
IS 7366
BP 570
EP 573
DI 10.1038/nature10389
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 825ZM
UT WOS:000295320900035
PM 21918514
ER
PT J
AU Grieman, FJ
Noell, AC
Davis-Van Atta, C
Okumura, M
Sander, SP
AF Grieman, Fred J.
Noell, Aaron C.
Davis-Van Atta, Casey
Okumura, Mitchio
Sander, Stanley P.
TI Determination of Equilibrium Constants for the Reaction between Acetone
and HO2 Using Infrared Kinetic Spectroscopy
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID GAS-PHASE; THEORETICAL CHARACTERIZATION; GASEOUS FORMALDEHYDE;
FLASH-PHOTOLYSIS; AB-INITIO; MECHANISM; RADICALS; OXIDATION;
PHOTOOXIDATION; TROPOSPHERE
AB The reaction between the hydroperoxy radical, HO2, and acetone may play an important role in acetone removal and the budget of HOx radicals in the upper troposphere. We measured the equilibrium constants of this reaction over the temperature range of 215-272 K at an overall pressure of 100 Torr using a flow tube apparatus and laser flash photolysis to produce HO2. The HO2 concentration was monitored as a function of time by near-IR diode laser wavelength modulation spectroscopy. The resulting [HO2] decay curves in the presence of acetone are characterized by an immediate decrease in initial [HO2] followed by subsequent decay. These curves are interpreted as a rapid (<100 mu s) equilibrium reaction between acetone and the HO2 radical that occurs on time scales faster than the time resolution of the apparatus, followed by subsequent reactions. This separation of time scales between the initial equilibrium and ensuing reactions enabled the determination of the equilibrium constant with values ranging from 4.0 x 10(-16) to 7.7 x 10(-48) cm(3) molecule(-1) for T = 215-272 K Thermodynamic parameters for the reaction determined from a second-law fit of our van't Hoff plot were Delta H-r degrees(245) = -35.4 +/- 2.0 kJ mol(-1) and Delta S-r degrees(245) = -88.2 +/- 8.5 J mol(-1) K-1. Recent ab initio calculations predict that the reaction proceeds through a prereactive hydrogen-bonded molecular complex (HO2-acetone) with subsequent isomerization to a hydroxyperoxy radical, 2-hydroxyisopropylperoxy (2-HIPP). The calculations differ greatly in the energetics of the complex and the peroxy radical, as well as the transition state for isomerization, leading to significant differences in their predictions of the extent of this reaction at tropospheric temperatures. The current results are consistent with equilibrium formation of the hydrogen-bonded molecular complex on a short time scale (100 mu s). Formation of the hydrogen-bonded complex will have a negligible impact on the atmosphere. However, the complex could subsequently isomerize to form the 2-HIPP radical on longer time scales. Further experimental studies are needed to assess the ultimate impact of the reaction of HO2 and acetone on the atmosphere.
C1 [Grieman, Fred J.; Noell, Aaron C.; Sander, Stanley P.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Noell, Aaron C.; Okumura, Mitchio] CALTECH, Arthur Amos Noyes Lab Chem Phys, Pasadena, CA 91125 USA.
[Grieman, Fred J.; Davis-Van Atta, Casey] Pomona Coll, Seaver Chem Lab, Claremont, CA 91711 USA.
RP Grieman, FJ (reprint author), CALTECH, NASA, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM fgrieman@pomona.edu; mo@caltech.edu; stanley.p.sander@jpl.nasa.gov
RI Okumura, Mitchio/I-3326-2013
OI Okumura, Mitchio/0000-0001-6874-1137
FU National Aeronautics and Space Administration (NASA); Pomona College
FX This research was carried out by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration (NASA). This work was supported by
the NASA Upper Atmosphere Research and Tropospheric Chemistry Programs
and the NASA Graduate Student Research Program (GSRP). This research was
supported by an appointment of Fred Grieman to the NASA Postdoctoral
Program at the Jet Propulsion Laboratory, administered by Oak Ridge
Associated Universities through a contract with NASA and a SURP grant
from Pomona College for CD.-V. A. We acknowledge the vital technical
support of Dave Natzic. Government sponsorship is acknowledged.
NR 41
TC 9
Z9 9
U1 1
U2 36
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD SEP 29
PY 2011
VL 115
IS 38
BP 10527
EP 10538
DI 10.1021/jp205347s
PG 12
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 822OP
UT WOS:000295058300017
PM 21827196
ER
PT J
AU Stolc, V
Shmygelska, A
Griko, Y
AF Stolc, Viktor
Shmygelska, Alena
Griko, Yuri
TI Adaptation of Organisms by Resonance of RNA Transcription with the
Cellular Redox Cycle
SO PLOS ONE
LA English
DT Article
ID YEAST METABOLIC CYCLE; IMBALANCED DNTP POOLS; SACCHAROMYCES-CEREVISIAE;
OXIDATIVE STRESS; DNA-DAMAGE; ESCHERICHIA-COLI; FUNCTIONAL-STATE; CODON
USAGE; MECHANISM; MUTATION
AB Sequence variation in organisms differs across the genome and the majority of mutations are caused by oxidation, yet its origin is not fully understood. It has also been shown that the reduction-oxidation reaction cycle is the fundamental biochemical cycle that coordinates the timing of all biochemical processes in the cell, including energy production, DNA replication, and RNA transcription. We show that the temporal resonance of transcriptome biosynthesis with the oscillating binary state of the reduction-oxidation reaction cycle serves as a basis for non-random sequence variation at specific genome-wide coordinates that change faster than by accumulation of chance mutations. This work demonstrates evidence for a universal, persistent and iterative feedback mechanism between the environment and heredity, whereby acquired variation between cell divisions can outweigh inherited variation.
C1 [Stolc, Viktor; Griko, Yuri] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Shmygelska, Alena] Carnegie Mellon Univ, Moffett Field, CA USA.
RP Stolc, V (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM vstolc@mail.arc.nasa.gov
FU NASA [NNX08BA52A]
FX This work was supported by the NASA Human Research Program, and NASA
contract to the Carnegie Mellon University Silicon Valley #NNX08BA52A.
The funders had no role in study design, data collection and analysis,
decision to publish, or preparation of the manuscript.
NR 60
TC 0
Z9 0
U1 0
U2 2
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD SEP 28
PY 2011
VL 6
IS 9
AR e25270
DI 10.1371/journal.pone.0025270
PG 12
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 834CT
UT WOS:000295936900044
PM 21980411
ER
PT J
AU Klenzing, JH
Rowland, DE
Pfaff, RF
Le, G
Freudenreich, H
Haaser, RA
Burrell, AG
Stoneback, RA
Coley, WR
Heelis, RA
AF Klenzing, J. H.
Rowland, D. E.
Pfaff, R. F.
Le, G.
Freudenreich, H.
Haaser, R. A.
Burrell, A. G.
Stoneback, R. A.
Coley, W. R.
Heelis, R. A.
TI Observations of low-latitude plasma density enhancements and their
associated plasma drifts
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID EQUATORIAL-SPREAD-F; HINOTORI SATELLITE; IMPEDANCE PROBE; DMSP F-15;
IRREGULARITIES; IONOSPHERE; KOMPSAT-1; REGION; BLOBS; BOARD
AB Plasma density structures are frequently encountered in the nighttime low-latitude ionosphere by probes on the Communication/Navigation Outage Forecasting System (C/NOFS) satellite. Of particular interest to us here are plasma density enhancements, which are typically observed +/- 15 degrees away from the magnetic equator. The low inclination of the C/NOFS satellite offers an unprecedented opportunity to examine these structures and their associated electric fields and plasma velocities, including their field-aligned components, along an east-west trajectory. Among other observations, the data reveal a clear asymmetry in the velocity structure within and around these density enhancements. Previous data have shown that the peak perturbation in drift velocity associated with a density enhancement occurs simultaneously both perpendicular and parallel to the magnetic field, while the results in this paper show that the peak perturbation in parallel flow typically occurs 25-100 km to the east of the peak perpendicular flow. The absence of such a longitudinal offset in previous observations suggests that multiple physical mechanisms may be responsible for creating plasma density enhancements as observed by satellite-borne instrumentation.
C1 [Klenzing, J. H.; Rowland, D. E.; Pfaff, R. F.; Freudenreich, H.] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Haaser, R. A.; Burrell, A. G.; Stoneback, R. A.; Coley, W. R.] Univ Texas Dallas, Ctr Space Sci, Richardson, TX 75083 USA.
RP Klenzing, JH (reprint author), NASA, Space Weather Lab, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA.
EM jeffrey.klenzing@nasa.gov
RI Le, Guan/C-9524-2012; Klenzing, Jeff/E-2406-2011; Rowland,
Douglas/F-5589-2012; Pfaff, Robert/F-5703-2012;
OI Le, Guan/0000-0002-9504-5214; Stoneback, Russell/0000-0001-7216-4336;
Klenzing, Jeff/0000-0001-8321-6074; Rowland,
Douglas/0000-0003-0948-6257; Pfaff, Robert/0000-0002-4881-9715; Burrell,
Angeline/0000-0001-8875-9326; Coley, William Robin/0000-0003-2047-0002
FU NASA [NAS5-01068]; USAF
FX J. H. Klenzing is supported by an appointment to the NASA Postdoctoral
Program at Goddard Space Flight Center, administered by Oak Ridge
Associated Universities through a contract withNASA. J. H. Klenzing
would like to thank C.-S. Huang for helpful discussions regarding the
electric field structure inside and around plasma density depletions.
The Communication/Navigation Outage Forecast System (C/NOFS) mission,
conceived and developed by the Air Force Research Laboratory, is
sponsored and executed by the USAF Space Test Program. The work at the
University of Texas at Dallas is supported by NASA grant NAS5-01068.
NR 29
TC 12
Z9 12
U1 0
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP 28
PY 2011
VL 116
AR A09324
DI 10.1029/2011JA016711
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 828VN
UT WOS:000295531800008
ER
PT J
AU Verkhoglyadova, OP
Tsurutani, BT
Mannucci, AJ
Mlynczak, MG
Hunt, LA
Komjathy, A
Runge, T
AF Verkhoglyadova, O. P.
Tsurutani, B. T.
Mannucci, A. J.
Mlynczak, M. G.
Hunt, L. A.
Komjathy, A.
Runge, T.
TI Ionospheric VTEC and thermospheric infrared emission dynamics during
corotating interaction region and high-speed stream intervals at solar
minimum: 25 March to 26 April 2008
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID LOW-LATITUDE IONOSPHERE; DISTURBANCE DYNAMO; ELECTRIC-FIELDS; HILDCAA
EVENTS; MU-M; STORMS; PENETRATION; SIMULATION; ORIGIN; MODEL
AB We analyze a portion of the Whole Heliospheric Interval from 25 March to 26 April 2008 to identify the ionospheric and thermospheric responses to high-speed solar wind streams. This period during solar sunspot minimum is of moderate geomagnetic activity (with the minimum Dst similar to -50 nT) with enhanced auroral activity seen in High-Intensity Long- Duration Continuous Auroral Activity events. The solar wind data show several corotating interaction regions (CIRs) and recurrent high-speed streams (HSSs). Using the infrared emission data obtained with Sounding of the Atmosphere using Broadband Emission Radiometry on Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics, we identify a distinct relationship between the infrared emission irradiated from the thermosphere and CIR-HSS intervals. Specifically, zonal flux of NO infrared radiation correlates well with AE indices. The most pronounced effects are found at high latitudes. We used Jet Propulsion Laboratory Global Ionospheric Maps (GIMs) software and the GPS total electron content (TEC) database to calculate the vertical total electron content (VTEC) and construct GIMs. It is shown that VTEC intensifies during HSSs periods. To illustrate the point, dynamics of daytime VTEC averaged over different latitude bands are presented. These results are compared to quiet time observations to contrast variations associated with geomagnetic activity. Data analyses show fast, global, and continuous ionospheric responses to external solar wind forcing. The largest variations are found in low-latitude (between -30 degrees and 30 degrees) VTEC. In conclusion, we suggest that CIRs/HSSs are external drivers for both thermospheric and ionospheric phenomena during the solar sunspot minimum. We discuss both prompt penetration electric fields and disturbance dynamos as possible mechanisms responsible for the observed VTEC effects. It is clear that efficient heliospheric-magnetosphericionospheric- thermospheric coupling occurs during CIR-HSS intervals even during solar sunspot minimum in 2008.
C1 [Verkhoglyadova, O. P.; Tsurutani, B. T.; Mannucci, A. J.; Komjathy, A.; Runge, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hunt, L. A.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Mlynczak, M. G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Verkhoglyadova, O. P.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL USA.
RP Verkhoglyadova, OP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM olga.verkhoglyadova@jpl.nasa.gov
RI Mlynczak, Martin/K-3396-2012;
OI Verkhoglyadova, Olga/0000-0002-9295-9539
FU NASA; NASA TIMED project office
FX Portions of this work were done at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA. M. G. M.
would like to acknowledge support from the NASA TIMED project office.
The authors appreciated discussions with A. G. Burns, S. C. Solomon
(HAO/NCAR), and other participants of the Boulder High-Speed Stream and
Solar Minimum Workshop (1-3 September 2010, Boulder, Colorado).
NR 49
TC 14
Z9 14
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 SEP 28
PY 2011
VL 116
AR A09325
DI 10.1029/2011JA016604
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 828VN
UT WOS:000295531800005
ER
PT J
AU Shen, C
Dunlop, M
Ma, YH
Chen, ZQ
Yan, GQ
Liu, ZX
Bogdanova, YV
Sibeck, DG
Carr, CM
Zhang, QH
Lucek, E
AF Shen, C.
Dunlop, M.
Ma, Y. H.
Chen, Z. Q.
Yan, G. Q.
Liu, Z. X.
Bogdanova, Y. V.
Sibeck, D. G.
Carr, C. M.
Zhang, Q. H.
Lucek, E.
TI The magnetic configuration of the high-latitude cusp and dayside
magnetopause under strong magnetic shears
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID HIGH-ALTITUDE CUSP; SOLAR-WIND CONTROL; CLUSTER OBSERVATIONS;
MAGNETOSPHERIC CUSPS; ENERGETIC ELECTRONS; EARTHS MAGNETOPAUSE;
GEOMAGNETIC FIELD; PRESSURE BALANCE; BOUNDARY-LAYER; NORTHWARD IMF
AB This paper investigates the structure of the magnetic field near the magnetopause (MP) by analyzing the multiple-point magnetic measurements from the Cluster mission. In this paper, the spatial distribution of the curvature radius of the MP surface at the noon-midnight meridian and for situations with moderate dynamical pressure of solar wind is implied from direct measurements of magnetic field curvature for the first time. The investigation focused on conditions of strong magnetic shear and in which a clear boundary layer is present at the MP. It has been confirmed that the magnetic field lines surrounding the cusp bend sunward at the precusp region and tailward at the postcusp region, implying the existence of a cusp field indentation. The minimum curvature radius of the near-MP field at both precusp and postcusp regions is about 2 R-E. As the latitude decreases, the curvature radius at the MP increases gradually, so that, as the subsolar point is approached, the curvature radius of the MP is nearly equal to the geocentric distance. These results compare well with existing MP models but reveal the limitations inherent in such statistical estimates of local MP curvature, particularly surrounding the cusp regions. The analysis of the magnetic measurements has also verified the existence of the magnetic bottles at both precusp and postcusp regions, which may play a role for the trapping of the charged particles of magnetosphere.
C1 [Shen, C.; Ma, Y. H.; Chen, Z. Q.; Yan, G. Q.; Liu, Z. X.] Chinese Acad Sci, State Key Lab Space Weather, Ctr Space Sci & Appl Res, Beijing 100190, Peoples R China.
[Bogdanova, Y. V.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Carr, C. M.; Lucek, E.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England.
[Dunlop, M.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Zhang, Q. H.] Polar Res Inst China, Shanghai 200136, Peoples R China.
RP Shen, C (reprint author), Chinese Acad Sci, State Key Lab Space Weather, Ctr Space Sci & Appl Res, 1 Nanertiao, Beijing 100190, Peoples R China.
RI Sibeck, David/D-4424-2012; dunlop, malcolm/F-1347-2010; Zhang,
Qing-He/G-4572-2014
OI Zhang, Qing-He/0000-0003-2429-4050
FU Ministry of Science and Technology of China [2011CB811404]; National
Natural Science Foundation of China [40921063, 40974101]; Chinese
Academy of Sciences (CAS) [2009S1-54]
FX This work was supported by Ministry of Science and Technology of China,
grant 2011CB811404, the National Natural Science Foundation of China,
grant. 40921063, 40974101, the Chinese Academy of Sciences (CAS)
Visiting Professorship for Senior International Scientists, grant
2009S1-54, the Specialized Research Fund for State Key Laboratories of
the CAS. The authors are grateful to the Cluster II FGM team and the
Hungarian Data Centre for providing us with four satellite magnetic
measurement data and Cluster position data, respectively. The authors
also thank R. L. Lin for the helpful discussions on the magnetopause
models.
NR 58
TC 1
Z9 2
U1 0
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP 27
PY 2011
VL 116
AR A09228
DI 10.1029/2011JA016501
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 828VI
UT WOS:000295531300002
ER
PT J
AU Schweiger, A
Lindsay, R
Zhang, JL
Steele, M
Stern, H
Kwok, R
AF Schweiger, Axel
Lindsay, Ron
Zhang, Jinlun
Steele, Mike
Stern, Harry
Kwok, Ron
TI Uncertainty in modeled Arctic sea ice volume
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID SURFACE TEMPERATURE; NUMERICAL-MODEL; THICKNESS; OCEAN; CLIMATE;
ASSIMILATION; COVER
AB Uncertainty in the Pan-Arctic Ice-Ocean Modeling and Assimilation System (PIOMAS) Arctic sea ice volume record is characterized. A range of observations and approaches, including in situ ice thickness measurements, ICESat retrieved ice thickness, and model sensitivity studies, yields a conservative estimate for October Arctic ice volume uncertainty of 1.35 x 10(3) km(3) and an uncertainty of the ice volume trend over the 1979-2010 period of 1.0 x 10(3) km(3) decade(-1). A conservative estimate of the trend over this period is -2.8 x 10(3) km(3) decade(-1). PIOMAS ice thickness estimates agree well with ICESat ice thickness retrievals (<0.1 m mean difference) for the area for which submarine data are available, while difference outside this area are larger. PIOMAS spatial thickness patterns agree well with ICESat thickness estimates with pattern correlations of above 0.8. PIOMAS appears to overestimate thin ice thickness and underestimate thick ice, yielding a smaller downward trend than apparent in reconstructions from observations. PIOMAS ice volume uncertainties and trends are examined in the context of climate change attribution and the declaration of record minima. The distribution of 32 year trends in a preindustrial coupled model simulation shows no trends comparable to those seen in the PIOMAS retrospective, even when the trend uncertainty is accounted for. Attempts to label September minima as new record lows are sensitive to modeling error. However, the September 2010 ice volume anomaly did in fact exceed the previous 2007 minimum by a large enough margin to establish a statistically significant new record.
C1 [Schweiger, Axel; Lindsay, Ron; Zhang, Jinlun; Steele, Mike; Stern, Harry] Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA.
[Kwok, Ron] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Schweiger, A (reprint author), Univ Washington, Appl Phys Lab, Polar Sci Ctr, 1013 NE 40th St, Seattle, WA 98105 USA.
EM axel@apl.washington.edu
RI Kwok, Ron/A-9762-2008; Lindsay, Ron/S-9083-2016
OI Kwok, Ron/0000-0003-4051-5896;
FU NASA; Arctic Section of the Office of Polar at NSF; NOAA; Office of
Science, U.S. Department of Energy
FX This research was supported by grants from NASA's Cryosphere Sciences
Program, the Arctic Section of the Office of Polar Programs at NSF, and
NOAA. Individual investigators contributed their in situ data sets to
the sea ice CDR. Their tremendous contribution in collectively
establishing an in situ measurement network that provides the critical
data to conduct a study at the present needs to be highlighted. Dick
Moritz is thanked for contributing NPEO data and many useful
discussions. We acknowledge the modeling groups, the Program for Climate
Model Diagnosis and Intercomparison (PCMDI) and WCRP's Working Group on
Coupled Modeling (WGCM) for their roles in making available the WCRP
CMIP3 multimodel data set. Support of this data set is provided by the
Office of Science, U.S. Department of Energy. NOAA Physical Science
Division is thanked for providing model NCEP forcing data.
NR 45
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Z9 136
U1 2
U2 29
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 SEP 27
PY 2011
VL 116
AR C00D06
DI 10.1029/2011JC007084
PG 21
WC Oceanography
SC Oceanography
GA 828TU
UT WOS:000295526800003
ER
PT J
AU Garfinkel, CI
Molod, AM
Oman, LD
Song, IS
AF Garfinkel, C. I.
Molod, A. M.
Oman, L. D.
Song, I. -S.
TI Improvement of the GEOS-5 AGCM upon updating the air-sea roughness
parameterization
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID FLUXES; WINDS; MODEL
AB The impact of an air-sea roughness parameterization over the ocean that more closely matches recent observations of air-sea exchange is examined in the NASA Goddard Earth Observing System, version 5 (GEOS-5) atmospheric general circulation model. Surface wind biases in the GEOS-5 AGCM are decreased by up to 1.2m/s. The new parameterization also has implications aloft as improvements extend into the stratosphere. Many other GCMs (both for operational weather forecasting and climate) use a similar class of parameterization for their air-sea roughness scheme. We therefore expect that results from GEOS-5 are relevant to other models as well. Citation: Garfinkel, C. I., A. M. Molod, L. D. Oman, and I.-S. Song (2011), Improvement of the GEOS-5 AGCM upon updating the air-sea roughness parameterization, Geophys. Res. Lett., 38, L18702, doi: 10.1029/2011GL048802.
C1 [Garfinkel, C. I.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21209 USA.
[Molod, A. M.] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Oman, L. D.] NASA, Atmospher Chem & Dynam Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Song, I. -S.] Korea Meteorol Adm, Next Generat Model Dev Project, Seoul 156710, South Korea.
[Molod, A. M.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Garfinkel, CI (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21209 USA.
EM cig4@jhu.edu
RI Oman, Luke/C-2778-2009; garfinkel, chaim/H-6215-2012
OI Oman, Luke/0000-0002-5487-2598; garfinkel, chaim/0000-0001-7258-666X
FU NASA [NNX06AE70G]
FX This work was supported by the NASA grant NNX06AE70G. The authors thank
J. Edson for making available data from Edson [2008] and his manuscript
in preparation, Larry Takacs for performing the model simulation in
forecast mode, Andrew Eichmann for performing the 1 degree model
simulations, and our anonymous reviewers for their comments.
NR 25
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U1 1
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 24
PY 2011
VL 38
AR L18702
DI 10.1029/2011GL048802
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 825MP
UT WOS:000295281700001
ER
PT J
AU Santee, ML
Manney, GL
Livesey, NJ
Froidevaux, L
Schwartz, MJ
Read, WG
AF Santee, M. L.
Manney, G. L.
Livesey, N. J.
Froidevaux, L.
Schwartz, M. J.
Read, W. G.
TI Trace gas evolution in the lowermost stratosphere from Aura Microwave
Limb Sounder measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CHEMISTRY-TRANSPORT MODEL; ARCTIC LOWER STRATOSPHERE; ANTARCTIC OZONE
HOLE; IN-SITU MEASUREMENTS; AIRCRAFT MEASUREMENTS STREAM; CHEMICAL
LAGRANGIAN MODEL; TOTAL REACTIVE NITROGEN; POLAR VORTEX; UPPER
TROPOSPHERE; TROPICAL TROPOPAUSE
AB Daily global measurements from NASA's Aura Microwave Limb Sounder (MLS) allow comprehensive investigation of interhemispheric and interannual variations in chemical and transport processes throughout the lowermost stratosphere (LMS). We analyze nearly seven years of MLS O-3, HNO3, HCl and ClO measurements along with meteorological analyses to place chemical processing in and dispersal of processed air from the winter polar lowermost vortex and subvortex in a global context. The MLS data, the first simultaneous observations of HCl and ClO covering much of the LMS, reveal that chlorine activation is widespread in the Antarctic subvortex and can occur to a significant degree in the Arctic subvortex. Unusually low temperatures and strong, prolonged chlorine activation in the lowermost vortex and subvortex promoted large ozone losses there in the 2006 (and 2008) Antarctic and 2004/2005 Arctic winters, consistent with reported record low column ozone. Processed air dispersing from the decaying vortex in spring induces rapid changes in extravortex trace gas abundances. After vortex breakdown, the subtropical jet/tropopause becomes the major transport barrier in the LMS. Quasi-isentropic transport of tropical tropospheric air into the LMS, associated with the summer monsoon circulations, leads to decreases in extratropical O-3, HNO3, and HCl in both hemispheres. Strong mixing in the summertime LMS homogenizes extratropical trace gas fields. MLS measurements in the tropics show signatures of monsoon-related cross-equatorial stratosphere-to-troposphere transport. Observed seasonal and interannual variations in trace gas abundances in the LMS are consistent with variations in the strength of transport barriers diagnosed from meteorological analyses.
C1 [Santee, M. L.; Manney, G. L.; Livesey, N. J.; Froidevaux, L.; Schwartz, M. J.; Read, W. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Manney, G. L.] New Mexico Inst Min & Technol, Dept Phys, Workman Ctr, Socorro, NM 87801 USA.
RP Santee, ML (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-701,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Michelle.L.Santee@jpl.nasa.gov
RI Schwartz, Michael/F-5172-2016
OI Schwartz, Michael/0000-0001-6169-5094
FU NASA
FX We thank Ryan Fuller, William Daffer, Bob Thurstans, Brian Knosp, and
Brian Mills for programming, system administration, and data management
support. Helpful discussions with Alyn Lambert, Karen Rosenlof, Emily
Shuckburgh, Sean Davis, Michaela Hegglin, Ken Minschwaner, and Doug
Allen are greatly appreciated. Comments from three anonymous reviewers
improved the manuscript. Work at the Jet Propulsion Laboratory,
California Institute of Technology, was done under contract with NASA.
NR 169
TC 17
Z9 17
U1 1
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 24
PY 2011
VL 116
AR D18306
DI 10.1029/2011JD015590
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 825JL
UT WOS:000295268500002
ER
PT J
AU Kwok, R
AF Kwok, R.
TI Observational assessment of Arctic Ocean sea ice motion, export, and
thickness in CMIP3 climate simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
AB We compare the CMIP3 model fields with observations of sea ice motion, export, extent, and thickness and analyze fields of sea level pressure and geostrophic wind of the Arctic Ocean. These variables play important roles in the distribution and annual balance of sea ice volume within the basin. While it is not expected that uninitialized simulations agree completely with observations, these assessments serve to summarize ensemble behavior, as baselines for measuring improvements, and to evaluate reliability of CMIP3 simulations (and potentially CMIP5) for projection of decline rates of Arctic sea ice coverage. We find the model-data differences and intermodel scatter in summarizing statistics are large. In a majority of model fields the mean high-pressure pattern in the southern Beaufort is significantly displaced toward the central Arctic Basin, leading to difficulties in reproducing the mean spatial patterns of sea ice circulation, thickness, and ice export. Thus, even though the CMIP3 multimodel data set agrees that increased greenhouse gas concentrations will result in reductions of Arctic sea ice area and volume, these comparisons suggest considerable uncertainties in the projected rates of sea ice decline.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, Mail Stop 300-331,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ron.kwok@jpl.nasa.gov
RI Kwok, Ron/A-9762-2008
OI Kwok, Ron/0000-0003-4051-5896
FU NASA
FX I wish to thank G. F. Cunningham and S. S. Pang for their software
support. We acknowledge the modeling groups, the PCMDI, and the WCRP's
Working Group on Coupled Modeling for their roles in making available
the WCRP CMIP3 multimodel data set. Support of this data set is provided
by the Office of Science, U. S. Department of Energy. The SMMR and SSM/I
brightness temperature and ice concentration fields are provided by the
World Data Center A for Glaciology/National Snow and Ice Data Center,
University of Colorado, Boulder, Colorado. This work was performed at
the Jet Propulsion Laboratory, California Institute of Technology, under
contract with NASA.
NR 15
TC 23
Z9 23
U1 0
U2 10
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 SEP 24
PY 2011
VL 116
AR C00D05
DI 10.1029/2011JC007004
PG 8
WC Oceanography
SC Oceanography
GA 825GX
UT WOS:000295260300001
ER
PT J
AU Fermo, RL
Drake, JF
Swisdak, M
Hwang, KJ
AF Fermo, R. L.
Drake, J. F.
Swisdak, M.
Hwang, K. -J.
TI Comparison of a statistical model for magnetic islands in large current
layers with Hall MHD simulations and Cluster FTE observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID FLUX-TRANSFER EVENTS; RECONNECTION; MAGNETOTAIL; MAGNETOPAUSE;
COALESCENCE; EVOLUTION; SHEET
AB Magnetic islands have been observed in long current layers for various space plasmas, including the magnetopause and solar corona. In previous work exploring these magnetic islands, a statistical model was developed that described their formation, growth, convection, and coalescence in very large systems, for which simulations prove inadequate. An integro-differential equation was derived for the island distribution function, which characterized islands by the flux they contain psi and the cross-sectional area they enclose A. The steady-state solution of the evolution equation predicted a distribution of islands. Here, we use a Hall MHD (magnetohydrodynamic) simulation of a very long current sheet with large numbers of magnetic islands to explore their dynamics, specifically their growth via two distinct mechanisms: quasi-steady reconnection and merging. We then use the simulation to validate the statistical model and benchmark its parameters. A database of 1,098 flux transfer events (FTEs) observed by Cluster between 2001 and 2003 is also compared with the model's predictions. In both simulations and observations, island merging plays a significant role. This suggests that the magnetopause is populated by many FTEs too small to be recognized by spacecraft instrumentation.
C1 [Fermo, R. L.; Drake, J. F.; Swisdak, M.] Univ Maryland, Inst Res Elect & Appl Phys, College Pk, MD 20742 USA.
[Hwang, K. -J.] Univ Maryland Baltimore Cty, Goddard Earth Sci Technol Ctr, Baltimore, MD 21228 USA.
[Hwang, K. -J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Fermo, RL (reprint author), Univ Maryland, Inst Res Elect & Appl Phys, College Pk, MD 20742 USA.
EM rfermo@umd.edu
FU NASA [NNX07A083H, NNX09A102G]
FX The authors would like to thank Yongli Wang at the NASA Goddard Space
Flight Center for helpful conversations and for generously sharing the
FTE database he compiled. This work was supported by NASA through the
Earth and Space Science Fellowship NNX07A083H and NNX09A102G.
Computations were performed at the National Energy Research Scientific
Computing Center. Spacecraft data from Cluster was obtained from the ESA
Cluster Active Archive.
NR 51
TC 15
Z9 15
U1 1
U2 2
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 SEP 24
PY 2011
VL 116
AR A09226
DI 10.1029/2010JA016271
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 825HP
UT WOS:000295262400001
ER
PT J
AU Su, YJ
Retterer, JM
Pfaff, RF
Roddy, PA
de La Beaujardiere, O
Ballenthin, JO
AF Su, Y. -J.
Retterer, J. M.
Pfaff, R. F.
Roddy, P. A.
de La Beaujardiere, O.
Ballenthin, J. O.
TI Assimilative modeling of observed postmidnight equatorial plasma
depletions in June 2008
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID LOW-LATITUDE; IONOSPHERE; JICAMARCA; MISSION
AB The Communications/Navigation Outage Forecasting System (C/NOFS) satellite observed large-scale density depletions at postmidnight and early morning local times in the Northern Hemisphere summer during solar minimum conditions. Using electric field data obtained from the vector electric field instrument (VEFI) as input, the assimilative physics-based model (PBMOD) qualitatively reproduced more than 70% of the large-scale density depletions observed by the Planar Langmuir Probe (PLP) onboard C/NOFS. In contrast, the use of a climatological specification of plasma drifts in the model produces no plasma depletions at night. Results from a one-month statistical study, we found that the large-scale depletion structures most often occur near longitudes of 60 degrees, 140 degrees, and 330 degrees, suggesting that these depletions may be associated with nonmigrating atmospheric tides, although the generation mechanisms of eastward electric fields at postmidnight local times are still uncertain. In this paper, densities obtained from both assimilation and climatology for the entire month of June 2008 are compared with PLP data from C/NOFS and the Challenging Minisatellite Payload (CHAMP), as well as special sensor ionospheric plasma drift/scintillation meter (SSIES) measurements from the Defense Meteorological Satellite Program (DMSP) satellites. Our statistical study has shown that, on average, the densities obtained by the PBMOD when it assimilates VEFI electric fields agree better with observed background densities than when PBMOD uses climatological electric fields.
C1 [Su, Y. -J.] USAF, RVBXP, Space Vehicles Directorate, Res Lab, Kirtland AFB, NM 87117 USA.
[Retterer, J. M.] USAF, Res Lab, Space Vehicles Directorate, Hanscom AFB, MA USA.
[Pfaff, R. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Su, YJ (reprint author), USAF, RVBXP, Space Vehicles Directorate, Res Lab, BEL Bldg 570,3671 Aberdeen Ave SE, Kirtland AFB, NM 87117 USA.
EM Yi-Jiun.Su@kirtland.af.mil
RI Pfaff, Robert/F-5703-2012
OI Pfaff, Robert/0000-0002-4881-9715
FU Air Force Research Laboratory; Department of Defense; NASA [NNH09AK051];
Naval Research Laboratory; Aerospace Corporation
FX The C/NOFS mission is supported by the Air Force Research Laboratory,
the Department of Defense Space Test Program, NASA, the Naval Research
Laboratory, and The Aerospace Corporation. The first author thanks
Gordon Wilson for providing DMSP data, Louise Gentile for useful
conversation regarding CIR events, Han-Li Liu at NCAR for providing
references on nonmigrating tides, and Ron Caton for proofreading the
manuscript. We also thank the referees for their positive comments and
helpful questions. This research task was supported in part by the NASA
grant NNH09AK051 to AFRL.
NR 34
TC 4
Z9 4
U1 1
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP 22
PY 2011
VL 116
AR A09318
DI 10.1029/2011JA016772
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 825HL
UT WOS:000295262000003
ER
PT J
AU Kellogg, PJ
Cattell, CA
Goetz, K
Monson, SJ
Wilson, LB
AF Kellogg, P. J.
Cattell, C. A.
Goetz, K.
Monson, S. J.
Wilson, L. B., III
TI Large amplitude whistlers in the magnetosphere observed with Wind-Waves
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID PLASMA SHEET BOUNDARY; STORM-TIME CHORUS; SOLITARY WAVES; SOURCE REGION;
AURORAL-ZONE; SATELLITE-OBSERVATIONS; RESONANT DIFFUSION; SPACECRAFT;
RADIATION; POLAR
AB We describe the results of a statistical survey of Wind-Waves data motivated by the recent STEREO/Waves discovery of large-amplitude whistlers in the inner magnetosphere. Although Wind was primarily intended to monitor the solar wind, the spacecraft spent 47 h inside 5 R-E and 431 h inside 10 R-E during the 8 years (1994-2002) that it orbited the Earth. Five episodes were found when whistlers had amplitudes comparable to those of Cattell et al. (2008), i.e., electric fields of 100 mV/m or greater. The whistlers usually occurred near the plasmapause. The observations are generally consistent with the whistlers observed by STEREO. In contrast with STEREO, Wind-Waves had a search coil, so magnetic measurements are available, enabling determination of the wave vector without a model. Eleven whistler events with useable magnetic measurements were found. The wave vectors of these are distributed around the magnetic field direction with angles from 4 to 48 degrees. Approximations to observed electron distribution functions show a Kennel-Petschek instability which, however, does not seem to produce the observed whistlers. One Wind episode was sampled at 120,000 samples s(-1), and these events showed a signature that is interpreted as trapping of electrons in the electrostatic potential of an oblique whistler. Similar waveforms are found in the STEREO data. In addition to the whistler waves, large amplitude, short duration solitary waves (up to 100 mV/m), presumed to be electron holes, occur in these passes, primarily on plasma sheet field lines mapping to the auroral zone.
C1 [Kellogg, P. J.; Cattell, C. A.; Goetz, K.; Monson, S. J.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Wilson, L. B., III] NASA, Heliophys Div, Goddard Space Flight Ctr, Greenbelt, MD 20707 USA.
RP Kellogg, PJ (reprint author), Univ Minnesota, Sch Phys & Astron, 116 Church St SE, Minneapolis, MN 55455 USA.
EM pauljkellogg@gmail.com
RI Wilson III, Lynn/D-4425-2012;
OI Wilson III, Lynn/0000-0002-4313-1970; Cattell,
Cynthia/0000-0002-3805-320X
FU National Aeronautics and Space Administration [NNX07AF23G (STEREO),
NNX11AB46G]; NESSF [NNX07AU72H, NNX07AM97G, NNX08AT81G]; Dr. L.
Burlaga/Arctowski Medal Fellowship
FX This work was supported by the National Aeronautics and Space
Administration under grants NNX07AF23G (STEREO), NNX11AB46G, NESSF grant
NNX07AU72H, and NNX07AM97G and NNX08AT81G (Wind). L. B. W was partially
supported by a Dr. L. Burlaga/Arctowski Medal Fellowship. We thank R.
Lepping, GSFC, and C. T. Russell, UCLA, and CDAWeb for the magnetic
field and density data, and for the electron distribution and ion
density data we thank R. Lin, UCBerkeley. We also thank Robert L. Lysak
and a reviewer for valuable discussions of the instability.
NR 48
TC 24
Z9 24
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP 21
PY 2011
VL 116
AR A09224
DI 10.1029/2010JA015919
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 825HJ
UT WOS:000295261800001
ER
PT J
AU Joudaki, S
Dore, O
Ferramacho, L
Kaplinghat, M
Santos, MG
AF Joudaki, Shahab
Dore, Olivier
Ferramacho, Luis
Kaplinghat, Manoj
Santos, Mario G.
TI Primordial Non-Gaussianity from the 21 cm Power Spectrum during the
Epoch of Reionization
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID PROBE WMAP OBSERVATIONS; CENTIMETER FLUCTUATIONS; INFLATIONARY UNIVERSE;
FLATNESS; HORIZON; MODELS
AB Primordial non-Gaussianity is a crucial test of inflationary cosmology. We consider the impact of non-Gaussianity on the ionization power spectrum from 21 cm emission at the epoch of reionization. We focus on the power spectrum on large scales at redshifts of 7 to 8 and explore the expected constraint on the local non-Gaussianity parameter f(NL) for current and next-generation 21 cm experiments. We show that experiments such as SKA and MWA could measure f(NL) values of order 10. This can be improved by an order of magnitude with a fast-Fourier transform telescope like Omniscope.
C1 [Joudaki, Shahab; Kaplinghat, Manoj] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA.
[Dore, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dore, Olivier] CALTECH, Pasadena, CA 91125 USA.
[Ferramacho, Luis] CNRS, IRAP, F-31400 Toulouse, France.
[Ferramacho, Luis] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Santos, Mario G.] Univ Tecn Lisbon, Inst Super Tecn, CENTRA, P-1049001 Lisbon, Portugal.
RP Joudaki, S (reprint author), Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA.
RI Santos, Mario/F-2484-2011;
OI Santos, Mario/0000-0003-3892-3073; Ferramacho, Luis/0000-0002-8481-1163
FU FCT [PTDC/FIS/100170/2008]; NSF [NSF 0855462]
FX We thank A. Amblard, Y. Mao, G. Martinez, M. McQuinn, J. Smidt, and E.
Tollerud for useful discussions. M. G. S. acknowledges support by FCT
under grant PTDC/FIS/100170/2008. M. K. acknowledges support by NSF
under grant NSF 0855462 at UCI. Part of the research described in this
Letter was carried out at JPL, Caltech, under contract with NASA.
NR 28
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U1 0
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 SEP 21
PY 2011
VL 107
IS 13
AR 131304
DI 10.1103/PhysRevLett.107.131304
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 822XF
UT WOS:000295083100004
PM 22026840
ER
PT J
AU Giles, DM
Holben, BN
Tripathi, SN
Eck, TF
Newcomb, WW
Slutsker, I
Dickerson, RR
Thompson, AM
Mattoo, S
Wang, SH
Singh, RP
Sinyuk, A
Schafer, JS
AF Giles, David M.
Holben, Brent N.
Tripathi, Sachchida N.
Eck, Thomas F.
Newcomb, W. Wayne
Slutsker, Ilya
Dickerson, Russell R.
Thompson, Anne M.
Mattoo, Shana
Wang, Sheng-Hsiang
Singh, Remesh P.
Sinyuk, Aliaksandr
Schafer, Joel S.
TI Aerosol properties over the Indo-Gangetic Plain: A mesoscale perspective
from the TIGERZ experiment
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID RESOLUTION IMAGING SPECTRORADIOMETER; SKY RADIANCE MEASUREMENTS; OPTICAL
DEPTH; BLACK CARBON; NORTHERN INDIA; SOLAR-RADIATION; AIR-POLLUTION;
WAVELENGTH DEPENDENCE; ATMOSPHERIC AEROSOLS; SEASONAL VARIABILITY
AB High aerosol loading over the northern Indian subcontinent can result in poor air quality leading to human health consequences and climate perturbations. The international 2008 TIGERZ experiment intensive operational period (IOP) was conducted in the Indo-Gangetic Plain (IGP) around the industrial city of Kanpur (26.51 degrees N, 80.23 degrees E), India, during the premonsoon (April-June). Aerosol Robotic Network (AERONET) Sun photometers performed frequent measurements of aerosol properties at temporary sites distributed within an area covering similar to 50 km(2) around Kanpur to characterize pollution and dust in a region where complex aerosol mixtures and semi-bright surface effects complicate satellite retrieval algorithms. TIGERZ IOP Sun photometers quantified aerosol optical depth (AOD) increases up to similar to 0.10 within and downwind of the city, with urban emissions accounting for similar to 10-20% of the IGP aerosol loading on deployment days. TIGERZ IOP area-averaged volume size distribution and single scattering albedo retrievals indicated spatially homogeneous, uniformly sized, spectrally absorbing pollution and dust particles. Aerosol absorption and size relationships were used to categorize black carbon and dust as dominant absorbers and to identify a third category in which both black carbon and dust dominate absorption. Moderate Resolution Imaging Spectroradiometer (MODIS) AOD retrievals with the lowest quality assurance (QA >= 0) flags were biased high with respect to TIGERZ IOP area-averaged measurements. MODIS AOD retrievals with QA >= 0 had moderate correlation (R-2 = 0.52-0.69) with the Kanpur AERONET site, whereas retrievals with QA > 0 were limited in number. Mesoscale-distributed Sun photometers quantified temporal and spatial variability of aerosol properties, and these results were used to validate satellite retrievals.
C1 [Giles, David M.; Slutsker, Ilya; Sinyuk, Aliaksandr; Schafer, Joel S.] Sigma Space Corp, Lanham, MD USA.
[Giles, David M.; Holben, Brent N.; Eck, Thomas F.; Slutsker, Ilya; Wang, Sheng-Hsiang; Sinyuk, Aliaksandr; Schafer, Joel S.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Giles, David M.; Dickerson, Russell R.; Wang, Sheng-Hsiang] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Tripathi, Sachchida N.] Indian Inst Technol, Dept Civil Engn, Kanpur 208016, Uttar Pradesh, India.
[Eck, Thomas F.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Thompson, Anne M.] Penn State Univ, Dept Meteorol, Coll Earth & Mineral Sci, University Pk, PA 16802 USA.
[Mattoo, Shana] Sci Syst & Applicat Inc, Lanham, MD USA.
[Wang, Sheng-Hsiang] Natl Cent Univ, Dept Atmospher Sci, Chungli 32054, Taiwan.
[Singh, Remesh P.] Chapman Univ, Sch Earth & Environm Sci, Schmid Coll Sci, Hashinger Sci Ctr 219, Orange, CA 92866 USA.
RP Giles, DM (reprint author), Sigma Space Corp, Lanham, MD USA.
EM David.M.Giles@nasa.gov
RI ECK, THOMAS/D-7407-2012; Singh, Ramesh/G-7240-2012; Dickerson,
Russell/F-2857-2010; Wang, Sheng-Hsiang/F-4532-2010; Tripathi,
Sachchida/J-4840-2016; Thompson, Anne /C-3649-2014
OI Dickerson, Russell/0000-0003-0206-3083; Wang,
Sheng-Hsiang/0000-0001-9675-3135; Thompson, Anne /0000-0002-7829-0920
FU NASA; Radiation Sciences Program; NASA Headquarters
FX The NASA AERONET project was supported by Michael D. King, who retired
in 2008 from the NASA EOS project office, and by Hal B. Maring,
Radiation Sciences Program, NASA Headquarters. The authors would like
thank all of the more than 30 participants and collaborators in the
NASA/GSFC TIGERZ campaign effort, including many Indian researchers and
graduate students as well as other national and international agencies
that provided personnel and equipment to perform the study. The authors
thank the AERONET team for calibrating and maintaining instrumentation
and processing these data. The authors would like to recognize Harish
Vishwakarma at IIT-Kanpur for field support during TIGERZ and continued
support of the long-term Kanpur AERONET site. The authors gratefully
acknowledge the NOAA Air Resources Laboratory (ARL) for providing data
from the HYSPLIT transport and dispersion model and/or READY website
(http://www.arl.noaa.gov/ready.php) used in this publication. The
authors thank Jeffrey Reid and two anonymous reviewers for their
constructive comments on an earlier version of the manuscript.
Furthermore, the authors recognize with great sadness their deceased
coauthor Wilber Wayne Newcomb for his major contributions to the TIGERZ
campaign and AERONET.
NR 112
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 20
PY 2011
VL 116
AR D18203
DI 10.1029/2011JD015809
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 825JD
UT WOS:000295267600003
ER
PT J
AU Kroon, M
de Haan, JF
Veefkind, JP
Froidevaux, L
Wang, R
Kivi, R
Hakkarainen, JJ
AF Kroon, M.
de Haan, J. F.
Veefkind, J. P.
Froidevaux, L.
Wang, R.
Kivi, R.
Hakkarainen, J. J.
TI Validation of operational ozone profiles from the Ozone Monitoring
Instrument
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID HALOGEN OCCULTATION EXPERIMENT; BALLOON SONDE MEASUREMENTS; SAGE-II;
TROPOSPHERIC OZONE; SATELLITE MEASUREMENTS; STRATOSPHERIC AEROSOL; AURA
SATELLITE; ENVISAT-GOMOS; EOS MLS; ART.
AB In this paper we present the validation results of the operational vertical ozone profiles retrieved from the nadir observations by the Ozone Monitoring Instrument (OMI) aboard the NASA Earth Observing System (EOS) Aura platform. The operational ozone profile retrieval algorithm was developed at the Royal Netherlands Meteorological Institute and the OMI mission data has been processed and made publicly available. Advantages of these nadir sounded ozone profiles are the excellent spatial resolution at nadir and daily global coverage while the vertical resolution is limited to 6-7 km. Comparisons with well-validated ozone profile recordings by the Microwave Limb Sounder (MLS) and the Tropospheric Emission Spectrometer (TES), both aboard the NASA EOS-Aura platform, provide an excellent opportunity for validation because of the large amount of collocations with OMI due to the instruments significant geographical overlap. In addition, comparisons with collocated ozone profiles from the Stratospheric Aerosol and Gas Experiment (SAGE-II), the Halogen Occultation Experiment (HALOE), the Global Ozone Monitoring by the Occultation of Stars (GOMOS) and the Optical Spectrograph and Infrared Imager System (OSIRIS) satellite instruments and balloon-borne electrochemical concentration cell (ECC) ozonesondes are presented. OMI stratospheric ozone profiles are found to agree within 20% with global correlative data except for both the polar regions during local spring. For ozone in the troposphere OMI shows a systematic positive bias versus the correlative data sets of order 60% in the tropics and 30% at midlatitude regions. The largest source of error in the tropospheric ozone profile is the fit to spectral stray light in the operational algorithm.
C1 [Kroon, M.; de Haan, J. F.; Veefkind, J. P.] Royal Netherlands Meteorol Inst, Dept Climate & Seismol, NL-3730 AE De Bilt, Netherlands.
[Froidevaux, L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wang, R.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Kivi, R.] Finnish Meteorol Inst, Arctic Res Ctr, FIN-99600 Sodankyla, Finland.
[Hakkarainen, J. J.] Finnish Meteorol Inst, Dept Earth Observat, FIN-00101 Helsinki, Finland.
RP Kroon, M (reprint author), Royal Netherlands Meteorol Inst, Dept Climate & Seismol, POB 201, NL-3730 AE De Bilt, Netherlands.
EM mark.kroon@knmi.nl
RI Hakkarainen, Janne/C-8404-2012;
OI Hakkarainen, Janne/0000-0002-5281-8985
FU Netherlands Space Office (NSO); Royal Netherlands Meteorological
Institute (KNMI); Netherlands Space Organization; Georgia Institute of
Technology (Georgia-Tech); Academy of Finland's NOVAC; Finnish
Meteorological Institute (FMI)
FX The Dutch-Finnish built Ozone Monitoring Instrument (OMI) is part of the
National Aeronautics and Space Administration (NASA) Earth Observing
System (EOS) Aura satellite payload. The OMI project is managed by the
Netherlands Space Office (NSO) and the Royal Netherlands Meteorological
Institute (KNMI). OMI vertical ozone profile data were processed at and
obtained from the NASA Goddard Earth Sciences (GES) Data and Information
Services Center (DISC). The work of M. Kroon, J.P. Veefkind and J.F de
Haan was supported by the Netherlands Space Organization via the
EOS-Aura OMI Science project. The work by L. Froidevaux and the MLS team
at the Jet Propulsion Laboratory, California Institute of Technology,
was performed under contract with the National Aeronautics and Space
Administration. The work of R. Wang was supported by Georgia Institute
of Technology (Georgia-Tech) via the EOS-Aura OMI Science project. The
work of J. Hakkarainen has been supported by the Academy of Finland's
NOVAC project. The work of R. Kivi has been supported by the Finnish
Meteorological Institute (FMI) via the EOS-Aura OMI Science project. We
thank Susan S. Kulawick of the TES team for stimulating discussions. We
wish to thank Lin Zhang of Harvard University for providing us with the
code for correcting our OMI-TES comparisons for the a-priori
differences. We wish to thank the three anonymous reviewers whose input
made this paper stronger and more useful. We dedicate this work to the
memory of Derek Martin Cunnold, who devoted his scientific career to the
understanding of the dynamics and chemistry of atmospheric ozone.
NR 60
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U1 2
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 20
PY 2011
VL 116
AR D18305
DI 10.1029/2010JD015100
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 825JD
UT WOS:000295267600001
ER
PT J
AU Rosario, NE
Yamasoe, MA
Brindley, H
Eck, TF
Schafer, J
AF Rosario, Nilton E.
Yamasoe, Marcia A.
Brindley, Helen
Eck, Thomas F.
Schafer, Joel
TI Downwelling solar irradiance in the biomass burning region of the
southern Amazon: Dependence on aerosol intensive optical properties and
role of water vapor
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ATMOSPHERIC AEROSOLS; RADIATIVE-TRANSFER; BRAZIL; ABSORPTION; CLIMATE;
AERONET; MODEL; SMOKE; APPORTIONMENT; VARIABILITY
AB The sensitivity of solar irradiance at the surface to the variability of aerosol intensive optical properties is investigated for a site (Alta Floresta) in the southern portion of the Amazon basin using detailed comparisons between measured and modeled irradiances. Apart from aerosol intensive optical properties, specifically single scattering albedo (omega(o lambda)) and asymmetry parameter (g(lambda)), which were assumed constant, all other relevant input to the model were prescribed based on observation. For clean conditions, the differences between observed and modeled irradiances were consistent with instrumental uncertainty. For polluted conditions, the agreement was significantly worse, with a root mean square difference three times larger (23.5 Wm(-2)). Analysis revealed a noteworthy correlation between the irradiance differences (observed minus modeled) and the column water vapor (CWV) for polluted conditions. Positive differences occurred mostly in wet conditions, while the differences became more negative as the atmosphere dried. To explore the hypothesis that the irradiance differences might be linked to the modulation of omega(o lambda) and g(lambda) by humidity, AERONET retrievals of aerosol properties and CWV over the same site were analyzed. The results highlight the potential role of humidity in modifying omega(o lambda) and g(lambda) and suggest that to explain the relationship seen between irradiances differences via aerosols properties the focus has to be on humidity-dependent processes that affect particles chemical composition. Undoubtedly, there is a need to better understand the role of humidity in modifying the properties of smoke aerosols in the southern portion of the Amazon basin.
C1 [Rosario, Nilton E.; Yamasoe, Marcia A.] Univ Sao Paulo, Dept Atmospher Sci, BR-05508090 Sao Paulo, Brazil.
[Rosario, Nilton E.; Brindley, Helen] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England.
[Eck, Thomas F.; Schafer, Joel] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Eck, Thomas F.] Univ Maryland Baltimore Cty, GEST Ctr, Catonsville, MD USA.
RP Rosario, NE (reprint author), Univ Sao Paulo, Dept Atmospher Sci, Rua Matao 1226, BR-05508090 Sao Paulo, Brazil.
EM nrosario@model.iag.usp.br
RI ECK, THOMAS/D-7407-2012; Rosario, Nilton/D-8687-2012; Yamasoe,
Marcia/L-3667-2013;
OI Yamasoe, Marcia/0000-0003-3066-9146; Brindley, Helen/0000-0002-7859-9207
FU CNPq (Conselho Nacional de Desenvolvimento Cientifico e Tecnologico)
[140559/2007-8, 201177/2009-9]; Space and Atmospheric Group at Imperial
College, London, United Kingdom; (Coordenacao de Aperfeioamento de
Pessoal de Nivel Superior (CAPES), Brazil); FAPESP (Fundacao de Amparo a
Pesquisa do Estado de Sao Paulo) [06/56550-5]
FX The first author wishes to thank CNPq (Conselho Nacional de
Desenvolvimento Cientifico e Tecnologico) for the financial support
(processes 140559/2007-8; 201177/2009-9) and the Space and Atmospheric
Group at Imperial College, London, United Kingdom, where the present
study was partially developed. M. A. Yamasoe thanks CAPES (Coordenacao
de Aperfeioamento de Pessoal de Nivel Superior (CAPES), Brazil) and
FAPESP (Fundacao de Amparo a Pesquisa do Estado de Sao Paulo, process
06/56550-5) for financial support. Additional thanks to AERONET,
SolRad-Net staff for making available the data used in this study. The
authors also thank the anonymous reviewers for their constructive
comments.
NR 35
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 20
PY 2011
VL 116
AR D18304
DI 10.1029/2011JD015956
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 825JD
UT WOS:000295267600004
ER
PT J
AU Castillo-Rogez, JC
Efroimsky, M
Lainey, V
AF Castillo-Rogez, Julie C.
Efroimsky, Michael
Lainey, Valery
TI The tidal history of Iapetus: Spin dynamics in the light of a refined
dissipation model
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID SEISMIC-WAVE ATTENUATION; ICE SINGLE-CRYSTALS; POLYCRYSTALLINE OLIVINE;
GRAVITATIONAL MOTION; PLANETARY SATELLITES; BOUNDARY DIFFUSION;
HIGH-TEMPERATURE; WATER ICE; FRICTION; CREEP
AB We study the tidal history of an icy moon, basing our approach on a dissipation model, which combines viscoelasticity with anelasticity and takes into account the microphysics of attenuation. We apply this approach to Iapetus, the most remote large icy moon in the Saturnian system. Different authors provide very different estimates for Iapetus's despinning timescale, by several orders of magnitude. One reason for these differences is the choice of the dissipation model used for computing the spin evolution. As laboratory data on viscoelastic properties of planetary ices are sparse, many studies relied on dissipation models that turned out to be inconsistent with experiment. A pure water ice composition, generally assumed in the previous studies of the kind, yields despinning times of the order of 3.7 Gyr for most initial conditions. We demonstrate that through accounting for the complexity of the material (like second-phase impurities) one arrives at despinning times as short as 0.9 Gyr. A more exact estimate will remain unavailable until we learn more about the influence of impurities on ice dissipation. By including the triaxial-shape-caused torque, we encounter a chaotic behavior at the final stage of despinning, with the possibility of entrapments in the intermediate resonances. The duration of these entrapments turns out to be sensitive to the dissipation model. No long entrapments have been found for Iapetus described with our laboratory-based dissipation model.
C1 [Castillo-Rogez, Julie C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Efroimsky, Michael] US Naval Observ, Washington, DC 20392 USA.
[Lainey, Valery] Observ Paris, IMCCE, CNRS, UMR 8028, F-75014 Paris, France.
RP Castillo-Rogez, JC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM julie.c.castillo@jpl.nasa.gov; michael.efroimsky@usno.navy.mil;
lainey@imcce.fr
OI Efroimsky, Michael/0000-0003-1249-9622
FU NASA
FX The Authors are indebted to the Associate Editor, Francis Nimmo, and to
the referee, James Roberts, for the attention they gave to this work.
The manuscript benefitted greatly from the numerous corrections and
improvements kindly offered by these colleagues. The authors also
acknowledge the extremely important comments by Stan Peale that proved
to be of great help. M.E. is grateful to Veronique Dehant and Tim Van
Hoolst for highly valuable consultations on the theory of tides, and to
Ignacio Mosqueira and Gabriel Tobie for enlightening e-mail
conversations on the properties of Iapetus. J.C. is thankful to
Christophe Sotin for pointing out proton reorientation as a possible
source of attenuation, to Mathieu Choukroun for discussions on the
distribution of second-phase impurities in ice, and to Bruce Bills for
useful comments on the earlier version of the text. A part of this work
has been conducted at the U.S. Naval Observatory (USNO). M.E.
acknowledges the support from his USNO colleagues, especially from John
Bangert. A part of this work has been conducted at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
NASA. J.C. acknowledges the extensive use of NASA's Astrophysical Data
System and JPL's Library Beacon server. All rights reserved. Government
sponsorship acknowledged.
NR 78
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD SEP 20
PY 2011
VL 116
AR E09008
DI 10.1029/2010JE003664
PG 29
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 825LA
UT WOS:000295275300001
ER
PT J
AU Arzoumanian, Z
Gotthelf, EV
Ransom, SM
Safi-Harb, S
Kothes, R
Landecker, TL
AF Arzoumanian, Z.
Gotthelf, E. V.
Ransom, S. M.
Safi-Harb, S.
Kothes, R.
Landecker, T. L.
TI DISCOVERY OF AN ENERGETIC PULSAR ASSOCIATED WITH SNR G76.9+1.0
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: supernova remnants; pulsars: individual (PSR J2022+3842); stars:
neutron; X-rays: stars
ID GAMMA-RAY SOURCE; SUPERNOVA REMNANT; VELA PULSAR; WIND NEBULA;
SPIN-DOWN; DA 495; YOUNG
AB We report the discovery of PSR J2022 + 3842, a 24 ms radio and X-ray pulsar in the supernova remnant G76.9 + 1.0, in observations with the Chandra X-ray Observatory, the Robert C. Byrd Green Bank Radio Telescope, and the Rossi X-ray Timing Explorer (RXTE). The pulsar's spin-down rate implies a rotation-powered luminosity (E) over dot = 1.2 x 10(38) erg s(-1), a surface dipole magnetic field strength B-s = 1.0 x 10(12) G, and a characteristic age of 8.9 kyr. PSR J2022 + 3842 is thus the second-most energetic Galactic pulsar known, after the Crab pulsar, as well as the most rapidly rotating young, radio-bright pulsar known. The radio pulsations are highly dispersed and broadened by interstellar scattering, and we find that a large (delta f/f approximate to 1.9 x 10(-6)) spin glitch must have occurred between our discovery and confirmation observations. The X-ray pulses are narrow (0.06 cycles FWHM) and visible up to 20 keV, consistent with magnetospheric emission from a rotation-powered pulsar. The Chandra X-ray image identifies the pulsar with a hard, unresolved source at the midpoint of the double-lobed radio morphology of G76.9 + 1.0 and embedded within faint, compact X-ray nebulosity. The spatial relationship of the X-ray and radio emissions is remarkably similar to the extended structure seen around the Vela pulsar. The combined Chandra and RXTE pulsar spectrum is well fitted by an absorbed power-law model with column density N-H = (1.7 +/- 0.3) x 10(22) cm(-2) and photon index Gamma = 1.0 +/- 0.2; this implies that the Chandra point-source flux is virtually 100% pulsed. For a distance of 10 kpc, the X-ray luminosity of PSR J2022 + 3842 is L-X(2-10 keV) = 7.0 x 10(33) erg s(-1). Despite being extraordinarily energetic, PSR J2022 + 3842 lacks a bright X-ray wind nebula and has an unusually low conversion efficiency of spin-down power to X-ray luminosity, L-X/(E) over dot = 5.9 x 10(-5).
C1 [Arzoumanian, Z.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
[Arzoumanian, Z.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Arzoumanian, Z.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Gotthelf, E. V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22901 USA.
[Safi-Harb, S.] Univ Manitoba, Canada Res Chair, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada.
[Kothes, R.; Landecker, T. L.] Domin Radio Astrophys Observ, Herzberg Inst Astrophys, Natl Res Council Canada, Penticton, BC V2A 6J9, Canada.
RP Arzoumanian, Z (reprint author), NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Code 662, Greenbelt, MD 20771 USA.
EM Zaven.Arzoumanian@nasa.gov
OI Ransom, Scott/0000-0001-5799-9714
FU National Aeronautics and Space Administration [GO5-6077Z, NAS8-03060];
National Science Foundation; Natural Sciences and Engineering Research
Council of Canada (NSERC); Canada Research Chairs program; Associated
Universities, Inc.
FX Support for this work was provided by the National Aeronautics and Space
Administration through Chandra Award Number GO5-6077Z issued by the
Chandra X-ray Observatory Center, which is operated by the Smithsonian
Astrophysical Observatory for and on behalf of NASA under contract
NAS8-03060. The National Radio Astronomy Observatory is a facility of
the National Science Foundation operated under cooperative agreement by
Associated Universities, Inc. We have also made use of RXTE data
provided by the High Energy Astrophysics Science Archive Research Center
at NASA's Goddard Space Flight Center, as well as data products from the
Two Micron All Sky Survey, a joint project of the University of
Massachusetts and the Infrared Processing and Analysis Center/Caltech,
funded by NASA and the National Science Foundation. S. S. H.
acknowledges support by the Natural Sciences and Engineering Research
Council of Canada (NSERC) and the Canada Research Chairs program.
NR 31
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2011
VL 739
IS 1
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DI 10.1088/0004-637X/739/1/39
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DS
UT WOS:000294955700039
ER
PT J
AU De Marchi, G
Paresce, F
Panagia, N
Beccari, G
Spezzi, L
Sirianni, M
Andersen, M
Mutchler, M
Balick, B
Dopita, MA
Frogel, JA
Whitmore, BC
Bond, H
Calzetti, D
Carollo, CM
Disney, MJ
Hall, DNB
Holtzman, JA
Kimble, RA
McCarthy, PJ
O'Connell, RW
Saha, A
Silk, JI
Trauger, JT
Walker, AR
Windhorst, RA
Young, ET
AF De Marchi, Guido
Paresce, Francesco
Panagia, Nino
Beccari, Giacomo
Spezzi, Loredana
Sirianni, Marco
Andersen, Morten
Mutchler, Max
Balick, Bruce
Dopita, Michael A.
Frogel, Jay A.
Whitmore, Bradley C.
Bond, Howard
Calzetti, Daniela
Carollo, C. Marcella
Disney, Michael J.
Hall, Donald N. B.
Holtzman, Jon A.
Kimble, Randy A.
McCarthy, Patrick J.
O'Connell, Robert W.
Saha, Abhijit
Silk, Joseph I.
Trauger, John T.
Walker, Alistair R.
Windhorst, Rogier A.
Young, Erick T.
TI STAR FORMATION IN 30 DORADUS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: star clusters: individual (30 Dor); galaxies: stellar content;
Magellanic Clouds; stars: formation; stars: pre-main sequence
ID HUBBLE-SPACE-TELESCOPE; LARGE-MAGELLANIC-CLOUD; INITIAL MASS FUNCTION;
YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS; RED GIANT CLUMP;
INTERMEDIATE-MASS; SN 1987A; DISTANCE DETERMINATIONS; FORMATION HISTORY
AB Using observations obtained with the Wide-Field Camera 3 on board the Hubble Space Telescope, we have studied the properties of the stellar populations in the central regions of 30 Dor in the Large Magellanic Cloud. The observations clearly reveal the presence of considerable differential extinction across the field. We characterize and quantify this effect using young massive main-sequence stars to derive a statistical reddening correction for most objects in the field. We then search for pre-main-sequence (PMS) stars by looking for objects with a strong (>4 sigma) H alpha excess emission and find about 1150 of them over the entire field. Comparison of their location in the Hertzsprung-Russell diagram with theoretical PMS evolutionary tracks for the appropriate metallicity reveals that about one-third of these objects are younger than similar to 4 Myr, compatible with the age of the massive stars in the central ionizing cluster R 136, whereas the rest have ages up to similar to 30 Myr, with a median age of similar to 12 Myr. This indicates that star formation has proceeded over an extended period of time, although we cannot discriminate between an extended episode and a series of short and frequent bursts that are not resolved in time. While the younger PMS population preferentially occupies the central regions of the cluster, older PMS objects are more uniformly distributed across the field and are remarkably few at the very center of the cluster. We attribute this latter effect to photo-evaporation of the older circumstellar disks caused by the massive ionizing members of R 136.
C1 [De Marchi, Guido; Spezzi, Loredana; Sirianni, Marco; Andersen, Morten] European Space Agcy, Dept Space Sci, NL-2200 AG Noordwijk, Netherlands.
[Paresce, Francesco] Ist Astrofis Spaziale & Fis Cosm, I-40129 Bologna, Italy.
[Panagia, Nino; Mutchler, Max; Whitmore, Bradley C.; Bond, Howard] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Panagia, Nino] Osserv Astrofis Catania, INAF CT, I-95123 Catania, Italy.
[Panagia, Nino] Supernova Ltd, Virgin Gorda, British Virgin, W Ind Assoc St.
[Beccari, Giacomo] European So Observ, D-85748 Garching, Germany.
[Balick, Bruce] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Dopita, Michael A.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo & Siding Spring Observ, Weston, ACT 2611, Australia.
[Dopita, Michael A.; Frogel, Jay A.] King Abdulaziz Univ, Dept Astron, Jeddah 21413, Saudi Arabia.
[Dopita, Michael A.; Hall, Donald N. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Frogel, Jay A.] Galaxies Unltd, Potomac, MD 20854 USA.
[Calzetti, Daniela] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Carollo, C. Marcella] ETH, Dept Phys, CH-8093 Zurich, Switzerland.
[Disney, Michael J.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Holtzman, Jon A.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Kimble, Randy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McCarthy, Patrick J.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[O'Connell, Robert W.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Saha, Abhijit] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Silk, Joseph I.] Univ Oxford, Dept Phys, Oxford OX1 3PU, England.
[Trauger, John T.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Walker, Alistair R.] Cerro Tololo Interamer Observ, La Serena, Chile.
[Windhorst, Rogier A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Young, Erick T.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
RP De Marchi, G (reprint author), European Space Agcy, Dept Space Sci, Keplerlaan 1, NL-2200 AG Noordwijk, Netherlands.
EM gdemarchi@rssd.esa.int
RI Dopita, Michael/P-5413-2014;
OI Dopita, Michael/0000-0003-0922-4986; silk, joe/0000-0002-1566-8148
FU HST-NASA [GO-11547.06A, GO-11653.12A]; STScI-DDRF [D0001.82435]
FX We are grateful to an anonymous referee, whose suggestions have helped
us to improve the presentation of this work. This paper is based on
Early Release Science observations made by the WFC3 Scientific Oversight
Committee. We are grateful to the Director of the Space Telescope
Science Institute for awarding Director's Discretionary time for this
programme. F. P. is grateful to the Space Science Department of ESA for
their hospitality via the visitor programme. N.P. acknowledges partial
support by HST-NASA grants GO-11547.06A and GO-11653.12A, and STScI-DDRF
grant D0001.82435.
NR 69
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2011
VL 739
IS 1
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DI 10.1088/0004-637X/739/1/27
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DS
UT WOS:000294955700027
ER
PT J
AU Dunkley, J
Hlozek, R
Sievers, J
Acquaviva, V
Ade, PAR
Aguirre, P
Amiri, M
Appel, JW
Barrientos, LF
Battistelli, ES
Bond, JR
Brown, B
Burger, B
Chervenak, J
Das, S
Devlin, MJ
Dicker, SR
Doriese, WB
Dunner, R
Essinger-Hileman, T
Fisher, RP
Fowler, JW
Hajian, A
Halpern, M
Hasselfield, M
Hernandez-Monteagudo, C
Hilton, GC
Hilton, M
Hincks, AD
Huffenberger, KM
Hughes, DH
Hughes, JP
Infante, L
Irwin, KD
Juin, JB
Kaul, M
Klein, J
Kosowsky, A
Lau, JM
Limon, M
Lin, YT
Lupton, RH
Marriage, TA
Marsden, D
Mauskopf, P
Menanteau, F
Moodley, K
Moseley, H
Netterfield, CB
Niemack, MD
Nolta, MR
Page, LA
Parker, L
Partridge, B
Reid, B
Sehgal, N
Sherwin, B
Spergel, DN
Staggs, ST
Swetz, DS
Switzer, ER
Thornton, R
Trac, H
Tucker, C
Warne, R
Wollack, E
Zhao, Y
AF Dunkley, J.
Hlozek, R.
Sievers, J.
Acquaviva, V.
Ade, P. A. R.
Aguirre, P.
Amiri, M.
Appel, J. W.
Barrientos, L. F.
Battistelli, E. S.
Bond, J. R.
Brown, B.
Burger, B.
Chervenak, J.
Das, S.
Devlin, M. J.
Dicker, S. R.
Doriese, W. Bertrand
Duenner, R.
Essinger-Hileman, T.
Fisher, R. P.
Fowler, J. W.
Hajian, A.
Halpern, M.
Hasselfield, M.
Hernandez-Monteagudo, C.
Hilton, G. C.
Hilton, M.
Hincks, A. D.
Huffenberger, K. M.
Hughes, D. H.
Hughes, J. P.
Infante, L.
Irwin, K. D.
Juin, J. B.
Kaul, M.
Klein, J.
Kosowsky, A.
Lau, J. M.
Limon, M.
Lin, Y-T.
Lupton, R. H.
Marriage, T. A.
Marsden, D.
Mauskopf, P.
Menanteau, F.
Moodley, K.
Moseley, H.
Netterfield, C. B.
Niemack, M. D.
Nolta, M. R.
Page, L. A.
Parker, L.
Partridge, B.
Reid, B.
Sehgal, N.
Sherwin, B.
Spergel, D. N.
Staggs, S. T.
Swetz, D. S.
Switzer, E. R.
Thornton, R.
Trac, H.
Tucker, C.
Warne, R.
Wollack, E.
Zhao, Y.
TI THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGICAL PARAMETERS FROM THE 2008
POWER SPECTRUM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmological parameters; cosmology:
observations
ID PROBE WMAP OBSERVATIONS; MICROWAVE BACKGROUND ANISOTROPIES; PRIMORDIAL
HELIUM ABUNDANCE; BIG-BANG NUCLEOSYNTHESIS; MASSIVE GALAXY CLUSTERS;
STAR-FORMING GALAXIES; SOUTH-POLE TELESCOPE; INFLATIONARY UNIVERSE;
HUBBLE CONSTANT; OBSERVED GROWTH
AB We present cosmological parameters derived from the angular power spectrum of the cosmic microwave background (CMB) radiation observed at 148 GHz and 218 GHz over 296 deg(2) with the Atacama Cosmology Telescope (ACT) during its 2008 season. ACT measures fluctuations at scales 500 < l < 10,000. We fit a model for the lensed CMB, Sunyaev-Zel'dovich (SZ), and foreground contribution to the 148 GHz and 218 GHz power spectra, including thermal and kinetic SZ, Poisson power from radio and infrared point sources, and clustered power from infrared point sources. At l = 3000, about half the power at 148 GHz comes from primary CMB after masking bright radio sources. The power from thermal and kinetic SZ is estimated to be B-3000 = 6.8 +/- 2.9 mu K-2, where B-l = l (l + 1) C-l/2 pi. The IR Poisson power at 148 GHz is B-3000 = 7.8 +/- 0.7 mu K-2 (Cl = 5.5 +/- 0.5 nK(2)), and a clustered IR component is required with B-3000 = 4.6 +/- 0.9 mu K-2, assuming an analytic model for its power spectrum shape. At 218 GHz only about 15% of the power, approximately 27 mu K-2, is CMB anisotropy at l = 3000. The remaining 85% is attributed to IR sources (approximately 50% Poisson and 35% clustered), with spectral index alpha = 3.69 +/- 0.14 for flux scaling as S(v) proportional to v(alpha). We estimate primary cosmological parameters from the less contaminated 148 GHz spectrum, marginalizing over SZ and source power. The Lambda CDM cosmological model is a good fit to the data (chi(2)/dof = 29/46), and Lambda CDM parameters estimated from ACT+Wilkinson Microwave Anisotropy Probe (WMAP) are consistent with the seven-year WMAP limits, with scale invariant ns = 1 excluded at 99.7% confidence level (CL) (3 sigma). A model with no CMB lensing is disfavored at 2.8 sigma. By measuring the third to seventh acoustic peaks, and probing the Silk damping regime, the ACT data improve limits on cosmological parameters that affect the small-scale CMB power. The ACT data combined with WMAP give a 6 sigma detection of primordial helium, with Y-P = 0.313 +/- 0.044, and a 4 sigma detection of relativistic species, assumed to be neutrinos, with N-eff = 5.3 +/- 1.3 (4.6 +/- 0.8 with BAO+H-0 data). From the CMB alone the running of the spectral index is constrained to be dn(s)/d ln k = - 0.034 +/- 0.018, the limit on the tensor-to-scalar ratio is r < 0.25 (95% CL), and the possible contribution of Nambu cosmic strings to the power spectrum is constrained to string tension G mu < 1.6 x 10(-7) ( 95% CL).
C1 [Dunkley, J.; Hlozek, R.] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England.
[Dunkley, J.; Appel, J. W.; Das, S.; Essinger-Hileman, T.; Fisher, R. P.; Fowler, J. W.; Hajian, A.; Hincks, A. D.; Lau, J. M.; Limon, M.; Niemack, M. D.; Page, L. A.; Parker, L.; Reid, B.; Sherwin, B.; Staggs, S. T.; Switzer, E. R.; Zhao, Y.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
[Dunkley, J.; Acquaviva, V.; Das, S.; Hajian, A.; Lin, Y-T.; Lupton, R. H.; Marriage, T. A.; Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Sievers, J.; Bond, J. R.; Hajian, A.; Nolta, M. R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Acquaviva, V.; Hughes, J. P.; Menanteau, F.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Ade, P. A. R.; Mauskopf, P.; Tucker, C.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Aguirre, P.; Barrientos, L. F.; Duenner, R.; Infante, L.; Juin, J. B.; Lin, Y-T.] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile.
[Amiri, M.; Battistelli, E. S.; Burger, B.; Halpern, M.; Hasselfield, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada.
[Battistelli, E. S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy.
[Brown, B.; Kosowsky, A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Chervenak, J.; Moseley, H.; Wollack, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Das, S.] Univ Calif Berkeley, LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Das, S.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Devlin, M. J.; Dicker, S. R.; Kaul, M.; Klein, J.; Limon, M.; Marsden, D.; Swetz, D. S.; Thornton, R.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Doriese, W. Bertrand; Fowler, J. W.; Hilton, G. C.; Irwin, K. D.; Niemack, M. D.; Swetz, D. S.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA.
[Hernandez-Monteagudo, C.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Hilton, M.; Moodley, K.; Warne, R.] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Hilton, M.; Moodley, K.] Rosebank, Ctr High Performance Comp, Cape Town, South Africa.
[Huffenberger, K. M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA.
[Hughes, D. H.] INAOE, Puebla, Mexico.
[Lau, J. M.; Sehgal, N.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Lau, J. M.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Limon, M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Lin, Y-T.] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan.
[Marriage, T. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Partridge, B.] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
[Reid, B.] Univ Barcelona, ICC, E-08028 Barcelona, Spain.
[Switzer, E. R.] Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Thornton, R.] W Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA.
[Trac, H.] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.
[Trac, H.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Dunkley, J (reprint author), Univ Oxford, Subdept Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England.
RI Klein, Jeffrey/E-3295-2013; Spergel, David/A-4410-2011; Hilton, Matthew
James/N-5860-2013; Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012;
OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451;
Huffenberger, Kevin/0000-0001-7109-0099; Sievers,
Jonathan/0000-0001-6903-5074; Limon, Michele/0000-0002-5900-2698
FU U.S. National Science Foundation [AST-0408698, PHY-0355328, AST-0707731,
PIRE-0507768]; Princeton University; University of Pennsylvania; RCUK
Fellowship; Rhodes Trust; NASA [NNX08AH30G]; Natural Science and
Engineering Research Council of Canada (NSERC); NSF [AST-0546035,
AST-0606975]; FONDAP Centro de Astrofisica; CONICYT; MECESUP; Fundacion
Andes; NSF Physics Frontier Center [PHY-0114422]; South African National
Research Foundation (NRF); South African Centre for High Performance
Computing (CHPC); South African Square Kilometer Array (SKA); Berkeley
Center for Cosmological Physics; World Premier International Research
Center Initiative, MEXT, Japan; U.S. Department of Energy
[DE-AC3-76SF00515]; Canada Foundation for Innovation under the auspices
of Compute Canada; Government of Toronto; NASA Office of Space Science
FX ACT is on the Chajnantor Science preserve, which was made possible by
the Chilean Comision Nacional de Investigacion Cientifica y Tecnologica.
We are grateful for the assistance we received at various times from the
ALMA, APEX, ASTE, CBI/QUIET, and NANTEN2 groups. The PWV data come from
the public APEX weather Web site. Field operations were based at the Don
Esteban facility run by Astro-Norte. Reed Plimpton and David Jacobson
worked at the telescope during the 2008 season. We thank Norm Jarosik
for support throughout the project. We also thank Adam Moss and Richard
Battye for sharing their cosmic string power spectrum, Laurie Shaw and
Nick Battaglia for providing SZ power spectra, and Bruce Bassett for
suggestions on testing lensing in the power spectrum. We thank Marco
Viero and Graeme Addison for providing useful input on clustered point
sources. This work was supported by the U.S. National Science Foundation
through awards AST-0408698 for the ACT project, and PHY-0355328,
AST-0707731 and PIRE-0507768. Funding was also provided by Princeton
University and the University of Pennsylvania. The PIRE program made
possible exchanges between Chile, South Africa, Spain, and the US that
enabled this research program. J.D. acknowledges support from an RCUK
Fellowship. R. H. received funding from the Rhodes Trust. V. A., S. D.,
A. H., and T. M. were supported through NASA grant NNX08AH30G. A. D. H.
received additional support from a Natural Science and Engineering
Research Council of Canada (NSERC) PGS-D scholarship. A. K. and B. P.
were partially supported through NSF AST-0546035 and AST-0606975,
respectively, for work on ACT. L. I. acknowledges partial support from
FONDAP Centro de Astrofisica. R. D. was supported by CONICYT, MECESUP,
and Fundacion Andes. E. S. acknowledges support by NSF Physics Frontier
Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics.
K. M., M. H., and R. W. received financial support from the South
African National Research Foundation (NRF), the Meraka Institute via
funding for the South African Centre for High Performance Computing
(CHPC), and the South African Square Kilometer Array (SKA) Project. S.
D. acknowledges support from the Berkeley Center for Cosmological
Physics. Y.T.L. acknowledges support from the World Premier
International Research Center Initiative, MEXT, Japan. N.S. is supported
by the U.S. Department of Energy contract to SLAC no. DE-AC3-76SF00515.
Computations were performed on the GPC supercomputer at the SciNet HPC
Consortium. SciNet is funded by the Canada Foundation for Innovation
under the auspices of Compute Canada, the Government of Toronto. We
acknowledge the use of the Legacy Archive for Microwave Background Data
Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of
Space Science. The data will be made public through LAMBDA
(http://lambda.gsfc.nasa.gov/) and the ACT Web site
(http://www.physics.princeton.edu/act/).
NR 139
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2011
VL 739
IS 1
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DI 10.1088/0004-637X/739/1/52
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DS
UT WOS:000294955700052
ER
PT J
AU Stello, D
Meibom, S
Gilliland, RL
Grundahl, F
Hekker, S
Mosser, B
Kallinger, T
Mathur, S
Garcia, RA
Huber, D
Basu, S
Bedding, TR
Brogaard, K
Chaplin, WJ
Elsworth, YP
Molenda-Zakowicz, J
Szabo, R
Still, M
Jenkins, JM
Christensen-Dalsgaard, J
Kjeldsen, H
Serenelli, AM
Wohler, B
AF Stello, Dennis
Meibom, Soren
Gilliland, Ronald L.
Grundahl, Frank
Hekker, Saskia
Mosser, Benoit
Kallinger, Thomas
Mathur, Savita
Garcia, Rafael A.
Huber, Daniel
Basu, Sarbani
Bedding, Timothy R.
Brogaard, Karsten
Chaplin, William J.
Elsworth, Yvonne P.
Molenda-Zakowicz, Joanna
Szabo, Robert
Still, Martin
Jenkins, Jon M.
Christensen-Dalsgaard, Jorgen
Kjeldsen, Hans
Serenelli, Aldo M.
Wohler, Bill
TI AN ASTEROSEISMIC MEMBERSHIP STUDY OF THE RED GIANTS IN THREE OPEN
CLUSTERS OBSERVED BY KEPLER: NGC 6791, NGC 6819, AND NGC 6811
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE open clusters and associations: individual (NGC 6791, NGC6819, NGC6811);
stars: fundamental parameters; stars: interiors; stars: oscillations;
techniques: photometric
ID SOLAR-LIKE OSCILLATIONS; BOLOMETRIC CORRECTIONS; STELLAR EVOLUTION;
METAL ABUNDANCES; NGC-6791; STARS; OLD; CONSTRAINTS; AMPLITUDES;
ISOCHRONES
AB Studying star clusters offers significant advances in stellar astrophysics due to the combined power of having many stars with essentially the same distance, age, and initial composition. This makes clusters excellent test benches for verification of stellar evolution theory. To fully exploit this potential, it is vital that the star sample is uncontaminated by stars that are not members of the cluster. Techniques for determining cluster membership therefore play a key role in the investigation of clusters. We present results on three clusters in the Kepler field of view based on a newly established technique that uses asteroseismology to identify fore-or background stars in the field, which demonstrates advantages over classical methods such as kinematic and photometry measurements. Four previously identified seismic non-members in NGC6819 are confirmed in this study, and three additional non-members are found-two in NGC6819 and one in NGC6791. We further highlight which stars are, or might be, affected by blending, which needs to be taken into account when analyzing these Kepler data.
C1 [Stello, Dennis; Huber, Daniel; Bedding, Timothy R.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Meibom, Soren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Grundahl, Frank; Brogaard, Karsten] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Hekker, Saskia; Chaplin, William J.; Elsworth, Yvonne P.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Mosser, Benoit] Univ Paris 07, LESIA, CNRS, Univ Paris 06,Observ Paris, F-92195 Meudon, France.
[Kallinger, Thomas] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Kallinger, Thomas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Mathur, Savita] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Garcia, Rafael A.] Univ Paris 07, Lab AIM, CEA DSM CNRS, IRFU SAp,Ctr Saclay, F-91191 Gif Sur Yvette, France.
[Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Brogaard, Karsten] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada.
[Molenda-Zakowicz, Joanna] Uniwersytetu Wroclawskiego, Inst Astron, PL-51622 Wroclaw, Poland.
[Szabo, Robert] Hungarian Acad Sci, Konkoly Observ, H-1121 Budapest, Hungary.
[Still, Martin] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Jenkins, Jon M.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Serenelli, Aldo M.] Fac Ciencies, Inst Ciencias Espacio CSIC IEEC, Bellaterra 08193, Spain.
[Wohler, Bill] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
RP Stello, D (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
OI Kallinger, Thomas/0000-0003-3627-2561; Brogaard,
Karsten/0000-0003-2001-0276; Bedding, Timothy/0000-0001-5943-1460;
Szabo, Robert/0000-0002-3258-1909; Bedding, Tim/0000-0001-5222-4661;
Basu, Sarbani/0000-0002-6163-3472; Garcia, Rafael/0000-0002-8854-3776;
Serenelli, Aldo/0000-0001-6359-2769
FU NASA's Science Mission Directorate; Australian Research Council;
Hungarian Academy of Sciences; Hungarian OTKA [K83790, MB08C 81013]; UK
Science and Technology Facilities Council (STFC); Carlsberg Foundation;
National Science Foundation; Janos Bolyai Research Scholarship
FX Funding for this Discovery mission is provided by NASA's Science Mission
Directorate. The authors thank the entire Kepler team without whom this
investigation would not have been possible. D. S. acknowledges support
from the Australian Research Council. This project has been supported by
the "Lendulet" program of the Hungarian Academy of Sciences and the
Hungarian OTKA grant K83790 and MB08C 81013. S. H. acknowledges
financial support from the UK Science and Technology Facilities Council
(STFC). K. B. acknowledges financial support from the Carlsberg
Foundation. NCAR is supported by the National Science Foundation. R. S.
thanks the support of the Janos Bolyai Research Scholarship.
NR 45
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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 SEP 20
PY 2011
VL 739
IS 1
AR 13
DI 10.1088/0004-637X/739/1/13
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DS
UT WOS:000294955700013
ER
PT J
AU Krauss, MI
Chomiuk, L
Rupen, M
Roy, N
Mioduszewski, AJ
Sokoloski, JL
Nelson, T
Mukai, K
Bode, MF
Eyres, SPS
O'Brien, TJ
AF Krauss, Miriam I.
Chomiuk, Laura
Rupen, Michael
Roy, Nirupam
Mioduszewski, Amy J.
Sokoloski, J. L.
Nelson, Thomas
Mukai, Koji
Bode, M. F.
Eyres, S. P. S.
O'Brien, T. J.
TI EXPANDED VERY LARGE ARRAY NOVA PROJECT OBSERVATIONS OF THE CLASSICAL
NOVA V1723 AQUILAE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE binaries: general; novae, cataclysmic variables; stars: individual
(V1723 Aql); white dwarfs
ID RADIO-EMISSION; RS OPHIUCHI; VULPECULAE 1984; OUTBURST; MODELS; SHELL
AB We present radio light curves and spectra of the classical nova V1723 Aql obtained with the Expanded Very Large Array (EVLA). This is the first paper to showcase results from the EVLA Nova Project, which comprises a team of observers and theorists utilizing the greatly enhanced sensitivity and frequency coverage of EVLA radio observations, along with observations at other wavelengths, to reach a deeper understanding of the energetics, morphology, and temporal characteristics of nova explosions. Our observations of V1723 Aql span 1-37 GHz in frequency, and we report on data from 14 to 175 days following the time of the nova explosion. The broad frequency coverage and frequent monitoring show that the radio behavior of V1723 Aql does not follow the classic Hubble-flow model of homologous spherically expanding thermal ejecta. The spectra are always at least partially optically thin, and the flux rises on faster timescales than can be reproduced with linear expansion. Therefore, any description of the underlying physical processes must go beyond this simple picture. The unusual spectral properties and light curve evolution might be explained by multiple emitting regions or shocked material. Indeed, X-ray observations from Swift reveal that shocks are likely present.
C1 [Krauss, Miriam I.; Chomiuk, Laura; Rupen, Michael; Roy, Nirupam; Mioduszewski, Amy J.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Sokoloski, J. L.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Nelson, Thomas; Mukai, Koji] NASA GSFC, CRESST, Greenbelt, MD 20771 USA.
[Nelson, Thomas; Mukai, Koji] NASA GSFC, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Nelson, Thomas; Mukai, Koji] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Bode, M. F.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Eyres, S. P. S.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[O'Brien, T. J.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Chomiuk, Laura; Roy, Nirupam] Harvard Smithsonian Astrophys Observ, Cambridge, MA 02139 USA.
RP Krauss, MI (reprint author), Natl Radio Astron Observ, Socorro, NM 87801 USA.
EM mkrauss@nrao.edu; lchomiuk@nrao.edu; mrupen@nrao.edu; nroy@nrao.edu;
amiodusz@nrao.edu; jsokoloski@astro.columbia.edu;
thomas.nelson@nasa.gov; koji.mukai-1@nasa.gov; mfb@astro.livjm.ac.uk;
spseyres@uclan.ac.uk; tim.obrien@manchester.ac.uk
NR 22
TC 11
Z9 11
U1 0
U2 7
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 SEP 20
PY 2011
VL 739
IS 1
AR L6
DI 10.1088/2041-8205/739/1/L6
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818OQ
UT WOS:000294762900006
ER
PT J
AU Melis, C
Duchene, G
Chomiuk, L
Palmer, P
Perrin, MD
Maddison, ST
Menard, F
Stapelfeldt, K
Pinte, C
Duvert, G
AF Melis, Carl
Duchene, G.
Chomiuk, Laura
Palmer, Patrick
Perrin, M. D.
Maddison, S. T.
Menard, F.
Stapelfeldt, K.
Pinte, C.
Duvert, G.
TI MICROWAVE OBSERVATIONS OF EDGE-ON PROTOPLANETARY DISKS: PROGRAM OVERVIEW
AND FIRST RESULTS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; circumstellar matter; planets and
satellites: formation; protoplanetary disks; stars: individual (IRAS
04368+2557); stars: variables: T Tauri, Herbig Ae/Be
ID YOUNG STELLAR OBJECTS; T-TAURI STARS; CIRCUMSTELLAR DISKS; DUST
DISTRIBUTION; CORONET CLUSTER; IRAS 18059-3211; GRAIN-GROWTH; DARK
CLOUD; X-RAY; AURIGA
AB We are undertaking a multi-frequency Expanded Very Large Array (EVLA) survey of edge-on protoplanetary disks to probe the growth of solids in each disk, sedimentation of such material into the disk midplane, and the connection of these phenomena to the planet formation process. The projection of edge-on disk systems along our line of sight enables a study of the vertical stratification of large grains with fewer model dependencies than would be required for disks that are more face-on. Robust studies of the spatial distribution of grains up to approximate to 1 cm in size are possible with the wavelength range and sensitivity of the EVLA. In this contribution, we describe target selection and observational strategies. First results concerning the Class 0 source IRAS 04368+2557 (L1527 IRS) are presented, including a study of this source's 8.46 GHz continuum variability over short and long time baselines and an indication that its protoplanetary disk may have a dearth of pebble-sized grains.
C1 [Melis, Carl] Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92093 USA.
[Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Duchene, G.; Menard, F.; Pinte, C.; Duvert, G.] UJF Grenoble 1 CNRS INSU, Inst Planetol & Astrophys Grenoble IPAG, UMR 5274, F-38041 Grenoble 9, France.
[Chomiuk, Laura] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Palmer, Patrick] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Perrin, M. D.] Space Telescope Sci Inst, Baltimore, MD 21231 USA.
[Maddison, S. T.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Stapelfeldt, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Melis, C (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92093 USA.
EM cmelis@ucsd.edu
RI Stapelfeldt, Karl/D-2721-2012
FU National Science Foundation (NSF) [AST-1003318, AST-0702933]; PNPS of
CNRS/INSU; ANR of France [ANR-07-BLAN-0221]; European Commission
[PIEF-GA-2008-220891]; ANR [ANR-2010-JCJC-0504-01]
FX We thank the anonymous referee for comments that helped improve this
work. C.M. acknowledges support from the National Science Foundation
under award No. AST-1003318. M.D.P. was supported by NSF Postdoctoral
Fellowship No. AST-0702933. F. M., C. P., and G. D. acknowledge PNPS of
CNRS/INSU, and ANR (contract ANR-07-BLAN-0221) of France for financial
support. C. P. acknowledges funding from the European Commission's 7th
Framework Program (contract PIEF-GA-2008-220891) and from ANR under
contract ANR-2010-JCJC-0504-01.
NR 50
TC 8
Z9 8
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 20
PY 2011
VL 739
IS 1
AR L7
DI 10.1088/2041-8205/739/1/L7
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818OQ
UT WOS:000294762900007
ER
PT J
AU Sahai, R
Claussen, MJ
Schnee, S
Morris, MR
Contreras, CS
AF Sahai, R.
Claussen, M. J.
Schnee, S.
Morris, M. R.
Sanchez Contreras, C.
TI AN EXPANDED VERY LARGE ARRAY AND CARMA STUDY OF DUSTY DISKS AND TORII
WITH LARGE GRAINS IN DYING STARS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; binaries: general; circumstellar matter;
radio continuum: stars; stars: AGB and post-AGB; stars: mass-loss
ID POST-AGB STARS; MORPHOLOGICAL CLASSIFICATION-SYSTEM; GIANT BRANCH STARS;
PREPLANETARY NEBULA; PLANETARY-NEBULAE; RED-RECTANGLE; ACCRETION DISKS;
EVOLVED STARS; DISCS; DEPLETION
AB We report the results of a pilot multiwavelength survey in the radio continuum (X, Ka, and Q bands, i.e., from 3.6 cm to 7 mm) carried out with the Expanded Very Large Array (EVLA) in order to confirm the presence of very large dust grains in dusty disks and torii around the central stars in a small sample of post-asymptotic giant branch (pAGB) objects, as inferred from millimeter (mm) and submillimeter (submm) observations. Supporting mm-wave observations were also obtained with the Combined Array for Research in Millimeter-wave Astronomy toward three of our sources. Our EVLA survey has resulted in a robust detection of our most prominent submm emission source, the pre-planetary nebula (PPN) IRAS 22036+5306, in all three bands, and the disk-prominent pAGB object, RV Tau, in one band. The observed fluxes are consistent with optically thin free-free emission, and since they are insignificant compared to their submm/mm fluxes, we conclude that the latter must come from substantial masses of cool, large (mm-sized) grains. We find that the power-law emissivity in the cm-to-submm range for the large grains in IRAS22036 is nu(beta), with beta = 1-1.3. Furthermore, the value of beta in the 3-0.85 mm range for the three disk-prominent pAGB sources (beta <= 0.4) is significantly lower than that of IRAS22036, suggesting that the grains in pAGB objects with circumbinary disks are likely larger than those in the dusty waists of pre-planetary nebulae.
C1 [Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Claussen, M. J.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Schnee, S.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Morris, M. R.] Univ Calif Los Angeles, Div Astron, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Sanchez Contreras, C.] Astrobiol Ctr CSIC INTA, E-28691 Madrid, Spain.
RP Sahai, R (reprint author), CALTECH, Jet Prop Lab, MS 183-900, Pasadena, CA 91109 USA.
EM raghvendra.sahai@jpl.nasa.gov
RI Sanchez-Contreras, Carmen/N-3718-2015
OI Sanchez-Contreras, Carmen/0000-0002-6341-592X
FU NASA
FX R.S.'s contribution to the research described here was carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with NASA. Financial support was provided by NASA through a
Long Term Space Astrophysics award (to R. S. and M. M.).
NR 38
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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 SEP 20
PY 2011
VL 739
IS 1
AR L3
DI 10.1088/2041-8205/739/1/L3
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818OQ
UT WOS:000294762900003
ER
PT J
AU Moisan, JR
Moisan, TAH
Linkswiler, MA
AF Moisan, John R.
Moisan, Tiffany A. H.
Linkswiler, Matthew A.
TI An inverse modeling approach to estimating phytoplankton pigment
concentrations from phytoplankton absorption spectra
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID LIGHT-ABSORPTION; SATELLITE RETRIEVAL; MATRIX-INVERSION; C-PHYCOCYANIN;
OCEAN COLOR; PHYCOERYTHRIN; COEFFICIENT; SIZE
AB Phytoplankton absorption spectra and High-Performance Liquid Chromatography (HPLC) pigment observations from the Eastern U. S. and global observations from NASA's SeaBASS archive are used in a linear inverse calculation to extract pigments-pecific absorption spectra. Using these pigment-specific absorption spectra to reconstruct the phytoplankton absorption spectra results in high correlations at all visible wavelengths (r(2) from 0.83 to 0.98), and linear regressions (slopes ranging from 0.8 to 1.1). Higher correlations (r(2) from 0.75 to 1.00) are obtained in the visible portion of the spectra when the total phytoplankton absorption spectra are 'unpackaged' by multiplying the entire spectra by a factor that sets the total absorption at 675 nm to that expected from absorption spectra reconstruction using measured pigment concentrations and laboratory-derived pigment-specific absorption spectra. The derived pigment-specific absorption spectra were further used with the total phytoplankton absorption spectra in a second linear inverse calculation to estimate the various phytoplankton HPLC pigments. A comparison between the estimated and measured pigment concentrations for the 18 pigment fields showed good correlations (r(2) > 0.5) for 7 pigments and very good correlations (r(2) > 0.7) for chlorophyll a and fucoxanthin. Higher correlations result when the analysis is carried out at more local geographic scales. The ability to estimate phytoplankton pigments using pigment-specific absorption spectra is critical for using hyperspectral inverse models to retrieve phytoplankton pigment concentrations and other Inherent Optical Properties (IOPs) from passive remote sensing observations.
C1 [Moisan, John R.; Moisan, Tiffany A. H.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Hydrospher & Biospher Sci Lab, Wallops Isl, VA 23337 USA.
[Linkswiler, Matthew A.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, URS Corp, Wallops Isl, VA 23337 USA.
RP Moisan, JR (reprint author), NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Hydrospher & Biospher Sci Lab, Bldg N159,Rm E217, Wallops Isl, VA 23337 USA.
EM john.r.moisan@nasa.gov
RI Moisan, John/B-8762-2016
OI Moisan, John/0000-0002-8078-8939
FU NASA
FX We thank Kristin Golmon for earlier validation, testing and development
of a MATLAB version of the inversion algorithm using MATLAB software
through the support of the NASA USRP Student Program. We thank Kristen
Blattner and Carla P. Makinen for processing of some of the absorption
data. We thank Frank Hoge and Paul Lyon for their careful reading and
insightful comments. We also would like to acknowledge the two reviewers
of the manuscript whose constructive criticisms have made this a much
more robust study. Our HPLC data sets (BIOME, COBY, and MAA cruises)
were processed by Laurie van Heukelum (UMCES, Univ. of MD, Horn Point).
Our work is partially funded by the Biodiversity Program (TAM) at NASA
and internal NASA funds. Special acknowledgments are made to those who
have contributed their valuable data sets on phytoplankton absorption
and HPLC pigment observations to the NASA SeaBASS data archive, and to
those who have maintained the SeaBASS archive, specifically Jeremy
Werdell (NASA/GSFC). Noteworthy contributors to the observations used in
this study include: Norman Nelson and David Siegel (UC Santa Barbara),
Lawrence Harding (UMCES, University of Maryland, Horn Point), Richard
Zimmerman and the late Glenn Cota (ODU), Adjit Subramaniam (LDGO), Heidi
Sosik (WHOI) and Heidi Dierssen (University of Connecticut).
NR 40
TC 11
Z9 11
U1 2
U2 23
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 SEP 17
PY 2011
VL 116
AR C09018
DI 10.1029/2010JC006786
PG 16
WC Oceanography
SC Oceanography
GA 823OV
UT WOS:000295132800004
ER
PT J
AU Church, JA
White, NJ
Konikow, LF
Domingues, CM
Cogley, JG
Rignot, E
Gregory, JM
van den Broeke, MR
Monaghan, AJ
Velicogna, I
AF Church, John A.
White, Neil J.
Konikow, Leonard F.
Domingues, Catia M.
Cogley, J. Graham
Rignot, Eric
Gregory, Jonathan M.
van den Broeke, Michiel R.
Monaghan, Andrew J.
Velicogna, Isabella
TI Revisiting the Earth's sea-level and energy budgets from 1961 to 2008
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID CLIMATE-CHANGE; MASS-BALANCE; WATER-VAPOR; LAND WATER; OCEAN; HEAT;
RISE; TRENDS; TEMPERATURE; DIOXIDE
AB We review the sea-level and energy budgets together from 1961, using recent and updated estimates of all terms. From 1972 to 2008, the observed sea-level rise (1.8 +/- 0.2 mm yr(-1) from tide gauges alone and 2.1 +/- 0.2 mm yr(-1) from a combination of tide gauges and altimeter observations) agrees well with the sum of contributions (1.8 +/- 0.4 mm yr(-1)) in magnitude and with both having similar increases in the rate of rise during the period. The largest contributions come from ocean thermal expansion (0.8 mm yr(-1)) and the melting of glaciers and ice caps (0.7 mm yr(-1)), with Greenland and Antarctica contributing about 0.4 mm yr(-1). The cryospheric contributions increase through the period (particularly in the 1990s) but the thermosteric contribution increases less rapidly. We include an improved estimate of aquifer depletion (0.3 mm yr(-1)), partially offsetting the retention of water in dams and giving a total terrestrial storage contribution of -0.1 mm yr(-1). Ocean warming (90% of the total of the Earth's energy increase) continues through to the end of the record, in agreement with continued greenhouse gas forcing. The aerosol forcing, inferred as a residual in the atmospheric energy balance, is estimated as -0.8 +/- 0.4 W m(-2) for the 1980s and early 1990s. It increases in the late 1990s, as is required for consistency with little surface warming over the last decade. This increase is likely at least partially related to substantial increases in aerosol emissions from developing nations and moderate volcanic activity. Citation: Church, J. A., N. J. White, L. F. Konikow, C. M. Domingues, J. G. Cogley, E. Rignot, J. M. Gregory, M. R. van den Broeke, A. J. Monaghan, and I. Velicogna (2011), Revisiting the Earth's sea-level and energy budgets from 1961 to 2008, Geophys. Res. Lett., 38, L18601, doi:10.1029/2011GL048794.
C1 [Church, John A.; White, Neil J.] CSIRO Marine & Atmospher Res, Ctr Australian Weather & Climate Res & Wealth Oce, Hobart, Tas 7001, Australia.
[Konikow, Leonard F.] US Geol Survey, Natl Ctr 431, Reston, VA 20192 USA.
[Domingues, Catia M.] CSIRO Marine & Atmospher Res, Antarctic Climate & Ecosyst Cooperat Res Ctr, Aspendale, Vic 3195, Australia.
[Cogley, J. Graham] Trent Univ, Dept Geog, Peterborough, ON K9J 7B8, Canada.
[Rignot, Eric; Velicogna, Isabella] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Rignot, Eric; Velicogna, Isabella] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Gregory, Jonathan M.] Univ Reading, Dept Meteorol, NCAS Climate, Reading RG6 6BB, Berks, England.
[Gregory, Jonathan M.] Hadley Ctr, Met Off, Exeter, Devon, England.
[van den Broeke, Michiel R.] Univ Utrecht, Inst Marine & Atmospher Res, NL-3508 TA Utrecht, Netherlands.
[Monaghan, Andrew J.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
RP Church, JA (reprint author), CSIRO Marine & Atmospher Res, Ctr Australian Weather & Climate Res, GPO Box 1538, Hobart, Tas 7001, Australia.
EM john.church@csiro.au
RI White, Neil/B-2077-2013; Church, John/A-1541-2012; Van den Broeke,
Michiel/F-7867-2011; Rignot, Eric/A-4560-2014; Domingues, Catia
/A-2901-2015; Gregory, Jonathan/J-2939-2016;
OI Church, John/0000-0002-7037-8194; Van den Broeke,
Michiel/0000-0003-4662-7565; Rignot, Eric/0000-0002-3366-0481;
Domingues, Catia /0000-0001-5100-4595; Gregory,
Jonathan/0000-0003-1296-8644; Monaghan, Andrew/0000-0002-8170-2359
FU Australian Climate Change Science Program; CSIRO Office of the Chief
Executive (OCE)
FX This paper is a contribution to the Common-wealth Scientific Industrial
Research Organization (CSIRO) Climate Change Research Program. J.A.C.,
N.J.W. were partly funded by the Australian Climate Change Science
Program C.M.D. was supported by a CSIRO Office of the Chief Executive
(OCE) Postdoctoral Fellowship. The Centre for Australian Weather and
Climate Research is a partnership between CSIRO and the Australian
Bureau of Meteorology. National Aeronautics and Space Administration &
Centre National d'Etudes Spaciales provided the satellite altimeter
data, Permanent Service for Meal Sea Level the tide-gauge data.
NR 58
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Z9 201
U1 9
U2 98
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 16
PY 2011
VL 38
AR L18601
DI 10.1029/2011GL048794
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA 823PQ
UT WOS:000295135500005
ER
PT J
AU Hsu, HW
Postberg, F
Kempf, S
Trieloff, M
Burton, M
Roy, M
Moragas-Klostermeyer, G
Srama, R
AF Hsu, H-W.
Postberg, F.
Kempf, S.
Trieloff, M.
Burton, M.
Roy, M.
Moragas-Klostermeyer, G.
Srama, R.
TI Stream particles as the probe of the dust-plasma-magnetosphere
interaction at Saturn
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID INTERPLANETARY MAGNETIC-FIELD; SECONDARY-ELECTRON EMISSION; E-RING
PARTICLES; ROTATION PERIOD; SPACE PLASMAS; NEUTRAL CLOUD; SOLAR-SYSTEM;
COSMIC DUST; WATER ICE; ENCELADUS
AB We analyze the dynamics and composition of Saturnian stream particles measured by the Cosmic Dust Analyser (CDA) onboard the Cassini spacecraft. To reconstruct the dynamical properties of Saturnian stream particles, we adopt a backward tracing method with in situ solar wind measurements to filter out the influence of the interplanetary magnetic field. Our results show that stream particles from Saturn have sizes ranging from 2 to 8 nm (radius) with ejection velocities between 50 and 200 kms(-1). Moreover, the derived "ejection region" of stream particles in the outer part of Saturn's E ring is indicative of the dust charging condition profile in the planet's magnetosphere. By using the Cassini magnetospheric plasma measurements as input, our ejection model considers stochastic charging and well reproduces the dynamical properties of stream particles derived from backward simulations. An updated analysis of CDA stream-particle mass spectra confirms that the silicateous material is the most probable composition of Saturnian stream particles, in contrast to E ring particles whose composition is dominated by water ice. This compositional discrepancy can be reproduced by our model if the different sputter efficiencies of silicateous material and water ice are considered. We suggest that silicateous impurities released from icy grains at the outer E ring are the most probable source of Saturnian stream particles. Finally, we discuss the role of dust particles as a mobile neutral reservoir in Saturn's magnetosphere which may be responsible for certain features in the Cassini O and O(2)(+) measurements.
C1 [Hsu, H-W.; Postberg, F.; Kempf, S.; Moragas-Klostermeyer, G.; Srama, R.] MPI Kernphys, D-69117 Heidelberg, Germany.
[Burton, M.; Roy, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hsu, H-W.; Postberg, F.; Trieloff, M.] Univ Heidelberg, Inst Geowissensch, D-69120 Heidelberg, Germany.
[Hsu, H-W.; Kempf, S.; Moragas-Klostermeyer, G.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Kempf, S.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, Braunschweig, Germany.
[Srama, R.] Univ Stuttgart, Inst Raumfahrtsyst, Stuttgart, Germany.
RP Hsu, HW (reprint author), MPI Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany.
EM hsu@mpi-hd.mpg.de
OI KEMPF, SASCHA/0000-0001-5236-3004
FU DFG [KE 1384/1-1]; Priority Programme [1385]; Deutsche
Forschungsgemeinschaft
FX This project is supported by the DFG under the grant KE 1384/1-1 at the
Max-Planck Institut fur Kernphysik. We acknowledge fruitful discussions
with J. Schmidt on the charging process. We thank M. E. Hill, who
graciously provided us with the solar wind speed data. We also
acknowledge anonymous referees for the valuable comments. H.-W.H. thanks
his family and Chun-Yu. M. T. and F. P. acknowledge support from the
Priority Programme 1385 "The first 10 million years of the solar
system-a planetary materials approach" funded by Deutsche
Forschungsgemeinschaft.
NR 97
TC 10
Z9 10
U1 1
U2 4
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 SEP 16
PY 2011
VL 116
AR A09215
DI 10.1029/2011JA016488
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823PE
UT WOS:000295134000002
ER
PT J
AU Doyle, LR
Carter, JA
Fabrycky, DC
Slawson, RW
Howell, SB
Winn, JN
Orosz, JA
Prsa, A
Welsh, WF
Quinn, SN
Latham, D
Torres, G
Buchhave, LA
Marcy, GW
Fortney, JJ
Shporer, A
Ford, EB
Lissauer, JJ
Ragozzine, D
Rucker, M
Batalha, N
Jenkins, JM
Borucki, WJ
Koch, D
Middour, CK
Hall, JR
McCauliff, S
Fanelli, MN
Quintana, EV
Holman, MJ
Caldwell, DA
Still, M
Stefanik, RP
Brown, WR
Esquerdo, GA
Tang, SM
Furesz, G
Geary, JC
Berlind, P
Calkins, ML
Short, DR
Steffen, JH
Sasselov, D
Dunham, EW
Cochran, WD
Boss, A
Haas, MR
Buzasi, D
Fischer, D
AF Doyle, Laurance R.
Carter, Joshua A.
Fabrycky, Daniel C.
Slawson, Robert W.
Howell, Steve B.
Winn, Joshua N.
Orosz, Jerome A.
Prsa, Andrej
Welsh, William F.
Quinn, Samuel N.
Latham, David
Torres, Guillermo
Buchhave, Lars A.
Marcy, Geoffrey W.
Fortney, Jonathan J.
Shporer, Avi
Ford, Eric B.
Lissauer, Jack J.
Ragozzine, Darin
Rucker, Michael
Batalha, Natalie
Jenkins, Jon M.
Borucki, William J.
Koch, David
Middour, Christopher K.
Hall, Jennifer R.
McCauliff, Sean
Fanelli, Michael N.
Quintana, Elisa V.
Holman, Matthew J.
Caldwell, Douglas A.
Still, Martin
Stefanik, Robert P.
Brown, Warren R.
Esquerdo, Gilbert A.
Tang, Sumin
Furesz, Gabor
Geary, John C.
Berlind, Perry
Calkins, Michael L.
Short, Donald R.
Steffen, Jason H.
Sasselov, Dimitar
Dunham, Edward W.
Cochran, William D.
Boss, Alan
Haas, Michael R.
Buzasi, Derek
Fischer, Debra
TI Kepler-16: A Transiting Circumbinary Planet
SO SCIENCE
LA English
DT Article
ID CM DRACONIS; BINARY-SYSTEMS; GIANT PLANETS; STARS; PERFORMANCE;
ALGORITHM; SCIENCE; RADII; MASS
AB We report the detection of a planet whose orbit surrounds a pair of low-mass stars. Data from the Kepler spacecraft reveal transits of the planet across both stars, in addition to the mutual eclipses of the stars, giving precise constraints on the absolute dimensions of all three bodies. The planet is comparable to Saturn in mass and size and is on a nearly circular 229-day orbit around its two parent stars. The eclipsing stars are 20 and 69% as massive as the Sun and have an eccentric 41-day orbit. The motions of all three bodies are confined to within 0.5 degrees of a single plane, suggesting that the planet formed within a circumbinary disk.
C1 [Doyle, Laurance R.; Slawson, Robert W.; Jenkins, Jon M.; Quintana, Elisa V.; Caldwell, Douglas A.] SETI Inst, Carl Sagan Ctr Study Life Universe, Mountain View, CA 94043 USA.
[Carter, Joshua A.; Quinn, Samuel N.; Latham, David; Torres, Guillermo; Ragozzine, Darin; Holman, Matthew J.; Stefanik, Robert P.; Brown, Warren R.; Esquerdo, Gilbert A.; Tang, Sumin; Furesz, Gabor; Geary, John C.; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fabrycky, Daniel C.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Middour, Christopher K.; Hall, Jennifer R.; McCauliff, Sean] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
[Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Orosz, Jerome A.; Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Furesz, Gabor] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Shporer, Avi] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Ford, Eric B.] 211 Bryant Space Sci Ctr, Gainesville, FL 32611 USA.
[Rucker, Michael; Batalha, Natalie] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA.
[Fanelli, Michael N.; Still, Martin] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Buchhave, Lars A.] Konkoly Observ Budapest, H-1121 Budapest, Hungary.
[Berlind, Perry; Calkins, Michael L.] Smithsonian Astrophys Observ, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Short, Donald R.] San Diego State Univ, Dept Math, San Diego, CA 92182 USA.
[Steffen, Jason H.] FermiLab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Boss, Alan] Carnegie Inst Washington, Washington, DC 20015 USA.
[Buzasi, Derek] Eureka Sci, Oakland, CA 94602 USA.
[Fischer, Debra] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
RP Doyle, LR (reprint author), SETI Inst, Carl Sagan Ctr Study Life Universe, 189 Bernardo Ave, Mountain View, CA 94043 USA.
EM ldoyle@seti.org
RI Steffen, Jason/A-4320-2013; Carter, Joshua/A-8280-2013; Ragozzine,
Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014;
OI Caldwell, Douglas/0000-0003-1963-9616; Fortney,
Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666;
Fabrycky, Daniel/0000-0003-3750-0183
FU NASA's Science Mission Directorate; NASA [NNX08AR15G, HF-51267.01-A,
HF-51272.01-A, NAS 5-26555, NNX09AB33G]; Space Telescope Science
Institute
FX NASA's Science Mission Directorate provided funding for the Kepler
Discovery mission. L. R. D. acknowledges the NASA Kepler Participating
Scientist Program (grant no. NNX08AR15G) and helpful discussions with
the Kepler Science Team. J.A.C. and D. C. F. acknowledge support for
this work provided by NASA through Hubble Fellowship grants
HF-51267.01-A and HF-51272.01-A awarded by the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy for NASA, under contract NAS 5-26555. J.N.W. is
grateful for support from the NASA Origins program (grant NNX09AB33G).
The Kepler data used in this analysis can be downloaded from
http://archive.stsci.edu/prepds/kepler_hlsp.
NR 29
TC 285
Z9 286
U1 0
U2 18
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 SEP 16
PY 2011
VL 333
IS 6049
BP 1602
EP 1606
DI 10.1126/science.1210923
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 820JE
UT WOS:000294900900035
PM 21921192
ER
PT J
AU Mangala, LS
Zhang, Y
He, ZH
Emami, K
Ramesh, GT
Story, M
Rohde, LH
Wu, HL
AF Mangala, Lingegowda S.
Zhang, Ye
He, Zhenhua
Emami, Kamal
Ramesh, Govindarajan T.
Story, Michael
Rohde, Larry H.
Wu, Honglu
TI Effects of Simulated Microgravity on Expression Profile of MicroRNA in
Human Lymphoblastoid Cells
SO JOURNAL OF BIOLOGICAL CHEMISTRY
LA English
DT Article
ID NF-KAPPA-B; GENE-EXPRESSION; MODELED MICROGRAVITY; HUMAN FIBROBLASTS;
BREAST-CANCER; T-CELLS; TRANSCRIPTION; STRESS; SPACE; DIFFERENTIATION
AB This study explores the changes in expression of microRNA (miRNA) and related genes under simulated microgravity conditions. In comparison with static 1 x g, microgravity has been shown to alter global gene expression patterns and protein levels in cultured cells or animals. miRNA has recently emerged as an important regulator of gene expression, possibly regulating as many as one-third of all human genes. However, very little is known about the effect of altered gravity on miRNA expression. To test the hypothesis that the miRNA expression profile would be altered in zero gravity resulting in altered regulation of gene expression leading to metabolic or functional changes in cells, we cultured TK6 human lymphoblastoid cells in a high aspect ratio vessel (bioreactor) for 72 h either in the rotating condition to model microgravity in space or in the static condition as a control. Expression of several miRNAs was changed significantly in the simulated microgravity condition including miR150, miR-34a, miR-423-5p, miR-22, miR-141, miR-618, and miR-222. To confirm whether this altered miRNA expression correlates with gene expression and functional changes of the cells, we performed DNA microarray and validated the related genes using quantitative RT-PCR. Expression of several transcription factors including EGR2, ETS1, and c-REL was altered in simulated microgravity conditions. Taken together, the results reported here indicate that simulated microgravity alters the expression of miRNAs and genes in TK6 cells. To our knowledge, this study is the first to report the effects of simulated microgravity on the expression of miRNA and related genes.
C1 [Mangala, Lingegowda S.; Zhang, Ye; Emami, Kamal; Wu, Honglu] NASA Johnson Space Ctr, Radiat Biophys Lab, Houston, TX 77058 USA.
[Mangala, Lingegowda S.; He, Zhenhua; Rohde, Larry H.] Univ Houston Clear Lake, Dept Biol Sci, Houston, TX 77058 USA.
[Zhang, Ye] Wyle Integrated Sci & Engn Grp, Houston, TX 77058 USA.
[Ramesh, Govindarajan T.] Norfolk State Univ, Mol Toxicol Lab, Norfolk, VA 23504 USA.
[Story, Michael] Univ Texas SW Med Ctr Dallas, Dept Radiat Oncol, Dallas, TX 75390 USA.
RP Mangala, LS (reprint author), NASA Johnson Space Ctr, Radiat Biophys Lab, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM lingegowda.s.mangala@nasa.gov
FU University of Houston Institute for Space Systems Operations
FX This work was supported in part by the University of Houston Institute
for Space Systems Operations Program.
NR 46
TC 22
Z9 29
U1 3
U2 14
PU AMER SOC BIOCHEMISTRY MOLECULAR BIOLOGY INC
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3996 USA
SN 0021-9258
J9 J BIOL CHEM
JI J. Biol. Chem.
PD SEP 16
PY 2011
VL 286
IS 37
BP 32483
EP 32490
DI 10.1074/jbc.M111.267765
PG 8
WC Biochemistry & Molecular Biology
SC Biochemistry & Molecular Biology
GA 818CK
UT WOS:000294726800058
PM 21775437
ER
PT J
AU Sokol, E
Noll, RJ
Cooks, RG
Beegle, LW
Kim, HI
Kanik, I
AF Sokol, Ewa
Noll, Robert J.
Cooks, R. Graham
Beegle, Luther W.
Kim, Hugh I.
Kanik, Isik
TI Miniature mass spectrometer equipped with electrospray and desorption
electrospray ionization for direct analysis of organics from solids and
solutions
SO INTERNATIONAL JOURNAL OF MASS SPECTROMETRY
LA English
DT Article
DE Tandem mass spectrometry; Quadrupole ion trap; Amino acids; Nucleosides;
Purine and pyrimidine bases; Portable instrumentation; Electrospray
ionization; Desorption electrospray ionization
ID RECTILINEAR ION-TRAP; EXTRATERRESTRIAL AMINO-ACIDS; MURCHISON METEORITE;
CARBONACEOUS CHONDRITES; COLLISIONAL ACTIVATION; ANALYTICAL PERFORMANCE;
ATMOSPHERIC-PRESSURE; URINARY NUCLEOSIDES; PARENT-BODY; MARS
AB We report on the use of a small light-weight mass spectrometer (MS) for chemical analysis of organic material directly from solution or from the solid state with potential value in future planetary missions. The mass spectrometer used in the experiments reported here is handheld and controlled from a laptop computer through custom software. Detection and identification of small organic molecules, including some that might be prebiotics, was achieved using methods relevant to in situ and remote sensing applications. The miniature MS was equipped with a discontinuous atmospheric pressure interface (DAPI) and a home-built electrosonic spray ionization (ESSI) source. Aqueous solutions of molecules of interest were examined using the ESSI technique, while desorption electrospray ionization (DESI) was applied to examine solid samples. The system performance was characterized by direct analysis of analytes belonging to several compound classes including biotic and abiotic amino acids, purines, pyrimidines, nucleosides and peptides. Detection limits in the sub-ppm range for solutions were achieved with the atmospheric pressure sampling/ionization interface. Tandem mass spectrometry (MS2) was successfully applied to confirm trace detection of target compounds in mixtures. Multiple stage (MSn) analysis, where n = 3-5. was employed for molecular structure confirmation and to demonstrate the high chemical specificity as well as the sensitivity of the instrumentation. The use of improved versions of this type of mass spectrometer on exploration missions could provide detailed chemical information on organic materials in physical states currently difficult to access. The high sensitivity and specificity, combined with rapid detection and the absence of requirements for sample preparation are encouraging features of the instrumentation. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Sokol, Ewa; Noll, Robert J.; Cooks, R. Graham] Purdue Univ, Dept Chem, W Lafayette, IN 47907 USA.
[Beegle, Luther W.; Kim, Hugh I.; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Cooks, RG (reprint author), Purdue Univ, Dept Chem, 560 Oval Dr, W Lafayette, IN 47907 USA.
EM cooks@purdue.edu; isik.kanik@jpl.nasa.gov
RI Kim, Hugh/G-4476-2011; Cooks, R/G-1051-2015
OI Cooks, R/0000-0002-9581-9603
FU National Aeronautics and Space Administration
FX Financial support through NASA's Astrobiology Science and Technology
Instrument Development (ASTID), Planetary Instrument Definition and
Development (PIDDP) and Mars Instrument Development programs (MIDP) is
gratefully acknowledged. The contributions of LB, HK and IK were carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. The authors acknowledge ICx Analytical Instruments for
technical assistance.
NR 71
TC 28
Z9 28
U1 3
U2 52
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1387-3806
J9 INT J MASS SPECTROM
JI Int. J. Mass Spectrom.
PD SEP 15
PY 2011
VL 306
IS 2-3
SI SI
BP 187
EP 195
DI 10.1016/j.ijms.2010.10.019
PG 9
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 826JU
UT WOS:000295351200014
ER
PT J
AU Botta, G
Aydin, K
Verlinde, J
Avramov, AE
Ackerman, AS
Fridlind, AM
McFarquhar, GM
Wolde, M
AF Botta, Giovanni
Aydin, Kultegin
Verlinde, Johannes
Avramov, Alexander E.
Ackerman, Andrew S.
Fridlind, Ann M.
McFarquhar, Greg M.
Wolde, Mengistu
TI Millimeter wave scattering from ice crystals and their aggregates:
Comparing cloud model simulations with X- and Ka-band radar measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID PARTICLE TERMINAL VELOCITIES; GENERAL HYDRODYNAMIC THEORY; MIXED-PHASE
MICROPHYSICS; CROSS-SECTIONS; ARCTIC CLOUD; BACKSCATTERING;
HYDROMETEORS; SNOWFLAKES; CLARIFICATION; REVISION
AB Arctic clouds are often mixed-phase, such that the radiative properties of the clouds are a strong function of the relative amounts of cloud liquid and ice. Modeling studies have shown that the poorly understood ice phase processes are the regulators of the liquid water fraction. However, evaluating the fidelity of the model ice parameterizations has proven to be a difficult task. This study evaluates results of different ice microphysics representations in a cloud resolving model (CRM) using cloud radar measurements. An algorithm is presented to generate realistic ice crystals and their aggregates from which radar backscattering cross sections may be calculated using a generalized solution for a cluster of spheres. The aggregate is composed of a collection of ice crystals, each of which is constructed from a cluster of tiny ice spheres. Each aggregate satisfies the constraints set by the component crystal type and the mass-dimensional relationship used in the cloud resolving model, but is free to adjust its aspect ratio. This model for calculating radar backscattering is compared to two spherical and two spheroidal (bulk model) representations for ice hydrometeors. It was found that a refined model for representing the ice hydrometeors, both pristine crystals and their aggregates, is required in order to obtain good comparisons between the CRM calculations and the radar measurements. The addition of the radar-CRM comparisons to CRM-in situ measurements comparisons allowed conclusions about the appropriateness of different CRM ice microphysics parameterizations.
C1 [Botta, Giovanni; Verlinde, Johannes] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Botta, Giovanni; Aydin, Kultegin] Penn State Univ, Dept Elect Engn, University Pk, PA 16802 USA.
[Avramov, Alexander E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Ackerman, Andrew S.; Fridlind, Ann M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[McFarquhar, Greg M.] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA.
[Wolde, Mengistu] CNR, Inst Aerosp Res, Flight Res Lab, Ottawa, ON K1A 0R6, Canada.
RP Botta, G (reprint author), Penn State Univ, Dept Meteorol, 503 Walker Bldg, University Pk, PA 16802 USA.
EM gub13@psu.edu
RI Ackerman, Andrew/D-4433-2012; Fridlind, Ann/E-1495-2012;
OI Ackerman, Andrew/0000-0003-0254-6253; McFarquhar,
Greg/0000-0003-0950-0135
FU Office of Biological and Environmental Research of the U.S. Department
of Energy [DE-FG02-05ER64058]; Office of Science of the U.S. Department
of Energy [DE-AC02-05CH11231]; DOE Office of Science, Office of
Biological and Environmental Research [DE-AI02-06ER64173,
DE-AI02-08ER64547]; NASA
FX The work was supported by the Office of Biological and Environmental
Research of the U.S. Department of Energy grant DE-FG02-05ER64058 as
part of the Atmospheric System Research Program. This research used
resources of the National Energy Research Scientific Computing Center,
which is supported by the Office of Science of the U.S. Department of
Energy under contract DE-AC02-05CH11231. A. A., A. S. A. and A. M. F.
were supported by the DOE Office of Science, Office of Biological and
Environmental Research, through Interagency Agreements DE-AI02-06ER64173
and DE-AI02-08ER64547, and the NASA Radiation Sciences Program.
NR 53
TC 22
Z9 22
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 SEP 15
PY 2011
VL 116
AR D00T04
DI 10.1029/2011JD015909
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 823OI
UT WOS:000295131400003
ER
PT J
AU Wu, LT
Su, H
Jiang, JH
AF Wu, Longtao
Su, Hui
Jiang, Jonathan H.
TI Regional simulations of deep convection and biomass burning over South
America: 1. Model evaluations using multiple satellite data sets
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID WRF-CHEM MODEL; GLOBAL PRECIPITATION; AURA SATELLITE; AEROSOL;
TRANSPORT; TROPOSPHERE; EMISSIONS; RETRIEVAL; ALGORITHM; CAMPAIGN
AB Multiple data sets, mostly from satellite observations, are used to evaluate the performance of the Weather Research and Forecasting model with Chemistry (WRF-Chem) in simulating the distribution and evolution of aerosol, clouds, precipitation and chemistry during the dry season in South America. A 9-day WRF-Chem simulation with 36 km horizontal resolution is performed from 15 to 24 September 2006, during which frequent biomass burnings were observed. It is shown that the model reproduces the spatial distribution of aerosols produced by biomass burning and approximately captures convective transport of trace gases (e. g., CO and O-3) into the upper troposphere. Surface precipitation is also in reasonable agreement with observation. The model simulations overestimate the magnitude of water vapor in the upper troposphere while the magnitude of cloud water content is lower than measurements from satellites, which may indicate problems in the cumulus and microphysical parameterizations. The model simulations capture temporal variations of outgoing longwave radiation at the top of atmosphere and downward shortwave radiation at the surface shown in the NASA GEWEX SRB data set. A sensitivity run at 4 km horizontal resolution shows similar results to the 36 km simulation, with a high bias of precipitation. The uncertainty and weakness in both satellite observations and model simulations are identified. This study demonstrates that satellite data are valuable to the evaluation of regional model simulations for climatologically important processes such as deep convection and biomass burning, especially in regions with little in situ observation.
C1 [Wu, Longtao; Su, Hui; Jiang, Jonathan H.] CALTECH, Jet Prop Lab, Aura Microwave Limb Sounder MLS Sci Team, Pasadena, CA 91109 USA.
RP Wu, LT (reprint author), CALTECH, Jet Prop Lab, Aura Microwave Limb Sounder MLS Sci Team, 4800 Oak Grove Dr,M-S 183-701, Pasadena, CA 91109 USA.
EM longtao.wu@jpl.nasa.gov
RI Wu, Longtao/G-5509-2012
FU NASA
FX The authors thank Steven Peckham, Chun Zhao, Mary Barth, Xiaohong Liu,
Xiaoming Hu, and the WRF support staff for their assistance with running
the WRF-Chem simulations. The comments from Jerome Fast and two
anonymous reviewers are appreciated. The authors also thank Mingzhao Luo
and Brian Kahn for assistance with processing the TES and AIRS data. We
thank the PI investigators and their staff for establishing and
maintaining the four AERONET sites used in the investigation. The
MOZART-4 data are from http://www.acd.ucar.edu/wrf-chem/mozart.shtml.
The NASA GEWEX SRB data sets are obtained from
http://eosweb.larc.nasa.gov/PRODOCS/srb/table_srb.html. This study was
supported by NASA IDS, ACMAP and AST programs. The work is conducted at
the Jet Propulsion Laboratory, California Institute of Technology, under
contract with NASA.
NR 60
TC 9
Z9 9
U1 0
U2 9
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 SEP 15
PY 2011
VL 116
AR D17208
DI 10.1029/2011JD016105
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 823OI
UT WOS:000295131400004
ER
PT J
AU Wu, LT
Su, H
Jiang, JH
AF Wu, Longtao
Su, Hui
Jiang, Jonathan H.
TI Regional simulations of deep convection and biomass burning over South
America: 2. Biomass burning aerosol effects on clouds and precipitation
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID RADIATIVE IMPACT; MODEL; PARAMETERIZATION; REPRESENTATION; SMOKE;
INHIBITION; ACTIVATION; POLLUTION; AMAZON
AB A fully coupled meteorology-chemistry-aerosol mesoscale model (WRF-Chem) is used to simulate a multiday biomass burning event in the dry season of South America. The effects of biomass burning aerosols on clouds and precipitation are described at both 36 km and 4 km horizontal resolutions. The dominant effect of the aerosols is to reduce the diurnal amplitude of convection by decreasing clouds and precipitation in the afternoon but increasing them at night, with the afternoon decrease greater than the nighttime increase on the daily mean. On average, the decrease of surface precipitation is about 5% (3%) and the amplitude of diurnal cycle is reduced by about 11% (5%) in the 36 km (4 km) simulations. Such a modulation of clouds and precipitation is primarily contributed by the aerosol radiative effect, i.e., their ability to scatter and absorb solar radiation. The aerosol microphysical effect as cloud condensation nuclei tends to act oppositely to the aerosol radiative effect but with a smaller magnitude, especially in the simulations at 36 km horizontal resolution. The 4 km resolution runs exhibit similar behaviors to the 36 km simulations, with a slightly stronger role of the aerosol microphysical effect relative to the aerosol radiative effect. We find another important effect of biomass burning aerosols. When uplifted into the upper troposphere by deep convection, they can significantly warm the upper troposphere through their local radiative heating effect and result in significant moistening in the upper troposphere, potentially affecting the water vapor transport from the troposphere to the stratosphere.
C1 [Wu, Longtao; Su, Hui; Jiang, Jonathan H.] CALTECH, Jet Prop Lab, Aura Microwave Limb Sounder MLS Sci Team, Pasadena, CA 91109 USA.
RP Wu, LT (reprint author), CALTECH, Jet Prop Lab, Aura Microwave Limb Sounder MLS Sci Team, 4800 Oak Grove Dr,M-S 183-701, Pasadena, CA 91109 USA.
EM longtao.wu@jpl.nasa.gov
RI Wu, Longtao/G-5509-2012
FU NASA; AST; Aura MLS
FX The authors thank Chun Zhao, Steven Peckham, Mary Barth, Xiaohong Liu,
Xiaoming Hu and the WRF support staff for their assistance with running
the WRF- Chem simulations. The authors also thank Jerome Fast, Georg
Grell and Minghuai Wang for valuable suggestions. The comments from
three anonymous reviewers are appreciated. This study was supported by
NASA IDS and AST programs, as well as the Aura MLS project. The work is
conducted at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with NASA.
NR 37
TC 17
Z9 17
U1 3
U2 25
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 SEP 15
PY 2011
VL 116
AR D17209
DI 10.1029/2011JD016106
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 823OI
UT WOS:000295131400005
ER
PT J
AU Glocer, A
Fok, MC
Nagai, T
Toth, G
Guild, T
Blake, J
AF Glocer, A.
Fok, M. -C.
Nagai, T.
Toth, G.
Guild, T.
Blake, J.
TI Rapid rebuilding of the outer radiation belt
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID BLOCK-ADAPTIVE GRIDS; RELATIVISTIC ELECTRONS; INNER MAGNETOSPHERE;
RESONANT INTERACTION; GEOMAGNETIC STORMS; MAGNETIC STORMS; PITCH-ANGLE;
ACCELERATION; DIFFUSION; MAGNETOHYDRODYNAMICS
AB Recent observations by the radiation monitor (RDM) on the spacecraft Akebono have shown several cases of >2.5 MeV radiation belt electron enhancements occurring on timescales of less than a few hours. Similar enhancements are also seen in detectors on board the NOAA/POES and TWINS 1 satellites. These intervals are shorter than typical radial diffusion or wave-particle interactions can account for. We choose two so-called "rapid rebuilding" events that occur during high speed streams (4 September 2008 and 22 July 2009) and simulated them with the Space Weather Modeling Framework configured with global magnetosphere, radiation belt, ring current, and ionosphere electrodynamics model. Our simulations produce a weaker and delayed dipolarization as compared to observations, but the associated inductive electric field in the simulations is still strong enough to rapidly transport and accelerate MeV electrons resulting in an energetic electron flux enhancement that is somewhat weaker than is observed. Nevertheless, the calculated flux enhancement and dipolarization is found to be qualitatively consistent with the observations. Taken together, the modeling results and observations support the conclusion that storm-time dipolarization events in the magnetospheric magnetic field result in strong radial transport and energization of radiation belt electrons.
C1 [Glocer, A.; Fok, M. -C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nagai, T.] Tokyo Inst Technol, Tokyo 1528551, Japan.
[Toth, G.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Guild, T.; Blake, J.] Aerosp Corp, Chantilly, VA USA.
RP Glocer, A (reprint author), NASA, Goddard Space Flight Ctr, Code 673, Greenbelt, MD 20771 USA.
EM alex.glocer-1@nasa.gov
RI Glocer, Alex/C-9512-2012; Fok, Mei-Ching/D-1626-2012; Toth,
Gabor/B-7977-2013; feggans, john/F-5370-2012
OI Glocer, Alex/0000-0001-9843-9094; Toth, Gabor/0000-0002-5654-9823;
FU JSPS [225404588]; NASA through the NASA Advanced Supercomputing (NAS)
Division at Ames Research Center; NASA Center for Climate Simulation
(NCCS) at Goddard Space Flight Center
FX T.N. was supported by JSPS Grand-in-Aid for Scientific Research (C)
(225404588). The Dst index is provided by World Data Center for
Geomagnetism, Kyoto and the Dst observatories (Kakioka, Honolulu, San
Juan, Hermanus, and Alibag). We would also like to thank National Space
Science Data Center for providing the ACE and GOES: ACE MAG instrument,
N. F. Ness, and SWEPAM instrument, D. McComas, and GOES Magnetometer, H.
Singer. NOAA POES data was obtained from
http://poes.ngdc.noaa.gov/data/. Resources supporting this work were
provided by the NASA High-End Computing (HEC) Program through the NASA
Advanced Supercomputing (NAS) Division at Ames Research Center and the
NASA Center for Climate Simulation (NCCS) at Goddard Space Flight
Center.
NR 56
TC 16
Z9 16
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 SEP 15
PY 2011
VL 116
AR A09213
DI 10.1029/2011JA016516
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823PD
UT WOS:000295133900001
ER
PT J
AU Coutts, JL
Devor, RW
Aitken, B
Hampton, MD
Quinn, JW
Clausen, CA
Geiger, CL
AF Coutts, Janelle L.
Devor, Robert W.
Aitken, Brian
Hampton, Michael D.
Quinn, Jacqueline W.
Clausen, Christian A.
Geiger, Cherie L.
TI The use of mechanical alloying for the preparation of palladized
magnesium bimetallic particles for the remediation of PCBs
SO JOURNAL OF HAZARDOUS MATERIALS
LA English
DT Article
DE Mg/Pd bimetal; Polychlorinated biphenyls; Dechlorination; Mechanical
alloying; Ball-milling
ID POLYCHLORINATED-BIPHENYLS; RAPID DECHLORINATION; DEGRADATION; IRON;
CONGENERS; SYSTEMS; SURFACE; PD/FE; MG/PD
AB The kinetic rate of dechlorination of a polychlorinated biphenyl (PCB-151) by mechanically alloyed Mg/Pd was studied for optimization of the bimetallic system. Bimetal production was first carried out in a small-scale environment using a SPEX 8000M high-energy ball mill with 4-mu m-magnesium and palladium impregnated on graphite, with optimized parameters including milling time and Pd-loading. A 5.57-g sample of bimetal containing 0.1257% Pd and ball milled for 3 min resulted in a degradation rate of 0.00176 min(-1) g(-1) catalyst as the most reactive bimetal. The process was then scaled-up, using a Red Devil 5400 Twin-Arm Paint Shaker, fitted with custom plates to hold milling canisters. Optimization parameters tested included milling time, number of ball bearings used, Pd-loading, and total bimetal mass milled. An 85-g sample of bimetal containing 0.1059% Pd and ball-milled for 23 min with 16 ball bearings yielded the most reactive bimetal with a degradation rate of 0.00122 min(-1) g(-1) catalyst. Further testing showed adsorption did not hinder extraction efficiency and that dechlorination products were only seen when using the bimetallic system, as opposed to any of its single components. The bimetallic system was also tested for its ability to degrade a second PCB congener, PCB-45, and a PCB mixture (Arochlor 1254); both contaminants were seen to degrade successfully. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Coutts, Janelle L.; Hampton, Michael D.; Clausen, Christian A.; Geiger, Cherie L.] Univ Cent Florida, Orlando, FL 32816 USA.
[Devor, Robert W.] ESC Team QNA, Kennedy Space Ctr, FL 32899 USA.
[Aitken, Brian] Univ Florida, Gainesville, FL 32611 USA.
[Quinn, Jacqueline W.] NASA, Kennedy Space Ctr, FL 32899 USA.
RP Geiger, CL (reprint author), Univ Cent Florida, 4000 Cent Florida Blvd, Orlando, FL 32816 USA.
EM jcoutts@knights.ucf.edu; cgeiger@mail.ucf.edu
FU NASA, Kennedy Space Center
FX The authors would like to thank NASA, Kennedy Space Center for its
support in this work and Research Scientist, James Captain of ESC-Team
QNA, for his extensive help with SEM imaging of the Mg/Pd produced for
this study.
NR 22
TC 7
Z9 7
U1 3
U2 26
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0304-3894
J9 J HAZARD MATER
JI J. Hazard. Mater.
PD SEP 15
PY 2011
VL 192
IS 3
BP 1380
EP 1387
DI 10.1016/j.jhazmat.2011.06.052
PG 8
WC Engineering, Environmental; Engineering, Civil; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA 824XZ
UT WOS:000295236800058
PM 21807459
ER
PT J
AU Morgan, JLL
Gordon, GW
Arrua, RC
Skulan, JL
Anbar, AD
Bullen, TD
AF Morgan, Jennifer L. L.
Gordon, Gwyneth W.
Arrua, Ruth C.
Skulan, Joseph L.
Anbar, Ariel D.
Bullen, Thomas D.
TI High-Precision Measurement of Variations in Calcium Isotope Ratios in
Urine by Multiple Collector Inductively Coupled Plasma Mass Spectrometry
SO ANALYTICAL CHEMISTRY
LA English
DT Article
ID OCTOPOLE COLLISION CELL; MC-ICP-MS; NONBIOLOGICAL FRACTIONATION; BONE;
OSTEOPOROSIS; ACCURACY; STANDARD
AB We describe a new chemical separation method to isolate Ca from other matrix elements in biological samples, developed with the long-term goal of making high-precision measurement of natural stable Ca isotope variations a clinically applicable tool to assess bone mineral balance. A new two-column procedure utilizing HBr achieves the purity required to accurately and precisely measure two Ca isotope ratios ((44)Ca/(42)Ca and (44)Ca/(43)Ca) on a Neptune multiple collector inductively coupled plasma mass spectrometer (MC-ICPMS) in urine. Purification requirements for Sr, Ti, and K (Ca/Sr > 10000; Ca/Ti > 10 000 000; and Ca/K > 10) were determined by addition of these elements to Ca standards of known isotopic composition. Accuracy was determined by (1) comparing Ca isotope results for samples and standards to published data obtained using thermal ionization mass spectrometry (TIMS), (2) adding a Ca standard of known isotopic composition to a urine sample purified of Ca, and (3) analyzing mixtures of urine samples and standards in varying proportions. The accuracy and precision of delta(44/42) Ca measurements of purified samples containing 25 mu g of Ca can be determined with typical errors less than +/- 0.2 parts per thousand (2 sigma).
C1 [Morgan, Jennifer L. L.; Anbar, Ariel D.] Arizona State Univ, Dept Chem & Biochem, Tempe, AZ 85287 USA.
[Gordon, Gwyneth W.; Arrua, Ruth C.; Anbar, Ariel D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Skulan, Joseph L.] Univ Wisconsin, Geol Museum, Madison, WI 53706 USA.
[Bullen, Thomas D.] US Geol Survey, Water Resources Discipline, Menlo Pk, CA 94025 USA.
RP Morgan, JLL (reprint author), NASA, Lyndon B Johnson Space Ctr, Biochem Lab, Human Adaptat & Countermeasures Div, Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA.
EM jenniferllmorgan@gmail.com
FU NASA [NNX08AQ36G]
FX Funding provided by NASA's Human Research Project Grant Number
NNX08AQ36G (A. D. Anbar). The authors thank Stephen Romaniello for
helpful discussions about the fractionation pattern of Ca during
elution. We thank Matt Fantle and an anonymous reviewer for their
thoughtful comments, which greatly improved this manuscript.
NR 30
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U1 2
U2 47
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0003-2700
J9 ANAL CHEM
JI Anal. Chem.
PD SEP 15
PY 2011
VL 83
IS 18
BP 6956
EP 6962
DI 10.1021/ac200361t
PG 7
WC Chemistry, Analytical
SC Chemistry
GA 818XM
UT WOS:000294790000008
PM 21740001
ER
PT J
AU Shi, W
Petersen, EB
Nguyen, DT
Yao, ZD
Chavez-Pirson, A
Peyghambarian, N
Yu, JR
AF Shi, Wei
Petersen, Eliot B.
Nguyen, Dan T.
Yao, Zhidong
Chavez-Pirson, Arturo
Peyghambarian, N.
Yu, Jirong
TI 220 mu J monolithic single-frequency Q-switched fiber laser at 2 mu m by
using highly Tm-doped germanate fibers
SO OPTICS LETTERS
LA English
DT Article
ID C-BAND; GENERATION; NM
AB We report a unique all fiber-based single-frequency Q-switched laser in a monolithic master oscillator power amplifier configuration at similar to 1920nm by using highly Tm-doped germanate fibers for the first time. The actively Q-switched fiber laser seed was achieved by using a piezo to press the fiber in the fiber Bragg grating cavity and modulate the fiber birefringence, enabling Q-switching with pulse width and repetition rate tunability. A single-mode polarization maintaining large core 25 mu m highly Tm-doped germanate fiber was used in the power amplifier stage. For 80 ns pulses with 20 kHz repetition rate, we achieved 220 mu J pulse energy, which corresponds to a peak power of 2.75kW with transform-limited linewidth. (C) 2011 Optical Society of America
C1 [Shi, Wei; Petersen, Eliot B.; Nguyen, Dan T.; Yao, Zhidong; Chavez-Pirson, Arturo; Peyghambarian, N.] NP Photon Inc, Tucson, AZ 85747 USA.
[Petersen, Eliot B.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA.
[Peyghambarian, N.] Univ Arizona, Coll Opt Sci, Tucson, AZ 85721 USA.
[Yu, Jirong] NASA Langley Res Ctr, Hampton, VA 23681 USA.
RP Shi, W (reprint author), NP Photon Inc, 9030 S Rita Rd, Tucson, AZ 85747 USA.
EM wshi@npphotonics.com
FU NASA [NX11CG95P]; Air Force Research Laboratory/Materials and
Manufacturing Directorate [FA8650-10 C-5208]
FX This work has been supported by NASA Small Business Innovation Research
(SBIR) project NX11CG95P, and Air Force Research Laboratory/Materials
and Manufacturing Directorate SBIR project FA8650-10 C-5208. The authors
acknowledge the technical support from Dr. Adam Cooney.
NR 13
TC 36
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U1 1
U2 11
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0146-9592
J9 OPT LETT
JI Opt. Lett.
PD SEP 15
PY 2011
VL 36
IS 18
BP 3575
EP 3577
PG 3
WC Optics
SC Optics
GA 821BZ
UT WOS:000294951100015
PM 21931395
ER
PT J
AU Blacksberg, J
Maruyama, Y
Charbon, E
Rossman, GR
AF Blacksberg, Jordana
Maruyama, Yuki
Charbon, Edoardo
Rossman, George R.
TI Fast single-photon avalanche diode arrays for laser Raman spectroscopy
SO OPTICS LETTERS
LA English
DT Article
ID MINERALOGY
AB We incorporate newly developed solid-state detector technology into time-resolved laser Raman spectroscopy, demonstrating the ability to distinguish spectra from Raman and fluorescence processes. As a proof of concept, we show fluorescence rejection on highly fluorescent mineral samples willemite and spodumene using a 128 x 128 single-photon avalanche diode (SPAD) array with a measured photon detection efficiency of 5%. The sensitivity achieved in this new instrument architecture is comparable to the sensitivity of a technically more complicated system using a traditional photocathode-based imager. By increasing the SPAD active area and improving coupling efficiency, we expect further improvements in sensitivity by over an order of magnitude. We discuss the relevance of these results to in situ planetary instruments, where size, weight, power, and radiation hardness are of prime concern. The potential large-scale manufacturability of silicon SPAD arrays makes them prime candidates for future portable and in situ Raman instruments spanning numerous applications where fluorescence interference is problematic. (C) 2011 Optical Society of America
C1 [Blacksberg, Jordana] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Maruyama, Yuki; Charbon, Edoardo] Delft Univ Technol, NL-2628 CD Delft, Netherlands.
[Rossman, George R.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Blacksberg, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jordana.blacksberg@jpl.nasa.gov
OI Rossman, George/0000-0002-4571-6884
FU National Aeronautics and Space Administration (NASA)
FX The research described in this publication was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration (NASA).
SPAD development was performed at Delft University of Technology, and CW
Raman measurements at Caltech.
NR 13
TC 15
Z9 15
U1 0
U2 10
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0146-9592
J9 OPT LETT
JI Opt. Lett.
PD SEP 15
PY 2011
VL 36
IS 18
BP 3672
EP 3674
PG 3
WC Optics
SC Optics
GA 821BZ
UT WOS:000294951100048
PM 21931428
ER
PT J
AU Nagel, MA
Choe, A
Cohrs, RJ
Traktinskiy, I
Sorensen, K
Mehta, SK
Pierson, DL
Tyring, SK
Haitz, K
DiGiorgio, C
LaPolla, W
Gilden, D
AF Nagel, Maria A.
Choe, Alexander
Cohrs, Randall J.
Traktinskiy, Igor
Sorensen, Kyle
Mehta, Satish K.
Pierson, Duane L.
Tyring, Stephen K.
Haitz, Kassie
DiGiorgio, Catherine
LaPolla, Whitney
Gilden, Don
TI Persistence of Varicella Zoster Virus DNA in Saliva After Herpes Zoster
SO JOURNAL OF INFECTIOUS DISEASES
LA English
DT Article
ID POSTHERPETIC NEURALGIA; MONONUCLEAR-CELLS; REACTIVATION; ASTRONAUTS; VZV
AB Analysis of saliva samples from individuals aged >= 60 years who had a history of zoster (group 1), zoster and postherpetic neuralgia (PHN; group 2), or no history of zoster (group 3) revealed varicella zoster virus (VZV) DNA in saliva samples from 11 of 17 individuals in group 1, 10 of 15 individuals in group 2, and 2 of 17 individuals in group 3. The frequency of VZV DNA detection was significantly higher (P = .001) in saliva of subjects with a history of zoster, with or without PHN (21 [67%] of 32 subjects in groups 1 and 2), than in saliva of age-matched subjects with no zoster history (2 [12%] of 17 subjects in group 3). Thus, persistence of VZV DNA in saliva is the outcome of zoster, independent of PHN. Because VZV infection can produce neurological and ocular disease without zoster rash, future studies are needed to establish whether VZV DNA can be detected in the saliva of such patients.
C1 [Nagel, Maria A.; Choe, Alexander; Cohrs, Randall J.; Traktinskiy, Igor; Gilden, Don] Univ Colorado, Sch Med, Dept Neurol, Aurora, CO 80045 USA.
[Sorensen, Kyle] Univ Colorado, Sch Med, Dept Phys & Biophys, Aurora, CO 80045 USA.
[Gilden, Don] Univ Colorado, Sch Med, Dept Microbiol, Aurora, CO 80045 USA.
[Mehta, Satish K.] Enterprise Advisory Serv, Houston, TX USA.
[Pierson, Duane L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Tyring, Stephen K.; Haitz, Kassie; DiGiorgio, Catherine; LaPolla, Whitney] Univ Texas Hlth Sci Ctr Houston, Dept Dermatol, Houston, TX USA.
RP Gilden, D (reprint author), Univ Colorado, Sch Med, Dept Neurol, 12700 E 19th Ave,Box B182, Aurora, CO 80045 USA.
EM don.gilden@ucdenver.edu
FU National Institutes of Health [AG032958, AG006127, NS067070]; National
Aeronautics and Space Administration [SMO-015]
FX This work was supported by the National Institutes of Health (grant
AG032958 to D. G. and R. J. C., grant AG006127 to D. G., and grant
NS067070 to M. A. N.); and the National Aeronautics and Space
Administration (grant SMO-015 to D. L. P.).
NR 15
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U1 0
U2 2
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 0022-1899
J9 J INFECT DIS
JI J. Infect. Dis.
PD SEP 15
PY 2011
VL 204
IS 6
BP 820
EP 824
DI 10.1093/infdis/jir425
PG 5
WC Immunology; Infectious Diseases; Microbiology
SC Immunology; Infectious Diseases; Microbiology
GA 809QJ
UT WOS:000294071500003
PM 21849278
ER
PT J
AU Gehrz, RD
Becklin, EE
de Buizer, J
Herter, T
Keller, LD
Krabbe, A
Marcum, PM
Roellig, TL
Sandell, GHL
Temi, P
Vacca, WD
Young, ET
Zinnecker, H
AF Gehrz, R. D.
Becklin, E. E.
de Buizer, J.
Herter, T.
Keller, L. D.
Krabbe, A.
Marcum, P. M.
Roellig, T. L.
Sandell, G. H. L.
Temi, P.
Vacca, W. D.
Young, E. T.
Zinnecker, H.
TI Status of the Stratospheric Observatory for Infrared Astronomy (SOFIA)
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Infrared Astronomy; Sub-millimeter astronomy; Airborne astronomy;
Infrared spectroscopy; Spectroscopy; SOFIA
ID SPACE-TELESCOPE; MISSION; LONG
AB The Stratospheric Observatory for Infrared Astronomy (SOFIA), a joint US/German project, is a 2.5-m infrared airborne telescope carried by a Boeing 747-SP that flies in the stratosphere at altitudes as high as 45,000 ft (13.72 km). This facility is capable of observing from 0.3 mu m to 1.6 mm with an average transmission greater than 80% averaged over all wavelengths. SOFIA will be staged out of the NASA Dryden Flight Research Center aircraft operations facility at Palmdale, CA. The SOFIA Science Mission Operations (SMO) will be located at NASA Ames Research Center, Moffett Field, CA. First science flights began in 2010 and a full operations schedule of up to one hundred 8 to 10 hour-long flights per year will be reached by 2014. The observatory is expected to operate until the mid-2030s. SOFIA's initial complement of seven focal plane instruments includes broadband imagers, moderate-resolution spectrographs that will resolve broad features due to dust and large molecules, and high-resolution spectrometers capable of studying the kinematics of atomic and molecular gas at sub-km/s resolution. We describe the SOFIA facility and outline the opportunities for observations by the general scientific community and for future instrumentation development. The operational characteristics of the SOFIA first-generation instruments are summarized. The status of the flight test program is discussed and we show First Light images obtained at wavelengths from 5.4 to 37 mu m with the FORCAST imaging camera. Additional information about SOFIA is available at http://www.sofia.usra.edu and http://www.sofia.usra.edu/Science/docs/SofiaScienceVision051809-1.pdf. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Gehrz, R. D.] Univ Minnesota, Sch Phys & Astron, Dept Astron, Minneapolis, MN 55455 USA.
[Becklin, E. E.; de Buizer, J.; Sandell, G. H. L.; Vacca, W. D.; Young, E. T.] NASA, Ames Res Ctr, Univ Space Res Assoc, Moffett Field, CA 94035 USA.
[Herter, T.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Keller, L. D.] Ithaca Coll, Dept Phys, Ithaca, NY 14850 USA.
[Krabbe, A.; Zinnecker, H.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany.
[Zinnecker, H.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
RP Gehrz, RD (reprint author), Univ Minnesota, Sch Phys & Astron, Dept Astron, 116 Church St SE, Minneapolis, MN 55455 USA.
EM gehrz@astro.umn.edu
FU USRA; NASA; US Air Force
FX We thank the entire SOFIA team for their tireless work on the SOFIA
Project. R. D. G. was supported by USRA, NASA, and the US Air Force.
Many thanks to Glenn Orton for assisting with the interpretation of the
SOFIA First Light observations of Jupiter. We thank a referee, M. W.
Werner for constructive suggestions that improved the manuscript.
NR 16
TC 7
Z9 7
U1 1
U2 3
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD SEP 15
PY 2011
VL 48
IS 6
BP 1004
EP 1016
DI 10.1016/j.asr.2011.05.023
PG 13
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 809EK
UT WOS:000294034400004
ER
PT J
AU Lipatov, AS
Sittler, EC
Hartle, RE
Cooper, JF
Simpson, DG
AF Lipatov, A. S.
Sittler, E. C., Jr.
Hartle, R. E.
Cooper, J. F.
Simpson, D. G.
TI Background and pickup ion velocity distribution dynamics in Titan's
plasma environment: 3D hybrid simulation and comparison with CAPS T9
observations
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Ionospheres; Atmospheres; Induced magnetospheres; Magnetic barrier;
Alfven wing; Satellites
ID SOLAR-WIND; MAGNETOSPHERIC INTERACTION; MHD MODEL; SPECTROMETER;
IONOSPHERE; COMET; SHOCK; FLOW
AB In this report we discuss the ion velocity distribution dynamics from the 3D hybrid simulation. In our model the background, pickup, and ionospheric ions are considered as a particles, whereas the electrons are described as a fluid. Inhomogeneous photoionization, electron-impact ionization and charge exchange are included in our model. We also take into account the collisions between the ions and neutrals. The current simulation shows that mass loading by pickup ions H+, H-2(+), CH4+ and N-2(+) is stronger than in the previous simulations when O+ ions are introduced into the background plasma. In our hybrid simulations we use Chamberlain profiles for the atmospheric components. We also include a simple ionosphere model with average mass M = 28 amu ions that were generated inside the ionosphere. The moon is considered as a weakly conducting body. Special attention will be paid to comparing the simulated pickup ion velocity distribution with CAPS T9 observations. Our simulation shows an asymmetry of the ion density distribution and the magnetic field, including the formation of the Alfven wing-like structures. The simulation also shows that the ring-like velocity distribution for pickup ions relaxes to a Maxwellian core and a shell-like halo. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Lipatov, A. S.] NASA, Goddard Space Flight Ctr, GPHI UMBC, Greenbelt, MD 20771 USA.
RP Lipatov, AS (reprint author), NASA, Goddard Space Flight Ctr, GPHI UMBC, Code 673,Bld 21,Rm 247,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Alexander.Lipatov-1@nasa.gov; Edward.C.Sittler@nasa.gov;
Richard.E.Hartle@nasa.gov; John.F.Cooper@nasa.gov;
David.G.Simp-son@nasa.gov
RI Cooper, John/D-4709-2012
FU NASA [08-CDAP08-0043]; GEST Center UMBC [900-37-172]; NASA GSFC
[670-90-315]
FX A.S.L., E.C.S., R.E.H., J.F.C., and D.G.S. were supported by the Grant
Analysis of Titan's Interaction with Saturn's Magnetosphere using
Cassini Titan Flyby Data and Kinetic-Fluid Model from the NASA Cassini
Data Analysis Program (08-CDAP08-0043). A.S.L. was also supported in
part by the Grants/Tasks 900-37-172 and 670-90-315 between the GEST
Center UMBC and NASA GSFC. Computational resources were provided by the
NASA Ames Advanced Supercomputing (NAS) Division (Projects SMD-09-1124
and SMD-10-1517). The authors thank the referees for fruitful comments.
NR 35
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PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD SEP 15
PY 2011
VL 48
IS 6
BP 1114
EP 1125
DI 10.1016/j.asr.2011.05.026
PG 12
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 809EK
UT WOS:000294034400016
ER
PT J
AU Nuevo, M
Milam, SN
Sandford, SA
De Gregorio, BT
Cody, GD
Kilcoyne, ALD
AF Nuevo, M.
Milam, S. N.
Sandford, S. A.
De Gregorio, B. T.
Cody, G. D.
Kilcoyne, A. L. D.
TI XANES analysis of organic residues produced from the UV irradiation of
astrophysical ice analogs
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Ices; UV irradiation; XANES spectroscopy; Extraterrestrial materials
ID INTERPLANETARY DUST PARTICLES; INNER-SHELL EXCITATION; ADVANCED
LIGHT-SOURCE; RACEMIC AMINO-ACIDS; INTERSTELLAR ICE; COMET 81P/WILD-2;
MURCHISON METEORITE; CARBONACEOUS METEORITES; ULTRAVIOLET-IRRADIATION;
LABORATORY SIMULATIONS
AB Organic residues formed in the laboratory from the ultraviolet (UV) photo-irradiation or ion bombardment of astrophysical ice analogs have been extensively studied for the last 15 years with a broad suite of techniques, including infrared (IR) and UV spectroscopies, as well as mass spectrometry. Analyses of these materials show that they consist of complex mixtures of organic compounds stable at room temperature, mostly soluble, that have not been fully characterized. However, the hydrolysis products of these residues have been partly identified using chromatography techniques, which indicate that they contain molecular precursors of prebiotic interest such as amino acids, nitrile-bearing compounds, and amphiphilic compounds. In this study, we present the first X-ray absorption near-edge structure (XANES) spectroscopy measurements of three organic residues made from the UV irradiation of ices having different starting compositions. XANES spectra confirm the presence of different chemical functions in these residues, and indicate that they are rich in nitrogen- and oxygen-bearing species. These data can be compared with XANES measurements of extraterrestrial materials. Finally, this study also shows how soft X rays can alter the chemical composition of samples. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Nuevo, M.; Milam, S. N.; Sandford, S. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Milam, S. N.] SETI Inst, Mountain View, CA 94043 USA.
[De Gregorio, B. T.] USN, Res Lab, Washington, DC 20375 USA.
[Cody, G. D.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA.
[Kilcoyne, A. L. D.] Univ Calif Berkeley, Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA 94720 USA.
RP Nuevo, M (reprint author), NASA, Ames Res Ctr, Mail Stop 245-6, Moffett Field, CA 94035 USA.
EM michel.nuevo-1@nasa.gov
RI Milam, Stefanie/D-1092-2012; De Gregorio, Bradley/B-8465-2008; Kilcoyne,
David/I-1465-2013
OI Milam, Stefanie/0000-0001-7694-4129; De Gregorio,
Bradley/0000-0001-9096-3545;
FU NASA
FX This work was supported by NASA grants from the "Origins of Solar
Systems" and "Astrobiology" programs.
NR 65
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PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD SEP 15
PY 2011
VL 48
IS 6
BP 1126
EP 1135
DI 10.1016/j.asr.2011.05.020
PG 10
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 809EK
UT WOS:000294034400017
ER
PT J
AU Keller, LP
Messenger, S
AF Keller, Lindsay P.
Messenger, Scott
TI On the origins of GEMS grains
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID INTERPLANETARY DUST PARTICLES; INTERSTELLAR SILICATE GRAINS; OXYGEN
ISOTOPIC ABUNDANCES; MOLECULAR-CLOUD MATERIAL; PRESOLAR SPINEL GRAINS;
RED GIANT STARS; CARBONACEOUS CHONDRITES; SOLAR NEBULA; CRYSTALLINE
SILICATES; EMBEDDED METAL
AB From their birth as condensates in the outflows of oxygen-rich evolved stars, processing in interstellar space, and incorporation into disks around new stars, amorphous silicates predominate in most astrophysical environments. Amorphous silicates were a major building block of our Solar System and are prominent in infrared spectra of comets. Anhydrous interplanetary dust particles (IDPs) thought to derive from comets contain abundant amorphous silicates known as GEMS (glass with embedded metal and sulfides) grains. GEMS grains have been proposed to be isotopically and chemically homogenized interstellar amorphous silicate dust. We evaluated this hypothesis through coordinated chemical and isotopic analyses of GEMS grains in a suite of IDPs to constrain their origins. GEMS grains show order of magnitude variations in Mg, Fe, Ca, and S abundances. GEMS grains do not match the average element abundances inferred for ISM dust containing on average, too little Mg, Fe, and Ca, and too much S. GEMS grains have complementary compositions to the crystalline components in IDPs suggesting that they formed from the same reservoir. We did not observe any unequivocal microstructural or chemical evidence that GEMS grains experienced prolonged exposure to radiation.
We identified four GEMS grains having O isotopic compositions that point to origins in red giant branch or asymptotic giant branch stars and supernovae. Based on their O isotopic compositions, we estimate that 1-6% of GEMS grains are surviving circumstellar grains. The remaining 94-99% of GEMS grains have O isotopic compositions that are indistinguishable from terrestrial materials and carbonaceous chondrites. These isotopically solar GEMS grains either formed in the Solar System or were completely homogenized in the interstellar medium (ISM). However, the chemical compositions of GEMS grains are extremely heterogeneous and seem to rule out this possibility. Based on their solar isotopic compositions and their non-solar elemental compositions we propose that most GEMS grains formed in the nebula as late-stage non-equilibrium condensates. Published by Elsevier Ltd.
C1 [Keller, Lindsay P.; Messenger, Scott] NASA, Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Robert M Walker Lab Space Sci,Code KR, Houston, TX 77058 USA.
RP Keller, LP (reprint author), NASA, Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Robert M Walker Lab Space Sci,Code KR, Houston, TX 77058 USA.
EM Lindsay.P.Keller@nasa.gov
FU NASA
FX This work was supported in part by grants from the NASA Cosmochemistry
program to LPK and SRM. The JEOL 2500SE STEM and the Cameca NanoSIMS 50L
were obtained with grants from the NASA SRLIDAP program. We thank Sara
Russell for her editorial handling. We also thank Conel Alexander and
two anonymous reviewers for their comments on the manuscript.
NR 132
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD SEP 15
PY 2011
VL 75
IS 18
BP 5336
EP 5365
DI 10.1016/j.gca.2011.06.040
PG 30
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 806BE
UT WOS:000293775200016
ER
PT J
AU Garcia-Garcia, D
Ummenhofer, CC
Zlotnicki, V
AF Garcia-Garcia, David
Ummenhofer, Caroline C.
Zlotnicki, Victor
TI Australian water mass variations from GRACE data linked to Indo-Pacific
climate variability
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Water mass variations; Australia; Indian Ocean Dipole; Tpime variable
gravity
ID TIME-VARIABLE GRAVITY; INDIAN-OCEAN; ANOMALIES; DIPOLE; FIELD
AB Time-variable gravity data from the Gravity Recovery And Climate Experiment (GRACE) mission are used to study total water content over Australia for the period 2002-2010. A time-varying annual signal explains 61% of the variance of the data, in good agreement with two independent estimates of the same quantity from hydrological models. Water mass content variations across Australia are linked to Pacific and Indian Ocean variability, associated with El Nino-Southern Oscillation (ENSO) and the Indian Ocean Dipole (IOD), respectively. From 1989, positive (negative) IOD phases were related to anomalously low (high) precipitation in southeastern Australia, associated with a reduced (enhanced) tropical moisture flux. In particular, the sustained water mass content reduction over central and southern regions of Australia during the period 2006-2008 is associated with three consecutive positive IOD events. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Garcia-Garcia, David] Univ Alicante, EPS, Dept Appl Math, Alicante, Spain.
[Ummenhofer, Caroline C.] Univ New S Wales, Climate Change Res Ctr, Sydney, NSW, Australia.
[Zlotnicki, Victor] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Garcia-Garcia, D (reprint author), Univ Alicante, EPS, Dept Appl Math, Alicante, Spain.
EM d.garcia@ua.es
RI Garcia-Garcia, David/L-7535-2014
OI Garcia-Garcia, David/0000-0002-7273-9037
FU NASA; MICIN [ESP2006-11357, AYA2009-07981]; Generalitat Valenciana
[ACOMP2009/031]; University of Alicante [GRE10-13]; GRACE Science Team
FX We thank F.W. Landerer for GRACE data processing support, and all the
organizations providing the used data: time-variable gravity data
provided by the GRACE team; GLDAS hydrological data by GSFC/NASA; ocean
bottom pressure by ECCO group; P-E data by ECMWF; HadISST from the
Hadley Centre, UK Met Office; winds and specific humidity from the
NCEP/NCAR reanalysis project provided by NOAA/OAR/ESRL PSD, Boulder,
USA, through their website http://www.cdc.noaa.gov; SOI by the
Australian Bureau of Meteorology, DMI by Ocean Observations Panel for
Climate from the UNESCO, Australian rainfall and soil moisture from AWAP
kindly provided by Peter Briggs. This work has been partly supported by
a NASA GRACE Science Team grant, two Spanish Projects from MICIN,
ESP2006-11357 and AYA2009-07981, one from Generalitat Valenciana,
ACOMP2009/031, and one from the University of Alicante, GRE10-13. The
third author acknowledges support from the GRACE Science Team; this work
was performed, in part, at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration.
NR 44
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U1 0
U2 25
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP 15
PY 2011
VL 115
IS 9
BP 2175
EP 2183
DI 10.1016/j.rse.2011.04.007
PG 9
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 788ZZ
UT WOS:000292484400001
ER
PT J
AU Roman, MO
Gatebe, CK
Schaaf, CB
Poudyal, R
Wang, ZS
King, MD
AF Roman, Miguel O.
Gatebe, Charles K.
Schaaf, Crystal B.
Poudyal, Rajesh
Wang, Zhuosen
King, Michael D.
TI Variability in surface BRDF at different spatial scales (30 m-500 m)
over a mixed agricultural landscape as retrieved from airborne and
satellite spectral measurements
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE BRDF; Surface albedo; Cloud Absorption Radiometer; MODIS; CLASIC'07; ARM
Climate Research Facility; US Southern Great Plains; Linear model;
Inversion; A priori knowledge; 6S; AERONET; Spatial analysis; APU;
Airborne measurements; Multiangle remote sensing; EOS land validation
core sites
ID REFLECTANCE DISTRIBUTION FUNCTION; BIDIRECTIONAL REFLECTANCE; ALBEDO
PRODUCTS; AVHRR DATA; MULTIANGULAR MEASUREMENTS; INSTRUMENT DESCRIPTION;
VEGETATION STRUCTURE; NADIR REFLECTANCE; DESERT GRASSLAND; MODIS
AB Over the past decade, the role of multiangle remote sensing has been central to the development of algorithms for the retrieval of global land surface properties including models of the bidirectional reflectance distribution function (BRDF), albedo, land cover/dynamics, burned area extent, as well as other key surface biophysical quantities impacted by the anisotropic reflectance characteristics of vegetation. In this study, a new retrieval strategy for fine-to-moderate resolution multiangle observations was developed, based on the operational sequence used to retrieve the Moderate Resolution Imaging Spectroradiometer (MODIS) Collection 5 reflectance and BRDF/albedo products. The algorithm makes use of a semiempirical kernel-driven bidirectional reflectance model to provide estimates of intrinsic albedo (i.e., directional-hemispherical reflectance and bihemispherical reflectance), model parameters describing the BRDF, and extensive quality assurance information. The new retrieval strategy was applied to NASA's Cloud Absorption Radiometer (CAR) data acquired during the 2007 Cloud and Land Surface Interaction Campaign (CLASIC) over the well-instrumented Atmospheric Radiation Measurement Program (ARM) Southern Great Plains (SGP) Cloud and Radiation Testbed (CART) site in Oklahoma, USA. For the case analyzed, we obtained similar to 1.6 million individual surface bidirectional reflectance factor (BRF) retrievals, from nadir to 75 degrees off-nadir, and at spatial resolutions ranging from 3 m to 500 m. This unique dataset was used to examine the interaction of the spatial and angular characteristics of a mixed agricultural landscape; and provided the basis for detailed assessments of: (1) the use of a land cover type-specific a priori knowledge in kernel-driven BRDF model inversions; (2) the interaction between surface reflectance anisotropy and instrument spatial resolution: and (3) the uncertainties that arise when sub-pixel differences in the BRDF are aggregated to a moderate resolution satellite pixel. Results offer empirical evidence concerning the influence of scale and spatial heterogeneity in kernel-driven BRDF models; providing potential new insights into the behavior and characteristics of different surface radiative properties related to land/use cover change and vegetation structure. Published by Elsevier Inc.
C1 [Roman, Miguel O.; Gatebe, Charles K.; Poudyal, Rajesh] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD USA.
[Gatebe, Charles K.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Schaaf, Crystal B.; Wang, Zhuosen] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA.
[Poudyal, Rajesh] Sci Syst & Applicat Inc, Lanham, MD USA.
[King, Michael D.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
RP Roman, MO (reprint author), NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD USA.
EM Miguel.O.Roman@nasa.gov
RI King, Michael/C-7153-2011; Gatebe, Charles/G-7094-2011; Roman,
Miguel/D-4764-2012
OI King, Michael/0000-0003-2645-7298; Gatebe, Charles/0000-0001-9261-2239;
Roman, Miguel/0000-0003-3953-319X
FU Science Mission Directorate of the National Aeronautics and Space
Administration; Earth Observing System; Radiation Sciences Program;
Airborne Science Program; NASA [NNX08AF89G, NNX07AT35H, NNX08AE94A];
U.S. Department of Energy (DOE) [DOE-DE-FG02-06ER64178]
FX The research reported in this article was supported by the Science
Mission Directorate of the National Aeronautics and Space Administration
as part of the Earth Observing System, Radiation Sciences Program and
Airborne Science Program. We thank the CLASIC Science team (B. Schmidt,
M. Miller, P. Lamb, J. Ogren, J. Mather et al.) and Sky Research, J-31
aircraft team (D. Thrasher, S. Kaiser, K. Zimmerer & R. Billings) for
their support during the CLASIC experiment; as well as Dr. Mark J.
Chopping (Montclair State University) and three anonymous reviewers, for
their valuable comments. The analysis was performed under NASA Grants
NNX08AF89G (CKG), NNX07AT35H and NNX08AE94A (CBS); and the U.S.
Department of Energy (DOE) Atmospheric Radiation Measurement (ARM)
Program under grant DOE-DE-FG02-06ER64178 (CBS).
NR 89
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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 SEP 15
PY 2011
VL 115
IS 9
BP 2184
EP 2203
DI 10.1016/j.rse.2011.04.012
PG 20
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 788ZZ
UT WOS:000292484400002
ER
PT J
AU Shuai, YM
Masek, JG
Gao, F
Schaaf, CB
AF Shuai, Yanmin
Masek, Jeffrey G.
Gao, Feng
Schaaf, Crystal B.
TI An algorithm for the retrieval of 30-m snow-free albedo from Landsat
surface reflectance and MODIS BRDF
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Surface albedo; Algorithm; Validation; Landsat; MODIS
ID BIDIRECTIONAL REFLECTANCE; NADIR REFLECTANCE; EARTHS SURFACE; COVER
CHANGE; CLIMATE; MODELS; SCALE; VALIDATION; VEGETATION; SPACE
AB We present a new methodology to generate 30-m resolution land surface albedo using Landsat surface reflectance and anisotropy information from concurrent MODIS 500-m observations. Albedo information at fine spatial resolution is particularly useful for quantifying climate impacts associated with land use change and ecosystem disturbance. The derived white-sky and black-sky spectral albedos may be used to estimate actual spectral albedos by taking into account the proportion of direct and diffuse solar radiation arriving at the ground. A further spectral-to-broadband conversion based on extensive radiative transfer simulations is applied to produce the broadband albedos at visible, near infrared, and shortwave regimes. The accuracy of this approach has been evaluated using 270 Landsat scenes covering six field stations supported by the SURFace RADiation Budget Network (SURFRAD) and Atmospheric Radiation Measurement Southern Great Plains (ARM/SGP) network Comparison with field measurements shows that Landsat 30-m snow-free shortwave albedos from all seasons generally achieve an absolute accuracy of +/- 0.02-0.05 for these validation sites during available clear days in 2003-2005, with a root mean square error less than 0.03 and a bias less than 0.02. This level of accuracy has been regarded as sufficient for driving global and regional climate models. The Landsat-based retrievals have also been compared to the operational 16-day MODIS albedo produced every 8-days from MODIS on Terra and Aqua (MCD43A). The Landsat albedo provides more detailed landscape texture, and achieves better agreement (correlation and dynamic range) with in-situ data at the validation stations, particularly when the stations include a heterogeneous mix of surface covers. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Shuai, Yanmin; Masek, Jeffrey G.; Gao, Feng] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Shuai, Yanmin; Gao, Feng] Earth Resources Technol Inc, Laurel, MD 20707 USA.
[Schaaf, Crystal B.] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA.
[Schaaf, Crystal B.] Boston Univ, Ctr Remote Sensing, Boston, MA 02215 USA.
RP Shuai, YM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Yanmin.Shuai@ertcorp.com
RI Masek, Jeffrey/D-7673-2012; Shuai, Yanmin/G-1329-2012
FU US Geological Survey Landsat Science Team; NASA; MODIS Science Team
[NNX08AE94A]
FX This study was supported by the US Geological Survey Landsat Science
Team and the NASA Terrestrial Ecology Program as well as funding for the
MODIS Science Team (NNX08AE94A). The authors would like to thank CAVE
for supplying the SURFRAD and ARM datasets, and the LEDAPS Project for
providing Landsat surface reflectance.
NR 59
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U1 4
U2 39
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 SEP 15
PY 2011
VL 115
IS 9
BP 2204
EP 2216
DI 10.1016/j.rse.2011.04.019
PG 13
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 788ZZ
UT WOS:000292484400003
ER
PT J
AU Phillips, T
Leyk, S
Rajaram, H
Colgan, W
Abdalati, W
McGrath, D
Steffen, K
AF Phillips, T.
Leyk, S.
Rajaram, H.
Colgan, W.
Abdalati, W.
McGrath, D.
Steffen, K.
TI Modeling moulin distribution on Sermeq Avannarleq glacier using ASTER
and WorldView imagery and fuzzy set theory
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Cryosphere; Fuzzy set theory; Surface melt; ASTER DEM; Ablation zone
ID GREENLAND ICE-SHEET; CLASSIFICATION; ACCELERATION; TEMPERATURE;
MULTISCALE; ELEVATION; DRAINAGE; SYSTEMS; FLOW; MELT
AB A fuzzy set overlay model is used to analyze the distribution of moulins (vertical meltwater conduits) on Sermeq Avannarleq ("Dead Glacier") in West Greenland in 1985 and 2008-09. Input data is derived from a historical topographic map based on airborne visible imagery and more recent WorldView-1 panchromatic imagery, as well as an Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) digital elevation model (DEM). A non-parametric best-fit model approach using a Monte Carlo simulation is used to derive the membership functions for moulin location based on three independent variables - elevation, slope and aspect - and to test for the robustness of the model. We determine that there is a topographic setting independent of time that favors the development of moulins in this region. Using the membership functions, and an optimal alpha cut derived for 1985, we could correctly predict the locations of -88% of the moulins in 2008-09. The model accounts for increased surface melt in 2008-09 in comparison to 1985. Our results demonstrate the potential of a fuzzy set based approach to improve models of ice sheet hydrology in Western Greenland, by providing more reliable spatial distributions of entry points of meltwater into the ice based on remotely sensed datasets of the ice surface, which are readily available. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Phillips, T.] Univ Colorado, Dept Aerosp Engn & Sci, Boulder, CO 80309 USA.
[Phillips, T.; Abdalati, W.] Univ Colorado, Earth Syst Observat Ctr, Boulder, CO 80309 USA.
[Leyk, S.; Colgan, W.; Abdalati, W.; McGrath, D.; Steffen, K.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA.
[Rajaram, H.] Univ Colorado, Dept Civil Environm & Architectural Engn, Boulder, CO 80309 USA.
[Colgan, W.; Abdalati, W.; McGrath, D.; Steffen, K.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Abdalati, W.] NASA Headquarters, Washington, DC USA.
RP Phillips, T (reprint author), Univ Colorado, Dept Aerosp Engn & Sci, Boulder, CO 80309 USA.
EM Thomas.Phillips@colorado.edu
RI Colgan, William/H-1570-2014; Steffen, Konrad/C-6027-2013;
OI Colgan, William/0000-0001-6334-1660; Steffen,
Konrad/0000-0001-8658-1026; MCGRATH, DANIEL/0000-0002-9462-6842
FU NASA [NNX08AT85G, NNX07AF15G]; NSF DDRI [0926911]; NSERC; CIRES
FX This research was supported by NASA Cryosphere Science Program grants
NNX08AT85G and NNX07AF15G and the NSF DDRI grant 0926911. WC thanks
NSERC and CIRES for fellowship support. We would also like to thank two
anonymous reviewers for their very valuable insights.
NR 48
TC 14
Z9 16
U1 5
U2 19
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP 15
PY 2011
VL 115
IS 9
BP 2292
EP 2301
DI 10.1016/j.rse.2011.04.029
PG 10
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 788ZZ
UT WOS:000292484400010
ER
PT J
AU Frankenberg, C
Fisher, JB
Worden, J
Badgley, G
Saatchi, SS
Lee, JE
Toon, GC
Butz, A
Jung, M
Kuze, A
Yokota, T
AF Frankenberg, Christian
Fisher, Joshua B.
Worden, John
Badgley, Grayson
Saatchi, Sassan S.
Lee, Jung-Eun
Toon, Geoffrey C.
Butz, Andre
Jung, Martin
Kuze, Akihiko
Yokota, Tatsuya
TI New global observations of the terrestrial carbon cycle from GOSAT:
Patterns of plant fluorescence with gross primary productivity
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID NET PRIMARY PRODUCTION; FOURIER-TRANSFORM SPECTROMETER; GASES OBSERVING
SATELLITE; SUN-INDUCED FLUORESCENCE; CHLOROPHYLL FLUORESCENCE;
PHOTOSYNTHESIS; CLIMATE; MODEL; LEAF; EFFICIENCY
AB Our ability to close the Earth's carbon budget and predict feedbacks in a warming climate depends critically on knowing where, when and how carbon dioxide is exchanged between the land and atmosphere. Terrestrial gross primary production (GPP) constitutes the largest flux component in the global carbon budget, however significant uncertainties remain in GPP estimates and its seasonality. Empirically, we show that global spaceborne observations of solar induced chlorophyll fluorescence - occurring during photosynthesis - exhibit a strong linear correlation with GPP. We found that the fluorescence emission even without any additional climatic or model information has the same or better predictive skill in estimating GPP as those derived from traditional remotely-sensed vegetation indices using ancillary data and model assumptions. In boreal summer the generally strong linear correlation between fluorescence and GPP models weakens, attributable to discrepancies in savannas/croplands (18-48% higher fluorescence-based GPP derived by simple linear scaling), and high-latitude needleleaf forests (28-32% lower fluorescence). Our results demonstrate that retrievals of chlorophyll fluorescence provide direct global observational constraints for GPP and open an entirely new viewpoint on the global carbon cycle. We anticipate that global fluorescence data in combination with consolidated plant physiological fluorescence models will be a step-change in carbon cycle research and enable an unprecedented robustness in the understanding of the current and future carbon cycle. Citation: Frankenberg, C., et al. (2011), New global observations of the terrestrial carbon cycle from GOSAT: Patterns of plant fluorescence with gross primary productivity, Geophys. Res. Lett., 38, L17706, doi: 10.1029/2011GL048738.
C1 [Frankenberg, Christian; Fisher, Joshua B.; Worden, John; Badgley, Grayson; Saatchi, Sassan S.; Lee, Jung-Eun; Toon, Geoffrey C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Butz, Andre] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-76344 Leopoldshafen, Germany.
[Jung, Martin] Max Planck Inst Biogeochem, Biogeochem Model Data Integrat Grp, D-07745 Jena, Germany.
[Kuze, Akihiko] Japan Aerosp Explorat Agcy, Tsukuba, Ibaraki 3058505, Japan.
[Yokota, Tatsuya] Natl Inst Environm Studies, Tsukuba, Ibaraki 3058506, Japan.
RP Frankenberg, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM christian.frankenberg@jpl.nasa.gov
RI Lee, Jung-Eun/F-8981-2012; Butz, Andre/A-7024-2013; KUZE,
AKIHIKO/J-2074-2016; Frankenberg, Christian/A-2944-2013;
OI Butz, Andre/0000-0003-0593-1608; KUZE, AKIHIKO/0000-0001-5415-3377;
Frankenberg, Christian/0000-0002-0546-5857; Fisher,
Joshua/0000-0003-4734-9085
NR 29
TC 121
Z9 123
U1 18
U2 101
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 SEP 14
PY 2011
VL 38
AR L17706
DI 10.1029/2011GL048738
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 823PN
UT WOS:000295135000002
ER
PT J
AU Jolivet, R
Grandin, R
Lasserre, C
Doin, MP
Peltzer, G
AF Jolivet, R.
Grandin, R.
Lasserre, C.
Doin, M. -P.
Peltzer, G.
TI Systematic InSAR tropospheric phase delay corrections from global
meteorological reanalysis data
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MOUNT-ETNA; DEFORMATION; GPS; FAULT; INTERFEROMETRY; INTERFEROGRAMS;
CHINA
AB Despite remarkable successes achieved by Differential InSAR, estimations of low tectonic strain rates remain challenging in areas where deformation and topography are correlated, mainly because of the topography-related atmospheric phase screen (APS). In areas of high relief, empirical removal of the stratified component of the APS may lead to biased estimations of tectonic deformation rates. Here we describe a method to correct interferograms from the effects of the spatial and temporal variations in tropospheric stratification by computing tropospheric delay maps coincident with SAR acquisitions using the ERA-Interim global meteorological model. The modeled phase delay is integrated along vertical profiles at the ERA-I grid nodes and interpolated at the spatial sampling of the interferograms above the elevation of each image pixel. This approach is validated on unwrapped interferograms. We show that the removal of the atmospheric signal before phase unwrapping reduces the risk of unwrapping errors in areas of rough topography. Citation: Jolivet, R., R. Grandin, C. Lasserre, M.-P. Doin, and G. Peltzer (2011), Systematic InSAR tropospheric phase delay corrections from global meteorological reanalysis data, Geophys. Res. Lett., 38, L17311, doi: 10.1029/2011GL048757.
C1 [Jolivet, R.; Lasserre, C.] Univ Grenoble 1, CNRS, UMR 5275, Inst Sci Terre, F-38041 Grenoble, France.
[Grandin, R.; Doin, M. -P.] Ecole Normale Super, CNRS, UMR 8538, Geol Lab, F-75005 Paris, France.
[Peltzer, G.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Peltzer, G.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Jolivet, R (reprint author), Univ Grenoble 1, CNRS, UMR 5275, Inst Sci Terre, BP 53, F-38041 Grenoble, France.
RI Lasserre, Cecile/D-7073-2017; Grandin, Raphael/K-4031-2012;
OI Lasserre, Cecile/0000-0002-0582-0775; Grandin,
Raphael/0000-0002-1837-011X; Jolivet, Romain/0000-0002-9896-3651
FU Young Scientist fellowship; French Agence Nationale pour la Recherche
(EFIDIR) [ANR-07-MDCO-04]; Institut National des Sciences de l'Univers
(Risk, PNTS); Centre National d'Etudes Spatiales; NASA
FX The SAR data set was provided by the European Space Agency (ESA) in the
framework of the Dragon program (projects ID 2509 and 5305). This
program also partly supported R. Jolivet and R. Grandin's work, through
the Young Scientist fellowship. Funding was provided by the French
Agence Nationale pour la Recherche (EFIDIR, project ANR-07-MDCO-04) and
Institut National des Sciences de l'Univers (Risk, PNTS). Postdoctoral
fellowship for R. Grandin was provided by Centre National d'Etudes
Spatiales. Part of G. Peltzer's contribution was done at the Jet
Propulsion Laboratory, California Institute of Technology under contract
with NASA. We thank two anonymous reviewers for their constructive
comments.
NR 31
TC 55
Z9 55
U1 0
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 SEP 14
PY 2011
VL 38
AR L17311
DI 10.1029/2011GL048757
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 823PN
UT WOS:000295135000003
ER
PT J
AU Lau, KM
Wu, HT
AF Lau, K. -M.
Wu, H. -T.
TI Climatology and changes in tropical oceanic rainfall characteristics
inferred from Tropical Rainfall Measuring Mission (TRMM) data
(1998-2009)
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ORBIT BOOST; PRECIPITATION RADAR; MICROWAVE IMAGER; VARIABILITY;
SATELLITE; TRENDS; MODEL; PR
AB This study investigates the climatological and changing characteristics of tropical rain and cloud systems in relation to sea surface temperature (SST) changes using Tropical Rainfall Measuring Mission (TRMM) data (1998-2009). Rainfall and cloud characteristics are determined from probability distribution functions (pdf), derived from daily TRMM Microwave Imager (TMI) and Precipitation Radar (PR) surface rain, Visible and Infrared Scanner (VIRS) brightness temperature (T-b), and PR echo top height (HET). Results show that the top 10% heavy rain is associated with cold cloud tops (T-b < 220 K) and elevated echo top heights (HET > 6 km), associated with ice phase rain in the Intertropical Convergence Zone and monsoon regions. The bottom 5% light rain occurs most frequently in the subtropics and also in the warm pool regions with low cloud top (T-b > 273 K) and H-ET similar to 1-4 km. Intermediate rain (25th to 75th percentile) is contributed by a wide range of middle clouds and mixed-phase rain centered at T-b similar to 230-260 K and HET similar to 4-6 km within the warm pool. The relationships between rainfall and SST depend strongly on rain types. We find that a warmer tropical ocean favors a large increase in annual heavy rain accumulation, a mild reduction in light to moderate rain, and a slight increase in extremely light rain. The annual accumulation of extreme heavy rain increases approximately 80%-90% for every degree rise in SST, much higher than that expected from the Clausius-Clapeyron equation for global water balance. This is possibly because heavy rain is only a component of the tropical water cycle and is strongly associated with ice phase processes and convective dynamics feedback.
C1 [Lau, K. -M.] NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wu, H. -T.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
RP Lau, KM (reprint author), NASA, Atmospheres Lab, Goddard Space Flight Ctr, Code 613,Bldg 33,Rm C121, Greenbelt, MD 20771 USA.
EM william.k.lau@nasa.gov
RI Lau, William /E-1510-2012
OI Lau, William /0000-0002-3587-3691
FU Precipitation Measurement Mission, NASA headquarters
FX This research is supported by the Precipitation Measurement Mission,
NASA headquarters (Program Manager R. Kakar). The authors would like to
thank three anonymous reviewers for providing constructive and critical
comments on the paper.
NR 28
TC 18
Z9 18
U1 1
U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 14
PY 2011
VL 116
AR D17111
DI 10.1029/2011JD015827
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 823OF
UT WOS:000295131100007
ER
PT J
AU Nemeth, Z
Szego, K
Bebesi, Z
Erdos, G
Foldy, L
Rymer, A
Sittler, EC
Coates, AJ
Wellbrock, A
AF Nemeth, Zoltan
Szego, Karoly
Bebesi, Zsofia
Erdos, Geza
Foldy, Lajos
Rymer, Abigail
Sittler, Edward C.
Coates, Andrew J.
Wellbrock, Anne
TI Ion distributions of different Kronian plasma regions
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID MASS-SPECTROMETER; WAVE OBSERVATIONS; CASSINI; RADIO
AB Plasma data from the Cassini Plasma Spectrometer experiment were used to investigate the properties of the variable plasma environment of Titan's orbit. The characteristics of this plasma environment play a crucial role in the plasma-moon interaction and also have a strong influence on the ionosphere of Titan. Using dynamic energy spectra of ions within +/- 3 h of the Titan flybys we identified different ambient plasma environments, similar to the ones proposed earlier based on electron measurements. Expanding the time interval to 12 h to cover full SKR periods, and taking into account the composition of the ions, we showed that the longer intervals include all the previous categories, and a special one, a short event, rich in heavy ions. Detailed study of the vicinity of these events revealed the fine structure of the magnetodisk of Saturn, having a narrow central sheet of very high heavy ion content, heavy rich events occurring when the spacecraft crosses this central sheet. We also proved that the heavy rich events appear periodically in longitude, but with a period slightly (by 0.35 degrees/day) longer than the SLS3 period.
C1 [Nemeth, Zoltan; Szego, Karoly; Erdos, Geza; Foldy, Lajos] KFKI Res Inst Particle & Nucl Phys, Dept Space Phys, H-1225 Budapest, Hungary.
[Bebesi, Zsofia] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Coates, Andrew J.; Wellbrock, Anne] Univ Coll London, Mullard Space Sci Labs, Planetary Grp, Dorking RH5 6NT, Surrey, England.
[Sittler, Edward C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rymer, Abigail] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Nemeth, Z (reprint author), KFKI Res Inst Particle & Nucl Phys, Dept Space Phys, POB 49, H-1225 Budapest, Hungary.
EM nemeth@rmki.kfki.hu
RI Coates, Andrew/C-2396-2008
OI Coates, Andrew/0000-0002-6185-3125
FU Hungarian Space Office
FX The authors thank Michelle F. Thomsen for helpful discussion. The
Hungarian authors acknowledge the financial support of the Hungarian
Space Office.
NR 29
TC 18
Z9 18
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP 13
PY 2011
VL 116
AR A09212
DI 10.1029/2011JA016585
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823PB
UT WOS:000295133700002
ER
PT J
AU Wan, P
Liu, J
Yang, LM
Amzajerdian, F
AF Wan, Peng
Liu, Jian
Yang, Lih-Mei
Amzajerdian, Farzin
TI Low repetition rate high energy 1.5 mu m fiber laser
SO OPTICS EXPRESS
LA English
DT Article
ID THRESHOLD; NM
AB In this paper, we report, for the first time, that by modulating pump beam to suppress ASE effect we realized ultra-low repetition rate output in an all fiber based Er:Yb codoped master oscillator power amplifiers (MOPA) system. Combined with pulse shaping technology, pulses with up to 205 mu J pulse energy and 200 ns pulse duration were obtained at Hz level. (C) 2011 Optical Society of America
C1 [Wan, Peng; Liu, Jian; Yang, Lih-Mei] Polaronyx Inc, San Jose, CA 95131 USA.
[Amzajerdian, Farzin] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Wan, P (reprint author), Polaronyx Inc, 2526 Qume Dr,Suite 17 & 18, San Jose, CA 95131 USA.
EM pwan@polaronyx.com
FU NASA SBIR
FX This paper is supported in part by NASA SBIR contracts.
NR 12
TC 11
Z9 12
U1 0
U2 3
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD SEP 12
PY 2011
VL 19
IS 19
BP 18067
EP 18071
DI 10.1364/OE.19.018067
PG 5
WC Optics
SC Optics
GA 818UL
UT WOS:000294781200036
PM 21935172
ER
PT J
AU Josset, D
Rogers, R
Pelon, J
Hu, YX
Liu, ZY
Omar, A
Zhai, PW
AF Josset, Damien
Rogers, Raymond
Pelon, Jacques
Hu, Yongxiang
Liu, Zhaoyan
Omar, Ali
Zhai, Peng-Wang
TI CALIPSO lidar ratio retrieval over the ocean
SO OPTICS EXPRESS
LA English
DT Article
ID SPECTRAL-RESOLUTION LIDAR; OPTICAL-PROPERTIES; AEROSOL; CLOUDS;
CALIBRATION; PARTICLES; ALGORITHM; PROFILES
AB We are demonstrating on a few cases the capability of CALIPSO to retrieve the 532 nm lidar ratio over the ocean when CloudSat surface scattering cross section is used as a constraint. We are presenting the algorithm used and comparisons with the column lidar ratio retrieved by the NASA airborne high spectral resolution lidar. For the three cases presented here, the agreement is fairly good. The average CALIPSO 532 nm column lidar ratio bias is 13.7% relative to HSRL, and the relative standard deviation is 13.6%. Considering the natural variability of aerosol microphysical properties, this level of accuracy is significant since the lidar ratio is a good indicator of aerosol types. We are discussing dependencies of the accuracy of retrieved aerosol lidar ratio on atmospheric aerosol homogeneity, lidar signal to noise ratio, and errors in the optical depth retrievals. We are obtaining the best result (bias 7% and standard deviation around 6%) for a nighttime case with a relatively constant lidar ratio (in the vertical) indicative of homogeneous aerosol type. (C) 2011 Optical Society of America
C1 [Josset, Damien; Zhai, Peng-Wang] SSAI, Hampton, VA 23681 USA.
[Rogers, Raymond; Hu, Yongxiang; Omar, Ali] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Pelon, Jacques] Univ Paris 06, LATMOS, CNRS, UMR 8190, F-75252 Paris 05, France.
[Liu, Zhaoyan] NLA, Hampton, VA 23681 USA.
RP Josset, D (reprint author), SSAI, Hampton, VA 23681 USA.
EM damien.b.josset@nasa.gov
RI Liu, Zhaoyan/B-1783-2010; Hu, Yongxiang/K-4426-2012; Omar,
Ali/D-7102-2017
OI Liu, Zhaoyan/0000-0003-4996-5738; Omar, Ali/0000-0003-1871-9235
FU CALIPSO NASA; NASA; CNES; Science Systems and Applications Inc. (SSAI);
National Institute of Aerospace (NIA)
FX The CALIPSO NASA project is greatly acknowledged for its support and for
funding the HSRL flights as well as CALIPSO NASA/CNES, CloudSat and
AMSR-E projects for data availability. The French Thematic center ICARE
(http://www.icare.univ-lille1.fr/) is greatly acknowledge for developing
and archiving the SODA project. NASA, CNES, Science Systems and
Applications Inc. (SSAI) and National Institute of Aerospace (NIA) are
greatly acknowledged for their support. The authors gratefully
acknowledge the NOAA Air Resources Laboratory (ARL) for the provision of
the HYSPLIT transport and dispersion model and READY website
(http://www.arl.noaa.gov/ready.php) used in this publication.
NR 29
TC 4
Z9 5
U1 1
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 SEP 12
PY 2011
VL 19
IS 19
BP 18696
EP 18706
DI 10.1364/OE.19.018696
PG 11
WC Optics
SC Optics
GA 818UL
UT WOS:000294781200102
PM 21935239
ER
PT J
AU Bauer, JM
Walker, RG
Mainzer, AK
Masiero, JR
Grav, T
Dailey, JW
McMillan, RS
Lisse, CM
Fernandez, YR
Meech, KJ
Pittichova, J
Blauvelt, EK
Masci, FJ
A'Hearn, MF
Cutri, RM
Scotti, JV
Tholen, DJ
DeBaun, E
Wilkins, A
Hand, E
Wright, EL
AF Bauer, James M.
Walker, Russell G.
Mainzer, A. K.
Masiero, Joseph R.
Grav, Tommy
Dailey, John W.
McMillan, Robert S.
Lisse, Carey M.
Fernandez, Yan R.
Meech, Karen J.
Pittichova, Jana
Blauvelt, Erin K.
Masci, Frank J.
A'Hearn, Michael F.
Cutri, Roc M.
Scotti, James V.
Tholen, David J.
DeBaun, Emily
Wilkins, Ashlee
Hand, Emma
Wright, Edward L.
CA WISE Team
TI WISE/NEOWISE OBSERVATIONS OF COMET 103P/HARTLEY 2
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets: individual (103P/Hartley 2); infrared: planetary systems
ID INFRARED-SURVEY-EXPLORER; NEAR-EARTH ASTEROIDS; SHORT-PERIOD COMETS;
DEEP IMPACT EJECTA; PHYSICAL-PROPERTIES; SPACE-TELESCOPE; THERMAL-MODEL;
SOLAR-SYSTEM; SPITZER; NUCLEUS
AB We report results based on mid-infrared photometry of comet 103P/Hartley 2 taken during 2010 May 4-13 ( when the comet was at a heliocentric distance of 2.3 AU, and an observer distance of 2.0 AU) by the Wide-field Infrared Survey Explorer. Photometry of the coma at 22 mu m and data from the University of Hawaii 2.2 m telescope obtained on 2010 May 22 provide constraints on the dust particle size distribution, d log n/d log m, yielding power-law slope values of alpha = - 0.97 +/- 0.10, steeper than that found for the inbound particle fluence during the Stardust encounter of comet 81P/Wild 2. The extracted nucleus signal at 12 mu m is consistent with a body of average spherical radius of 0.6 +/- 0.2 km ( one standard deviation), assuming a beaming parameter of 1.2. The 4.6 mu m band signal in excess of dust and nucleus reflected and thermal contributions may be attributed to carbon monoxide or carbon dioxide emission lines and provides limits and estimates of species production. Derived carbon dioxide coma production rates are 3.5(+/- 0.9) x 1024 molecules per second. Analyses of the trail signal present in the stacked image with an effective exposure time of 158.4 s yields optical-depth values near 9 x 10(-10) at a delta mean anomaly of 0.2 deg trailing the comet nucleus, in both 12 and 22 mu m bands. A minimum chi-squared analysis of the dust trail position yields a beta-parameter value of 1.0 x 10(-4), consistent with a derived mean trail-grain diameter of 1.1/rho cm for grains of rho g cm(-3) density. This leads to a total detected trail mass of at least 4 x 10(10) rho kg.
C1 [Bauer, James M.; Mainzer, A. K.; Masiero, Joseph R.; Blauvelt, Erin K.; DeBaun, Emily; Wilkins, Ashlee; Hand, Emma] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bauer, James M.; Dailey, John W.; Masci, Frank J.; Cutri, Roc M.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Walker, Russell G.] Monterey Inst Res Astron, Marina, CA 93933 USA.
[Grav, Tommy] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[McMillan, Robert S.; Scotti, James V.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Fernandez, Yan R.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA.
[Meech, Karen J.; Pittichova, Jana; Tholen, David J.] Univ Hawaii, Inst Astron, Manoa, HI 96822 USA.
[A'Hearn, Michael F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Wright, Edward L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Bauer, JM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-401, Pasadena, CA 91109 USA.
EM bauer@scn.jpl.nasa.gov
RI Lisse, Carey/B-7772-2016;
OI Lisse, Carey/0000-0002-9548-1526; Blauvelt, Erin/0000-0002-2944-5818;
Masiero, Joseph/0000-0003-2638-720X; Fernandez,
Yanga/0000-0003-1156-9721
FU National Aeronautics and Space Administration; Planetary Science
Division of the National Aeronautics and Space Administration
FX This publication makes use of data products from the Wide-field Infrared
Survey Explorer, which is a joint project of the University of
California, Los Angeles, and the Jet Propulsion Laboratory/California
Institute of Technology, funded by the National Aeronautics and Space
Administration. This publication also makes use of data products from
NEOWISE, which is a project of the Jet Propulsion Laboratory/California
Institute of Technology, funded by the Planetary Science Division of the
National Aeronautics and Space Administration. Observing time was
allocated at the University of Hawaii 88 inch telescope at Mauna Kea
Observatory, the Palomar Observatory Hale 200 inch telescope, by the
National Optical Astronomy Observatory at the SOAR telescope, and on
Steward Observatory's 2.3 m on Kitt Peak. The SOAR Telescope is a joint
project of Conselho Nacional de Pesquisas Cientificas e Tecnologicas
CNPq-Brazil, The University of North Carolina at Chapel Hill, Michigan
State University, and the National Optical Astronomy Observatory. The
Hale Telescope at Palomar Observatory is operated as part of a
collaborative agreement between the California Institute of Technology,
its divisions Caltech Optical Observatories and the Jet Propulsion
Laboratory (operated for NASA), and Cornell University. J.M.B. thanks
Dr. M. Hanner for her valuable advice on the analysis and the anonymous
reviewer for their helpful comments.
NR 42
TC 18
Z9 18
U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2011
VL 738
IS 2
AR 171
DI 10.1088/0004-637X/738/2/171
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DE
UT WOS:000294954200053
ER
PT J
AU Bonamente, M
Nevalainen, J
AF Bonamente, Massimiliano
Nevalainen, Jukka
TI X-RAY SPECTROSCOPY OF AS1101 WITH CHANDRA, XMM-NEWTON, AND ROSAT:
BANDPASS DEPENDENCE OF THE TEMPERATURE PROFILE AND SOFT EXCESS EMISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual (AS1101); large-scale structure of
universe
ID HOT INTERGALACTIC MEDIUM; LINE-OF-SIGHT; EXTREME-ULTRAVIOLET EMISSION;
ABSORPTION CROSS-SECTIONS; COMA CLUSTER; GALAXY CLUSTERS; NONTHERMAL
NATURE; HUBBLE CONSTANT; SCULPTOR WALL; DISCOVERY
AB We present spatially resolved spectroscopy of the galaxy cluster AS1101, also known as Sersic 159-03, with Chandra, XMM-Newton, and ROSAT, and investigate the presence of soft X-ray excess emission above the contribution from the hot intracluster medium. In earlier papers we reported an extremely bright soft excess component that reached 100% of the thermal radiation in the R2 ROSAT band (0.2-0.4 keV), using the Hi column density measurement by Dickey and Lockman. In this paper we use the newer Leiden-Argentine-Bonn survey measurements of the Hi column density toward AS1101, significantly lower than the previous value, and show that the soft excess emission in AS1101 is now at the level of 10%-20% of the hot gas emission, in line with those of a large sample of clusters analyzed by Bonamente et al. in 2002. The ROSAT soft excess emission is detected regardless of calibration uncertainties between Chandra and XMM-Newton. This new analysis of AS1101 indicates that the 1/4 keV band emission is compatible with the presence of warm-hot intergalactic medium (WHIM) filaments connected to the cluster and extending outward into the intergalactic medium; the temperatures we find in this study are typically lower than those of the WHIM probed in other X-ray studies. We also show that the soft excess emission is compatible with a non-thermal origin as the inverse Compton scattering of relativistic electrons off the cosmic microwave background, with pressure less than 1% of the thermal electrons.
C1 [Bonamente, Massimiliano] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Bonamente, Massimiliano] NASA, Natl Space & Technol Ctr, Huntsville, AL 35899 USA.
[Nevalainen, Jukka] Univ Turku, Finnish Ctr Astron ESO, FI-21500 Piikkio, Finland.
[Nevalainen, Jukka] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland.
RP Bonamente, M (reprint author), Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
NR 51
TC 2
Z9 2
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 SEP 10
PY 2011
VL 738
IS 2
AR 149
DI 10.1088/0004-637X/738/2/149
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DE
UT WOS:000294954200031
ER
PT J
AU Catanzarite, J
Shao, M
AF Catanzarite, Joseph
Shao, Michael
TI THE OCCURRENCE RATE OF EARTH ANALOG PLANETS ORBITING SUN-LIKE STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; methods: statistical; planets and satellites:
fundamental parameters; planetary systems; stars: solar type;
techniques: photometric
ID EXTRASOLAR PLANETS; MASS; DISTRIBUTIONS
AB Kepler is a space telescope that searches Sun-like stars for planets. Its major goal is to determine eta(Earth), the fraction of Sun-like stars that have planets like Earth. When a planet "transits" or moves in front of a star, Kepler can measure the concomitant dimming of the starlight. From analysis of the first four months of those measurements for over 150,000 stars, Kepler's Science Team has determined sizes, surface temperatures, orbit sizes, and periods for over a thousand new planet candidates. In this paper, we characterize the period probability distribution function of the super-Earth and Neptune planet candidates with periods up to 132 days, and find three distinct period regimes. For candidates with periods below 3 days, the density increases sharply with increasing period; for periods between 3 and 30 days, the density rises more gradually with increasing period, and for periods longer than 30 days, the density drops gradually with increasing period. We estimate that 1%-3% of stars like the Sun are expected to have Earth analog planets, based on the Kepler data release of 2011 February. This estimate of eta(Earth) is based on extrapolation from a fiducial subsample of the Kepler planet candidates that we chose to be nominally "complete" (i.e., no missed detections) to the realm of the Earth-like planets, by means of simple power-law models. The accuracy of the extrapolation will improve as more data from the Kepler mission are folded in. Accurate knowledge of eta(Earth) is essential for the planning of future missions that will image and take spectra of Earth-like planets. Our result that Earths are relatively scarce means that a substantial effort will be needed to identify suitable target stars prior to these future missions.
C1 [Catanzarite, Joseph; Shao, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Catanzarite, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
FU NASA
FX This work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA. Copyright 2011
California Institute of Technology. Government sponsorship acknowledged.
We thank Wes Traub for useful discussions. J.C. thanks Stuart Shaklan
for asking how the Kepler data constrain etaEarth.
NR 17
TC 37
Z9 37
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2011
VL 738
IS 2
AR 151
DI 10.1088/0004-637X/738/2/151
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DE
UT WOS:000294954200033
ER
PT J
AU Fujii, Y
Kawahara, H
Suto, Y
Fukuda, S
Nakajima, T
Livengood, TA
Turner, EL
AF Fujii, Yuka
Kawahara, Hajime
Suto, Yasushi
Fukuda, Satoru
Nakajima, Teruyuki
Livengood, Timothy A.
Turner, Edwin L.
TI COLORS OF A SECOND EARTH. II. EFFECTS OF CLOUDS ON PHOTOMETRIC
CHARACTERIZATION OF EARTH-LIKE EXOPLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; Earth; planets and satellites: surfaces
ID EXTRASOLAR TERRESTRIAL PLANETS; DISK-AVERAGED SPECTRA; LIGHT-CURVES;
VEGETATION SIGNATURE; ATMOSPHERES; OCEAN; MODEL; DETECTABILITY;
SCATTERING; RADIATION
AB As a test bed for future investigations of directly imaged terrestrial exoplanets, we present the recovery of the surface components of the Earth from multi-band diurnal light curves obtained with the EPOXI spacecraft. We find that the presence and longitudinal distribution of ocean, soil, and vegetation are reasonably well reproduced by fitting the observed color variations with a simplified model composed of a priori known albedo spectra of ocean, soil, vegetation, snow, and clouds. The effect of atmosphere, including clouds, on light scattered from surface components is modeled using a radiative transfer code. The required noise levels for future observations of exoplanets are also determined. Our model-dependent approach allows us to infer the presence of major elements of the planet (in the case of the Earth, clouds, and ocean) with observations having signal-to-noise ratio (S/N) greater than or similar to 10 in most cases and with high confidence if S/N greater than or similar to 20. In addition, S/N greater than or similar to 100 enables us to detect the presence of components other than ocean and clouds in a fairly model-independent way. Degradation of our inversion procedure produced by cloud cover is also quantified. While cloud cover significantly dilutes the magnitude of color variations compared with the cloudless case, the pattern of color changes remains. Therefore, the possibility of investigating surface features through light-curve fitting remains even for exoplanets with cloud cover similar to Earth's.
C1 [Fujii, Yuka; Suto, Yasushi; Turner, Edwin L.] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan.
[Kawahara, Hajime] Tokyo Metropolitan Univ, Dept Phys, Tokyo 1920397, Japan.
[Suto, Yasushi] Univ Tokyo, Grad Sch Sci, Res Ctr Early Universe, Tokyo 1130033, Japan.
[Suto, Yasushi; Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Fukuda, Satoru; Nakajima, Teruyuki] Univ Tokyo, Ctr Climate Syst Res, Kashiwa, Chiba 2778568, Japan.
[Livengood, Timothy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Turner, Edwin L.] Univ Tokyo, Inst Phys & Math Univ, Kashiwa, Chiba 2778568, Japan.
RP Fujii, Y (reprint author), Univ Tokyo, Dept Phys, Tokyo 1130033, Japan.
EM yuka.fujii@utap.phys.s.u-tokyo.ac.jp
RI Turner, Edwin/A-4295-2011; Livengood, Timothy/C-8512-2012; Nakajima,
Teruyuki/H-2370-2013;
OI Nakajima, Teruyuki/0000-0002-9042-504X; Kawahara,
Hajime/0000-0003-3309-9134
FU Global Collaborative Research Fund (GCRF) "A World-wide Investigation of
Other Worlds"; Princeton University; JSPS (Japan Society for the
Promotion of Science) [PD:22-5467]; GCRF; World Premier International
Research Center Initiative (WPI Initiative), MEXT, Japan
FX We thank Atsushi Taruya for useful discussion and comments, Giovanna
Tinetti for providing the reflection spectra shown in Figure 7 as a
reference, and Nicolas B. Cowan for his advice concerning the EPOXI data
processing. We are grateful to the OpenCLASTR project for providing the
rstar6b package. Y.F. thanks the staff of the Department of
Astrophysical Sciences of Princeton University for their warm
hospitality during her visit, in particular Dmitry Savransky, Tyler
Groff, and David Spergel for their helpful discussions. Y.F. and Y.S.
gratefully acknowledge support from the Global Collaborative Research
Fund (GCRF) "A World-wide Investigation of Other Worlds" grant, and the
Global Scholars Program of Princeton University, respectively. H. K. is
supported by JSPS (Japan Society for the Promotion of Science)
Fellowship for Research (PD:22-5467). E. L. T. is supported in part by
the GCRF grant and the World Premier International Research Center
Initiative (WPI Initiative), MEXT, Japan. This work is also supported by
JSPS Core-to-Core Program "International Research Network for Dark
Energy."
NR 44
TC 22
Z9 22
U1 1
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2011
VL 738
IS 2
AR 184
DI 10.1088/0004-637X/738/2/184
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DE
UT WOS:000294954200066
ER
PT J
AU Gavazzi, R
Cooray, A
Conley, A
Aguirre, JE
Amblard, A
Auld, R
Beelen, A
Blain, A
Blundell, R
Bock, J
Bradford, CM
Bridge, C
Brisbin, D
Burgarella, D
Chanial, P
Chapin, E
Christopher, N
Clements, DL
Cox, P
Djorgovski, SG
Dowell, CD
Eales, S
Earle, L
Ellsworth-Bowers, TP
Farrah, D
Franceschini, A
Fu, H
Glenn, J
Solares, EAG
Griffin, M
Gurwell, MA
Halpern, M
Ibar, E
Ivison, RJ
Jarvis, M
Kamenetzky, J
Kim, S
Krips, M
Levenson, L
Lupu, R
Mahabal, A
Maloney, PD
Maraston, C
Marchetti, L
Marsden, G
Matsuhara, H
Mortier, AMJ
Murphy, E
Naylor, BJ
Neri, R
Nguyen, HT
Oliver, SJ
Omont, A
Page, MJ
Papageorgiou, A
Pearson, CP
Perez-Fournon, I
Pohlen, M
Rangwala, N
Rawlings, JI
Raymond, G
Riechers, D
Rodighiero, G
Roseboom, IG
Rowan-Robinson, M
Schulz, B
Scott, D
Scott, KS
Serra, P
Seymour, N
Shupe, DL
Smith, AJ
Symeonidis, M
Tugwell, KE
Vaccari, M
Valiante, E
Valtchanov, I
Verma, A
Vieira, JD
Vigroux, L
Wang, L
Wardlow, J
Wiebe, D
Wright, G
Xu, CK
Zeimann, G
Zemcov, M
Zmuidzinas, J
AF Gavazzi, R.
Cooray, A.
Conley, A.
Aguirre, J. E.
Amblard, A.
Auld, R.
Beelen, A.
Blain, A.
Blundell, R.
Bock, J.
Bradford, C. M.
Bridge, C.
Brisbin, D.
Burgarella, D.
Chanial, P.
Chapin, E.
Christopher, N.
Clements, D. L.
Cox, P.
Djorgovski, S. G.
Dowell, C. D.
Eales, S.
Earle, L.
Ellsworth-Bowers, T. P.
Farrah, D.
Franceschini, A.
Fu, H.
Glenn, J.
Solares, E. A. Gonzalez
Griffin, M.
Gurwell, M. A.
Halpern, M.
Ibar, E.
Ivison, R. J.
Jarvis, M.
Kamenetzky, J.
Kim, S.
Krips, M.
Levenson, L.
Lupu, R.
Mahabal, A.
Maloney, P. D.
Maraston, C.
Marchetti, L.
Marsden, G.
Matsuhara, H.
Mortier, A. M. J.
Murphy, E.
Naylor, B. J.
Neri, R.
Nguyen, H. T.
Oliver, S. J.
Omont, A.
Page, M. J.
Papageorgiou, A.
Pearson, C. P.
Perez-Fournon, I.
Pohlen, M.
Rangwala, N.
Rawlings, J. I.
Raymond, G.
Riechers, D.
Rodighiero, G.
Roseboom, I. G.
Rowan-Robinson, M.
Schulz, B.
Scott, Douglas
Scott, K. S.
Serra, P.
Seymour, N.
Shupe, D. L.
Smith, A. J.
Symeonidis, M.
Tugwell, K. E.
Vaccari, M.
Valiante, E.
Valtchanov, I.
Verma, A.
Vieira, J. D.
Vigroux, L.
Wang, L.
Wardlow, J.
Wiebe, D.
Wright, G.
Xu, C. K.
Zeimann, G.
Zemcov, M.
Zmuidzinas, J.
TI MODELING OF THE HERMES SUBMILLIMETER SOURCE LENSED BY A DARK MATTER
DOMINATED FOREGROUND GROUP OF GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: elliptical and lenticular, cD; galaxies: groups: general;
galaxies: halos; gravitational lensing: strong; submillimeter: galaxies
ID HIGH-DENSITY ENVIRONMENTS; ELLIPTIC GALAXIES; HIGH-REDSHIFT; ACS SURVEY;
STAR-FORMATION; NUMBER COUNTS; MASS PROFILE; HALOS; FIELD; EVOLUTION
AB We present the results of a gravitational lensing analysis of the bright z(s) = 2.957 submillimeter galaxy (SMG) HERMES found in the Herschel/SPIRE science demonstration phase data from the Herschel Multi-tiered Extragalactic Survey (HerMES) project. The high-resolution imaging available in optical and near-IR channels, along with CO emission obtained with the Plateau de Bure Interferometer, allows us to precisely estimate the intrinsic source extension and hence estimate the total lensing magnification to be mu = 10.9 +/- 0.7. We measure the half-light radius R-eff of the source in the rest-frame near-UV and V bands that characterize the unobscured light coming from stars and find R-eff,R-* = [2.0 +/- 0.1] kpc, in good agreement with recent studies on the SMG population. This lens model is also used to estimate the size of the gas distribution (R-eff,R-gas = [1.1 +/- 0.5] kpc) by mapping back in the source plane the CO (J = 5 -> 4) transition line emission. The lens modeling yields a relatively large Einstein radius R-Ein = 4 ''.10 +/- 0 ''.02, corresponding to a deflector velocity dispersion of [483 +/- 16] km s(-1). This shows that HERMES is lensed by a galaxy group-size dark matter halo at redshift z(l) similar to 0.6. The projected dark matter contribution largely dominates the mass budget within the Einstein radius with f(dm)(= 100 GeV) range at a flux level detectable by the current generation of ground-based Cherenkov telescopes. This enables us to place constraints on models of extragalactic background light within LAT energies and features the source as a promising candidate for VHE studies of the universe at an unprecedented redshift of z = 0.896.
C1 [McConville, W.; Donato, D.; McEnery, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McConville, W.; Donato, D.; McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McConville, W.; Donato, D.; McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Ostorero, L.] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy.
[Ostorero, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Ostorero, L.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Ostorero, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Moderski, R.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Stawarz, L.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Kanagawa 2525210, Japan.
[Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[Cheung, C. C.] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA.
[Ajello, M.; Monzani, M. E.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Ajello, M.; Monzani, M. E.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Bouvier, A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Bouvier, A.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Bregeon, J.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Donato, D.] CRESST, Greenbelt, MD 20771 USA.
[Finke, J.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Orienti, M.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Orienti, M.; Rossetti, A.] Ist Radioastron INAF, I-40129 Bologna, Italy.
[Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
RP McConville, W (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.
EM wmcconvi@umd.edu; stawarz@astro.isas.jaxa.jp;
Teddy.Cheung.ctr@nrl.navy.mil
RI McEnery, Julie/D-6612-2012;
OI Ostorero, Luisa/0000-0003-3983-5980; orienti, monica/0000-0003-4470-7094
FU INFN [PD51]; ASI [I/016/07/0]; MNiSW [N-N203-301635]
FX L.O. acknowledges support by a 2009 National Fellowship "L'OREAL Italia
Per le Donne e la Scienza" of the L'OREAL-UNESCO program "ForWomen in
Science," and partial support from the INFN grant PD51 and the ASI
Contract No. I/016/07/0 COFIS. L. S. is grateful for the support from
Polish MNiSW through the grant N-N203-380336. R. M. was supported by the
MNiSW grant no. N-N203-301635
NR 114
TC 21
Z9 21
U1 0
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2011
VL 738
IS 2
AR 148
DI 10.1088/0004-637X/738/2/148
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DE
UT WOS:000294954200030
ER
PT J
AU Racusin, JL
Oates, SR
Schady, P
Burrows, DN
de Pasquale, M
Donato, D
Gehrels, N
Koch, S
McEnery, J
Piran, T
Roming, P
Sakamoto, T
Swenson, C
Troja, E
Vasileiou, V
Virgili, F
Wanderman, D
Zhang, B
AF Racusin, J. L.
Oates, S. R.
Schady, P.
Burrows, D. N.
de Pasquale, M.
Donato, D.
Gehrels, N.
Koch, S.
McEnery, J.
Piran, T.
Roming, P.
Sakamoto, T.
Swenson, C.
Troja, E.
Vasileiou, V.
Virgili, F.
Wanderman, D.
Zhang, B.
TI FERMI AND SWIFT GAMMA-RAY BURST AFTERGLOW POPULATION STUDIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general; gamma rays: general; X-rays: bursts
ID LARGE-AREA TELESCOPE; HIGH-ENERGY EMISSION; INITIAL LORENTZ FACTOR;
LIGHT CURVES; ALERT TELESCOPE; EXTERNAL SHOCK; GRB 080916C; SPECTRAL
COMPONENTS; OPTICAL AFTERGLOWS; HOST GALAXIES
AB The new and extreme population of gamma-ray bursts (GRBs) detected by the Fermi Large Area Telescope (LAT) shows several new features in high-energy gamma rays that are providing interesting and unexpected clues into GRB prompt and afterglow emission mechanisms. Over the last six years, it has been Swift that has provided the robust data set of UV/optical and X-ray afterglow observations that opened many windows into components of GRB emission structure. The relationship between the LAT-detected GRBs and the well-studied, fainter, and less energetic GRBs detected by the Swift Burst Alert Telescope is only beginning to be explored by multi-wavelength studies. We explore the large sample of GRBs detected by BAT only, BAT and the Fermi Gamma-ray Burst Monitor (GBM), and GBM and LAT, focusing on these samples separately in order to search for statistically significant differences between the populations, using only those GRBs with measured redshifts in order to physically characterize these objects. We disentangle which differences are instrumental selection effects versus intrinsic properties in order to better understand the nature of the special characteristics of the LAT bursts.
C1 [Racusin, J. L.; Donato, D.; Gehrels, N.; McEnery, J.; Sakamoto, T.; Troja, E.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Oates, S. R.; de Pasquale, M.] Univ Coll London, Mullard Space Sci Lab, Surrey, England.
[Schady, P.] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany.
[Burrows, D. N.; Koch, S.; Roming, P.; Swenson, C.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Donato, D.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Donato, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Donato, D.] Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
[Piran, T.; Wanderman, D.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
[Roming, P.] SW Res Inst, Dept Space Sci, San Antonio, TX 78238 USA.
[Vasileiou, V.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21228 USA.
[Vasileiou, V.] Univ Montpellier 2, Lab Phys Theor & Astroparticules, CNRS, IN2P3, Montpellier, France.
[Virgili, F.; Zhang, B.] Univ Las Vegas, Dept Phys, Las Vegas, NV USA.
RP Racusin, JL (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.
RI Racusin, Judith/D-2935-2012; Gehrels, Neil/D-2971-2012; McEnery,
Julie/D-6612-2012
NR 76
TC 44
Z9 44
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2011
VL 738
IS 2
AR 138
DI 10.1088/0004-637X/738/2/138
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DE
UT WOS:000294954200020
ER
PT J
AU Saur, J
Feldman, PD
Roth, L
Nimmo, F
Strobel, DF
Retherford, KD
McGrath, MA
Schilling, N
Gerard, JC
Grodent, D
AF Saur, Joachim
Feldman, Paul D.
Roth, Lorenz
Nimmo, Francis
Strobel, Darrell F.
Retherford, Kurt D.
McGrath, Melissa A.
Schilling, Nico
Gerard, Jean-Claude
Grodent, Denis
TI HUBBLE SPACE TELESCOPE/ADVANCED CAMERA FOR SURVEYS OBSERVATIONS OF
EUROPA'S ATMOSPHERIC ULTRAVIOLET EMISSION AT EASTERN ELONGATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: observational; planets and satellites: atmospheres; planets and
satellites: aurorae; planets and satellites: individual (Jupiter and
Europa); techniques: imaging spectroscopy; ultraviolet: planetary
systems
ID JOVIAN MAGNETOSPHERE; SUBSURFACE OCEAN; GALILEAN SATELLITES; OXYGEN
ATMOSPHERE; IOS INTERACTION; ICE SHELL; ENCELADUS; MAGNETOMETER;
CONSTRAINTS; CALLISTO
AB We report results of a Hubble Space Telescope (HST) campaign with the Advanced Camera for Surveys to observe Europa at eastern elongation, i.e., Europa's leading side, on 2008 June 29. With five consecutive HST orbits, we constrain Europa's atmospheric OI 1304 angstrom and OI 1356 angstrom emissions using the prism PR130L. The total emissions of both oxygen multiplets range between 132 +/- 14 and 226 +/- 14 Rayleigh. An additional systematic error with values on the same order as the statistical errors may be due to uncertainties in modeling the reflected light from Europa's surface. The total emission also shows a clear dependence of Europa's position with respect to Jupiter's magnetospheric plasma sheet. We derive a lower limit for the O-2 column density of 6 x 10(18) m(-2). Previous observations of Europa's atmosphere with the Space Telescope Imaging Spectrograph in 1999 of Europa's trailing side show an enigmatic surplus of radiation on the anti-Jovian side within the disk of Europa. With emission from a radially symmetric atmosphere as a reference, we searched for an anti-Jovian versus sub-Jovian asymmetry with respect to the central meridian on the leading side and found none. Likewise, we searched for departures from a radially symmetric atmospheric emission and found an emission surplus centered around 90 degrees west longitude, for which plausible mechanisms exist. Previous work about the possibility of plumes on Europa due to tidally driven shear heating found longitudes with strongest local strain rates which might be consistent with the longitudes of maximum UV emissions. Alternatively, asymmetries in Europa's UV emission can also be caused by inhomogeneous surface properties, an optically thick atmospheric contribution of atomic oxygen, and/or by Europa's complex plasma interaction with Jupiter's magnetosphere.
C1 [Saur, Joachim; Roth, Lorenz; Schilling, Nico] Univ Cologne, Inst Geophys & Meteorol, D-5000 Cologne, Germany.
[Feldman, Paul D.; Strobel, Darrell F.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Nimmo, Francis] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
[Strobel, Darrell F.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Retherford, Kurt D.] SW Res Inst, San Antonio, TX USA.
[McGrath, Melissa A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Gerard, Jean-Claude; Grodent, Denis] Univ Liege, Lab Planetary & Atmospher Phys, Liege, Belgium.
RP Saur, J (reprint author), Univ Cologne, Inst Geophys & Meteorol, D-5000 Cologne, Germany.
EM saur@geo.uni-koeln.de
OI Retherford, Kurt/0000-0001-9470-150X; GERARD,
Jean-Claude/0000-0002-8565-8746
FU NASA [NAS 5-26555, HST-GO-11186.01-A]; Verbundforschung Astronomie und
Astrophysik durch das Bundesministerium fuer Wirtschaft und Technologie;
Belgian Fund for Scientific Research (FNRS); PRODEX; European Space
Agency
FX This work is based on observations with the NASA/ESA Hubble Space
Telescope obtained at the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy
(AURA), Inc., under NASA contract NAS 5-26555. We thank A. Roman for
scheduling the observations. J.S. appreciates the hospitality of the
Johns Hopkins University during his sabbatical stay in spring/summer
2011. L. R. and J.S. acknowledge support by the Verbundforschung
Astronomie und Astrophysik durch das Bundesministerium fuer Wirtschaft
und Technologie. P. D. F., D. F. S., and K. D. R. were supported by NASA
grant HST-GO-11186.01-A. J.C.G. and D. G. are supported by the Belgian
Fund for Scientific Research (FNRS) and by a PRODEX contract with the
European Space Agency, managed by the Belgian Federal Space Policy
Office.
NR 61
TC 14
Z9 14
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2011
VL 738
IS 2
AR 153
DI 10.1088/0004-637X/738/2/153
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DE
UT WOS:000294954200035
ER
PT J
AU Seifina, E
Titarchuk, L
AF Seifina, Elena
Titarchuk, Lev
TI ON THE CONSTANCY OF THE PHOTON INDEX OF X-RAY SPECTRA OF 4U 1728-34
THROUGH ALL SPECTRAL STATES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; radiation mechanisms:
non-thermal; stars: individual (4U 1728-34); stars: neutron
ID QUASI-PERIODIC OSCILLATIONS; BLACK-HOLE BINARIES; ENERGY CONCENTRATOR
SPECTROMETER; MONTE-CARLO SIMULATIONS; ACCRETING NEUTRON-STARS;
OBSERVATIONAL EVIDENCE; COMPTONIZATION MODELS; FREQUENCY CORRELATION;
INTRINSIC SIGNATURE; ASTRONOMY SATELLITE
AB We present an analysis of the spectral properties observed in X-rays from neutron star X-ray binary 4U 1728-34 during transitions between the low-and high-luminosity states when the electron temperature kT(e) of the Compton cloud monotonically decreases from 15 to 2.5 keV. We analyze the transition episodes from this source observed with BeppoSAX and RXTE satellites. We find that the X-ray broadband energy spectra of 4U 1728-34 during all spectral states can be modeled by a combination of a thermal (blackbody-like) component, a Comptonized component (which we herein denote as COMPTB), and a Gaussian component. Spectral analysis using this model provides evidence that the photon power-law index Gamma is almost constant (Gamma = 1.99 +/- 0.02) when kT(e) changes from 15 to 2.5 keV during these spectral transitions. We explain this quasi-stability of the index G by the model in which the spectrum is dominated by the strong thermal Comptonized component formed in the transition layer (TL) between the accretion disk and neutron star surface. The index quasi-stability takes place when the energy release in the TL is much higher than the flux coming to the TL from the accretion disk. Moreover, this index stability effect now established for 4U 1728-34 during spectral evolution of the source was previously suggested for a number of other neutron binaries. This intrinsic property of the neutron star is fundamentally different from that in black hole binary sources for which the index monotonically increases during spectral transition from the low state to the high state and saturates at high values of the mass accretion rate.
C1 [Seifina, Elena] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Titarchuk, Lev] Univ Ferrara, Dipartimento Fis, I-44100 Ferrara, Italy.
[Titarchuk, Lev] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA.
[Titarchuk, Lev] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
RP Seifina, E (reprint author), Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Prospect 13, Moscow 119992, Russia.
EM seif@sai.msu.ru; titarchuk@fe.infn.it
FU ADP NASA [NNX09AF02G]
FX We thank Chris Shrader and Cristiano Guidorzi for careful reading and
editing of this paper. We are very grateful to the referee for his/her
valuable comments and corrections to the content of this paper. L.T.
acknowledges the support of this paper by the ADP NASA grant,
NNX09AF02G.
NR 56
TC 10
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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 SEP 10
PY 2011
VL 738
IS 2
AR 128
DI 10.1088/0004-637X/738/2/128
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DE
UT WOS:000294954200010
ER
PT J
AU Williamson, R
Benson, BA
High, FW
Vanderlinde, K
Ade, PAR
Aird, KA
Andersson, K
Armstrong, R
Ashby, MLN
Bautz, M
Bazin, G
Bertin, E
Bleem, LE
Bonamente, M
Brodwin, M
Carlstrom, JE
Chang, CL
Chapman, SC
Clocchiatti, A
Crawford, TM
Crites, AT
de Haan, T
Desai, S
Dobbs, MA
Dudley, JP
Fazio, GG
Foley, RJ
Forman, WR
Garmire, G
George, EM
Gladders, MD
Gonzalez, AH
Halverson, NW
Holder, GP
Holzapfel, WL
Hoover, S
Hrubes, JD
Jones, C
Joy, M
Keisler, R
Knox, L
Lee, AT
Leitch, EM
Lueker, M
Luong-Van, D
Marrone, DP
McMahon, JJ
Mehl, J
Meyer, SS
Mohr, JJ
Montroy, TE
Murray, SS
Padin, S
Plagge, T
Pryke, C
Reichardt, CL
Rest, A
Ruel, J
Ruhl, JE
Saliwanchik, BR
Saro, A
Schaffer, KK
Shaw, L
Shirokoff, E
Song, J
Spieler, HG
Stalder, B
Stanford, SA
Staniszewski, Z
Stark, AA
Story, K
Stubbs, CW
Vieira, JD
Vikhlinin, A
Zenteno, A
AF Williamson, R.
Benson, B. A.
High, F. W.
Vanderlinde, K.
Ade, P. A. R.
Aird, K. A.
Andersson, K.
Armstrong, R.
Ashby, M. L. N.
Bautz, M.
Bazin, G.
Bertin, E.
Bleem, L. E.
Bonamente, M.
Brodwin, M.
Carlstrom, J. E.
Chang, C. L.
Chapman, S. C.
Clocchiatti, A.
Crawford, T. M.
Crites, A. T.
de Haan, T.
Desai, S.
Dobbs, M. A.
Dudley, J. P.
Fazio, G. G.
Foley, R. J.
Forman, W. R.
Garmire, G.
George, E. M.
Gladders, M. D.
Gonzalez, A. H.
Halverson, N. W.
Holder, G. P.
Holzapfel, W. L.
Hoover, S.
Hrubes, J. D.
Jones, C.
Joy, M.
Keisler, R.
Knox, L.
Lee, A. T.
Leitch, E. M.
Lueker, M.
Luong-Van, D.
Marrone, D. P.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Mohr, J. J.
Montroy, T. E.
Murray, S. S.
Padin, S.
Plagge, T.
Pryke, C.
Reichardt, C. L.
Rest, A.
Ruel, J.
Ruhl, J. E.
Saliwanchik, B. R.
Saro, A.
Schaffer, K. K.
Shaw, L.
Shirokoff, E.
Song, J.
Spieler, H. G.
Stalder, B.
Stanford, S. A.
Staniszewski, Z.
Stark, A. A.
Story, K.
Stubbs, C. W.
Vieira, J. D.
Vikhlinin, A.
Zenteno, A.
TI A SUNYAEV-ZEL'DOVICH-SELECTED SAMPLE OF THE MOST MASSIVE GALAXY CLUSTERS
IN THE 2500 deg(2) SOUTH POLE TELESCOPE SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; galaxies:
clusters: general
ID ATACAMA COSMOLOGY TELESCOPE; GREATER-THAN 1; ALL-SKY SURVEY; PHOTOMETRIC
REDSHIFTS; SCALING RELATIONS; STELLAR LOCUS; POWER SPECTRA; DARK-MATTER;
CATALOG; CONSTRAINTS
AB The South Pole Telescope (SPT) is currently surveying 2500 deg(2) of the southern sky to detect massive galaxy clusters out to the epoch of their formation using the Sunyaev-Zel'dovich (SZ) effect. This paper presents a catalog of the 26 most significant SZ cluster detections in the full survey region. The catalog includes 14 clusters which have been previously identified and 12 that are new discoveries. These clusters were identified in fields observed to two differing noise depths: 1500 deg2 at the final SPT survey depth of 18 mu K arcmin at 150 GHz and 1000 deg2 at a depth of 54 mu K arcmin. Clusters were selected on the basis of their SZ signal-to-noise ratio (S/N) in SPT maps, a quantity which has been demonstrated to correlate tightly with cluster mass. The S/N thresholds were chosen to achieve a comparablemass selection across survey fields of both depths. Cluster redshifts were obtained with optical and infrared imaging and spectroscopy from a variety of ground-and space-based facilities. The redshifts range from 0.098 <= z <= 1.132 with a median of z(med) = 0.40. The measured SZ S/N and redshifts lead to unbiased mass estimates ranging from 9.8 x 10(14) M-circle dot h(70)(-1) <= M-200(rho(mean)) <= 3.1 x 10(15) M-circle dot h(-1). Based on the SZ mass estimates, we find that none of the clusters are individually in significant tension with the Lambda CDM cosmological model. We also test for evidence of non-Gaussianity based on the cluster sample and find the data show no preference for non-Gaussian perturbations.
C1 [Williamson, R.; Benson, B. A.; High, F. W.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Hoover, S.; Keisler, R.; Leitch, E. M.; Marrone, D. P.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Schaffer, K. K.; Story, K.; Vieira, J. D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Williamson, R.; High, F. W.; Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; McMahon, J. J.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Vanderlinde, K.; de Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Shaw, L.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Ade, P. A. R.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales.
[Andersson, K.; Bazin, G.; Mohr, J. J.; Saro, A.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Andersson, K.; Bautz, M.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Armstrong, R.; Desai, S.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA.
[Ashby, M. L. N.; Brodwin, M.; Fazio, G. G.; Foley, R. J.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bazin, G.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Bertin, E.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
[Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Bonamente, M.; Joy, M.] NASA, Dept Space Sci, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Clocchiatti, A.] Dept Astron & Astrophys, Santiago 22, Chile.
[Desai, S.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Garmire, G.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA.
[McMahon, J. J.; Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Staniszewski, Z.] Case Western Reserve Univ, CERCA, Cleveland, OH 44106 USA.
[Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA.
[Padin, S.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
[Rest, A.; Ruel, J.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Schaffer, K. K.] Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
RP Williamson, R (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
EM rw247@kicp.uchicago.edu
RI Stubbs, Christopher/C-2829-2012; Williamson, Ross/H-1734-2015;
Holzapfel, William/I-4836-2015;
OI Stubbs, Christopher/0000-0003-0347-1724; Williamson,
Ross/0000-0002-6945-2975; Marrone, Daniel/0000-0002-2367-1080; Aird,
Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169;
Forman, William/0000-0002-9478-1682; Stark, Antony/0000-0002-2718-9996
FU National Science Foundation (NSF) [ANT-0638937, AST-1009012,
AST-1009649, MRI-0723073, NAS 8-03060]; NSF Physics Frontier Center
[PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation;
JPL/Caltech; NASA [12800071, 12800088, NAS8-03060]; NASA Office of Space
Science; National Sciences and Engineering Research Council of Canada,
Canad; Canadian Institute for Advanced Research; Excellence Cluster
Universe; DFG [TR33]; Clay Fellowship; KICP Fellowship; Pennsylvania
State University [2834-MIT-SAO-4018]; Alfred P. Sloan Research
Fellowship; Smithsonian Institution; Brinson Foundation
FX The South Pole Telescope program is supported by the National Science
Foundation through grant ANT-0638937. Partial support is also provided
by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli
Institute of Cosmological Physics at the University of Chicago, the
Kavli Foundation, and the Gordon and Betty Moore Foundation. This work
is based in part on observations obtained with the Spitzer Space
Telescope (PID 60099), which is operated by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA. Support for this work was provided by NASA through an award issued
by JPL/Caltech. Additional data were obtained with the 6.5 m Magellan
Telescopes located at the Las Campanas Observatory, Chile. Support for
X-ray analysis was provided by NASA through Chandra Award Numbers
12800071 and 12800088 issued by the Chandra X-ray Observatory Center,
which is operated by the Smithsonian Astrophysical Observatory for and
on behalf of NASA under contract NAS8-03060. Optical imaging data from
the Blanco 4 m at Cerro Tololo Inter-American Observatories (programs
2005B-0043, 2009B-0400, 2010A-0441, 2010B-0598) and spectroscopic
observations from VLT programs 086.A-0741 and 286.A-5021 and Gemini
program GS-2009B-Q-16 were included in this work. We acknowledge the use
of the Legacy Archive for Microwave Background Data Analysis (LAMBDA).
Support for LAMBDA is provided by the NASA Office of Space Science.
Galaxy cluster research at Harvard is supported by NSF grant
AST-1009012. Galaxy cluster research at SAO is supported in part by NSF
grants AST-1009649 and MRI-0723073. The McGill group acknowledges
funding from the National Sciences and Engineering Research Council of
Canada, Canada Research Chairs program, and the Canadian Institute for
Advanced Research. X-ray research at the CfA is supported through NASA
Contract NAS 8-03060. The Munich group acknowledges support from the
Excellence Cluster Universe and the DFG research program TR33. R.J.F. is
supported by a Clay Fellowship. B.A.B. is supported by a KICP
Fellowship, support for M. Brodwin was provided by the W. M. Keck
Foundation, M. Bautz acknowledges support from contract
2834-MIT-SAO-4018 from the Pennsylvania State University to the
Massachusetts Institute of Technology. M.D. acknowledges support from an
Alfred P. Sloan Research Fellowship, W.F. and C.J. acknowledge support
from the Smithsonian Institution, and B. S. acknowledges support from
the Brinson Foundation.
NR 68
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2011
VL 738
IS 2
AR 139
DI 10.1088/0004-637X/738/2/139
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DE
UT WOS:000294954200021
ER
PT J
AU Tsurutani, BT
Falkowski, BJ
Verkhoglyadova, OP
Pickett, JS
Santolik, O
Lakhina, GS
AF Tsurutani, Bruce T.
Falkowski, Barbara J.
Verkhoglyadova, Olga P.
Pickett, Jolene S.
Santolik, Ondrej
Lakhina, Gurbax S.
TI Quasi-coherent chorus properties: 1. Implications for wave-particle
interactions
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID WHISTLER-MODE CHORUS; RELATIVISTIC ELECTRON MICROBURSTS; PITCH ANGLE
SCATTERING; RADIATION BELT; AURORAL-ZONE; RESONANT DIFFUSION; MAGNETIC
STORMS; GENDRIN MODE; VLF WAVES; MAGNETOSPHERE
AB A study of dayside ELF/VLF electromagnetic (EM) waves from L* = 2 to 9 and magnetic local time (MLT) from 09 to 15 was conducted using plasma wave data from the Polar spacecraft. EM waves were detected from L* = 4 to 9 from 09 to 12 MLT with a decrease in the afternoon sector (12 to 15 MLT). Some of the chorus was clearly related to generation by substorm injected similar to 5 to 100 keV electrons drifting from the midnight sector to the local noon sector. However, dayside chorus also showed two solar wind ram pressure dependences: increased (above average) pressures and unusually low pressures. Possible chorus generation mechanisms are discussed. Chorus detected by Polar away from the magnetic equator generation region (similar to 25 degrees to 55 degrees magnetic latitude) was substantially different than chorus detected in previous studies within the similar to 0 degrees to 10 degrees generation region. (1) Two separate bands of chorus were often detected simultaneously: a higher-frequency downgoing (toward the Earth) band of waves and a lower-frequency upcoming band. (2) The downgoing waves are similar to 2 orders of magnitude more intense (similar to 10(-2) nT(2)) than simultaneously detected lower-frequency upcoming waves (similar to 10(-4) nT(2)). (3) Chorus, when viewed as a Fourier spectrum, appears as a band of semicoherent hiss. (4) A scenario and schematic is presented to explain these observations: chorus is presumed to be generated at the equator at large L*, propagate downward toward Earth and inward across L* shells, and then refract back up to the spacecraft location. (5) The waves detected at Polar latitudes did not possess the temporal structure or the coherency of the similar to 10 to 100 ms duration equatorial chorus subelements, although full single cycles with right-hand, circularly polarized structures were identified. This quasi-coherent EM turbulence may be formed by wave dispersive effects. The longer the wave path length, the greater is the reduction in coherency. (6) This feature of chorus has significant consequences for off-equatorial wave-particle interactions. For example, the microburst mechanism of Lakhina et al. (2010) that can account for rapid pitch angle diffusion of similar to 5 to 100 keV electrons in the chorus generation region will not work for off-equatorial scattering of relativistic electrons because of the lack of chorus coherence there. (7) Some comments about semicoherent chorus (hiss) in the outer magnetosphere are made as challenges to theorists in the field.
C1 [Tsurutani, Bruce T.; Falkowski, Barbara J.; Verkhoglyadova, Olga P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Falkowski, Barbara J.] Glendale Community City Coll, Dept Phys, Glendale, CA USA.
[Falkowski, Barbara J.] Glendale Community City Coll, Dept Astron, Glendale, CA USA.
[Verkhoglyadova, Olga P.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Pickett, Jolene S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Santolik, Ondrej] Inst Atmospher Phys, Prague 14131, Czech Republic.
[Santolik, Ondrej] Charles Univ Prague, Fac Math & Phys, Prague, Czech Republic.
[Lakhina, Gurbax S.] Indian Inst Geomagnetism, Navi Mumbai 410218, India.
RP Tsurutani, BT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM bruce.tsurutani@jpl.nasa.gov
RI Lakhina, Gurbax /C-9295-2012; Santolik, Ondrej/F-7766-2014;
OI Lakhina, Gurbax /0000-0002-8956-486X; Verkhoglyadova,
Olga/0000-0002-9295-9539
FU NASA; Indian National Science Academy, New Delhi; JPL [1246597]; [GACR
205/10/2279]; [ME10001]
FX Portions of this research were carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA. G. S. L. thanks the Indian National Science Academy, New Delhi,
for the support under the Senior Scientist Scheme. J.S.P. and O.S.
acknowledge JPL support under subcontract 1246597. O.S. acknowledges
additional support from grants GACR 205/10/2279 and ME10001. B. T. T.
acknowledges the Technical University of Braunschweig (TUB) for their
hospitality during his sabbatical in the summer of 2010. Portions of the
revisions to this paper were written during his stay at TUB. We thank E.
Echer of INPE for help with the geomagnetic indices. We thank D. Boscher
for maintaining the ONERA-DESP library that was used to calculate the L*
values.
NR 80
TC 27
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U1 1
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP 10
PY 2011
VL 116
AR A09210
DI 10.1029/2010JA016237
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 819BC
UT WOS:000294799400001
ER
PT J
AU Verner, GA
Chaplin, WJ
Basu, S
Brown, TM
Hekker, S
Huber, D
Karoff, C
Mathur, S
Metcalfe, TS
Mosser, B
Quirion, PO
Appourchaux, T
Bedding, TR
Bruntt, H
Campante, TL
Elsworth, Y
Garcia, RA
Handberg, R
Regulo, C
Roxburgh, IW
Stello, D
Christensen-Dalsgaard, J
Gilliland, RL
Kawaler, SD
Kjeldsen, H
Allen, C
Clarke, BD
Girouard, FR
AF Verner, G. A.
Chaplin, W. J.
Basu, S.
Brown, T. M.
Hekker, S.
Huber, D.
Karoff, C.
Mathur, S.
Metcalfe, T. S.
Mosser, B.
Quirion, P. -O.
Appourchaux, T.
Bedding, T. R.
Bruntt, H.
Campante, T. L.
Elsworth, Y.
Garcia, R. A.
Handberg, R.
Regulo, C.
Roxburgh, I. W.
Stello, D.
Christensen-Dalsgaard, J.
Gilliland, R. L.
Kawaler, S. D.
Kjeldsen, H.
Allen, C.
Clarke, B. D.
Girouard, F. R.
TI VERIFICATION OF THE KEPLER INPUT CATALOG FROM ASTEROSEISMOLOGY OF
SOLAR-TYPE STARS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE stars: fundamental parameters; stars: interiors; stars: oscillations
ID OSCILLATIONS; MISSION; PARAMETERS; ISOCHRONES; EVOLUTION; MODELS; RADIUS
AB We calculate precise stellar radii and surface gravities from the asteroseismic analysis of over 500 solar-type pulsating stars observed by the Kepler space telescope. These physical stellar properties are compared with those given in the Kepler Input Catalog (KIC), determined from ground-based multi-color photometry. For the stars in our sample, we find general agreement but we detect an average overestimation bias of 0.23 dex in the KIC determination of log(g) for stars with log(g)(KIC) > 4.0 dex, and a resultant underestimation bias of up to 50% in the KIC radii estimates for stars with R-KIC < 2 R-circle dot. Part of the difference may arise from selection bias in the asteroseismic sample; nevertheless, this result implies there may be fewer stars characterized in the KIC with R similar to 1 R-circle dot than is suggested by the physical properties in the KIC. Furthermore, if the radius estimates are taken from the KIC for these affected stars and then used to calculate the size of transiting planets, a similar underestimation bias may be applied to the planetary radii.
C1 [Verner, G. A.; Chaplin, W. J.; Hekker, S.; Elsworth, Y.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Verner, G. A.; Roxburgh, I. W.] Univ London, Astron Unit, London E1 4NS, England.
[Basu, S.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Brown, T. M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Huber, D.; Bedding, T. R.; Stello, D.] Univ Sydney, Sch Phys, SIfA, Sydney, NSW 2006, Australia.
[Karoff, C.; Bruntt, H.; Handberg, R.; Christensen-Dalsgaard, J.; Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Mathur, S.; Metcalfe, T. S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Mathur, S.; Metcalfe, T. S.] Natl Ctr Atmospher Res, Div Comp Sci, Boulder, CO 80307 USA.
[Mosser, B.] Univ Paris 07, Observ Paris, Univ Paris 06, LESIA,CNRS, F-92195 Meudon, France.
[Quirion, P. -O.] Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada.
[Appourchaux, T.] Univ Paris 11, Inst Astrophys Spatiale, CNRS, UMR8617, F-91405 Orsay, France.
[Campante, T. L.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Garcia, R. A.] Univ Paris Diderot, IRFU, CNRS, Lab AIM,CEA,DSM,SAp, F-91191 Gif Sur Yvette, France.
[Regulo, C.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Regulo, C.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Allen, C.; Girouard, F. R.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
[Clarke, B. D.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
RP Verner, GA (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
OI Bedding, Timothy/0000-0001-5943-1460; Metcalfe,
Travis/0000-0003-4034-0416; Karoff, Christoffer/0000-0003-2009-7965;
Bedding, Tim/0000-0001-5222-4661; Garcia, Rafael/0000-0002-8854-3776;
Handberg, Rasmus/0000-0001-8725-4502; Kawaler,
Steven/0000-0002-6536-6367
FU UK Science and Technology Facilities Council; Netherlands Organisation
for Scientific Research; NASA's Science Mission Directorate; KASC
Working Group 1
FX G.A.V., W.J.C., Y.E., and I.W.R. acknowledge the support of the UK
Science and Technology Facilities Council. S.H. acknowledges support
from the Netherlands Organisation for Scientific Research. Funding for
the Kepler Mission is provided by NASA's Science Mission Directorate.
The authors thank the entire Kepler team, without whom these results
would not be possible. We also thank all funding councils and agencies
that have supported the activities of KASC Working Group 1.
NR 34
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U2 7
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 SEP 10
PY 2011
VL 738
IS 2
AR L28
DI 10.1088/2041-8205/738/2/L28
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818NY
UT WOS:000294760700012
ER
PT J
AU Yegorova, EA
Allen, DJ
Loughner, CP
Pickering, KE
Dickerson, RR
AF Yegorova, E. A.
Allen, D. J.
Loughner, C. P.
Pickering, K. E.
Dickerson, R. R.
TI Characterization of an eastern US severe air pollution episode using
WRF/Chem
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID FREE TROPOSPHERIC OZONE; PERFORMANCE EVALUATION; UNITED-STATES;
NEW-ENGLAND; PART II; QUALITY; CHEMISTRY; NITROGEN; MODEL; VARIABILITY
AB On 8-11 July 2007 the eastern United States experienced a severe heat wave and smog event with maximum temperatures approaching 38 degrees C and maximum 8 h average ozone mixing ratios of 125 ppbv. We examine this episode with observations and numerical simulations using the Weather Research and Forecasting model with online chemistry (WRF/Chem with RADM2). The general features of this severe smog event-a broad area of high pressure, weak winds and heavy pollution, terminated by the passage of a cold front-were well simulated by the model. WRF/Chem underpredicted O-3 maxima by 5-8 ppbv where air quality was poor, usually in the northeast, but overpredicted maxima by up to 16 ppbv where ozone amounts were low, usually in the southeast. Simulated O-3 vertical profiles over Beltsville, Maryland, showed good agreement with ozonesonde measurements, but the model boundary layer was too deep on 9 July, contributing to the low bias over this region. The representation of NOx chemistry in RADM2 may lead to an underestimation of NOx lifetime and is likely partially responsible for low O-3 biases in the most polluted area in the northeast. To simulate the maximum effect of nighttime multiphase NOy loss, we set the N2O5 heterogeneous hydrolysis reaction rate constant to zero. This increased the mean bias outside the area of highest ozone concentration but substantially improved O-3 and NOy over most of the domain, especially in smoggy areas such as the rural, Pinnacles site.
C1 [Yegorova, E. A.; Loughner, C. P.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Yegorova, E. A.; Loughner, C. P.; Pickering, K. E.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Allen, D. J.; Pickering, K. E.; Dickerson, R. R.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
RP Yegorova, EA (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
EM elena.a.yegorova@nasa.gov
RI Yegorova, Elena/H-3825-2011; Dickerson, Russell/F-2857-2010; Pickering,
Kenneth/E-6274-2012; Allen, Dale/F-7168-2010;
OI Dickerson, Russell/0000-0003-0206-3083; Allen, Dale/0000-0003-3305-9669;
Loughner, Christopher/0000-0002-3833-2014
FU Maryland Department of the Environment
FX The authors acknowledge G. Grell and S. Peckham for help with the
WRF/Chem model; L. Emmons for providing MOZART-4 model output; and M.
Woodman and D. Krask of the Maryland Department of the Environment's
Ambient Air Monitoring Program for support and for providing the
Beltsville ozonesonde data and Aldino, Maryland, data, respectively. We
thank the anonymous reviewers for their contribution to this work.
NR 37
TC 14
Z9 15
U1 0
U2 21
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 SEP 10
PY 2011
VL 116
AR D17306
DI 10.1029/2010JD015054
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 819BQ
UT WOS:000294800800001
ER
PT J
AU Ray, RD
Zaron, ED
AF Ray, R. D.
Zaron, E. D.
TI Non-stationary internal tides observed with satellite altimetry
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID BAROCLINIC TIDES; TIDAL CURRENTS; ATLANTIC-OCEAN; NORTH-ATLANTIC;
PACIFIC-OCEAN; HAWAII; PROPAGATION; GENERATION; MODEL
AB Temporal variability of the internal tide is inferred from a 17-year combined record of Topex/Poseidon and Jason satellite altimeters. A global sampling of along-track se-asurface height wavenumber spectra finds that nonstationary variance is generally 25% or less of the average variance at wavenumbers characteristic of mode-1 tidal internal waves. With some exceptions the non-stationary variance does not exceed 0.25 cm(2). The mode-2 signal, where detectable, contains a larger fraction of nonstationary variance, typically 50% or more. Temporal subsetting of the data reveals interannual variability barely significant compared with tidal estimation error from 3-year records. Comparison of summer vs. winter conditions shows only one region of noteworthy seasonal changes, the northern South China Sea. Implications for the anticipated SWOT altimeter mission are briefly discussed. Citation: Ray, R. D., and E. D. Zaron (2011), Non-stationary internal tides observed with satellite altimetry, Geophys. Res. Lett., 38, L17609, doi: 10.1029/2011GL048617.
C1 [Ray, R. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Zaron, E. D.] Portland State Univ, Dept Civil & Environm Engn, Portland, OR 97207 USA.
RP Ray, RD (reprint author), NASA, Goddard Space Flight Ctr, Code 698, Greenbelt, MD 20771 USA.
EM richard.ray@nasa.gov
RI Ray, Richard/D-1034-2012
FU National Aeronautics and Space Administration; National Science
Foundation [OCE-0623540]
FX This work was supported by the Ocean Surface Topography program of the
National Aeronautics and Space Administration. Additional financial
support from the National Science Foundation, award OCE-0623540 (Zaron),
is gratefully acknowledged.
NR 25
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U1 0
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 9
PY 2011
VL 38
AR L17609
DI 10.1029/2011GL048617
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 818WE
UT WOS:000294785800003
ER
PT J
AU Wilson, LB
Cattell, CA
Kellogg, PJ
Wygant, JR
Goetz, K
Breneman, A
Kersten, K
AF Wilson, L. B., III
Cattell, C. A.
Kellogg, P. J.
Wygant, J. R.
Goetz, K.
Breneman, A.
Kersten, K.
TI The properties of large amplitude whistler mode waves in the
magnetosphere: Propagation and relationship with geomagnetic activity
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID RADIATION BELT ELECTRONS; WIND SPACECRAFT; CHORUS; PLASMA; DIFFUSION;
FLUXES
AB We present results of a study of the characteristics of very large amplitude whistler mode waves inside the terrestrial magnetosphere at radial distances of less than 15 R-E using waveform capture data from the Wind spacecraft. We observed 247 whistler mode waves with at least one electric field component (105/247 had >= 80 mV/m peak-to-peak amplitudes) and 66 whistler mode waves with at least one search coil magnetic field component (38/66 had >= 0.8 nT peak-to-peak amplitudes). Wave vectors determined from events with three magnetic field components indicate that 30/46 propagate within 20 degrees of the ambient magnetic field, though some are more oblique ( up to similar to 50 degrees). No relationship was observed between wave normal angle and GSM latitude. 162/247 of the large amplitude whistler mode waves were observed during magnetically active periods (AE > 200 nT). 217 out of 247 total whistler mode waves examined were observed inside the radiation belts. We present a waveform capture with the largest whistler wave magnetic field amplitude (greater than or similar to 8 nT peak-to-peak) ever reported in the radiation belts. The estimated Poynting flux magnitude associated with this wave is greater than or similar to 300 mu W/m(2), roughly four orders of magnitude above estimates from previous satellite measurements. Such large Poynting flux values are consistent with rapid energization of electrons. Citation: Wilson, L. B., III, C. A. Cattell, P. J. Kellogg, J. R. Wygant, K. Goetz, A. Breneman, and K. Kersten (2011), The properties of large amplitude whistler mode waves in the magnetosphere: Propagation and relationship with geomagnetic activity, Geophys. Res. Lett., 38, L17107, doi: 10.1029/2011GL048671.
C1 [Wilson, L. B., III] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wilson, L. B., III; Cattell, C. A.; Kellogg, P. J.; Wygant, J. R.; Goetz, K.; Breneman, A.; Kersten, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
RP Wilson, LB (reprint author), NASA, Goddard Space Flight Ctr, Code 672,Bldg 21,Room 143A, Greenbelt, MD 20771 USA.
EM lynn.b.wilsoniii@gmail.com; cattell@fields.space.umn.edu;
pauljkellogg@gmail.com; jwygant@fields.space.umn.edu;
goetz@waves.space.umn.edu; awbrenem@gmail.com; kkersten@physics.umn.edu
RI Wilson III, Lynn/D-4425-2012;
OI Wilson III, Lynn/0000-0002-4313-1970; Cattell,
Cynthia/0000-0002-3805-320X
FU NESSF [NNX07AU72H, NNX07AI05G]; Dr. Leonard Burlaga/Arctowski Medal
Fellowship
FX We thank R. Lin (3DP), K. Ogilvie (SWE), R. Lepping (MFI), and E. Dors
(LANL data) for the use of data from their instruments. We would also
like to thank M. Pulupa, S. D. Bale, and P. Schroeder for technical help
with the 3DP software and analysis. We thank L. Wang for help in
calibration of the SST Foil data. The authors thank World Data Center
for Geomagnetism, Kyoto, for providing the AE index. This research was
supported by NESSF grant NNX07AU72H, grant NNX07AI05G, the Dr. Leonard
Burlaga/Arctowski Medal Fellowship, and a contract from APL for the
development of RBSP/EFW.
NR 31
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Z9 35
U1 0
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 SEP 9
PY 2011
VL 38
AR L17107
DI 10.1029/2011GL048671
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 818WE
UT WOS:000294785800004
ER
PT J
AU Strahan, SE
Douglass, AR
Stolarski, RS
Akiyoshi, H
Bekki, S
Braesicke, P
Butchart, N
Chipperfield, MP
Cugnet, D
Dhomse, S
Frith, SM
Gettelman, A
Hardiman, SC
Kinnison, DE
Lamarque, JF
Mancini, E
Marchand, M
Michou, M
Morgenstern, O
Nakamura, T
Olivie, D
Pawson, S
Pitari, G
Plummer, DA
Pyle, JA
Scinocca, JF
Shepherd, TG
Shibata, K
Smale, D
Teyssedre, H
Tian, W
Yamashita, Y
AF Strahan, S. E.
Douglass, A. R.
Stolarski, R. S.
Akiyoshi, H.
Bekki, S.
Braesicke, P.
Butchart, N.
Chipperfield, M. P.
Cugnet, D.
Dhomse, S.
Frith, S. M.
Gettelman, A.
Hardiman, S. C.
Kinnison, D. E.
Lamarque, J. -F.
Mancini, E.
Marchand, M.
Michou, M.
Morgenstern, O.
Nakamura, T.
Olivie, D.
Pawson, S.
Pitari, G.
Plummer, D. A.
Pyle, J. A.
Scinocca, J. F.
Shepherd, T. G.
Shibata, K.
Smale, D.
Teyssedre, H.
Tian, W.
Yamashita, Y.
TI Using transport diagnostics to understand chemistry climate model ozone
simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID STRATOSPHERIC OZONE; LAGRANGIAN TRANSPORT; MIDDLE ATMOSPHERE; TECHNICAL
NOTE; N2O; AIR; CONSTITUENTS; UNCERTAINTY; PREDICTIONS; SENSITIVITY
AB We use observations of N2O and mean age to identify realistic transport in models in order to explain their ozone predictions. The results are applied to 15 chemistry climate models (CCMs) participating in the 2010 World Meteorological Organization ozone assessment. Comparison of the observed and simulated N2O, mean age and their compact correlation identifies models with fast or slow circulations and reveals details of model ascent and tropical isolation. This process-oriented diagnostic is more useful than mean age alone because it identifies models with compensating transport deficiencies that produce fortuitous agreement with mean age. The diagnosed model transport behavior is related to a model's ability to produce realistic lower stratosphere (LS) O-3 profiles. Models with the greatest tropical transport problems compare poorly with O-3 observations. Models with the most realistic LS transport agree more closely with LS observations and each other. We incorporate the results of the chemistry evaluations in the Stratospheric Processes and their Role in Climate (SPARC) CCMVal Report to explain the range of CCM predictions for the return-to-1980 dates for global (60 degrees S-60 degrees N) and Antarctic column ozone. Antarctic O-3 return dates are generally correlated with vortex Cl-y levels, and vortex Cly is generally correlated with the model's circulation, although model Cl chemistry and conservation problems also have a significant effect on return date. In both regions, models with good LS transport and chemistry produce a smaller range of predictions for the return-to-1980 ozone values. This study suggests that the current range of predicted return dates is unnecessarily broad due to identifiable model deficiencies.
C1 [Strahan, S. E.] Univ Space Res Assoc, Columbia, MD USA.
[Strahan, S. E.; Douglass, A. R.; Stolarski, R. S.; Frith, S. M.; Pawson, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Akiyoshi, H.; Nakamura, T.; Yamashita, Y.] Natl Inst Environm Studies, Tsukuba, Ibaraki 3058506, Japan.
[Bekki, S.; Cugnet, D.; Marchand, M.] UPMC, LATMOS, IPSL, UVSQ,CNRS,INSU, F-75252 Paris 05, France.
[Braesicke, P.; Pyle, J. A.] Univ Cambridge, Dept Chem, NCAS Climate Chem, Ctr Atmospher Sci, Cambridge CB2 1EW, England.
[Butchart, N.; Hardiman, S. C.] Met Off Hadley Ctr, Exeter EX1 3PB, Devon, England.
[Chipperfield, M. P.; Dhomse, S.; Tian, W.] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England.
[Frith, S. M.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Gettelman, A.; Kinnison, D. E.; Lamarque, J. -F.] Natl Ctr Atmospher Res, Boulder, CO 80305 USA.
[Mancini, E.; Pitari, G.] Univ Aquila, Dipartimento Fis, I-67010 Laquila, Italy.
[Michou, M.; Teyssedre, H.] CNRS, GAME CNRM, F-31057 Toulouse, France.
[Morgenstern, O.; Smale, D.] Natl Inst Water & Atmospher Res, Lauder 9352, Central Otago, New Zealand.
[Olivie, D.] Univ Oslo, Dept Geosci, N-0315 Oslo, Norway.
[Plummer, D. A.; Scinocca, J. F.] Environm Canada, Canadian Ctr Climate Modeling & Anal, Victoria, BC V8W 3V6, Canada.
[Shepherd, T. G.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Shibata, K.] Japan Meteorol Agcy, Meteorol Res Inst, Tsukuba, Ibaraki 3050052, Japan.
RP Strahan, SE (reprint author), Univ Space Res Assoc, Columbia, MD USA.
EM susan.e.strahan@nasa.gov
RI Douglass, Anne/D-4655-2012; Strahan, Susan/H-1965-2012; Stolarski,
Richard/B-8499-2013; Chipperfield, Martyn/H-6359-2013; Lamarque,
Jean-Francois/L-2313-2014; bekki, slimane/J-7221-2015; Nakamura,
Tetsu/M-7914-2015; Braesicke, Peter/D-8330-2016; Dhomse,
Sandip/C-8198-2011; Pawson, Steven/I-1865-2014; Pitari,
Giovanni/O-7458-2016; Emmons, Louisa/R-8922-2016
OI Mancini, Eva/0000-0001-7071-0292; Morgenstern, Olaf/0000-0002-9967-9740;
Stolarski, Richard/0000-0001-8722-4012; Chipperfield,
Martyn/0000-0002-6803-4149; Lamarque, Jean-Francois/0000-0002-4225-5074;
bekki, slimane/0000-0002-5538-0800; Nakamura, Tetsu/0000-0002-2056-7392;
Braesicke, Peter/0000-0003-1423-0619; Dhomse,
Sandip/0000-0003-3854-5383; Pawson, Steven/0000-0003-0200-717X; Pitari,
Giovanni/0000-0001-7051-9578; Emmons, Louisa/0000-0003-2325-6212
FU Global Environmental Research Foundation of the Ministry of the
Environment of Japan [A-071]; NASA
FX We thank Ashley Jones for use of the ACE N2O climatology,
Andreas Engel for use of the mean age profiles, and the Aura MLS team
for daily O3 data. We thank Michael Prather, Huisheng Bian,
Ross Salawitch, and Tim Canty for their contributions to the
photochemical evaluations in the SCR. We thank Luke Oman for helpful
conversations. CCSRNIES research was supported by the Global
Environmental Research Foundation of the Ministry of the Environment of
Japan (A-071). CCSRNIES and MRI simulations were completed with the
supercomputer at NIES, Japan. This work was supported by the NASA
Modeling, Analysis, and Prediction Program.
NR 47
TC 39
Z9 39
U1 1
U2 32
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 9
PY 2011
VL 116
AR D17302
DI 10.1029/2010JD015360
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 819BO
UT WOS:000294800600001
ER
PT J
AU A'Hearn, MF
Kelley, MS
AF A'Hearn, M. F.
Kelley, Michael S.
TI EPOXI at Comet Hartley 2 (vol 332, pg 1396, 2011)
SO SCIENCE
LA English
DT Correction
C1 [A'Hearn, M. F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
NASA Headquarters, Planetary Sci Div, Washington, DC 20546 USA.
RP A'Hearn, MF (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD SEP 9
PY 2011
VL 333
IS 6048
BP 1381
EP 1381
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 817KU
UT WOS:000294672200018
ER
PT J
AU Rignot, E
Mouginot, J
Scheuchl, B
AF Rignot, E.
Mouginot, J.
Scheuchl, B.
TI Ice Flow of the Antarctic Ice Sheet
SO SCIENCE
LA English
DT Article
ID PINE ISLAND GLACIER; EAST ANTARCTICA; RADAR INTERFEROMETRY; TOPOGRAPHY;
STREAMS; MOTION; BASAL
AB We present a reference, comprehensive, high-resolution, digital mosaic of ice motion in Antarctica assembled from multiple satellite interferometric synthetic-aperture radar data acquired during the International Polar Year 2007 to 2009. The data reveal widespread, patterned, enhanced flow with tributary glaciers reaching hundreds to thousands of kilometers inland over the entire continent. This view of ice sheet motion emphasizes the importance of basal-slip-dominated tributary flow over deformation-dominated ice sheet flow, redefines our understanding of ice sheet dynamics, and has far-reaching implications for the reconstruction and prediction of ice sheet evolution.
C1 [Rignot, E.; Mouginot, J.; Scheuchl, B.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Rignot, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
RP Rignot, E (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
EM erignot@uci.edu
RI Rignot, Eric/A-4560-2014; Mouginot, Jeremie/G-7045-2015;
OI Rignot, Eric/0000-0002-3366-0481; Mouginot, Jeremie/0000-0001-9155-5455
NR 24
TC 336
Z9 350
U1 11
U2 108
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 SEP 9
PY 2011
VL 333
IS 6048
BP 1427
EP 1430
DI 10.1126/science.1208336
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 817KU
UT WOS:000294672200037
PM 21852457
ER
PT J
AU Drucker, R
Martin, S
Kwok, R
AF Drucker, Robert
Martin, Seelye
Kwok, Ronald
TI Sea ice production and export from coastal polynyas in the Weddell and
Ross Seas
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID THICKNESS; VARIABILITY; WESTERN; FLUX
AB For 1992-2008, we use data from the Special Sensor Microwave/Imager (SSM/I) and the Advanced Microwave Scanning Radiometer-EOS (AMSR-E) to examine differences in ice production and export in the Weddell and Ross Seas. We find that the Ross production is three times that in the Weddell; the Ross export, twice that in the Weddell. In the Ross, the ice production has a statistically significant positive trend of about 21 km(3) y(-1) and approximately equals the export, while in the Weddell, the production trend is statistically flat and provides only about 60% of the export. For each sea, comparison of the ice production with the total winter sea ice volume shows that the Weddell polynyas produce 5-10% of the total; the Ross polynyas, 20-50%. The explanation for these differences is that in the Ross, the low-pressure system is better situated for generation of large polynyas than in the Weddell. Citation: Drucker, R., S. Martin, and R. Kwok (2011), Sea ice production and export from coastal polynyas in the Weddell and Ross Seas, Geophys. Res. Lett., 38, L17502, doi: 10.1029/2011GL048668.
C1 [Drucker, Robert; Martin, Seelye] Univ Washington, Sch Oceanog, Seattle, WA 98195 USA.
[Kwok, Ronald] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Drucker, R (reprint author), Univ Washington, Sch Oceanog, Box 357940, Seattle, WA 98195 USA.
EM robert@ocean.washington.edu; seelye@u.washington.edu;
ronald.kwok@jpl.nasa.gov
RI Kwok, Ron/A-9762-2008
OI Kwok, Ron/0000-0003-4051-5896
FU NASA [NNG04GM69G]
FX SM and RD acknowledge the NASA support under contract NNG04GM69G. RK
performed this work at the Jet Propulsion Laboratory under contract with
NASA. We thank the National Snow Ice Center (NSIDC) for provision of the
AMSR-E and SSM/I data.
NR 13
TC 24
Z9 24
U1 0
U2 21
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 SEP 8
PY 2011
VL 38
AR L17502
DI 10.1029/2011GL048668
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 818WC
UT WOS:000294785600004
ER
PT J
AU Gatebe, CK
Wilcox, E
Poudyal, R
Wang, J
AF Gatebe, C. K.
Wilcox, E.
Poudyal, R.
Wang, J.
TI Effects of ship wakes on ocean brightness and radiative forcing over
ocean
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID AIRBORNE SPECTRAL MEASUREMENTS; SURFACE ALBEDO; SCATTERING; IMAGES;
BUDGET; IMPACT; LIGHT
AB Changes in surface albedo represent one of the main forcing agents that can counteract, to some extent, the positive forcing from increasing greenhouse gas concentrations. Here, we report on enhanced ocean reflectance from ship wakes over the Pacific Ocean near the California coast, where we determined, based on airborne radiation measurements that ship wakes can increase reflected sunlight by more than 100%. We assessed the importance of this increase to climate forcing, where we estimated the global radiative forcing of ship wakes to be -(0.14 +/- 50%) mWm(-2) assuming a global distribution of 32331 ships of size >= 100000 gross tonnage. The forcing is smaller than the forcing of aircraft contrails (-0.007 to + 0.02Wm(-2)), but considering that the global shipping fleet has rapidly grown in the last five decades and this trend is likely to continue because of the need of more intercontinental transportation as a result of economic globalization, we argue that the radiative forcing of wakes is expected to be increasingly important especially in harbors and coastal regions. Citation: Gatebe, C. K., E. Wilcox, R. Poudyal, and J. Wang (2011), Effects of ship wakes on ocean brightness and radiative forcing over ocean, Geophys. Res. Lett., 38, L17702, doi: 10.1029/2011GL048819.
C1 [Gatebe, C. K.] Univ Space Res Assoc, Columbia, MD USA.
[Gatebe, C. K.; Poudyal, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wilcox, E.] Desert Res Inst, Reno, NV 89512 USA.
[Poudyal, R.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Wang, J.] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA.
RP Gatebe, CK (reprint author), Univ Space Res Assoc, Columbia, MD USA.
EM charles.k.gatebe@nasa.gov
RI Gatebe, Charles/G-7094-2011; Wang, Jun/A-2977-2008
OI Gatebe, Charles/0000-0001-9261-2239; Wang, Jun/0000-0002-7334-0490
FU Science Mission Directorate of the National Aeronautics and Space
Administration; NASA [NNX08AF89G]
FX This research was supported by the Science Mission Directorate of the
National Aeronautics and Space Administration as part of the Radiation
Sciences Program under Hal B. Maring and Airborne Science Program, Bruce
Tagg. This work was performed under NASA grant NNX08AF89G. We thank the
editors and two anonymous reviewers for their valuable comments.
NR 30
TC 4
Z9 4
U1 1
U2 7
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 SEP 8
PY 2011
VL 38
AR L17702
DI 10.1029/2011GL048819
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 818WC
UT WOS:000294785600006
ER
PT J
AU Zhang, X
Sander, SP
AF Zhang, Xu
Sander, Stanley P.
TI Infrared Absorption Spectra of the CO2/H2O Complex in a Cryogenic
Nitrogen Matrix-Detection of a New Bending Frequency
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID ISOLATED MOLECULAR-COMPLEXES; WATER-CARBON-DIOXIDE; AB-INITIO; ARGON
MATRICES; SOLID NITROGEN; IR-SPECTRA; CO2; DIMER; FTIR; ROTATION
AB Infrared absorption spectra have been measured for the mixture of CO2 and H2O in a cryogenic nitrogen matrix. The 1:1 CO2/H2O complex has been observed. Each structure of this complex should have two bending frequencies corresponding to the CO2 fundamental bending mode (nu(2)). In this work, three bending frequencies corresponding to the CO2 fundamental bending mode (nu(2)) have been detected; one of them at 660.3 cm(-1) is reported here for the first time. This finding helps confirm the existence of two structures for this complex. A new feature attributed to a CO2 and H2O complex is observed at 3604.4 cm(-1) and is tentatively assigned to the CO2/H2O complex band corresponding to the CO2 combination mode (v(3) + 2 nu(2)). In addition, a band that belongs to a CO2 and H2O complex is detected at 3623.8 cm(-1) for the first time and is tentatively assigned to the (CO2)(2)/H2O complex band corresponding to the symmetric stretching mode (nu(1)) of H2O.
C1 [Zhang, Xu; Sander, Stanley P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Zhang, X (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM xu.zhang@jpl.nasa.gov; Stanley.p.sander@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA)
FX This research was carried out by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration (NASA). This work was supported by
the NASA Planetary Atmospheres, Upper Atmosphere Research and
Tropospheric Chemistry programs, and the NASA Postdoctoral Program. The
authors would also like to thank Dave Nazic for his laboratory support.
NR 21
TC 6
Z9 6
U1 2
U2 17
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD SEP 8
PY 2011
VL 115
IS 35
BP 9854
EP 9860
DI 10.1021/jp203739v
PG 7
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 813RO
UT WOS:000294385800010
PM 21702496
ER
PT J
AU Wang, Y
Helvensteijn, B
Nizamidin, N
Erion, AM
Steiner, LA
Mulloth, LM
Luna, B
Levan, MD
AF Wang, Yu
Helvensteijn, Bernardus
Nizamidin, Nabijan
Erion, Angelae M.
Steiner, Laura A.
Mulloth, Lila M.
Luna, Bernadette
LeVan, M. Douglas
TI High Pressure Excess Isotherms for Adsorption of Oxygen and Nitrogen in
Zeolites
SO LANGMUIR
LA English
DT Article
ID GIBBS DIVIDING SURFACE; ADSORBED PHASE VOLUME; A TYPE ZEOLITE; ACTIVATED
CARBON; SUPERCRITICAL GASES; LOW-TEMPERATURE; METHANE; ARGON;
EQUILIBRIUM; SIMULATION
AB High-pressure oxygen is an integral part of fuel cell systems, many NASA in situ resource utilization concepts, and life support systems for extravehicular activity. Due to the limited information available for system designs over wide ranges of temperature and pressure, volumetric methods are applied to measure adsorption isotherms of O(2) and N(2) on NaX and NaY zeolites covering temperatures from 105 to 448 K and pressures up to 150 bar. Experimental data measured using two apparatuses with distinctly different designs show good agreement for overlapping temperatures. Excess adsorption isotherms are modeled using a traditional isotherm model for absolute adsorption with a correction for the gas capacity of the adsorption space. Comparing two models with temperature-dependent coefficients, a virial isotherm model provides a better description than a Toth isotherm model, even with the same number of parameters. With more virial coefficients, such as a cubic form in loading and quadratic form in reciprocal temperature, the virial model can describe all data accurately over wide ranges of temperature and pressure.
C1 [Wang, Yu; Nizamidin, Nabijan; Erion, Angelae M.; Steiner, Laura A.; LeVan, M. Douglas] Vanderbilt Univ, Dept Chem & Biomol Engn, Nashville, TN 37235 USA.
[Helvensteijn, Bernardus; Mulloth, Lila M.; Luna, Bernadette] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Levan, MD (reprint author), Vanderbilt Univ, Dept Chem & Biomol Engn, 221 Kirkland Hall, Nashville, TN 37235 USA.
EM m.douglas.levan@vanderbilt.edu
FU NASA [NNX09AM42A, NNX09AW24A, NCC 9-58]; NSBRI [SMST02002]
FX Financial support for this research was provided by NASA Cooperative
Agreements NNX09AM42A and NNX09AW24A and NSBRI funded project SMST02002
under NASA Cooperative Agreement NCC 9-58.
NR 44
TC 9
Z9 9
U1 0
U2 27
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0743-7463
J9 LANGMUIR
JI Langmuir
PD SEP 6
PY 2011
VL 27
IS 17
BP 10648
EP 10656
DI 10.1021/la201690x
PG 9
WC Chemistry, Multidisciplinary; Chemistry, Physical; Materials Science,
Multidisciplinary
SC Chemistry; Materials Science
GA 813ND
UT WOS:000294373300040
PM 21744870
ER
PT J
AU Hallar, AG
Chirokova, G
McCubbin, I
Painter, TH
Wiedinmyer, C
Dodson, C
AF Hallar, A. Gannet
Chirokova, Galina
McCubbin, Ian
Painter, Thomas H.
Wiedinmyer, Christine
Dodson, Craig
TI Atmospheric bioaerosols transported via dust storms in the western
United States
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID PERFORMANCE EVALUATION; COLORADO PLATEAU; ICE NUCLEATION; PARTICLE
SIZER; WIND EROSION; IMMERSION; AEROSOLS; FLUORESCENCE; CRYSTALS;
DROPLETS
AB Measurements are presented showing the presence of biological material within frequent dust storms in the western United States. Previous work has indicated that biological particles were enhancing the impact of dust storms on the formation of clouds. This paper presents multiple case studies, between April and May 2010, showing the presence of and quantifying the amount of biological material via an Ultraviolet Aerodynamic Particle Sizer during dust events. All dust storms originated in the Four Corners region in the western Untied States and were measured at Storm Peak Laboratory, a high elevation facility in northwestern Colorado. From an Aerodynamic Particle Sizer, the mean dust particle size during these events was approximately 1 mu m, with number concentrations between 6 cm(-3) and 12 cm(-3). Approximately 0.2% of these dust particles had fluorescence signatures, indicating the presence of biological material. Citation: Hallar, A. G., G. Chirokova, I. McCubbin, T. H. Painter, C. Wiedinmyer, and C. Dodson (2011), Atmospheric bioaerosols transported via dust storms in the western United States, Geophys. Res. Lett., 38, L17801, doi: 10.1029/2011GL048166.
C1 [Hallar, A. Gannet; Chirokova, Galina; McCubbin, Ian; Dodson, Craig] Desert Res Inst, Storm Peak Lab, Steamboat Springs, CO 80488 USA.
[Painter, Thomas H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wiedinmyer, Christine] Natl Ctr Atmospher Res, Boulder, CO 80305 USA.
RP Hallar, AG (reprint author), Desert Res Inst, Storm Peak Lab, POB 882530, Steamboat Springs, CO 80488 USA.
EM ghallar@dri.edu
RI Hallar, Anna Gannet/I-9104-2012; Painter, Thomas/B-7806-2016
OI Hallar, Anna Gannet/0000-0001-9972-0056;
FU NASA
FX The authors greatly appreciate the advice of Alex Huffman on the
operation of the UV-APS. The Steamboat Ski Resort provided logistical
support and in-kind donations. The DRI's SPL is an equal opportunity
service provider and employer and is a permitee of the Medicine-Bow
Routt National Forests. Part of this work was performed at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA.
NR 32
TC 35
Z9 35
U1 2
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 3
PY 2011
VL 38
AR L17801
DI 10.1029/2011GL048166
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 816RQ
UT WOS:000294620200001
ER
PT J
AU Limpasuvan, V
Alexander, MJ
Orsolini, YJ
Wu, DL
Xue, M
Richter, JH
Yamashita, C
AF Limpasuvan, Varavut
Alexander, M. Joan
Orsolini, Yvan J.
Wu, Dong L.
Xue, Ming
Richter, Jadwiga H.
Yamashita, Chihoko
TI Mesoscale simulations of gravity waves during the 2008-2009 major
stratospheric sudden warming
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID PREDICTION SYSTEM ARPS; GENERAL-CIRCULATION; MIDDLE ATMOSPHERE; MOUNTAIN
WAVES; EOS MLS; MODEL; BREAKING; VORTEX; PROPAGATION; SATELLITE
AB A series of 24 h mesoscale simulations (of 10 km horizontal and 400 m vertical resolution) are performed to examine the characteristics and forcing of gravity waves (GWs) relative to planetary waves (PWs) during the 2008-2009 major stratospheric sudden warming (SSW). Just prior to SSW occurrence, widespread westward propagating GWs are found along the vortex's edge and associated predominantly with major topographical features and strong near-surface winds. Momentum forcing due to GWs surpasses PW forcing in the upper stratosphere and tends to decelerate the polar westerly jet in excess of 30 m s(-1) d(-1). With SSW onset, PWs dominate the momentum forcing, providing decelerative effects in excess of 50 m s(-1) d(-1) throughout the upper polar stratosphere. GWs related to topography become less widespread largely due to incipient wind reversal as the vortex starts to elongate. During the SSW maturation and early recovery, the polar vortex eventually splits and both wave signatures and forcing greatly subside. Nonetheless, during SSW, westward and eastward propagating GWs are found in the polar region and may be generated in situ by flow adjustment processes in the stratosphere or by secondary GW breaking. The simulated large-scale features agree well with those resolved in satellite observations and analysis products.
C1 [Limpasuvan, Varavut] Coastal Carolina Univ, Dept Appl Phys, Minneapolis, SC 29528 USA.
[Alexander, M. Joan] NW Res Associates, Colorado Res Associates Div, Boulder, CO 80301 USA.
[Orsolini, Yvan J.] Norwegian Inst Air Res, N-2027 Kjeller, Norway.
[Richter, Jadwiga H.; Yamashita, Chihoko] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Wu, Dong L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Xue, Ming] Univ Oklahoma, Ctr Anal & Predict Storms, Norman, OK 73072 USA.
[Xue, Ming] Univ Oklahoma, Sch Meteorol, Norman, OK 73072 USA.
RP Limpasuvan, V (reprint author), Coastal Carolina Univ, Dept Appl Phys, POB 261954, Minneapolis, SC 29528 USA.
EM var@coastal.edu
RI Xue, Ming/F-8073-2011; Limpasuvan, Varavut/K-6266-2013; Cullens,
Chihoko/P-2425-2015; Wu, Dong/D-5375-2012
OI Xue, Ming/0000-0003-1976-3238; Cullens, Chihoko/0000-0002-9951-9763;
FU National Science Foundation (NSF) [ATM-0646672, AGS-0958616, 0943506];
National Aeronautics and Space Administration (NASA) [NNX07AR25G];
Norwegian Research Council; NASA through NASA Advanced Supercomputing
(NAS) Division at Ames Research Center
FX V.L. is supported in part by Large Scale Dynamics Program and Major
Research Instrumentation Program at National Science Foundation (NSF)
under awards ATM-0646672 and AGS-0958616, respectively, and National
Aeronautics and Space Administration (NASA) contract NNX07AR25G. Part of
this work was done while V. L. was on sabbatical at National Center for
Atmospheric Research (NCAR). Support for M.J.A.'s contribution to this
manuscript comes from NSF under award 0943506. Y.O. was supported by
Norwegian Research Council (project ARCTIC LIS). Resources supporting
this work were provided in part by NASA High-End Computing (HEC) Program
through NASA Advanced Supercomputing (NAS) Division at Ames Research
Center. Finally, we are greatly indebted to the anonymous reviewers and
Matt Hitchman, who provided very helpful suggestions and ideas to
greatly improve this paper.
NR 57
TC 11
Z9 11
U1 0
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 3
PY 2011
VL 116
AR D17104
DI 10.1029/2010JD015190
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 816UW
UT WOS:000294628600001
ER
PT J
AU Halkides, DJ
Lucas, LE
Waliser, DE
Lee, T
Murtugudde, R
AF Halkides, D. J.
Lucas, Lisanne E.
Waliser, Duane E.
Lee, Tong
Murtugudde, Raghu
TI Mechanisms controlling mixed-layer temperature variability in the
eastern tropical Pacific on the intraseasonal timescale
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID EQUATORIAL PACIFIC; OCEAN GCM; EL-NINO; MODEL; OSCILLATION; BALANCE;
CYCLE
AB The Madden Julian Oscillation (MJO) is a prominent mode of intraseasonal (similar to 35-95 day) variability in the tropical Indian and western Pacific Oceans. Its impacts on ocean mixed-layer temperatures (MLT) in the eastern tropical Pacific Ocean (ETPO) are not well-understood. A previous study of mooring data at (110 degrees W, EQ) implies vertical advection forced by MJO-generated Kelvin waves is important to ETPO intraseasonal MLT; another, based on model output over (120-100 degrees W, 3 degrees S-3 degrees N), indicates meridional advection dominates. We analyze an ocean state estimate at (110 degrees W, EQ) and find combined subsurface processes, including a notable vertical advection component like that expected from MJO-forced Kelvin waves, dominate. However, when averaged over (120-100 degrees W, 3 degrees S-3 degrees N), subsurface processes and horizontal advection are both important, and effects of thermocline forcing (e. g., Kelvin waves) are small compared to those by local wind driven mixing and horizontal advection. The results highlight the importance of understanding regional physics on different spatial scales. Citation: Halkides, D. J., L. E. Lucas, D. E. Waliser, T. Lee, and R. Murtugudde (2011), Mechanisms controlling mixed-layer temperature variability in the eastern tropical Pacific on the intraseasonal timescale, Geophys. Res. Lett., 38, L17602, doi:10.1029/2011GL048545.
C1 [Halkides, D. J.; Waliser, Duane E.; Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lucas, Lisanne E.] NOAA, Univ Corp Atmospher Res, Climate Program Off, Silver Spring, MD 20910 USA.
[Halkides, D. J.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Murtugudde, Raghu] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Halkides, DJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM halkides@jpl.nasa.gov
FU NASA; PO.DAAC; Divecha Center for Climate Change at IISc, Bangalore
FX Research conducted at Jet Propulsion Laboratory, California Institute of
Technology, in contract with NASA. Support by PO.DAAC
(http://podaac.jpl.nasa.gov), NASA PO grants and the Divecha Center for
Climate Change at IISc, Bangalore, is acknowledged.
NR 27
TC 6
Z9 6
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 2
PY 2011
VL 38
AR L17602
DI 10.1029/2011GL048545
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 816QB
UT WOS:000294616100002
ER
PT J
AU Montes-Hugo, MA
Weidemann, A
Gould, R
Arnone, R
Churnside, JH
Jaroz, E
AF Montes-Hugo, Martin A.
Weidemann, Alan
Gould, Richard
Arnone, Robert
Churnside, James H.
Jaroz, Ewa
TI Ocean color patterns help to predict depth of optical layers in
stratified coastal waters
SO JOURNAL OF APPLIED REMOTE SENSING
LA English
DT Article
DE ocean color; vertical structure; coastal waters; remote sensing
reflectance; spatial statistics; thin layers
ID SCATTERING LAYERS; AIRBORNE LIDAR; TEMPERATURE; DEPENDENCE; ABSORPTION
AB Subsurface optical layers distributed at two different depths were investigated in Monterrey Bay, East Sound, and the Black Sea based on spatial statistics of remote sensing reflectance (R-rs). The main objective of this study was to evaluate the use of R-rs(443)/R-rs(490) (hereafter R1) skewness (psi) as an indicator of vertical optical structure in different marine regions. Measurements of inherent optical properties were obtained using a remotely operated towed vehicle and R1 was theoretically derived from optical profiles. Although the broad range of trophic status and water stratification, a common statistical pattern consisting of lower psi R1-a deeper optical layer was found in all study cases. This variation was attributed to optical changes above the opticline and related to horizontal variability of particulates and spectral variations with depth. We recommend more comparisons in stratified coastal waters with different phytoplankton communities before the use of psi R1 can be generalized as a noninvasive optical proxy for screening depth changes on subsurface optical layers. (C) 2011 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI:10.1117/1.3634055]
C1 [Montes-Hugo, Martin A.] Mississippi State Univ, Geosyst Res Inst, Starkville, MS 39529 USA.
[Weidemann, Alan; Gould, Richard; Arnone, Robert; Jaroz, Ewa] USN, NASA, Stennis Space Ctr, Res Lab, Hancock, MS 39529 USA.
[Churnside, James H.] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA.
RP Montes-Hugo, MA (reprint author), Mississippi State Univ, Geosyst Res Inst, Starkville, MS 39529 USA.
EM mmontes@gri.msstate.edu; alan.weidemann@nrlssc.navy.mil;
Rick.Gould@nrlssc.navy.mil; Bob.Arnone@nrlssc.navy.mil;
James.H.Churnside@noaa.gov; ewa.jarosz@nrlssc.navy.mil
RI Churnside, James/H-4873-2013; Manager, CSD Publications/B-2789-2015
FU NRL [PE0601153N]
FX We appreciate the valuable scientific comments given by Dr. Emmanuel
Boss that helped to improve the original manuscript version. This work
was supported by the NRL internal project "3D Remote Sensing with a
Multiple-Band Active and Passive System: Theoretical Basis," PE0601153N.
NR 12
TC 5
Z9 5
U1 0
U2 21
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 1931-3195
J9 J APPL REMOTE SENS
JI J. Appl. Remote Sens.
PD SEP 2
PY 2011
VL 5
AR 053548
DI 10.1117/1.3634055
PG 6
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 820IK
UT WOS:000294898700001
ER
PT J
AU Verronen, PT
Santee, ML
Manney, GL
Lehmann, R
Salmi, SM
Seppala, A
AF Verronen, P. T.
Santee, M. L.
Manney, G. L.
Lehmann, R.
Salmi, S. -M.
Seppaelae, A.
TI Nitric acid enhancements in the mesosphere during the January 2005 and
December 2006 solar proton events
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID OCTOBER-NOVEMBER 2003; CHEMICAL-REACTION SYSTEMS; OZONE DEPLETION;
PARTICLE-PRECIPITATION; NORTHERN-HEMISPHERE; ODD HYDROGEN; HNO3;
STRATOSPHERE; CHEMISTRY; TEMPERATURE
AB We investigate enhancements of mesospheric nitric acid (HNO3) in the Northern Hemisphere polar night regions during the January 2005 and December 2006 solar proton events (SPEs). The enhancements are caused by ionization due to proton precipitation, followed by ionic reactions that convert NO and NO2 to HNO3. We utilize mesospheric observations of HNO3 from the Microwave Limb Sounder (MLS/Aura). Although in general MLS HNO3 data above 50 km (1.5 hPa) are outside the standard recommended altitude range, we show that in these special conditions, when SPEs produce order-of-magnitude enhancements in HNO3, it is possible to monitor altitudes up to 70 km (0.0464 hPa) reliably. MLS observations show HNO3 enhancements of about 4 ppbv and 2 ppbv around 60 km in January 2005 and December 2006, respectively. The highest mixing ratios are observed inside the polar vortex north of 75 degrees N latitude, right after the main peak of SPE forcing. These measurements are compared with results from the one-dimensional Sodankyla Ion and Neutral Chemistry (SIC) model. The model has been recently revised in terms of rate coefficients of ionic reactions, so that at 50-80 km it produces about 40% less HNO3 during SPEs compared to the earlier version. This is a significant improvement that results in better agreement with the MLS observations. By a few days after the SPEs, HNO3 is heavily influenced by horizontal transport and mixing, leading to its redistribution and decrease of the SPE-enhanced mixing ratios in the polar regions.
C1 [Verronen, P. T.; Salmi, S. -M.; Seppaelae, A.] Finnish Meteorol Inst, FI-00101 Helsinki, Finland.
[Santee, M. L.; Manney, G. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lehmann, R.] Alfred Wegener Inst Polar & Marine Res, D-14473 Potsdam, Germany.
[Seppaelae, A.] British Antarctic Survey, NERC, Cambridge CB3 0ET, England.
RP Verronen, PT (reprint author), Finnish Meteorol Inst, POB 503,Erik Palmenin Aukio 1, FI-00101 Helsinki, Finland.
EM pekka.verronen@fmi.fi; michelle.l.santee@jpl.nasa.gov;
gloria.l.manney@jpl.nasa.gov; ralph.lehmann@awi.de;
sanna-mari.salmi@fmi.fi; annika.seppala@bas.ac.uk
RI Seppala, Annika/C-8031-2014; Paivarinta, Sanna-Mari/D-1084-2014;
Verronen, Pekka/G-6658-2014
OI Seppala, Annika/0000-0002-5028-8220; Paivarinta,
Sanna-Mari/0000-0001-9390-7282; Verronen, Pekka/0000-0002-3479-9071
FU Academy of Finland [136225/SPOC, 123275/THERMES]; European Commission
[FP7-PEOPLE-IEF-2008/237461-EPPIC]; Vilho; Yrjo; Kalle Vaisala
foundation; National Aeronautics and Space Administration
FX The authors would like to thank Nathaniel Livesey for useful comments.
The work of P.T.V. and S.M.S. was supported by the Academy of Finland
through the projects 136225/SPOC (Significance of Energetic Electron
Precipitation to Odd Hydrogen, Ozone, and Climate) and 123275/THERMES
(Thermosphere and Mesosphere Affecting the Stratosphere). A.S. was
supported by the European Commission through the project
FP7-PEOPLE-IEF-2008/237461-EPPIC. P.T.V.'s visit to Jet Propulsion
Laboratory in March 2008 was supported by the Vilho, Yrjo, and Kalle
Vaisala foundation. Research at the Jet Propulsion Laboratory,
California Institute of Technology, is performed under contract with the
National Aeronautics and Space Administration. MLS data were provided by
the Goddard Earth Sciences Data and Information Service Center.
NR 51
TC 19
Z9 19
U1 1
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 2
PY 2011
VL 116
AR D17301
DI 10.1029/2011JD016075
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 816UR
UT WOS:000294628100003
ER
PT J
AU Matsuura, M
Dwek, E
Meixner, M
Otsuka, M
Babler, B
Barlow, MJ
Roman-Duval, J
Engelbracht, C
Sandstrom, K
Lakicevic, M
van Loon, JT
Sonneborn, G
Clayton, GC
Long, KS
Lundqvist, P
Nozawa, T
Gordon, KD
Hony, S
Panuzzo, P
Okumura, K
Misselt, KA
Montiel, E
Sauvage, M
AF Matsuura, M.
Dwek, E.
Meixner, M.
Otsuka, M.
Babler, B.
Barlow, M. J.
Roman-Duval, J.
Engelbracht, C.
Sandstrom, K.
Lakicevic, M.
van Loon, J. Th
Sonneborn, G.
Clayton, G. C.
Long, K. S.
Lundqvist, P.
Nozawa, T.
Gordon, K. D.
Hony, S.
Panuzzo, P.
Okumura, K.
Misselt, K. A.
Montiel, E.
Sauvage, M.
TI Herschel Detects a Massive Dust Reservoir in Supernova 1987A
SO SCIENCE
LA English
DT Article
ID LARGE-MAGELLANIC-CLOUD; INNER CIRCUMSTELLAR RING;
HUBBLE-SPACE-TELESCOPE; GALAXY EVOLUTION SAGE; SN 1987A; SPIRE
INSTRUMENT; NEUTRINO BURST; SPITZER SURVEY; LINE EMISSION; MILKY-WAY
AB We report far-infrared and submillimeter observations of supernova 1987A, the star whose explosion was observed on 23 February 1987 in the Large Magellanic Cloud, a galaxy located 160,000 light years away. The observations reveal the presence of a population of cold dust grains radiating with a temperature of about 17 to 23 kelvin at a rate of about 220 times the luminosity of the Sun. The intensity and spectral energy distribution of the emission suggest a dust mass of about 0.4 to 0.7 times the mass of the Sun. The radiation must originate from the supernova ejecta and requires the efficient precipitation of all refractory material into dust. Our observations imply that supernovae can produce the large dust masses detected in young galaxies at very high redshifts.
C1 [Matsuura, M.; Barlow, M. J.] UCL, Dept Phys & Astron, Astrophys Grp, London WC1E 6BT, England.
[Matsuura, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Dwek, E.; Sonneborn, G.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Meixner, M.; Otsuka, M.; Roman-Duval, J.; Long, K. S.; Gordon, K. D.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Babler, B.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Engelbracht, C.; Misselt, K. A.; Montiel, E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Sandstrom, K.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Lakicevic, M.; van Loon, J. Th] Keele Univ, Lennard Jones Labs, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Lakicevic, M.] European So Observ, D-85748 Garching, Germany.
[Clayton, G. C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
[Lundqvist, P.] Stockholm Univ, AlbaNova Univ Ctr, Oskar Klein Ctr, Dept Astron, SE-10691 Stockholm, Sweden.
[Nozawa, T.] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778583, Japan.
[Hony, S.; Panuzzo, P.; Okumura, K.; Sauvage, M.] Commissariat Energie Atom & Energies Alternat, Lab Astrophys Instrumentat & Modelisat, Irfu SAp, F-91191 Gif Sur Yvette, France.
RP Matsuura, M (reprint author), UCL, Dept Phys & Astron, Astrophys Grp, Gower St, London WC1E 6BT, England.
EM mikako@star.ucl.ac.uk
RI Barlow, Michael/A-5638-2009; Dwek, Eli/C-3995-2012; Sonneborn,
George/D-5255-2012;
OI Barlow, Michael/0000-0002-3875-1171; Babler, Brian/0000-0002-6984-5752
FU NASA Herschel Science Center, JPL [1381522, 1381650]; ESA; PACS; SPIRE
teams; Herschel Science Centre; NASA Herschel Science Center; University
College London Institute of Origins; European Southern Observatory-Keele
studentship
FX Herschel is a European Space Agency (ESA) space observatory with science
instruments provided by European-led principal investigator consortia
and with important participation from NASA. We acknowledge financial
support from the NASA Herschel Science Center, JPL contracts 1381522 and
1381650. We acknowledge the contributions and support of the ESA, the
PACS and SPIRE teams, the Herschel Science Centre, the NASA Herschel
Science Center, and the PACS and SPIRE instrument control centers,
without which none of this work would have been possible. We also thank
the HERITAGE team for various inputs on the data reduction. M. M.
appreciates many discussions and inputs from H. Hirashita, I. Sakon, R.
Wesson, K. Nomoto, and B. M. Swinyard. M. M. acknowledges the award of a
University College London Institute of Origins Fellowship, and M. L.
acknowledges a European Southern Observatory-Keele studentship.
NR 52
TC 157
Z9 157
U1 0
U2 5
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD SEP 2
PY 2011
VL 333
IS 6047
BP 1258
EP 1261
DI 10.1126/science.1205983
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 813YM
UT WOS:000294406400045
PM 21737700
ER
PT J
AU Cohen, CS
McCann, L
Davis, T
Shaw, L
Ruiz, G
AF Cohen, C. Sarah
McCann, Linda
Davis, Tammy
Shaw, Linda
Ruiz, Gregory
TI Discovery and significance of the colonial tunicate Didemnum vexillum in
Alaska
SO AQUATIC INVASIONS
LA English
DT Article
DE Didemnum vexillum; ascidian; nonindigenous species; genetic species
identification; citizen science; aquaculture; multilocus
ID HABITAT; CALIFORNIA; INVASIONS
AB The colonial tunicate, Didemnum vexillum Kott, 2002, has a history of invading and overgrowing marine communities in temperate waters worldwide. The species can colonize and dominate remarkably large areas of benthic habitat, including coastal bays and outer coastal areas, causing concerns about potential long-term effects on community structure, critical habitats, and fisheries resources. We report here the confirmed occurrence of D. vexillum in Alaska, representing a dramatic 1000 km northward extension of this non-native species along the western coast of North America. The species was detected as part of a " bioblitz", engaging citizen scientists to survey local biota and detect non-native marine species incursions. Following detection, the identity of D. vexillum was confirmed with robust genetic methods, and morphological characters were also consistent with previous species descriptions. Although invasions have been relatively rare in Alaskan waters to date, it is now clear that D. vexillum is established in at least one site (Whiting Harbor) near Sitka, Alaska. Given the explosive growth and spread of this species in other global regions, and its potential for significant impacts across diverse habitats in Alaska, current efforts are underway to evaluate its distribution and options to eradicate or control the species.
C1 [Cohen, C. Sarah] San Francisco State Univ, Romberg Tiburon Ctr, Tiburon, CA 94920 USA.
[Cohen, C. Sarah] San Francisco State Univ, Dept Biol, Tiburon, CA 94920 USA.
[McCann, Linda] Smithsonian Environm Res Ctr, Romberg Tiburon Ctr, Tiburon, CA 94920 USA.
[Davis, Tammy] Invas Species Program, Alaska Dept Fish & Game, Juneau, AK 99811 USA.
[Shaw, Linda] Natl Marine Fisheries Serv, Habitat Conservat Div, Juneau, AK 99802 USA.
[Ruiz, Gregory] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Cohen, CS (reprint author), San Francisco State Univ, Romberg Tiburon Ctr, 3150 Paradise Dr, Tiburon, CA 94920 USA.
EM sarahcoh@rtc.sfsu.edu; mccannl@si.edu; tammy.davis@alaska.gov;
Linda.Shaw@noaa.gov; ruizg@si.edu
OI Ruiz, Gregory/0000-0003-2499-441X
FU Alaska Department of Fish and Game, San Francisco State University, and
the Smithsonian Institution
FX We thank many people who helped in this research. Marnie Chapman and
Heather Woody assisted tirelessly in all aspects of this research.
Heather Woody also inspired us to undertake the bioblitz. Richard
Coleman and David Lake obtained genetic data at the SFSU RTC molecular
facility (NSF FSML award 0435033). John Stein provided lab space at the
Sitka Science Center, and Grant Miller provided access to Whiting
Harbor. Carolyn Bergstrom, Krissy Dunker, Jon Martin, Katharine Miller,
Ken Rear, David Tallmon, Sherry Tamone, and many others assisted in the
field surveys. Larry Harris and Benjamin Becker provided additional
samples from non-Alaskan regions for genetic analyses. Gretchen Lambert
examined morphological characters of Alaskan samples. This research was
supported by funding from Alaska Department of Fish and Game, San
Francisco State University, and the Smithsonian Institution.
NR 28
TC 12
Z9 13
U1 3
U2 27
PU REGIONAL EURO-ASIAN BIOLOGICAL INVASIONS CENTRE-REABIC
PI HELSINKI
PA PL 3, HELSINKI, 00981, FINLAND
SN 1798-6540
EI 1818-5487
J9 AQUAT INVASIONS
JI Aquat. Invasions
PD SEP
PY 2011
VL 6
IS 3
BP 263
EP 271
DI 10.3391/ai.2011.6.3.03
PG 9
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 972LA
UT WOS:000306277400003
ER
PT J
AU Han, JW
Meyyappan, M
AF Han, Jin-Woo
Meyyappan, M.
TI Copper oxide resistive switching memory for e-textile
SO AIP ADVANCES
LA English
DT Article
ID DEVICES
AB A resistive switching memory suitable for integration into textiles is demonstrated on a copper wire network. Starting from copper wires, a Cu/CuxO/Pt sandwich structure is fabricated. The active oxide film is produced by simple thermal oxidation of Cu in atmospheric ambient. The devices display a resistance switching ratio of 10(2) between the high and low resistance states. The memory states are reversible and retained over 10(7) seconds, with the states remaining nondestructive after multiple read operations. The presented device on the wire network can potentially offer a memory for integration into smart textile. Copyright 2011 Author(s). This article is distributed under a Creative Commons Attribution 3.0 Unported License. [doi: 10.1063/1.3645967]
C1 [Han, Jin-Woo; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
RP Han, JW (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
EM jin-woo.han@nasa.gov
NR 36
TC 13
Z9 13
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 2158-3226
J9 AIP ADV
JI AIP Adv.
PD SEP
PY 2011
VL 1
IS 3
AR 032162
DI 10.1063/1.3645967
PG 8
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 916YR
UT WOS:000302139600062
ER
PT J
AU Kitching, T
Amara, A
Gill, M
Harmeling, S
Heymans, C
Massey, R
Rowe, B
Schrabback, T
Voigt, L
Balan, S
Bernstein, G
Bethge, M
Bridle, S
Courbin, F
Gentile, M
Heavens, A
Hirsch, M
Hosseini, R
Kiessling, A
Kirk, D
Kuijken, K
Mandelbaum, R
Moghaddam, B
Nurbaeva, G
Paulin-Henriksson, S
Rassat, A
Rhodes, J
Scholkopf, B
Shawe-Taylor, J
Shmakova, M
Taylor, A
Velander, M
van Waerbeke, L
Witherick, D
Wittman, D
AF Kitching, Thomas
Amara, Adam
Gill, Mandeep
Harmeling, Stefan
Heymans, Catherine
Massey, Richard
Rowe, Barnaby
Schrabback, Tim
Voigt, Lisa
Balan, Sreekumar
Bernstein, Gary
Bethge, Matthias
Bridle, Sarah
Courbin, Frederic
Gentile, Marc
Heavens, Alan
Hirsch, Michael
Hosseini, Reshad
Kiessling, Alina
Kirk, Donnacha
Kuijken, Konrad
Mandelbaum, Rachel
Moghaddam, Baback
Nurbaeva, Guldariya
Paulin-Henriksson, Stephane
Rassat, Anais
Rhodes, Jason
Schoelkopf, Bernhard
Shawe-Taylor, John
Shmakova, Marina
Taylor, Andy
Velander, Malin
van Waerbeke, Ludovic
Witherick, Dugan
Wittman, David
TI GRAVITATIONAL LENSING ACCURACY TESTING 2010 (GREAT10) CHALLENGE HANDBOOK
SO ANNALS OF APPLIED STATISTICS
LA English
DT Article
DE Statistical inference; imaging processing; cosmology
ID POINT-SPREAD FUNCTION; GALAXY SHAPE MEASUREMENT; COSMIC SHEAR; WEAK;
IMAGES; DECONVOLUTION; BLUR
AB GRavitational lEnsing Accuracy Testing 2010 (GREAT10) is a public image analysis challenge aimed at the development of algorithms to analyze astronomical images. Specifically, the challenge is to measure varying image distortions in the presence of a variable convolution kernel, pixelization and noise. This is the second in a series of challenges set to the astronomy, computer science and statistics communities, providing a structured environment in which methods can be improved and tested in preparation for planned astronomical surveys. GREAT10 extends upon previous work by introducing variable fields into the challenge. The "Galaxy Challenge" involves the precise measurement of galaxy shape distortions, quantified locally by two parameters called shear, in the presence of a known convolution kernel. Crucially, the convolution kernel and the simulated gravitational lensing shape distortion both now vary as a function of position within the images, as is the case for real data. In addition, we introduce the "Star Challenge" that concerns the reconstruction of a variable convolution kernel, similar to that in a typical astronomical observation. This document details the GREAT10 Challenge for potential participants. Continually updated information is also available from www.greatchallenges.info.
C1 [Kitching, Thomas; Heymans, Catherine; Massey, Richard; Heavens, Alan; Kiessling, Alina; Taylor, Andy] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Amara, Adam] ETH, Zurich, Switzerland.
[Gill, Mandeep; Shmakova, Marina] Kavli Inst Particle Astrophys & Cosmol, Stanford, CA USA.
[Rowe, Barnaby; Moghaddam, Baback; Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Voigt, Lisa; Bridle, Sarah; Kirk, Donnacha; Shawe-Taylor, John; Witherick, Dugan] UCL, London WC1E 6BT, England.
[Bernstein, Gary] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Courbin, Frederic; Gentile, Marc; Nurbaeva, Guldariya] Ecole Polytech Fed Lausanne, Astrophys Lab, CH-1015 Lausanne, Switzerland.
[Paulin-Henriksson, Stephane; Rassat, Anais] CEA Saclay, Serv Astrophys, Paris, France.
[Wittman, David] Univ Calif Davis, Davis, CA 95616 USA.
[Harmeling, Stefan; Bethge, Matthias; Hirsch, Michael; Hosseini, Reshad; Schoelkopf, Bernhard] Univ Tubingen, Max Planck Inst Biol Cybernet, D-72074 Tubingen, Germany.
[Schrabback, Tim; Kuijken, Konrad; Velander, Malin] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Balan, Sreekumar] Univ Cambridge, Cavendish Lab, Cambridge CB2 1TN, England.
[Bethge, Matthias] Univ Tubingen, Inst Theoret Phys, D-72074 Tubingen, Germany.
[Mandelbaum, Rachel] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[van Waerbeke, Ludovic] Univ British Columbia, Vancouver, BC V5Z 1M9, Canada.
[Gill, Mandeep] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA.
RP Kitching, T (reprint author), Univ Edinburgh, Royal Observ, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland.
EM tdk@roe.ac.uk
RI Bethge, Matthias/B-1554-2008; Scholkopf, Bernhard/A-7570-2013;
Witherick, Dugan/C-9403-2014; Mandelbaum, Rachel/N-8955-2014;
OI Witherick, Dugan/0000-0002-9175-0151; Mandelbaum,
Rachel/0000-0003-2271-1527; Hosseini, Reshad/0000-0002-3669-760X; Rowe,
Barnaby/0000-0002-7042-9174
FU STFC [RA0888, PP/E006450/1, ST/H008543/1]; RAS; Zwicky Fellowship at ETH
Zurich; European Research Council [240185, MIRG-CT-208994]; European
DUEL Research-Training Network [MRTN-CT-2006-036133]; Royal Society;
Swiss National Science Foundation (SNSF)
FX Supported by STFC Rolling Grant Number RA0888 and an RAS 2010
Fellowship.; Supported by the Zwicky Fellowship at ETH Zurich.;
Supported by the European Research Council under the EC FP7 ERC Grant
Number 240185.; Supported by STFC Advanced Fellowship #PP/E006450/1 and
ERC Grant MIRG-CT-208994.; Supported by the European DUEL
Research-Training Network (MRTN-CT-2006-036133).; Supported by a Royal
Society University Research Fellowship and a European Research Council
Starting grant.; Supported in part by the Swiss National Science
Foundation (SNSF).; Supported by STFC Grant ST/H008543/1.
NR 41
TC 21
Z9 21
U1 0
U2 5
PU INST MATHEMATICAL STATISTICS
PI CLEVELAND
PA 3163 SOMERSET DR, CLEVELAND, OH 44122 USA
SN 1932-6157
J9 ANN APPL STAT
JI Ann. Appl. Stat.
PD SEP
PY 2011
VL 5
IS 3
BP 2231
EP 2263
DI 10.1214/11-AOAS484
PG 33
WC Statistics & Probability
SC Mathematics
GA 893UR
UT WOS:000300382500021
ER
PT J
AU Dekker, AG
Phinn, SR
Anstee, J
Bissett, P
Brando, VE
Casey, B
Fearns, P
Hedley, J
Klonowski, W
Lee, ZP
Lynch, M
Lyons, M
Mobley, C
Roelfsema, C
AF Dekker, Arnold G.
Phinn, Stuart R.
Anstee, Janet
Bissett, Paul
Brando, Vittorio E.
Casey, Brandon
Fearns, Peter
Hedley, John
Klonowski, Wojciech
Lee, Zhong P.
Lynch, Merv
Lyons, Mitchell
Mobley, Curtis
Roelfsema, Chris
TI Intercomparison of shallow water bathymetry, hydro-optics, and benthos
mapping techniques in Australian and Caribbean coastal environments
SO LIMNOLOGY AND OCEANOGRAPHY-METHODS
LA English
DT Article
ID DISSOLVED ORGANIC-MATTER; REMOTE-SENSING IMAGERY; LEE-STOCKING ISLAND;
MORETON BAY; CORAL-REEF; REFLECTANCE; ABSORPTION; CLASSIFICATION;
SEDIMENTS; BAHAMAS
AB Science, resource management, and defense need algorithms capable of using airborne or satellite imagery to accurately map bathymetry, water quality, and substrate composition in optically shallow waters. Although a variety of inversion algorithms are available, there has been limited assessment of performance and no work has been published comparing their accuracy and efficiency. This paper compares the absolute and relative accuracies and computational efficiencies of one empirical and five radiative-transfer-based published approaches applied to coastal sites at Lee Stocking Island in the Bahamas and Moreton Bay in eastern Australia. These sites have published airborne hyperspectral data and field data. The assessment showed that (1) radiative-transfer-based methods were more accurate than the empirical approach for bathymetric retrieval, and the accuracies and processing times were inversely related to the complexity of the models used; (2) all inversion methods provided moderately accurate retrievals of bathymetry, water column inherent optical properties, and benthic reflectance in waters less than 13 m deep with homogeneous to heterogeneous benthic/substrate covers; (3) slightly higher accuracy retrievals were obtained from locally parameterized methods; and (4) no method compared here can be considered optimal for all situations. The results provide a guide to the conditions where each approach may be used (available image and field data and processing capability). A re-analysis of these same or additional sites with satellite hyperspectral data with lower spatial and radiometric resolution, but higher temporal resolution would be instructive to establish guidelines for repeatable regional to global scale shallow water mapping approaches.
C1 [Dekker, Arnold G.; Anstee, Janet; Brando, Vittorio E.] CSIRO, Environm Earth Observat Grp, Div Land & Water, Canberra, ACT 2601, Australia.
[Dekker, Arnold G.; Phinn, Stuart R.; Brando, Vittorio E.; Lyons, Mitchell; Roelfsema, Chris] Univ Queensland, Sch Geog Planning & Environm Management, Ctr Spatial Environm Res, Brisbane, Qld 4072, Australia.
[Lee, Zhong P.] Mississippi State Univ, Stennis Space Ctr, Geosyst Res Inst, Mississippi State, MS USA.
[Fearns, Peter; Klonowski, Wojciech; Lynch, Merv] Curtin Univ, Dept Imaging & Appl Phys, Perth, WA 6845, Australia.
[Hedley, John] Univ Exeter, Sch Biosci, Exeter EX4 4PS, Devon, England.
[Mobley, Curtis] Sequoia Sci Inc, Bellevue, WA 98005 USA.
RP Dekker, AG (reprint author), CSIRO, Environm Earth Observat Grp, Div Land & Water, Canberra, ACT 2601, Australia.
EM arnold.dekker@csiro.au; s.phinn@uq.edu.au
RI Dekker, Arnold/G-8863-2011; Fearns, Peter/A-5291-2008; Brando,
Vittorio/A-1321-2008; Roelfsema, Chris/B-1591-2015; Anstee,
Janet/B-1032-2012;
OI Fearns, Peter/0000-0002-2747-9037; Brando, Vittorio/0000-0002-2193-5695;
Phinn, Stuart/0000-0002-2605-6104
FU Australian Research Council (ARC); United States Office of Naval
Research (ONR); Australia's Commonwealth Scientific and Research
Organisation (CSIRO); University of Queensland; ONR; Cooperative
Research Centre; ONR as part of the Coastal Benthic Optical Properties
(COBOP) accelerated research initiative
FX The workshops that resulted in this paper were funded by an Australian
Research Council (ARC) International Linkage Grant (LP) to S. Phinn,
United States Office of Naval Research (ONR) Funds, Australia's
Commonwealth Scientific and Research Organisation (CSIRO), and the
University of Queensland. Dr. Joan Cleveland (ONR) also provided support
funds. The data sets used in this work were produced from two previously
funded large scale international collaborative research projects: (1)
Moreton Bay work was funded through an ARC Linkage Grant to J. Marshall
and S. Phinn at the University of Queensland and a Cooperative Research
Centre grant to S. Phinn and A. Dekker; and (2) Lee Stocking Island work
was funded through ONR as part of the Coastal Benthic Optical Properties
(COBOP) accelerated research initiative. C. Mobley and Z. Lee received
support from ONR. A special thanks to the PHILLS project team at the
Naval Research Laboratory. A number of other scientists were involved in
earlier discussions to design this project: Prof. Peter Mumby, Dr. Steve
Ackleson, and Dr. Curt Davis. Rebecca Edwards at CSIRO provided
editorial and formatting assistance.
NR 54
TC 69
Z9 71
U1 3
U2 77
PU AMER SOC LIMNOLOGY OCEANOGRAPHY
PI WACO
PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710-4446 USA
SN 1541-5856
J9 LIMNOL OCEANOGR-METH
JI Limnol. Oceanogr. Meth.
PD SEP
PY 2011
VL 9
BP 396
EP 425
DI 10.4319/lom.2011.9.396
PG 30
WC Limnology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA 893TE
UT WOS:000300377600004
ER
PT J
AU Bujorianu, M
Fisher, M
Pasareanu, C
AF Bujorianu, Manuela
Fisher, Michael
Pasareanu, Corina
TI Special Issue: Formal Methods in Aerospace Preface
SO ANNALS OF MATHEMATICS AND ARTIFICIAL INTELLIGENCE
LA English
DT Editorial Material
C1 [Fisher, Michael] Univ Liverpool, Dept Comp Sci, Liverpool, Merseyside, England.
[Bujorianu, Manuela] Univ Manchester, Sch Math, Manchester, Lancs, England.
[Pasareanu, Corina] CMU, Mountain View, CA USA.
[Pasareanu, Corina] NASA Ames, Robust Software Engn Grp, Sunnyvale, CA USA.
RP Fisher, M (reprint author), Univ Liverpool, Dept Comp Sci, Liverpool, Merseyside, England.
EM Manuela.Bujorianu@manchester.ac.uk; MFisher@liverpool.ac.uk;
Corina.S.Pasareanu@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1012-2443
J9 ANN MATH ARTIF INTEL
JI Ann. Math. Artif. Intell.
PD SEP
PY 2011
VL 63
IS 1
SI SI
BP 1
EP 3
DI 10.1007/s10472-011-9273-7
PG 3
WC Computer Science, Artificial Intelligence; Mathematics, Applied
SC Computer Science; Mathematics
GA 888RG
UT WOS:000300020800001
ER
PT J
AU Giannakopoulou, D
Bushnell, DH
Schumann, J
Erzberger, H
Heere, K
AF Giannakopoulou, Dimitra
Bushnell, David H.
Schumann, Johann
Erzberger, Heinz
Heere, Karen
TI Formal testing for separation assurance
SO ANNALS OF MATHEMATICS AND ARTIFICIAL INTELLIGENCE
LA English
DT Article
DE Software testing; Verification; Model checking; Automatic test
generation; Clustering; Separation assurance; Air-traffic control
ID TEST-GENERATION; ALGORITHM; SYSTEMS
AB In order to address the rapidly increasing load of air traffic operations, innovative algorithms and software systems must be developed for the next generation air traffic control. Extensive verification of such novel algorithms is key for their adoption by industry. Separation assurance algorithms aim at predicting if two aircraft will get closer to each other than a minimum safe distance; if loss of separation is predicted, they also propose a change of course for the aircraft to resolve this potential conflict. In this paper, we report on our work towards developing an advanced testing framework for separation assurance. Our framework supports automated test case generation and testing, and defines test oracles that capture algorithm requirements. We discuss three different approaches to test-case generation, their application to a separation assurance prototype, and their respective strengths and weaknesses. We also present an approach for statistical analysis of the large numbers of test results obtained from our framework.
C1 [Schumann, Johann] SGT Inc, NASA Ames, Moffett Field, CA USA.
[Giannakopoulou, Dimitra] Carnegie Mellon Univ, NASA Ames, Moffett Field, CA USA.
[Bushnell, David H.] TRACLabs, NASA Ames, Moffett Field, CA USA.
[Erzberger, Heinz] UC Santa Cruz, NASA Ames, Moffett Field, CA USA.
[Heere, Karen] Univ Affiliated Res Ctr, Moffett Field, CA USA.
RP Schumann, J (reprint author), SGT Inc, NASA Ames, Moffett Field, CA USA.
EM dimitra.giannakopoulou@nasa.gov; david.h.bushnell@nasa.gov;
johann.m.schumann@nasa.gov; heinz.erzberger@nasa.gov
FU NextGen program
FX We gratefully acknowledge Peter Mehlitz for his help with
JavaPathfinder, and Todd Farley and the NextGen program for funding this
work.
NR 43
TC 7
Z9 7
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1012-2443
EI 1573-7470
J9 ANN MATH ARTIF INTEL
JI Ann. Math. Artif. Intell.
PD SEP
PY 2011
VL 63
IS 1
SI SI
BP 5
EP 30
DI 10.1007/s10472-011-9224-3
PG 26
WC Computer Science, Artificial Intelligence; Mathematics, Applied
SC Computer Science; Mathematics
GA 888RG
UT WOS:000300020800002
ER
PT J
AU Mahabal, AA
Djorgovski, SG
Drake, AJ
Donalek, C
Graham, MJ
Williams, RD
Chen, Y
Moghaddam, B
Turmon, M
Beshore, E
Larson, S
AF Mahabal, A. A.
Djorgovski, S. G.
Drake, A. J.
Donalek, C.
Graham, M. J.
Williams, R. D.
Chen, Y.
Moghaddam, B.
Turmon, M.
Beshore, E.
Larson, S.
TI Discovery, classification, and scientific exploration of transient
events from the Catalina Real-time Transient Survey
SO BULLETIN OF THE ASTRONOMICAL SOCIETY OF INDIA
LA English
DT Article
DE surveys; galaxies: active; quasars; supernovae; stars: variables: other
ID SKY SURVEY; TELESCOPE; SYSTEM
AB Exploration of the time domain - variable and transient objects and phenomena - is rapidly becoming a vibrant research frontier, touching on essentially every field of astronomy and astrophysics, from the Solar system to cosmology. Time domain astronomy is being enabled by the advent of the new generation of synoptic sky surveys that cover large areas on the sky repeatedly, and generating massive data streams. Their scientific exploration poses many challenges, driven mainly by the need for a real-time discovery, classification, and follow-up of the interesting events. Here we describe the Catalina Real-Time Transient Survey (CRTS), that discovers and publishes transient events at optical wavelengths in real time, thus benefiting the entire community. We describe some of the scientific results to date, and then focus on the challenges of the automated classification and prioritization of transient events. CRTS represents a scientific and a technological testbed and precursor for the larger surveys in the future, including the Large Synoptic Survey Telescope (LSST) and the Square Kilometer Array (SKA).
C1 [Mahabal, A. A.; Djorgovski, S. G.; Drake, A. J.; Donalek, C.; Graham, M. J.; Williams, R. D.; Chen, Y.] CALTECH, Pasadena, CA 91125 USA.
[Djorgovski, S. G.] King Abdulaziz Univ, Jeddah 21413, Saudi Arabia.
[Moghaddam, B.; Turmon, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Beshore, E.; Larson, S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
RP Mahabal, AA (reprint author), CALTECH, 1200 E Calif Bl, Pasadena, CA 91125 USA.
EM aam@astro.caltech.edu
FU NSF [AST-0909182, AST-0407448, OCI-0915473]; Ajax Foundation; NASA
[08-AISR08-0085, 08-FERMI08-0025, NNG05GF22G]; Microsoft Research
WorldWide Telescope team
FX We wish to thank numerous collaborators who have contributed to the
survey and its scientific exploitation so far. CRTS is supported by the
NSF grant AST-0909182, and in part by the Ajax Foundation. The initial
support was provided by the NSF grant AST-0407448, and some of the
software technology development by the NASA grant 08-AISR08-0085. The
analysis of the blazar data was supported in part by the NASA grant
08-FERMI08-0025. Education and public outreach activities are supported
in part by the Microsoft Research WorldWide Telescope team. The CSS
survey is supported by the NASA grant NNG05GF22G. Some VOEvent related
work was supported by NSF grant OCI-0915473. We are grateful to the
staff of Palomar, Keck, and other pertinent observatories for their
expert help during our follow-up observations. Event publishing and
analysis benefits from the tools and services developed by the U. S.
National Virtual Observatory (now Virtual Astronomical Observatory).
NR 27
TC 22
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U1 1
U2 6
PU INDIAN INST ASTROPHYSICS
PI BANGALORE
PA G C ANUPAMA EDITOR, BANGALORE, 560 034, INDIA
SN 0304-9523
J9 B ASTRON SOC INDIA
JI Bull. Astron. Soc. India.
PD SEP
PY 2011
VL 39
IS 3
SI SI
BP 387
EP 408
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 877EW
UT WOS:000299161000006
ER
PT J
AU Bhat, PN
Guiriec, S
AF Bhat, P. N.
Guiriec, S.
TI An overview of the current understanding of Gamma Ray Bursts in the
Fermi era
SO BULLETIN OF THE ASTRONOMICAL SOCIETY OF INDIA
LA English
DT Article
DE gamma-rays: bursts; gamma-rays: observations; gamma-rays: theory
ID AFTERGLOW LIGHT CURVES; EXTERNAL-SHOCK MODEL; LARGE-AREA TELESCOPE;
VERY-HIGH-ENERGY; 28 FEBRUARY 1997; SPECTRAL COMPONENT; PEAK LUMINOSITY;
COSMIC-RAYS; GRB 090510; BATSE OBSERVATIONS
AB Gamma-ray bursts are the most luminous explosions in the Universe, and their origin as well as mechanism are the focus of intense research and debate. More than three decades since their serendipitous discovery, followed by several breakthroughs from space-borne and ground-based observations, they remain one of the most interesting astrophysical phenomena yet to be completely understood. Since the launch of Fermi with its unprecedented energy band width spanning seven decades, the study of gamma-ray burst research has entered a new phase. Here we review the current theoretical understanding and observational highlights of gamma-ray burst astronomy and point out some of the potential promises of multi-wavelength observations in view of the upcoming ground based observational facilities.
C1 [Bhat, P. N.; Guiriec, S.] Univ Alabama, Huntsville, AL 35805 USA.
[Guiriec, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Bhat, PN (reprint author), Univ Alabama, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM Narayana.Bhat@nasa.gov; sylvain.guiriec@nasa.gov
FU Goddard Space Flight Center; NASA
FX SG was supported by an appointment to the NASA Postdoctoral Program at
the Goddard Space Flight Center, administered by Oak Ridge Associated
Universities through a contract with NASA.
NR 170
TC 6
Z9 7
U1 0
U2 3
PU INDIAN INST ASTROPHYSICS
PI BANGALORE
PA G C ANUPAMA EDITOR, BANGALORE, 560 034, INDIA
SN 0304-9523
J9 B ASTRON SOC INDIA
JI Bull. Astron. Soc. India.
PD SEP
PY 2011
VL 39
IS 3
SI SI
BP 471
EP 515
PG 45
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 877EW
UT WOS:000299161000010
ER
PT J
AU Matthews, BL
Srivastava, AN
Iverson, D
Bell, B
Lane, B
AF Matthews, Bryan L.
Srivastava, Ashok N.
Iverson, David
Bell, Bob
Lane, Bill
TI Space Shuttle Main Propulsion System Anomaly Detection: A Case Study
SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE
LA English
DT Article
AB The space shuttle main engine (SSME) is part of the Main Propulsion System (MPS) which is an extremely complex system containing several sub-systems and components, each of which must work precisely in order to achieve a successful mission. A critical component under study is the flow control valve (FCV) which controls the pressure of the gaseous hydrogen between the SSME and the external fuel tank. The FCV has received added attention since a Space Shuttle Mission in November 2008, where it was discovered during the mission that an anomaly had occurred in one of the three FCV's. Subsequent inspection revealed that one FCV cracked during ascent. This type of fault is of high criticality because it can lead to potentially catastrophic gaseous hydrogen leakage. A supervised learning method known as Virtual Sensors (VS), and an unsupervised learning method known as the Inductive Monitoring System (IMS) were used to detect anomalies related to the FCV in the MPS. Both algorithms identify the time of the anomaly in a multi-dimensional time series of temperatures, pressures, and control signals related to the FCV. This discovery corroborates the results of the inspection and also reveals the time at which the anomaly likely occurred. The methods were applied to data obtained from the March 2009 launch of Space Shuttle Discovery to determine whether an anomaly occurred in the same sub-system. According to our models, the FCV sub-system showed nominal behavior during ascent.
RP Matthews, BL (reprint author), NASA, SGT Inc, Ames Res Ctr, Moffett Field, CA 94035 USA.
FU NASA; NASA Engineering and Safety Center (NESC)
FX This research was supported by the Integrated Vehicle Health Management
Project in the NASA Aviation Safety Program and the NASA Engineering and
Safety Center (NESC). The authors thank Melissa Levy for providing the
pre-processed data.
NR 20
TC 0
Z9 0
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0885-8985
J9 IEEE AERO EL SYS MAG
JI IEEE Aerosp. Electron. Syst. Mag.
PD SEP
PY 2011
VL 26
IS 9
BP 4
EP 13
DI 10.1109/MAES.2011.6069898
PG 10
WC Engineering, Aerospace; Engineering, Electrical & Electronic
SC Engineering
GA 844EA
UT WOS:000296729300001
ER
PT J
AU Murphy, CA
Jackson, JM
Sturhahn, W
Chen, B
AF Murphy, Caitlin A.
Jackson, Jennifer M.
Sturhahn, Wolfgang
Chen, Bin
TI Melting and thermal pressure of hcp-Fe from the phonon density of states
SO PHYSICS OF THE EARTH AND PLANETARY INTERIORS
LA English
DT Article
DE Earth's core; Nuclear resonant scattering; High pressure; Phonon density
of states; Melting of iron; Thermal pressure
ID EARTHS INNER-CORE; IN-SITU; IRON; TEMPERATURES; CURVE; SPECTROSCOPY;
GIGAPASCALS; LINDEMANN; EQUATIONS; LAW
AB We directly probed the phonon density of states (DOS) of hexagonal close-packed iron (epsilon-Fe) with high statistical quality between pressures of 30 GPa and 151 GPa using nuclear resonant inelastic X-ray scattering and in situ synchrotron X-ray diffraction experiments at 300 K. From each measured phonon DOS, we determined the vibrational free energy (F(vib),) and mean-square displacement of atoms, (u(2)). The volume dependence of F(vib) is directly related to the vibrational thermal pressure, which we combine with previously reported theoretical values for the electronic and anharmonic thermal pressures to find the total thermal pressure (P(th)). In addition, we obtained the shape of epsilon-Fe's melting curve from the volume dependence of our (u(2)), and anchored it with an experimentally determined melting point to obtain the high-pressure melting behavior of epsilon-Fe. Considering thermal pressure and anharmonic effects, we found epsilon-Fe's melting temperature at the pressure of Earth's core-mantle boundary (P = 135 GPa) to be 3500 +/- 100 K. Extrapolating our melting curve to the pressure of the inner-core boundary (ICB, P = 330 GPa), where Earth's solid inner-core and liquid outer-core are in contact, we determined a melting temperature for epsilon-Fe of 5600 +/- 200 K. Finally, combining this temperature constraint with our P(th), we determined the density of epsilon-Fe under ICB conditions to be 13.50 +/- 0.03 g/cm(3), which is 5.5 +/- 0.2% higher than the seismically inferred density at the ICB. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Murphy, Caitlin A.; Jackson, Jennifer M.; Chen, Bin] CALTECH, Seismol Lab, Pasadena, CA 91125 USA.
[Sturhahn, Wolfgang] Argonne Natl Lab, Adv Photon Source, Argonne, IL 60439 USA.
RP Murphy, CA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM caitlinm@caltech.edu
RI Chen, Bin/A-5980-2008; Murphy, Caitlin/A-9754-2014
OI Murphy, Caitlin/0000-0003-3658-5568
FU Caltech; U.S. D.O.E., O.S., O.B.E.S. [DE-AC02-06CH11357]; COM-PRES [NSF
EAR 06-49658]; [NSF-EAR-0711542]; [NSF-CAREER-0956166]
FX We would like to thank D. Zhang, H. Yavas, and J.K. Wicks for assistance
during the experiments, and NSF-EAR-0711542, NSF-CAREER-0956166, and
Caltech for support of this research. We thank two anonymous reviewers
for their comments that helped to improve our manuscript. Use of the
Advanced Photon Source was supported by the U.S. D.O.E., O.S., O.B.E.S.
(DE-AC02-06CH11357). Sector 3 operations are supported in part by
COM-PRES (NSF EAR 06-49658).
NR 43
TC 16
Z9 17
U1 1
U2 22
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0031-9201
J9 PHYS EARTH PLANET IN
JI Phys. Earth Planet. Inter.
PD SEP
PY 2011
VL 188
IS 1-2
BP 114
EP 120
DI 10.1016/j.pepi.2011.07.001
PG 7
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 848WS
UT WOS:000297086400009
ER
PT J
AU Stecker, FW
AF Stecker, Floyd W.
TI A new limit on Planck scale Lorentz violation from gamma-ray burst
polarization
SO ASTROPARTICLE PHYSICS
LA English
DT Article
DE Lorentz invariance; Quantum gravity; gamma-Rays; gamma-Ray bursts
ID EMISSION; SPECTRA; ENERGY; PROBE
AB Constraints on possible Lorentz invariance violation (LIV) to first order in E/M(planck) for photons in the framework of effective field theory (EFT) are discussed, taking cosmological factors into account. Then, using the reported detection of polarized soft gamma-ray emission from the gamma-ray burst GRB041219a that is indicative of an absence of vacuum birefringence, together with a very recent improved method for estimating the redshift of the burst, we derive constraints on the dimension 5 Lorentz violating modification to the Lagrangian of an effective local QFT for QED. Our new constraints are more than five orders of magnitude better than recent constraints from observations of the Crab Nebula. We obtain the upper limit on the Lorentz violating dimension 5 EFT parameter vertical bar xi vertical bar of 2.4 x 10(-15), corresponding to a constraint on the dimension 5 standard model extension parameter, k(left perpendicularVright perpendicular)(left perpendicular5right perpendicular) <= 4.2 x 10(-34) GeV(-1). Published by Elsevier B.V.
C1 NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Stecker, FW (reprint author), NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM floyd.w.stecker@nasa.gov
RI Stecker, Floyd/D-3169-2012
NR 24
TC 21
Z9 21
U1 0
U2 2
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-6505
J9 ASTROPART PHYS
JI Astropart Phys.
PD SEP
PY 2011
VL 35
IS 2
BP 95
EP 97
DI 10.1016/j.astropartphys.2011.06.007
PG 3
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 839YW
UT WOS:000296406400007
ER
PT J
AU Vargas, M
Feo, A
AF Vargas, Mario
Feo, Alex
TI Deformation and Breakup of Water Droplets near an Airfoil Leading Edge
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT AIAA/GNC/AFM/MST/ASC/ASE Conference
CY AUG 02-05, 2010
CL Toronto, CANADA
SP AIAA, GNC, AFM, MST, ASC, ASE
AB This work presents the results of an experimental study on droplet deformation and breakup near the leading edge of an airfoil. The experiment was conducted in the rotating rig test cell at the National Institute of Aerospace Technology (INTA) in Madrid, Spain. An airfoil model placed at the end of the rotating arm was moved at speeds of 50 to 90 m/s. A monosized droplet generator was employed to produce droplets that were allowed to fall from above, perpendicular to the path of the airfoil at a given location. High-speed imaging was employed to observe the interaction between the droplets and the airfoil. The high-speed imaging allowed observation of droplet deformation and breakup as the droplet approached the airfoil near the stagnation line. A tracking software program was used to measure, from the high-speed movies, the horizontal and vertical displacement of the droplet against time. The velocity, acceleration, Weber number, Bond number, Reynolds number, and drag coefficients were calculated along the path of a given droplet from the beginning of the deformation to the breakup and/or hitting of the airfoil. Results are presented for droplets with a diameter of 490 mu m at airfoil speeds of 50, 60, 70, 80, and 90 m/s.
C1 [Vargas, Mario] NASA, John H Glenn Res Ctr Lewis Field, Icing Branch, Cleveland, OH 44135 USA.
[Feo, Alex] Natl Inst Aerosp Technol INTA, Expt Aerodynam Dept, Madrid 28850, Spain.
RP Vargas, M (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Icing Branch, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
NR 13
TC 2
Z9 3
U1 1
U2 3
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 SEP-OCT
PY 2011
VL 48
IS 5
BP 1749
EP 1765
DI 10.2514/1.C031363
PG 17
WC Engineering, Aerospace
SC Engineering
GA 831TR
UT WOS:000295754500025
ER
PT J
AU Berton, JJ
Guynn, MD
AF Berton, Jeffrey J.
Guynn, Mark D.
TI Multi-Objective Optimization of a Turbofan for an Advanced, Single-Aisle
Transport
SO JOURNAL OF AIRCRAFT
LA English
DT Article
AB Considerable interest surrounds the design of the next generation of single-aisle commercial transports in the Boeing 737 and Airbus A320 class. Aircraft designers will depend on advanced, next-generation turbofan engines to power these airplanes. The focus of this study is to apply single- and multi-objective optimization algorithms to the conceptual design of ultrahigh bypass turbofan engines for this class of aircraft, using NASA's Subsonic Fixed Wing Project metrics as multidisciplinary objectives for optimization. The independent design variables investigated include three continuous variables: sea level static thrust, wing reference area, and aerodynamic design point fan pressure ratio, and four discrete variables: overall pressure ratio, fan drive system architecture (i.e., direct- or gear-driven), bypass nozzle architecture (i.e., fixed- or variable geometry), and the high- and low-pressure compressor work split. Ramp weight, fuel burn, noise, and emissions are the parameters treated as dependent objective functions. These optimized solutions provide insight to the ultrahigh bypass engine design process and provide information to NASA program management to help guide its technology development efforts.
C1 [Berton, Jeffrey J.] NASA Glenn Res Ctr, Multidisciplinary Design Anal & Optimizat Branch, Cleveland, OH 44135 USA.
[Guynn, Mark D.] NASA Langley Res Ctr, Aeronaut Syst Anal Branch, Hampton, VA 23681 USA.
RP Berton, JJ (reprint author), NASA Glenn Res Ctr, Multidisciplinary Design Anal & Optimizat Branch, MS 5-11, Cleveland, OH 44135 USA.
NR 29
TC 1
Z9 1
U1 1
U2 12
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 SEP-OCT
PY 2011
VL 48
IS 5
BP 1795
EP 1805
DI 10.2514/1.C031333
PG 11
WC Engineering, Aerospace
SC Engineering
GA 831TR
UT WOS:000295754500029
ER
PT J
AU Sigler, MF
Renner, M
Danielson, SL
Eisner, LB
Lauth, RR
Kuletz, KJ
Logerwell, EA
Hunt, GL
AF Sigler, Michael F.
Renner, Martin
Danielson, Seth L.
Eisner, Lisa B.
Lauth, Robert R.
Kuletz, Kathy J.
Logerwell, Elizabeth A.
Hunt, George L., Jr.
TI Fluxes, Fins, and Feathers Relationships Among the Bering, Chukchi, and
Beaufort Seas in a Time of Climate Change
SO OCEANOGRAPHY
LA English
DT Article
ID WESTERN ARCTIC-OCEAN; BOWHEAD WHALE DISTRIBUTION; MACKENZIE SHELF
ESTUARY; ALASKA COASTAL CURRENT; MARINE ECOSYSTEM; FISH ASSEMBLAGES;
WALLEYE POLLOCK; LATE SUMMER; WATER MASS; FOOD WEBS
AB Ocean currents, water masses, and seasonal sea ice formation determine linkages among and barriers between the biotas of the Bering, Chukchi, and Beaufort Seas. The Bering Sea communicates with the Chukchi and Beaufort Seas via northward advection of water, nutrients, and plankton through Bering Strait. However, continuity of the ocean's physical properties is modulated by regional differences in heat, salt, and sea ice budgets, in particular, along the meridional gradient. Using summer density data from zooplankton, fish (bottom and surface trawl), and seabird surveys, we define three biogeographic provinces: the Eastern Bering Shelf Province (the eastern Bering Sea shelf south of Saint Lawrence Island), the Chirikov-Chukchi Province (the eastern Bering Sea shelf north of Saint Lawrence Island [Chirikov Basin] and Chukchi Sea), and the Beaufort Sea Province. Regional differences in summer distributions of biota largely reflect the underlying oceanography. Climate warming will reduce the duration and possibly the extent of seasonal ice cover in the Eastern Bering Shelf Province, but this warming may not lead to increased abundance of some subarctic species because seasonal ice cover and cold (< 2 degrees C) bottom waters on the Bering shelf form a barrier to the northward migration of subarctic bottom fish species typical of the southeastern Bering Sea. While Arctic species that are dependent upon the summer extent of sea ice face an uncertain future, other Arctic species' resilience to a changing climate will be derived from waters that continue to freeze each winter.
C1 [Sigler, Michael F.; Eisner, Lisa B.] Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, NOAA, Juneau, AK USA.
[Renner, Martin; Hunt, George L., Jr.] Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98195 USA.
[Danielson, Seth L.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Fairbanks, AK USA.
[Lauth, Robert R.; Logerwell, Elizabeth A.] NMFS, Alaska Fisheries Sci Ctr, NOAA, Seattle, WA USA.
[Kuletz, Kathy J.] US Fish & Wildlife Serv, Anchorage, AK USA.
RP Sigler, MF (reprint author), Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, NOAA, Juneau, AK USA.
EM mike.sigler@noaa.gov
OI Hunt, George/0000-0001-8709-2697
FU NSF [ARC-0908262]; NOAA/PMEL Eco-FOCI
FX Several recent scientific programs, including BEST, BSIERP, BASIS,
NPCREP, RUSALCA, and SBI have contributed to our knowledge of these
regions. We thank John Piatt and Gary Drew for developing the North
Pacific Pelagic Seabird Database and Ivonne Ortiz and Ed Farley for the
fish diet data used to classify foraging guilds. We thank Peter Boveng,
Ken Coyle, Ed Farley, Franz Mueter, Jeff Napp, Lori Quakenbush, Bill
Sydeman, and an anonymous reviewer for comments on an earlier version of
this article. The participation of G. Hunt and M. Renner was supported
by NSF Grant ARC-0908262. We thank K. Aagaard, P. Stabeno, and T.
Weingartner for use of moored data records. NOAA mooring M2 is supported
by the NOAA/PMEL Eco-FOCI program. This is BEST-BSIERP publication no.
24 and NPRB publication no. 301. This is a publication of the IMBER
Regional Program, Ecosystem Studies of Sub-Arctic Seas (ESSAS). The
findings and conclusions of the paper are those of the authors and do
not necessarily represent the views of the National Marine Fisheries
Service.
NR 106
TC 32
Z9 33
U1 4
U2 40
PU OCEANOGRAPHY SOC
PI ROCKVILLE
PA P.O. BOX 1931, ROCKVILLE, MD USA
SN 1042-8275
J9 OCEANOGRAPHY
JI Oceanography
PD SEP
PY 2011
VL 24
IS 3
SI SI
BP 250
EP 265
PG 16
WC Oceanography
SC Oceanography
GA 826ZS
UT WOS:000295394700032
ER
PT J
AU Feynman, J
Ruzmaikin, A
AF Feynman, J.
Ruzmaikin, A.
TI The Sun's Strange Behavior: Maunder Minimum or Gleissberg Cycle?
SO SOLAR PHYSICS
LA English
DT Article
DE Observations; Solar cycle
ID WIND HELIUM ABUNDANCE; CORONAL MAGNETIC-FIELD; SOLAR-ACTIVITY; GRAND
MINIMA; RING-CURRENT; TIME SCALES; DYNAMO; AURORA; SPEED
AB During the last few years the Sun and solar wind have shown a behavior that was so unexpected that the phenomena was described as "the strange solar minimum". It has been speculated that the 23/24 solar cycle minimum may have indicated the onset of a Maunder-Minimum-type Grand Minimum. Here we review what is known from 1500 years of proxy data about Maunder-type Grand Minima and the minima of the cyclic Centennial Gleissberg variations. We generate criteria that distinguish between the two types of event. Applying these criteria to the observed solar terrestrial data we conclude that the unexpected behavior began well before the solar cycle 23/24 minimum. The data do not support the Maunder Minimum conjecture. However, the behavior can be understood as a minimum of the Centennial Gleissberg Cycle that previously minimized in the beginning of the 20th century. We conclude that the Centennial Gleissberg Cycle is a persistent variation that has been present 80% of the time during the last 1500 years and should be explained by solar dynamo theory.
C1 [Feynman, J.; Ruzmaikin, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Ruzmaikin, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM Joan.Feynman@jpl.nasa.gov; Alexander.Ruzmaikin@jpl.nasa.gov
FU Jet Propulsion Laboratory of the California Institute of Technology
under National Aeronautics and Space Administration
FX We thank Ruth Skoug for discussion of alpha/p ratio. This work was
supported in part by the Jet Propulsion Laboratory of the California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration.
NR 52
TC 24
Z9 24
U1 0
U2 8
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD SEP
PY 2011
VL 272
IS 2
BP 351
EP 363
DI 10.1007/s11207-011-9828-0
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 831NX
UT WOS:000295739500008
ER
PT J
AU Dahlgren, H
Sundberg, T
Collier, AB
Koen, E
Meyer, S
AF Dahlgren, Hanna
Sundberg, Torbjorn
Collier, Andrew B.
Koen, Etienne
Meyer, Stephen
TI Solar flares detected by the new narrowband VLF receiver at SANAE IV
SO SOUTH AFRICAN JOURNAL OF SCIENCE
LA English
DT Article
ID D-REGION ENHANCEMENTS; IONOSPHERIC PARAMETERS; PROPAGATION; AMPLITUDE;
PHASE
AB A narrowband receiver was installed at the SANAE IV base in Antarctica to monitor specific very low frequency (VLF) radio signals from transmitters around the world. VLF waves propagating through the Earth-Ionosphere Waveguide are excellent probes of the varying properties of the lower region of the ionosphere. This paper describes the set-up of the narrowband system and demonstrates its capabilities with data from a set of solar flares on 08 February and 12 February 2010.
C1 [Dahlgren, Hanna] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
[Dahlgren, Hanna; Sundberg, Torbjorn; Koen, Etienne] Royal Inst Technol, Stockholm, Sweden.
[Dahlgren, Hanna] Boston Univ, Dept Elect & Comp Engn, Boston, MA 02215 USA.
[Sundberg, Torbjorn] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Collier, Andrew B.; Koen, Etienne; Meyer, Stephen] SANSA Space Sci, Hermanus, South Africa.
[Collier, Andrew B.; Meyer, Stephen] Univ KwaZulu Natal, Durban, South Africa.
RP Dahlgren, H (reprint author), Boston Univ, Ctr Space Phys, 725 Commonwealth Ave,Room 408, Boston, MA 02215 USA.
EM hannad@bu.edu
RI Collier, Andrew/H-3752-2011; Koen, Etienne/E-8947-2012
OI Koen, Etienne/0000-0002-4030-1014
FU UltraMSK
FX We are grateful to the SANAE IV 2009-2010 relief team, and especially
Daleen Koch, Mar lie van Zyl and S.J. van der Merwe for valuable help on
the installation of the system. We wish to thank the developer of
UltraMSK, James Brundell, for discussions and support. We also thank
Rory Meyer and James Hayes for operation and maintenance of the system
during the long Antarctic winter. GOES data was provided by the Space
Weather Prediction Center (Boulder, CO, USA) and the National Oceanic
and Atmospheric Administration (NOAA), US Department of Commerce.
NR 13
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PI LYNWOOD RIDGE
PA PO BOX 72135, LYNWOOD RIDGE 0040, SOUTH AFRICA
SN 0038-2353
J9 S AFR J SCI
JI S. Afr. J. Sci.
PD SEP-OCT
PY 2011
VL 107
IS 9-10
BP 39
EP 46
DI 10.4102/sajs.v107i9/10.491
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 843RM
UT WOS:000296690100012
ER
PT J
AU Emslie, AG
Dennis, BR
Hudson, H
Lin, RP
AF Emslie, A. Gordon
Dennis, Brian R.
Hudson, Hugh
Lin, Robert P.
TI High-Energy Aspects of Solar Flares: A RHESSI-inspired monograph Preface
SO SPACE SCIENCE REVIEWS
LA English
DT Editorial Material
C1 [Hudson, Hugh] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Emslie, A. Gordon] Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA.
[Dennis, Brian R.] NASA, Solar Phys Lab Code 671, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lin, Robert P.] US Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Lin, Robert P.] US Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Lin, Robert P.] Kyung Hee Univ, Sch Space Res, Seoul, South Korea.
RP Hudson, H (reprint author), Univ Calif Berkeley, Berkeley, CA 94720 USA.
EM hhudson@ssl.berkeley.edu
RI Dennis, Brian/C-9511-2012
NR 0
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J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2011
VL 159
IS 1-4
BP 1
EP 2
DI 10.1007/s11214-011-9815-7
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 831NM
UT WOS:000295738400001
ER
PT J
AU Dennis, BR
Emslie, AG
Hudson, HS
AF Dennis, B. R.
Emslie, A. G.
Hudson, H. S.
TI Overview of the Volume
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Sun: flares; Sun: X-rays; Sun: acceleration; Sun: energetic particles
ID RETURN CURRENT SYSTEMS; X-RAY BREMSSTRAHLUNG;
SOLAR-SPECTROSCOPIC-IMAGER; ALFVEN WAVES; ENERGY PARTITION; FLARE/CME
EVENTS; BEAM; ACCELERATION; ELECTRONS; RHESSI
AB In this introductory chapter, we provide a brief summary of the successes and remaining challenges in understanding the solar flare phenomenon and its attendant implications for particle acceleration mechanisms in astrophysical plasmas. We also provide a brief overview of the contents of the other chapters in this volume, with particular reference to the well-observed flare of 2002 July 23.
C1 [Dennis, B. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Emslie, A. G.] Western Kentucky Univ, Bowling Green, KY 42101 USA.
[Hudson, H. S.] UC Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Dennis, BR (reprint author), NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
EM brian.r.dennis@nasa.gov; emslieg@wku.edu; hhudson@ssl.berkeley.edu
RI Dennis, Brian/C-9511-2012
FU NASA [NAS5-98033, NNX10AT78G]
FX H. Hudson was supported by NASA under contract NAS5-98033 for RHESSI. A.
G. Emslie was supported by NASA Grant NNX10AT78G.
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JI Space Sci. Rev.
PD SEP
PY 2011
VL 159
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BP 3
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PG 15
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SC Astronomy & Astrophysics
GA 831NM
UT WOS:000295738400002
ER
PT J
AU Fletcher, L
Dennis, BR
Hudson, HS
Krucker, S
Phillips, K
Veronig, A
Battaglia, M
Bone, L
Caspi, A
Chen, Q
Gallagher, P
Grigis, PT
Ji, H
Liu, W
Milligan, RO
Temmer, M
AF Fletcher, L.
Dennis, B. R.
Hudson, H. S.
Krucker, S.
Phillips, K.
Veronig, A.
Battaglia, M.
Bone, L.
Caspi, A.
Chen, Q.
Gallagher, P.
Grigis, P. T.
Ji, H.
Liu, W.
Milligan, R. O.
Temmer, M.
TI An Observational Overview of Solar Flares
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Sun
ID HARD X-RAY; CORONAL MASS EJECTION; WHITE-LIGHT FLARES; PHOTOSPHERIC
MAGNETIC-FIELD; HIGH TIME RESOLUTION; LOOP RADIATIVE HYDRODYNAMICS;
QUIET ACTIVE REGIONS; 2003 OCTOBER 29; GENTLE CHROMOSPHERIC EVAPORATION;
ENERGETIC PARTICLE EVENTS
AB We present an overview of solar flares and associated phenomena, drawing upon a wide range of observational data primarily from the RHESSI era. Following an introductory discussion and overview of the status of observational capabilities, the article is split into topical sections which deal with different areas of flare phenomena (footpoints and ribbons, coronal sources, relationship to coronal mass ejections) and their interconnections. We also discuss flare soft X-ray spectroscopy and the energetics of the process. The emphasis is to describe the observations from multiple points of view, while bearing in mind the models that link them to each other and to theory. The present theoretical and observational understanding of solar flares is far from complete, so we conclude with a brief discussion of models, and a list of missing but important observations.
C1 [Fletcher, L.; Battaglia, M.] Univ Glasgow, Sch Phys & Astron, Astron & Astrophys Grp, Glasgow G12 8QQ, Lanark, Scotland.
[Dennis, B. R.; Liu, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Milligan, R. O.] Queens Univ Belfast, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland.
[Hudson, H. S.; Krucker, S.; Caspi, A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Phillips, K.; Bone, L.] Mullard Space Sci Lab, Dorking RH5 CNT, Surrey, England.
[Veronig, A.] Graz Univ, Inst Geophys Astrophys & Meteorol, A-8010 Graz, Austria.
[Temmer, M.] Graz Univ, Inst Phys, A-8010 Graz, Austria.
[Chen, Q.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Gallagher, P.] Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland.
[Grigis, P. T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ji, H.] Purple Mt Observ, Nanjing 210008, Peoples R China.
[Ji, H.] New Jersey Inst Technol, Big Bear Solar Observ, Big Bear City, CA 92314 USA.
[Liu, W.] Stanford Lockheed Inst Space Res, Stanford, CA 94305 USA.
RP Fletcher, L (reprint author), Univ Glasgow, Sch Phys & Astron, Astron & Astrophys Grp, Glasgow G12 8QQ, Lanark, Scotland.
EM lyndsay.fletcher@glasgow.ac.uk
RI Dennis, Brian/C-9511-2012; Veronig, Astrid/B-8422-2009; Gallagher,
Peter/C-7717-2011;
OI Gallagher, Peter/0000-0001-9745-0400; Battaglia,
Marina/0000-0003-1438-9099; Caspi, Amir/0000-0001-8702-8273; Temmer,
Manuela/0000-0003-4867-7558
FU UK STFC [ST/F0026371]; EU [MTRN-CT-2006-035484]; Leverhulme Foundation
[F/00 179/AY]; NSFC [10833007W]; NASA at Goddard Space Flight Center;
Hinode SOT [NNM07AA01C]; NASA [NAS5-98033, NAG5-12878, NNX08AJ18G];
Austrian Science Fund (FWF) [P20867-N16, P20145-N16]
FX The authors would collectively like to acknowledge the work by the many
instrument teams and software teams, whose sustained efforts over the
years have made this kind of multiwavelength analysis possible. The
chief architects of and major contributors to the Solarsoft library
deserve particular thanks (Sam Freeland, Richard Schwartz, William
Thompson, Kim Tolbert and Dominic Zarro). L. F. would like to
acknowledge financial support from the UK STFC (Rolling grant
ST/F0026371), the EU's SOLAIRE Research and Training Network
(MTRN-CT-2006-035484) and L. F. and M. B. also acknowledge the support
of the Leverhulme Foundation (Grant F/00 179/AY). The work of H. Ji was
supported by NSFC 10833007W. W. Liu was partly supported by an
appointment to the NASA Postdoctoral Program at Goddard Space Flight
Center, administered by Oak Ridge Associated Universities through a
contract with NASA. Partial support to W. Liu's work was also provided
by Hinode SOT contract NNM07AA01C. A. Caspi, H. Hudson, and S. Krucker
were supported by NASA under contract NAS5-98033 and grants NAG5-12878
and NNX08AJ18G. A. V. and M. T. acknowledge the Austrian Science Fund
(FWF) projects no. P20867-N16 and P20145-N16. We are grateful to several
insitutions for granting permission for the use of previously published
figures. In addition to those noted in figure captions, we also
acknowledge the following figures from A&A, reproduced with permission
(c) ESO: Fig. 12 (Mandrini et al. 1995, 303, 927); Fig. 18 (Miklenic et
al. 2007, 461, 697); Fig. 34 (Mann et al. 2003, 400, 329). The following
figures are reproduced with kind permission from Springer
Science+Business Media: Fig. 19 (Lindsey and Donea 2008); Fig. 27
(Krucker et al. 2008a); and Fig. 29 (Gallagher et al. 2002).
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JI Space Sci. Rev.
PD SEP
PY 2011
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BP 19
EP 106
DI 10.1007/s11214-010-9701-8
PG 88
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 831NM
UT WOS:000295738400003
ER
PT J
AU Holman, GD
Aschwanden, MJ
Aurass, H
Battaglia, M
Grigis, PC
Kontar, EP
Liu, W
Saint-Hilaire, P
Zharkova, VV
AF Holman, G. D.
Aschwanden, M. J.
Aurass, H.
Battaglia, M.
Grigis, P. C.
Kontar, E. P.
Liu, W.
Saint-Hilaire, P.
Zharkova, V. V.
TI Implications of X-ray Observations for Electron Acceleration and
Propagation in Solar Flares
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Sun: flares; Sun: X-rays; Gamma rays; Sun: radio radiation
ID 2002 JULY 23; LOW-ENERGY CUTOFFS; HIGH TIME RESOLUTION; MAGNETIC
RECONNECTION; PARTICLE-ACCELERATION; SPECTRAL EVOLUTION; CHROMOSPHERIC
EVAPORATION; IMPULSIVE PHASE; NONTHERMAL ELECTRONS; RETURN CURRENTS
AB High-energy X-rays and gamma-rays from solar flares were discovered just over fifty years ago. Since that time, the standard for the interpretation of spatially integrated flare X-ray spectra at energies above several tens of keV has been the collisional thick-target model. After the launch of the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) in early 2002, X-ray spectra and images have been of sufficient quality to allow a greater focus on the energetic electrons responsible for the X-ray emission, including their origin and their interactions with the flare plasma and magnetic field. The result has been new insights into the flaring process, as well as more quantitative models for both electron acceleration and propagation, and for the flare environment with which the electrons interact. In this article we review our current understanding of electron acceleration, energy loss, and propagation in flares. Implications of these new results for the collisional thick-target model, for general flare models, and for future flare studies are discussed.
C1 [Holman, G. D.; Liu, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Aschwanden, M. J.] Org ADBS, Lockheed Martin Adv Technol Ctr, Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Aurass, H.] Astrophys Inst Potsdam, Potsdam, Germany.
[Battaglia, M.; Kontar, E. P.] Univ Glasgow, Dept Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
[Grigis, P. C.] Harvard Smithsonian Ctr Astrophys P 148, Cambridge, MA 02138 USA.
[Saint-Hilaire, P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA USA.
[Zharkova, V. V.] Univ Bradford, Dept Comp & Math, Bradford BD7 1DP, W Yorkshire, England.
RP Holman, GD (reprint author), NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
EM Gordon.D.Holman@nasa.gov
RI Kontar, Eduard/B-7897-2008; Holman, Gordon/C-9548-2012
OI Battaglia, Marina/0000-0003-1438-9099; Kontar,
Eduard/0000-0002-8078-0902;
FU NASA [NAS5-98033, NAS5-38099, NNM07AB07C]; University of California,
Berkeley [SA2241-26308PG]; German Space Agency Deutsches Zentrum fur
Luft- und Raumfahrt (DLR) [50 QL 0001]; Leverhulme Trust; Science and
Technology Facilities Council
FX We thank the chapter editor, Brian Dennis, and the two reviewers for
comments that led to many improvements to the text. G. D. H.
acknowledges support from the RHESSI Project and NASA's Heliophysics
Guest Investigator Program. M.J.A. acknowledges support from NASA
contract NAS5-98033 of the RHESSI mission through University of
California, Berkeley (subcontract SA2241-26308PG), and NASA contract
NAS5-38099 for the TRACE mission. H. A. acknowledges support by the
German Space Agency Deutsches Zentrum fur Luft- und Raumfahrt (DLR),
under grant No. 50 QL 0001. M. B. acknowledges support by the Leverhulme
Trust. P. C. G. acknowledges support from NASA contract NNM07AB07C. EPK
acknowledges support from a Science and Technology Facilities Council
Advanced Fellowship. NASA's Astrophysics Data System Bibliographic
Services have been an invaluable tool in the writing of this article.
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PD SEP
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BP 107
EP 166
DI 10.1007/s11214-010-9680-9
PG 60
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 831NM
UT WOS:000295738400004
ER
PT J
AU White, SM
Benz, AO
Christe, S
Farnik, F
Kundu, MR
Mann, G
Ning, Z
Raulin, JP
Silva-Valio, AVR
Saint-Hilaire, P
Vilmer, N
Warmuth, A
AF White, S. M.
Benz, A. O.
Christe, S.
Farnik, F.
Kundu, M. R.
Mann, G.
Ning, Z.
Raulin, J. -P.
Silva-Valio, A. V. R.
Saint-Hilaire, P.
Vilmer, N.
Warmuth, A.
TI The Relationship Between Solar Radio and Hard X-ray Emission
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Sun: radio radiation; Sun: X-rays; Sun: flares; Sun: energetic particles
ID CORONAL MASS EJECTION; 03 NOVEMBER 2003; GAMMA-RAY; GYROSYNCHROTRON
EMISSION; ELECTRON ACCELERATION; MICROWAVE OBSERVATIONS;
PARTICLE-ACCELERATION; NONTHERMAL ELECTRONS; SYNCHROTRON EMISSION;
RHESSI MICROFLARES
AB This review discusses the complementary relationship between radio and hard Xray observations of the Sun using primarily results from the era of the Reuven Ramaty High Energy Solar Spectroscopic Imager satellite. A primary focus of joint radio and hard X-ray studies of solar flares uses observations of nonthermal gyrosynchrotron emission at radio wavelengths and bremsstrahlung hard X-rays to study the properties of electrons accelerated in the main flare site, since it is well established that these two emissions show very similar temporal behavior. A quantitative prescription is given for comparing the electron energy distributions derived separately from the two wavelength ranges: this is an important application with the potential for measuring the magnetic field strength in the flaring region, and reveals significant differences between the electrons in different energy ranges. Examples of the use of simultaneous data from the two wavelength ranges to derive physical conditions are then discussed, including the case of microflares, and the comparison of images at radio and hard X-ray wavelengths is presented. There have been puzzling results obtained from observations of solar flares at millimeter and submillimeter wavelengths, and the comparison of these results with corresponding hard X-ray data is presented. Finally, the review discusses the association of hard X-ray releases with radio emission at decimeter and meter wavelengths, which is dominated by plasma emission (at lower frequencies) and electron cyclotron maser emission (at higher frequencies), both coherent emission mechanisms that require small numbers of energetic electrons. These comparisons show broad general associations but detailed correspondence remains more elusive.
C1 [White, S. M.] AFRL, Space Vehicles Directorate, Albuquerque, NM 87123 USA.
[Benz, A. O.] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Christe, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Farnik, F.] Acad Sci Czech Republic, Inst Astron, CS-25165 Ondrejov, Czech Republic.
[White, S. M.; Kundu, M. R.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Mann, G.; Warmuth, A.] Astrophys Inst Potsdam, D-14482 Potsdam, Germany.
[Ning, Z.] Purple Mt Observ, Nanjing 210008, Peoples R China.
[Raulin, J. -P.; Silva-Valio, A. V. R.] Ctr Radio Astron & Astrofis Mackenzie, BR-01302907 Sao Paulo, Brazil.
[Saint-Hilaire, P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Vilmer, N.] Observ Paris, LESIA CNRS UMR 8109, F-92190 Meudon, France.
RP White, SM (reprint author), AFRL, Space Vehicles Directorate, Albuquerque, NM 87123 USA.
EM Stephen.White@kirtland.af.mil
RI Farnik, Frantisek/G-9010-2014; Christe, Steven/D-4648-2012; Valio,
Adriana/I-2531-2012; 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013
OI Christe, Steven/0000-0001-6127-795X; Valio, Adriana/0000-0002-1671-8370;
FU University of Maryland by NSF [ATM 02-33907]; NASA [NAG 5-12860,
NNG-05-GI91G, NNX-06-AC18G]
FX This paper is dedicated to the memory of Mukul Kundu, who passed away
during revision. Mukul was a pioneer of solar radiophysics and one of
the first to realize the close association of radio and hard X-ray
emission and the importance of this relationship for advancing our
understanding of flares. We thank the organizers of the RHESSI Workshop
series (Gordon Emslie and Brian Dennis in particular) and the local
organizing committees for each of the workshops for their hospitality
and great efforts to make the workshop series such a success. Two
referees and Bob Lin provided thoughtful comments that helped to improve
the manuscript. Research using RHESSI and radio observations was
supported at the University of Maryland by NSF grant ATM 02-33907 and
NASA contracts NAG 5-12860, NNG-05-GI91G, and NNX-06-AC18G.
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 831NM
UT WOS:000295738400006
ER
PT J
AU Hannah, IG
Hudson, HS
Battaglia, M
Christe, S
Kasparova, J
Krucker, S
Kundu, MR
Veronig, A
AF Hannah, I. G.
Hudson, H. S.
Battaglia, M.
Christe, S.
Kasparova, J.
Krucker, S.
Kundu, M. R.
Veronig, A.
TI Microflares and the Statistics of X-ray Flares
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Sun; Flares; X-rays
ID CORONAL MASS EJECTIONS; WAITING-TIME DISTRIBUTION; REGION TRANSIENT
BRIGHTENINGS; ENERGETIC PARTICLE EVENTS; NONTHERMAL RADIO-EMISSION;
SOLAR ACTIVE REGIONS; FREQUENCY-DISTRIBUTIONS; QUIET SUN; CHROMOSPHERIC
EVAPORATION; NANOFLARE STATISTICS
AB This review surveys the statistics of solar X-ray flares, emphasising the new views that RHESSI has given us of the weaker events (the microflares). The new data reveal that these microflares strongly resemble more energetic events in most respects; they occur solely within active regions and exhibit high-temperature/nonthermal emissions in approximately the same proportion as major events. We discuss the distributions of flare parameters (e. g., peak flux) and how these parameters correlate, for instance via the Neupert effect. We also highlight the systematic biases involved in intercomparing data representing many decades of event magnitude. The intermittency of the flare/microflare occurrence, both in space and in time, argues that these discrete events do not explain general coronal heating, either in active regions or in the quiet Sun.
C1 [Hannah, I. G.; Battaglia, M.] Univ Glasgow, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
[Hudson, H. S.; Krucker, S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christe, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kasparova, J.] Astron Ustav AV CR, VVI, Ondrejov 25165, Czech Republic.
[Kundu, M. R.] Univ Maryland, Dept Astron, College Pk, MD 20740 USA.
[Veronig, A.] Graz Univ, Inst Phys IGAM, A-8010 Graz, Austria.
RP Hannah, IG (reprint author), Univ Glasgow, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
EM iain@astro.gla.ac.uk
RI Hannah, Iain/F-1972-2011; Christe, Steven/D-4648-2012; Veronig,
Astrid/B-8422-2009; Kasparova, Jana/G-9024-2014;
OI Hannah, Iain/0000-0003-1193-8603; Battaglia, Marina/0000-0003-1438-9099;
Christe, Steven/0000-0001-6127-795X
FU NASA [NAS 5-98033]; STFC; European Commission [MTRN-CT-2006-035484]; GA
CR [205/06/P135, AV0Z10030501]
FX The authors thank the editor (B. R. Dennis) and the two referees for
providing many constructive comments that have greatly improved this
review. IGH would also like to thank the Glasgow SSH (Solar Self Help)
group for their comments. This work is financially supported through
NASA contract NAS 5-98033, an STFC rolling grant, and by the European
Commission through the SOLAIRE Network (MTRN-CT-2006-035484), and all
are gratefully acknowledged. JK acknowledges support from Grant
205/06/P135 of the GA CR and the research plan AV0Z10030501.
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SC Astronomy & Astrophysics
GA 831NM
UT WOS:000295738400007
ER
PT J
AU Kontar, EP
Brown, JC
Emslie, AG
Hajdas, W
Holman, GD
Hurford, GJ
Kasparova, J
Mallik, PCV
Massone, AM
McConnell, ML
Piana, M
Prato, M
Schmahl, EJ
Suarez-Garcia, E
AF Kontar, E. P.
Brown, J. C.
Emslie, A. G.
Hajdas, W.
Holman, G. D.
Hurford, G. J.
Kasparova, J.
Mallik, P. C. V.
Massone, A. M.
McConnell, M. L.
Piana, M.
Prato, M.
Schmahl, E. J.
Suarez-Garcia, E.
TI Deducing Electron Properties from Hard X-ray Observations
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Sun: flares; Sun: X-rays; Sun: acceleration; Sun: energetic particles
ID 2002 JULY 23; LOW-ENERGY CUTOFFS; SOLAR-SPECTROSCOPIC-IMAGER; FLUX
SPECTRA; THICK-TARGET; PHOTOSPHERIC ALBEDO; GAMMA-RAYS; BREMSSTRAHLUNG
EMISSION; NONTHERMAL ELECTRONS; IMAGING SPECTROSCOPY
AB X-radiation from energetic electrons is the prime diagnostic of flare-accelerated electrons. The observed X-ray flux (and polarization state) is fundamentally a convolution of the cross-section for the hard X-ray emission process(es) in question with the electron distribution function, which is in turn a function of energy, direction, spatial location and time. To address the problems of particle propagation and acceleration one needs to infer as much information as possible on this electron distribution function, through a deconvolution of this fundamental relationship. This review presents recent progress toward this goal using spectroscopic, imaging and polarization measurements, primarily from the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI). Previous conclusions regarding the energy, angular (pitch angle) and spatial distributions of energetic electrons in solar flares are critically reviewed. We discuss the role and the observational evidence of several radiation processes: free-free electron-ion, free-free electron-electron, free-bound electron-ion, photoelectric absorption and Compton backscatter (albedo), using both spectroscopic and imaging techniques. This unprecedented quality of data allows for the first time inference of the angular distributions of the X-ray-emitting electrons and improved model-independent inference of electron energy spectra and emission measures of thermal plasma. Moreover, imaging spectroscopy has revealed hitherto unknown details of solar flare morphology and detailed spectroscopy of coronal, footpoint and extended sources in flaring regions. Additional attempts to measure hard X-ray polarization were not sufficient to put constraints on the degree of anisotropy of electrons, but point to the importance of obtaining good quality polarization data in the future.
C1 [Kontar, E. P.; Brown, J. C.; Mallik, P. C. V.] Univ Glasgow, Dept Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
[Emslie, A. G.] Oklahoma State Univ, Dept Phys, Stillwater, OK 74078 USA.
[Emslie, A. G.] Western Kentucky Univ, Bowling Green, KY 42101 USA.
[Hajdas, W.; Suarez-Garcia, E.] Paul Scherrer Inst, Villigen, Switzerland.
[Holman, G. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hurford, G. J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Kasparova, J.] Astron Ustav AV CR, VVI, Ondrejov 25165, Czech Republic.
[Massone, A. M.; Prato, M.] CNR SPIN, I-16146 Genoa, Italy.
[McConnell, M. L.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Piana, M.] Univ Genoa, Dipartimento Matemat, I-16146 Genoa, Italy.
[Schmahl, E. J.] NWRA CoRA, Boulder, CO 80301 USA.
[Suarez-Garcia, E.] Univ Geneva, Dept Nucl & Particle Phys, CH-1212 Geneva, Switzerland.
RP Kontar, EP (reprint author), Univ Glasgow, Dept Phys & Astron, Kelvin Bldg, Glasgow G12 8QQ, Lanark, Scotland.
EM eduard@astro.gla.ac.uk
RI Kasparova, Jana/G-9024-2014; piana, michele/H-9376-2015; Prato,
Marco/G-4096-2011; Kontar, Eduard/B-7897-2008; Holman,
Gordon/C-9548-2012; Suarez, Estela/J-5939-2012
OI PIANA, MICHELE/0000-0003-1700-991X; Prato, Marco/0000-0002-7327-3347;
Kontar, Eduard/0000-0002-8078-0902;
FU PPARC/STFC; UC Berkeley NASA; Royal Society; Dorothy Hodgkin
Scholarship; Agency of the Czech Republic [205/06/P135]; Astronomical
Institute [AV0Z10030501]; NASA [NNX10AT78G, 06-HGI06-15]; University of
California-Berkeley; International Space Science Institute (ISSI) in
Bern, Switzerland; NASA Goddard Space Flight Center; European Commission
through the SOLAIRE Network [MTRN-CT-2006-035484]; Italian MIVR
FX E. P. K., J.C.B. and P. C. V. M. acknowledge the support of a PPARC/STFC
Rolling Grant, UC Berkeley NASA RHESSI Visitor funds (J.C.B.), a
PPARC/STFCr UK Advanced Fellowship and Royal Society Conference Grant
(E. P. K.) and a Dorothy Hodgkin Scholarship (P. C. V. M.). J.K.
acknowledges support from Grant 205/06/P135 of the Grant Agency of the
Czech Republic and the research plan AV0Z10030501 of the Astronomical
Institute AS CR, v.v.i. A. G. E. was supported by NASA Grant NNX10AT78G
and through a grant from the University of California-Berkeley. E. P.
K., J.C.B., A. G. E., G. D. H., G.J.H., J.K., A. M. M., M. P. and M. P.
have been supported in part by a grant from the International Space
Science Institute (ISSI) in Bern, Switzerland. E.J.S. acknowledges a
grant from NASA Goddard Space Flight Center to the University of
Maryland and a Heliophysics GI grant 06-HGI06-15 from NASA HQ to NWRA
for research in RHESSI albedo determination and applications. Financial
support by the European Commission through the SOLAIRE Network
(MTRN-CT-2006-035484) is gratefully acknowledged by E. P. K. and J.C.B.
A. M. M., M. P. and M. P. acknowledge a grant by the Italian MIVR.
NR 175
TC 69
Z9 69
U1 2
U2 7
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 SEP
PY 2011
VL 159
IS 1-4
BP 301
EP 355
DI 10.1007/s11214-011-9804-x
PG 55
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 831NM
UT WOS:000295738400008
ER
PT J
AU Vaughan, WW
Johnson, DL
AF Vaughan, William W.
Johnson, Dale L.
TI AEROSPACE METEOROLOGY Some Lessons Learned from the Development and
Application of NASA Terrestrial Environment Design Criteria
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
C1 [Vaughan, William W.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35899 USA.
[Johnson, Dale L.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Vaughan, WW (reprint author), Univ Alabama, Dept Atmospher Sci, 301 Sparkman Dr, Huntsville, AL 35899 USA.
EM vaughan@nsstc.uah.edu
NR 13
TC 1
Z9 1
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 SEP
PY 2011
VL 92
IS 9
BP 1149
EP 1157
DI 10.1175/2011BAMS3133.1
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 835YK
UT WOS:000296072900010
ER
PT J
AU McFarquhar, G
Schmid, B
Korolev, A
Ogren, JA
Russell, PB
Tomlinson, J
Turner, DD
Wiscombe, W
AF McFarquhar, Greg
Schmid, Beat
Korolev, Alexei
Ogren, John A.
Russell, Philip B.
Tomlinson, Jason
Turner, David D.
Wiscombe, Warren
TI AIRBORNE INSTRUMENTATION NEEDS FOR CLIMATE AND ATMOSPHERIC RESEARCH
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Editorial Material
C1 [McFarquhar, Greg] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA.
[Schmid, Beat; Tomlinson, Jason] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Korolev, Alexei] Environm Canada, Sci & Technol Branch, Downsview, ON, Canada.
[Ogren, John A.] NOAA, Boulder, CO USA.
[Russell, Philip B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Turner, David D.] Univ Wisconsin, Madison, WI USA.
[Wiscombe, Warren] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP McFarquhar, G (reprint author), Univ Illinois, Dept Atmospher Sci, 105 S Gregory St, Urbana, IL 61801 USA.
EM mcfarq@atmos.uiuc.edu
RI Tomlinson, Jason/C-6566-2009; Wiscombe, Warren/D-4665-2012; Ogren,
John/M-8255-2015;
OI Wiscombe, Warren/0000-0001-6844-9849; Ogren, John/0000-0002-7895-9583;
McFarquhar, Greg/0000-0003-0950-0135
NR 0
TC 7
Z9 7
U1 0
U2 6
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 SEP
PY 2011
VL 92
IS 9
BP 1193
EP 1196
DI 10.1175/2011BAMS3180.1
PG 4
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 835YK
UT WOS:000296072900014
ER
PT J
AU Hendon, HH
Sperber, KR
Waliser, DE
Wheeler, MC
AF Hendon, Harry H.
Sperber, Kenneth R.
Waliser, Duane E.
Wheeler, Matthew C.
TI MODELING MONSOON INTRASEASONAL VARIABILITY From Theory to Operational
Forecasting
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Editorial Material
C1 [Hendon, Harry H.; Wheeler, Matthew C.] Bur Meteorol, Ctr Australian Weather & Climate Res, Melbourne, Vic 3001, Australia.
[Sperber, Kenneth R.] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Wheeler, MC (reprint author), Bur Meteorol, Ctr Australian Weather & Climate Res, GPO Box 1289, Melbourne, Vic 3001, Australia.
EM m.wheeler@bom.gov.au
RI Wheeler, Matthew/C-9038-2011; Sperber, Kenneth/H-2333-2012
OI Wheeler, Matthew/0000-0002-9769-1973;
NR 1
TC 0
Z9 0
U1 0
U2 6
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 SEP
PY 2011
VL 92
IS 9
BP ES32
EP ES35
DI 10.1175/2011BAMS3164.1
PG 4
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 835YK
UT WOS:000296072900015
ER
PT J
AU Holtan, SG
Dronca, RS
Nevala, WK
Porrata, LF
Mansfield, AS
Block, MS
Leontovich, AA
Grotz, TE
Turner, JD
Frisch, HP
Markovic, SN
AF Holtan, Shernan G.
Dronca, Roxana S.
Nevala, Wendy K.
Porrata, Luis F.
Mansfield, Aaron S.
Block, Matthew S.
Leontovich, Alexey A.
Grotz, Travis E.
Turner, James D.
Frisch, Harold P.
Markovic, Svetomir N.
TI The dynamic human immune response to cancer: it might just be rocket
science
SO IMMUNOTHERAPY
LA English
DT Editorial Material
DE angiogenesis; biorhythm; melanoma; mouse model; placenta; predictive
modeling; tolerance
ID INVASION; MELANOMA
C1 [Holtan, Shernan G.; Porrata, Luis F.; Mansfield, Aaron S.; Markovic, Svetomir N.] Mayo Clin Grad Sch Med, Dept Med, Div Hematol, Rochester, MN 55905 USA.
[Dronca, Roxana S.; Mansfield, Aaron S.; Block, Matthew S.; Markovic, Svetomir N.] Mayo Clin Grad Sch Med, Dept Oncol, Rochester, MN 55905 USA.
[Nevala, Wendy K.; Markovic, Svetomir N.] Mayo Clin Grad Sch Med, Dept Immunol, Rochester, MN 55905 USA.
[Leontovich, Alexey A.] Mayo Clin Grad Sch Med, Dept Biomed Stat & Informat, Rochester, MN 55905 USA.
[Grotz, Travis E.] Mayo Clin Grad Sch Med, Dept Surg, Rochester, MN 55905 USA.
[Turner, James D.] Texas A&M Univ, Dept Aerosp Engn, College Stn, TX 77843 USA.
[Frisch, Harold P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Markovic, SN (reprint author), Mayo Clin Grad Sch Med, Dept Med, Div Hematol, 200 1st St SW, Rochester, MN 55905 USA.
EM markovic.svetomir@mayo.edu
OI Mansfield, Aaron/0000-0002-9483-6903
NR 16
TC 4
Z9 5
U1 0
U2 3
PU FUTURE MEDICINE LTD
PI LONDON
PA UNITEC HOUSE, 3RD FLOOR, 2 ALBERT PLACE, FINCHLEY CENTRAL, LONDON, N3
1QB, ENGLAND
SN 1750-743X
J9 IMMUNOTHERAPY-UK
JI Immunotherapy
PD SEP
PY 2011
VL 3
IS 9
BP 1021
EP 1024
DI 10.2217/IMT.11.109
PG 4
WC Immunology
SC Immunology
GA 838LS
UT WOS:000296293800001
PM 21913823
ER
PT J
AU Standish, M
AF Standish, Myles
TI The Hill-Brown Theory of the Moon's Motion: Its Coming-to-Be and
Short-Lived Ascendancy (1877-1984)
SO ISIS
LA English
DT Book Review
C1 [Standish, Myles] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Standish, M (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0021-1753
J9 ISIS
JI Isis
PD SEP
PY 2011
VL 102
IS 3
BP 547
EP 548
DI 10.1086/663026
PG 4
WC History & Philosophy Of Science
SC History & Philosophy of Science
GA 835TT
UT WOS:000296059600018
ER
PT J
AU Curtis, TH
Adams, DH
Burgess, GH
AF Curtis, Tobey H.
Adams, Douglas H.
Burgess, George H.
TI Seasonal Distribution and Habitat Associations of Bull Sharks in the
Indian River Lagoon, Florida: A 30-Year Synthesis
SO TRANSACTIONS OF THE AMERICAN FISHERIES SOCIETY
LA English
DT Article
ID CARCHARHINUS-LEUCAS; COASTAL LAGOONS; ATLANTIC COAST; NURSERY AREAS;
NORTHERN GULF; UNITED-STATES; TOMALES BAY; FRESH-WATER; ESTUARY;
MOVEMENTS
AB Many coastal shark species use shallow estuarine regions as nursery habitat, but there are considerable gaps in our understanding of the seasonal distribution and habitat use patterns of sharks within these systems. We compiled all available sampling data from the Indian River Lagoon (IRL) along Florida's central Atlantic coast to examine the distribution of bull sharks Carcharhinus leucas. The data synthesized in this study spanned the 30-year period 1975-2005 and included information on the seasonal distribution, size structure, and habitat associations of 449 bull sharks. For comparison, data from an additional 106 bull sharks captured in shelf waters adjacent to the IRL were also examined. The IRL is dominated by young-of-the-year (age-0) and juvenile bull sharks, which were most abundant during spring, summer, and autumn. Shark captures were most often associated with shallow freshwater creeks, power plant outfalls, ocean inlets, and seagrass habitats with temperatures greater than 20 degrees C, salinities of 10-30%, and dissolved oxygen concentrations between 4 and 7 mg/L. Juvenile bull sharks were found in waters with higher mean salinities than were age-0 sharks. Although the IRL is one of the most important bull shark nursery areas on the U. S. Atlantic coast, catch-per-unit-effort data indicate that bull shark abundance decreases with increasing latitude within and north of the IRL, suggesting that the IRL is the northern limit of functional nursery habitat for this species in the northwest Atlantic Ocean.
C1 [Curtis, Tobey H.; Burgess, George H.] Univ Florida, Florida Program Shark Res, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
[Adams, Douglas H.] Florida Fish & Wildlife Conservat Commiss, Fish & Wildlife Res Inst, Melbourne, FL 32901 USA.
RP Curtis, TH (reprint author), Natl Marine Fisheries Serv, NE Reg Off, Gloucester, MA 01930 USA.
EM tobey.curtis@noaa.gov
FU National Marine Fisheries Service (NMFS) Highly Migratory Species
Division
FX We express our gratitude to the individuals and organizations that
shared bull shark records for this study including F. Snelson, F. Murru,
M. Stolen, L. Ehrhart, R. Paperno, S. Kubis, D. Bagley, J. Provancha, S.
Tyson, and Cape Canaveral Scientific, Inc. For assistance with field
work we acknowledge T. Vigliotti, T. Ford, E. Reyier, B. Delius, and
numerous other volunteers. F. Snelson, D. Parkyn, M. Heupel, and E.
Phlips provided helpful guidance over the course of this study. A.
Morgan and L. Hale provided bull shark data from the BLL observer
program. For logistical support and permitting we additionally thank the
Florida Fish and Wildlife Conservation Commission (permit 02R-718),
Merritt Island National Wildlife Refuge (permit SUP 35 Burgess), and
Canaveral National Seashore (Permit No. CANA-2002-SCI-0007). This
research was supported by a grant from the National Marine Fisheries
Service (NMFS) Highly Migratory Species Division to the National Shark
Research Consortium, and tagging supplies were provided by C. McCandless
and the NMFS Apex Predators Program, Cooperative Atlantic States Shark
Pupping and Nursery Survey (COASTSPAN). Comments provided by three
anonymous reviewers greatly improved the manuscript.
NR 62
TC 21
Z9 23
U1 2
U2 39
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA
SN 0002-8487
J9 T AM FISH SOC
JI Trans. Am. Fish. Soc.
PD SEP
PY 2011
VL 140
IS 5
BP 1213
EP 1226
DI 10.1080/00028487.2011.618352
PG 14
WC Fisheries
SC Fisheries
GA 836VM
UT WOS:000296143900007
ER
PT J
AU Rockwell, RD
Goyne, CP
Haw, W
Krauss, RH
McDaniel, JC
Trefny, CJ
AF Rockwell, Robert D., Jr.
Goyne, Christopher P.
Haw, Willie
Krauss, Roland H.
McDaniel, James C.
Trefny, Charles J.
TI Experimental Study of Test-Medium Vitiation Effects on Dual-Mode
Scramjet Performance
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article; Proceedings Paper
CT 48th AIAA Aerospace Sciences Meeting
CY JAN 04-07, 2010
CL Orlando, FL
SP AIAA
ID ENGINE PERFORMANCE; COMBUSTOR
AB An experimental study was performed to characterize the effects of vitiation due to combustion-air preheating on dual-mode scramjet combustion. Major combustion vitiation species (H(2)O and CO(2)) were added to the freestream of an electrical-resistance-heated, direct-connect facility simulating Mach 5 flight enthalpy. With clean, dry air, the combustor operated in the supersonic mode at fuel equivalence ratios below 0.22, and in the subsonic mode for equivalence ratios above 0.26. Hysteresis was observed in the dual-mode transition region between 0.22 and 0.26, as the mode of combustion was dependent on whether the fuel rate was increasing or decreasing. Adding increasing amounts of water vapor and carbon dioxide to the freestream decreased combustor pressures by 10 to 30% for the same fuel equivalence ratio. Vitiation also caused transition between supersonic and subsonic combustion to occur at a higher fuel equivalence ratio than with clean air. This work represents the first direct evaluation of the effect of test-medium vitiation on dual-mode scramjet combustion at Mach 5 enthalpy simulation in the same facility. The results indicate the importance of accounting for test-medium vitiation when extrapolating from ground-testing to flight, particularly in the dual-mode transition region between subsonic and supersonic combustion regimes.
C1 [Rockwell, Robert D., Jr.; Goyne, Christopher P.; Haw, Willie; McDaniel, James C.] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22904 USA.
[Trefny, Charles J.] NASA, John H Glenn Res Ctr, Lewis Field, Cleveland, OH 44138 USA.
RP Rockwell, RD (reprint author), Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22904 USA.
NR 18
TC 12
Z9 12
U1 1
U2 15
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 SEP-OCT
PY 2011
VL 27
IS 5
BP 1135
EP 1142
DI 10.2514/1.B34180
PG 8
WC Engineering, Aerospace
SC Engineering
GA 831CG
UT WOS:000295705700024
ER
PT J
AU Grover, MR
Cichy, BD
Desai, PN
AF Grover, Myron R., III
Cichy, Benjamin D.
Desai, Prasun N.
TI Overview of the Phoenix Entry, Descent, and Landing System Architecture
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA/AAS Astrodynamics Specialist Conference and Exhibit
CY AUG 18-21, 2008
CL Honolulu, HI
SP Amer Inst Aeronaut & Astronaut (AIAA), AAS
AB NASA's Mars Phoenix Lander began its journey to Mars from Cape Canaveral, Florida in August 2007, but its journey to the launch pad began many years earlier in 1997 as NASA's Mars Surveyor Program 2001 Lander. In the intervening years, the entry, descent, and landing system architecture went through a series of changes, resulting in the system that flew to the surface of Mars on 25 May 2008. Some changes, such as entry velocity and landing site elevation, were the result of differences in mission design. Other changes, including the removal of hypersonic guidance, the reformulation of the parachute deployment algorithm, and the addition of the backshell avoidance maneuver, were driven by constant efforts to augment system robustness. An overview of the Phoenix entry, descent, and landing system architecture is presented along with rationales driving the entry, descent, and landing system design choices. These design choices resulted in the robust Phoenix landing system that successfully landed on Mars on 25 May 2008.
C1 [Grover, Myron R., III] CALTECH, Jet Prop Lab, Entry Descent & Landing Syst Adv Technol Grp, Pasadena, CA 91109 USA.
[Desai, Prasun N.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA.
RP Grover, MR (reprint author), CALTECH, Jet Prop Lab, Entry Descent & Landing Syst Adv Technol Grp, 4800 Oak Grove Dr,Mail Stop 264-623, Pasadena, CA 91109 USA.
EM myron.r.grover@jpl.nasa.gov; benjamin.d.cichy@jpl.nasa.gov;
prasun.n.desai@nasa.gov
NR 5
TC 10
Z9 12
U1 0
U2 4
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 SEP-OCT
PY 2011
VL 48
IS 5
BP 706
EP 712
DI 10.2514/1.46548
PG 7
WC Engineering, Aerospace
SC Engineering
GA 834WW
UT WOS:000295996200002
ER
PT J
AU Edquist, KT
Desai, PN
Schoenenberger, M
AF Edquist, Karl T.
Desai, Prasun N.
Schoenenberger, Mark
TI Aerodynamics for Mars Phoenix Entry Capsule
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA/AAS Astrodynamics Specialist Conference and Exhibit
CY AUG 18-21, 2008
CL Honolulu, HI
SP Amer Inst Aeronaut & Astronaut (AIAA), AAS
ID DESCENT; SYSTEM
AB The preflight aerodynamic database for the Mars Phoenix entry capsule is presented. The aerodynamic coefficients were generated as a function of total angle of attack and either Knudsen number, velocity, or Mach number, depending on the flight regime. The database was constructed using continuum flowfield computations and data from the Mars Exploration Rover and Viking programs. Hypersonic and supersonic static coefficients were derived from Navier-Stokes solutions on a preflight design trajectory. High-altitude data (free-molecular and transitional regimes) and dynamic pitch damping characteristics were taken from Mars Exploration Rover analysis and testing. Transonic static coefficients from Viking wind-tunnel tests were used for capsule aerodynamics under the parachute. Static instabilities were predicted at two points along the reference trajectory and were verified by reconstructed flight data. During the hypersonic instability, the capsule was predicted to trim at angles as high as 2.5 deg with an onaxis center of gravity. Peak trim angles for an offnominal pitching moment and a 5 mm offaxis center of gravity were predicted to be 4.2 and 4.8 deg, respectively. Finally, hypersonic static coefficient sensitivities to atmospheric density were predicted to be within uncertainty bounds.
C1 [Edquist, Karl T.; Desai, Prasun N.; Schoenenberger, Mark] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA.
RP Edquist, KT (reprint author), NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Mail Stop 489, Hampton, VA 23681 USA.
EM Karl.T.Edquist@nasa.gov; Prasun.N.Desai@nasa.gov;
Mark.Schoenenberger@nasa.gov
NR 22
TC 10
Z9 12
U1 2
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 SEP-OCT
PY 2011
VL 48
IS 5
BP 713
EP 726
DI 10.2514/1.46219
PG 14
WC Engineering, Aerospace
SC Engineering
GA 834WW
UT WOS:000295996200003
ER
PT J
AU McDaniel, RD
Wright, MJ
Songer, JT
AF McDaniel, Ryan D.
Wright, Michael J.
Songer, Jarvis T.
TI Aeroheating Predictions for Phoenix Entry Vehicle
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA 46th Aerospace Sciences Meeting and Exhibit
CY JAN 07-10, 2008
CL Reno, NV
SP Amer Inst Aeronaut & Astronaut (AIAA)
ID NAVIER-STOKES EQUATIONS; LINE RELAXATION
AB Computational aerothermal analyses of the Phoenix entry vehicle in the Martian atmosphere are presented. Two Navier-Stokes flow solvers were used to predict the environments experienced by the vehicle along several design trajectories. An assessment of the likelihood of turbulent transition was also performed using several correlations. The nominal entry was ballistic; therefore, the majority of the solutions were computed as axisymmetric. Several three-dimensional cases were also computed to assess the acreage heating at offnominal angles of attack and local heating enhancement caused by surface singularities.
C1 [McDaniel, Ryan D.; Wright, Michael J.] NASA, Ames Res Ctr, Reacting Flow Environm Branch, Moffett Field, CA 94035 USA.
[Songer, Jarvis T.] Lockheed Martin Space Syst, Aero Entry Syst, Littleton, CO 80125 USA.
RP McDaniel, RD (reprint author), NASA, Ames Res Ctr, Reacting Flow Environm Branch, Mail Stop 230-2, Moffett Field, CA 94035 USA.
NR 32
TC 2
Z9 2
U1 0
U2 1
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 SEP-OCT
PY 2011
VL 48
IS 5
BP 727
EP 745
DI 10.2514/1.48357
PG 19
WC Engineering, Aerospace
SC Engineering
GA 834WW
UT WOS:000295996200004
ER
PT J
AU Dyakonov, AA
Glass, CE
Desai, PN
Van Norman, JW
AF Dyakonov, Artem A.
Glass, Christopher E.
Desai, Prasun N.
Van Norman, John W.
TI Analysis of Effectiveness of Phoenix Entry Reaction Control System
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA/AAS Astrodynamics Specialist Conference and Exhibit
CY AUG 18-21, 2008
CL Honolulu, HI
SP Amer Inst Aeronaut & Astronaut (AIAA), AAS
AB Interaction between the external flowfield and the reaction control system thruster plumes of the Phoenix capsule during entry has been investigated. The analysis covered rarefied, transitional, hypersonic, and supersonic flight regimes. Performance of pitch, yaw, and roll control authority channels was evaluated, with specific emphasis on the yaw channel due to its low nominal yaw control authority. Because Phoenix had already been constructed and its reaction control system could not be modified before flight, an assessment of reaction control system efficacy along the trajectory was needed to determine possible issues and to make necessary software changes. Effectiveness of the system at various regimes was evaluated using a hybrid direct simulation Monte-Carlo-computational fluid dynamics technique, based on direct simulation Monte-Carlo analysis code and general aerodynamic simulation program, the Langley aerothermal upwind relaxation algorithm code, and the fully unstructured 3-D code. Results of the analysis at hypersonic and supersonic conditions suggest a significant aeroreaction control system interference, which reduced the efficacy of the thrusters and could likely produce control reversal. Very little aeroreaction control system interference was predicted in rarefied and transitional regimes. A recommendation was made to the project to widen controller system deadbands to minimize (if not eliminate) the use of reaction control system thrusters through hypersonic and supersonic flight regimes, where their performance would be uncertain.
C1 [Dyakonov, Artem A.; Desai, Prasun N.] NASA, Langley Res Ctr, Atmospher Flight Entry Syst Brach, Hampton, VA 23681 USA.
[Glass, Christopher E.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
[Van Norman, John W.] Analyt Mech Associates, Atmospher Flight Entry Syst Branch, Hampton, VA 23666 USA.
RP Dyakonov, AA (reprint author), NASA, Langley Res Ctr, Atmospher Flight Entry Syst Brach, Hampton, VA 23681 USA.
NR 10
TC 9
Z9 9
U1 1
U2 4
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 SEP-OCT
PY 2011
VL 48
IS 5
BP 746
EP 755
DI 10.2514/1.40965
PG 10
WC Engineering, Aerospace
SC Engineering
GA 834WW
UT WOS:000295996200005
ER
PT J
AU Prince, JL
Desai, PN
Queen, EM
Grover, MR
AF Prince, Jill L.
Desai, Prasun N.
Queen, Eric M.
Grover, Myron. R.
TI Mars Phoenix Entry, Descent, and Landing Simulation Design and Modeling
Analysis
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA Guidance, Navigation, and Control Conference
CY AUG 18-21, 2008
CL Honolulu, HI
SP Amer Inst Aeronaut & Astronaut (AIAA)
AB In the five years before the 25 May 2008 landing of the Mars Phoenix Lander, hundreds of thousands of simulations were conducted and analyzed to define a robust sequence of events for the entry, descent, and landing phase of the Phoenix mission. Based on performance predictions, Phoenix was designed with an unguided, ballistic, hypersonic entry; a 11.73 m disk-gap-band parachute deployment; and a terminal descent system delivering it to the surface with a soft landing. Each model incorporated into the simulation was scrutinized, verified, and validated. Deterministic and statistical analyses were performed, building confidence that Phoenix would land safely in the northern plains of Mars.
C1 [Prince, Jill L.; Desai, Prasun N.; Queen, Eric M.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA.
[Grover, Myron. R.] CALTECH, Jet Prop Lab, EDL Syst Adv Technol Grp, Pasadena, CA 91109 USA.
RP Prince, JL (reprint author), NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Mail Stop 489, Hampton, VA 23681 USA.
EM jill.l.prince@nasa.gov; prasun.n.desai@nasa.gov; eric.m.queen@nasa.gov;
myron.r.grover@jpl.nasa.gov
NR 15
TC 12
Z9 14
U1 1
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 SEP-OCT
PY 2011
VL 48
IS 5
BP 756
EP 764
DI 10.2514/1.46561
PG 9
WC Engineering, Aerospace
SC Engineering
GA 834WW
UT WOS:000295996200006
ER
PT J
AU Queen, EM
Prince, JL
Desai, PN
AF Queen, Eric M.
Prince, Jill L.
Desai, Prasun N.
TI Multibody Modeling and Simulation for Mars Phoenix Entry, Descent, and
Landing
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA/AAS Astrodynamics Specialist Conference
CY AUG 18-21, 2008
CL Oahu, HI
SP Amer Inst Aeronaut & Astronaut (AIAA), AAS
AB A multibody flight simulation for the Phoenix Mars Lander was developed that included high-fidelity six-degree-of-freedom rigid-body models for the parachute and lander system. The simulation predicted attitude and rate histories of all bodies throughout the flight. In so doing, a realistic behavior of the descending parachute/lander system dynamics was simulated that allowed assessment of the Phoenix descent performance and identification of sensitivities for landing. This simulation provided a complete end-to-end capability of modeling the entire entry, descent, and landing sequence for the mission. The simulation was used to predict the parachute and lander aerodynamic angles during entry and the response of the lander system to various wind models and windshears. Several different wind models were analyzed to determine which was most effective at exciting vehicle attitude dynamics. The simulation was used to drive a Monte Carlo analysis that provided a statistical evaluation of the performance capability of the Phoenix landing system.
C1 [Queen, Eric M.; Prince, Jill L.; Desai, Prasun N.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA.
RP Queen, EM (reprint author), NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Mail Stop 489, Hampton, VA 23681 USA.
EM eric.m.queen@nasa.gov; jill.l.prince@nasa.gov; prasun.n.desai@nasa.gov
NR 9
TC 3
Z9 3
U1 0
U2 2
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 SEP-OCT
PY 2011
VL 48
IS 5
BP 765
EP 771
DI 10.2514/1.46918
PG 7
WC Engineering, Aerospace
SC Engineering
GA 834WW
UT WOS:000295996200007
ER
PT J
AU Belz, JE
Chen, C
Cichy, B
AF Belz, J. Eric
Chen, Curtis
Cichy, Ben
TI Phoenix Landing Radar Heatshield Anomaly
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID MARS; MISSION
AB This paper details a specific and unexpected problem faced by the Entry, Descent, and Landing team on the Phoenix Mars Mission that demonstrates two problems in mission architecture: 1) the difficulties inherent in adapting commercial-off-the-shelf technology to a system different from the product's intended scope; and 2) the design of test environments sufficiently flightlike as to reveal systemic problems in new architectures. Specifically, the interaction of the entry heat shield with the landing radar could not be tested in a flightlike manner; hence, detailed simulation of the landing radar was conducted with the expectation that the radar could lock on echoes from the heat shield and report an erroneous altitude, and that phenomenon could be handled with appropriate flight software. Surprisingly, it was discovered that the heat shield spoofed the radar's internal logic that was designed to prevent locking on ambiguous radar returns. Mitigating the unexpected problem proved to be much more challenging than the anticipated heatshield lock scenario, ultimately requiring last-minute changes to both the radar firmware and the flight software.
C1 [Belz, J. Eric; Chen, Curtis; Cichy, Ben] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
FU NASA
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, with Lockheed Martin, Vertigo, Inc.,
and Honeywell. Inc., under a contract with NASAThe authors gratefully
acknowledges the work of the entire Phoenix Project Team and, in
particular, the following people: Erik Bailey, Matt Graham, Thierry
Michel, Kyung Pak, Ernesto Rodriguez, Dara Sabahi, Scott Shaffer, David
Shafter, and David Skulsky. The authors would also like to thank Prasun
Desai for his careful help in preparing the final manuscript and Rob
Manning for inspiring this work.
NR 10
TC 3
Z9 3
U1 0
U2 0
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 SEP-OCT
PY 2011
VL 48
IS 5
BP 772
EP 777
DI 10.2514/1.51801
PG 6
WC Engineering, Aerospace
SC Engineering
GA 834WW
UT WOS:000295996200008
ER
PT J
AU Prince, JL
Desai, PN
Queen, EM
Grove, MR
AF Prince, Jill L.
Desai, Prasun N.
Queen, Eric M.
Grove, Myron R.
TI Entry, Descent, and Landing Operations Analysis for the Mars Phoenix
Lander
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA/AAS Astrodynamics Specialist Conference and Exhibit
CY AUG 18-21, 2008
CL Honolulu, HI
SP Amer Inst Aeronaut & Astronaut (AIAA), AAS
AB The entry, descent, and landing operations phase of the Mars Phoenix Lander occurred in the month before its safe landing on the surface of Mars on 25 May 2008. The operations phase was spent analyzing simulation results and ensuring that the spacecraft was on target to land within the designed landing ellipse while providing robust performance. Trajectories were analyzed to determine if changes to the onboard spacecraft configuration files were necessary before each file upload opportunity, as well as trajectory correction maneuver necessity and magnitude. During the operations phase, only two of the planned four nominal trajectory correction maneuvers were required, setting an approach trajectory on target to the desired nominal landing site.
C1 [Prince, Jill L.; Desai, Prasun N.; Queen, Eric M.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA.
[Grove, Myron R.] CALTECH, Jet Prop Lab, Entry Descent & Landing Syst Adv Technol Grp, Pasadena, CA 91109 USA.
RP Prince, JL (reprint author), NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Mail Stop 489, Hampton, VA 23681 USA.
EM Jill.L.Prince@nasa.gov; Prasun.N.Desai@nasa.gov; Eric.M.Queen@nasa.gov;
myron.r.grover@jpl.nasa.gov
NR 8
TC 6
Z9 7
U1 0
U2 1
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 SEP-OCT
PY 2011
VL 48
IS 5
BP 778
EP 783
DI 10.2514/1.46563
PG 6
WC Engineering, Aerospace
SC Engineering
GA 834WW
UT WOS:000295996200009
ER
PT J
AU Bonfiglio, EP
Adams, D
Craig, L
Spencer, DA
Arvidson, R
Heet, T
AF Bonfiglio, Eugene P.
Adams, Douglas
Craig, Lynn
Spencer, David A.
Arvidson, Ray
Heet, Tabatha
TI Landing-Site Dispersion Analysis and Statistical Assessment for the Mars
Phoenix Lander
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA/AAS Astrodynamics Specialist Conference and Exhibit
CY AUG 18-21, 2008
CL Honolulu, HI
SP Amer Inst Aeronaut & Astronaut (AIAA), AAS
AB The Mars Phoenix Lander launched on 4 August 2007 and successfully landed on Mars 10 months later on 25 May 2008. Landing ellipse predicts and hazard maps were instrumental in selecting safe surface targets for Phoenix. Hazard maps were based on terrain slopes, geomorphology maps, and automated rock counts from the Mars Reconnaissance Obiter's High Resolution Imaging Science Experiment images. The expected landing dispersion was used in conjunction with the hazard maps, which led to the selection of Phoenix's surface target. The same statistical assessment was performed with the actual landing dispersion predictions determined during operations in the weeks, days, and hours before landing and compared with criteria levied by the project in order to determine whether or not to perform entry aim-point targeting maneuvers. The statistical analysis was also used by the Phoenix project to verify the effectiveness of a preplanned maneuver menu and to calculate the probability of future maneuvers. An assessment of the statistical distribution of Phoenix landing points (Monte Carlo results) was performed to justify the Phoenix assumption of a bivariate Gaussian distribution, which showed that this assumption did not play a role in Phoenix landing downrange of the expected landing site.
C1 [Bonfiglio, Eugene P.] CALTECH, Jet Prop Lab, Guidance Nav & Control Sect, Pasadena, CA 91109 USA.
[Arvidson, Ray; Heet, Tabatha] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
RP Bonfiglio, EP (reprint author), CALTECH, Jet Prop Lab, Guidance Nav & Control Sect, Mail Stop 264-623, Pasadena, CA 91109 USA.
NR 14
TC 5
Z9 5
U1 1
U2 4
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 SEP-OCT
PY 2011
VL 48
IS 5
BP 784
EP 797
DI 10.2514/1.48813
PG 14
WC Engineering, Aerospace
SC Engineering
GA 834WW
UT WOS:000295996200010
ER
PT J
AU Desai, PN
Prince, JL
Queen, EM
Schoenenberger, M
Cruz, JR
Grover, MR
AF Desai, Prasun N.
Prince, Jill L.
Queen, Eric M.
Schoenenberger, Mark
Cruz, Juan R.
Grover, Myron R.
TI Entry, Descent, and Landing Performance of the Mars Phoenix Lander
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA/AAS Astrodynamics Specialist Conference and Exhibit
CY AUG 18-21, 2008
CL Honolulu, HI
SP Amer Inst Aeronaut & Astronaut (AIAA), AAS
AB On 25 May 2008, the Mars Phoenix Lander successfully landed on the northern arctic plains of Mars. An overview of reconstruction analyses performed on each entry, descent, and landing phase to assess the performance of Phoenix as it descended is presented and a comparison to preentry predictions is provided. The landing occurred 21 km further downrange than the predicted landing location. Analysis of the flight data revealed that the primary cause of Phoenix's downrange landing was a higher trim total angle of attack during the hypersonic phase of the entry, which resulted in Phoenix flying a slightly lifting trajectory. The likely cause of this higher trim attitude was a combination of a larger radial center-of-gravity offset than the preflight measurement and a lower hypersonic aerodynamic static stability than predicted. Parachute deployment was 6.4 s later than predicted. The parachute deployment and inflation process occurred as expected with no anomalies identified. The subsequent parachute descent and powered terminal landing also behaved as expected. A reconstruction of the landing day atmospheric density profile was found to be less dense than the best a priori prediction, ranging from a few percent to 8% lower in the altitude region where nearly all of the deceleration occurs. A comparison of the flight reconstructed trajectory parameters showed that the actual Phoenix entry, descent, and landing was close to preentry predictions.
C1 [Desai, Prasun N.; Prince, Jill L.; Queen, Eric M.; Schoenenberger, Mark; Cruz, Juan R.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA.
[Grover, Myron R.] CALTECH, Jet Prop Lab, EDL Syst Adv Technol Grp, Pasadena, CA 91109 USA.
RP Desai, PN (reprint author), NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Mail Stop 489, Hampton, VA 23681 USA.
EM prasun.n.desai@nasa.gov; jill.l.prince@nasa.gov; eric.m.queen@nasa.gov;
mark.schoenenberger@nasa.gov; juan.r.cruz@nasa.gov;
myron.r.grover@jpl.nasa.gov
NR 15
TC 21
Z9 24
U1 1
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 SEP-OCT
PY 2011
VL 48
IS 5
BP 798
EP 808
DI 10.2514/1.48239
PG 11
WC Engineering, Aerospace
SC Engineering
GA 834WW
UT WOS:000295996200011
ER
PT J
AU Blanchard, RC
Desai, PN
AF Blanchard, Robert C.
Desai, Prasun N.
TI Mars Phoenix Entry, Descent, and Landing Trajectory and Atmosphere
Reconstruction
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
AB The details of the trajectory and atmospheric reconstruction for the Mars Phoenix entry, descent, and landing are presented. The trajectory reconstruction used a six-degree-of-freedom process that included integrating the 200 Hz onboard inertial measurement unit incremental velocity change Delta V data and incremental angle change Delta theta data, the derivatives from the Delta V and the Delta theta data, smoothing, and correcting the inertial measurement unit accelerations for physical location on the Lander. Lander orientation angles (angle of attack and sideslip) during descent were reconstructed independently of the aerodynamics and atmosphere models. Before parachute deployment, the angle of attack and sideslip were found to be small (less than 3 deg) leading up to about 5 deg at parachute deploy, where the deployment altitude was determined to be approximately 13 km at a Mach number of about 1.7 and a dynamic pressure of 489 N/m(2). In a separate process, the atmosphere structure (i.e., density, pressure, and temperature) encountered for altitudes up to 80 km was determined. The atmosphere structure determination process involved a detailed aerodynamics model of the Lander and the parachute, as well as accounting for configuration changes during descent. Comparisons made with the preflight atmosphere model used in the mission design show good agreement with the three reconstructed atmosphere structure parameters.
C1 [Desai, Prasun N.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Blanchard, Robert C.] George Washington Univ, Hampton, VA 23681 USA.
FU NASA [NNX08A055G]
FX Work was performed at George Washington University under NASA award no.
NNX08A055G
NR 12
TC 9
Z9 10
U1 0
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
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 SEP-OCT
PY 2011
VL 48
IS 5
BP 809
EP 821
DI 10.2514/1.46274
PG 13
WC Engineering, Aerospace
SC Engineering
GA 834WW
UT WOS:000295996200012
ER
PT J
AU Kornfeld, RP
Bruvold, KN
Morabito, DD
Craig, LE
Asmar, SW
Ilott, PA
AF Kornfeld, Richard P.
Bruvold, Kristoffer N.
Morabito, David D.
Craig, Lynn E.
Asmar, Sami W.
Ilott, Peter A.
TI Reconstruction of Entry, Descent and Landing Communications for the
Phoenix Mars Lander
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
AB The Phoenix spacecraft landed successfully on 25 May 2008 on the northern plains of Mars to conduct a five-month study of the Martian environment. In response to NASA's requirement to provide spacecraft communications during critical events, the Phoenix Mars Lander provided continuous telecommunications coverage during entry, descent and landing allowing NASA's mission control teams and the public to witness in real time the events that led to the successful landing. Phoenix thereby employed a number of first-time communication strategies. The paper briefly reviews the constraints and degrees of freedom in designing an entry, descent and landing communications link and presents Phoenix's novel and robust implementation approach to entry, descent, and landing communications. It then compares the actual and the predicted communications performance using data collected by the Mars Odyssey, Mars Reconnaissance, and Mars Express orbiters as well as by terrestrial ground stations. The overall lessons learned and conclusions described herein can serve as a pathfinder for the entry, descent, and landing communications architecture and implementation of future Mars landed missions.
C1 [Kornfeld, Richard P.] CALTECH, Jet Prop Lab, Syst Engn Sect, Pasadena, CA 91109 USA.
[Bruvold, Kristoffer N.; Ilott, Peter A.] CALTECH, Jet Prop Lab, Flight Commun Syst Sect, Pasadena, CA 91109 USA.
[Morabito, David D.; Asmar, Sami W.] CALTECH, Jet Prop Lab, Commun Architectures & Res Sect, Pasadena, CA 91109 USA.
[Craig, Lynn E.] CALTECH, Jet Prop Lab, Guidance Nav & Control Sect, Pasadena, CA 91109 USA.
RP Kornfeld, RP (reprint author), CALTECH, Jet Prop Lab, Syst Engn Sect, M-S 301-490,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU National Aeronautics and Space Administration
FX This development work was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. Reference herein to any specific
commercial product, process, or service by trade name, trademark,
manufacturer, or otherwise, does not constitute or imply its endorsement
by the United States Government or the Jet Propulsion Laboratory,
California Institute of Technology.
NR 6
TC 3
Z9 4
U1 3
U2 4
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 SEP-OCT
PY 2011
VL 48
IS 5
BP 822
EP 835
DI 10.2514/1.47909
PG 14
WC Engineering, Aerospace
SC Engineering
GA 834WW
UT WOS:000295996200013
ER
PT J
AU Bilimoria, KD
Mueller, ER
Frost, CR
AF Bilimoria, Karl D.
Mueller, Eric R.
Frost, Chad R.
TI Handling Qualities Evaluation of Piloting Tools for Spacecraft Docking
in Earth Orbit
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA Guidance, Navigation, and Control Conference
CY AUG 10-13, 2009
CL Chicago, IL
SP Amer Inst Aeronaut & Astronaut (AIAA)
ID CONTROL POWER; SHUTTLE
AB A piloted simulation was conducted to study handling qualities for the final phase of spacecraft docking in Earth orbit. Twelve evaluation pilots, including 10 pilot astronauts, provided Cooper-Harper ratings, task load index component ratings, and qualitative comments. The piloting task was manual translational control with automatic attitude hold during the final 10 ft (3 m) of the approach to docking. A previous study established that with conventional translational control, handling qualities for this task degrade significantly as the level of translation-into-rotation dynamic coupling increases. The goal of the present study was to evaluate the efficacy of various piloting tools designed to mitigate the handling qualities degradation caused by this coupling. Four piloting tools were evaluated: deadband indicator, flight-path marker, translational flight director, and feedforward control. These piloting tools improved handling qualities, generally with greater improvements resulting from using these tools in combination. A key result of this study is that feedforward control effectively counteracts coupling effects while significantly decreasing propellant consumption, providing satisfactory handling qualities for the spacecraft configuration evaluated.
C1 [Bilimoria, Karl D.; Mueller, Eric R.] NASA, Ames Res Ctr, Flight Trajectory Dynam & Controls Branch, Moffett Field, CA 94035 USA.
[Frost, Chad R.] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
RP Bilimoria, KD (reprint author), NASA, Ames Res Ctr, Flight Trajectory Dynam & Controls Branch, Mail Stop 210-10, Moffett Field, CA 94035 USA.
EM Karl.Bilimoria@nasa.gov; Eric.Mueller@nasa.gov; Chad.R.Frost@nasa.gov
NR 32
TC 5
Z9 7
U1 0
U2 2
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 SEP-OCT
PY 2011
VL 48
IS 5
BP 846
EP 855
DI 10.2514/1.48505
PG 10
WC Engineering, Aerospace
SC Engineering
GA 834WW
UT WOS:000295996200015
ER
PT J
AU Roth, DJ
Reyes-Rodriguez, S
Zimdars, DA
Rauser, RW
Ussery, WW
AF Roth, D. J.
Reyes-Rodriguez, S.
Zimdars, D. A.
Rauser, R. W.
Ussery, W. W.
TI Terahertz Computed Tomography of NASA Thermal Protection System Foam
Materials
SO MATERIALS EVALUATION
LA English
DT Article
DE terahertz; computed tomography; imaging; X-ray; spray-on foam insulation
AB A terahertz (THz) axial computed tomography system has been developed that uses time-domain measurements in order to form cross-sectional image slices and 3D volume renderings of THz-transparent materials. The system can test samples as large as 0.0283 m(3) with no safety concerns. In this study, the system was evaluated for its ability to detect and characterize drilled holes and embedded voids in foam materials that were utilized as thermal protection on the external fuel tanks of space shuttles. X-ray micro-computed tomography was also performed on the samples to compare against the THz computed tomography results and better define embedded voids. Limits of detectability are loosely defined, based on depth and size for the samples used in this study. Image sharpness and morphology characterization ability for THz computed tomography are qualitatively described.
C1 [Roth, D. J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Reyes-Rodriguez, S.] Michigan State Univ, E Lansing, MI 48824 USA.
[Zimdars, D. A.] Picometrix LLC, Ann Arbor, MI 48104 USA.
[Rauser, R. W.] Univ Toledo, Toledo, OH 43606 USA.
[Ussery, W. W.] Lockheed Martin Space Syst Co, Denver, CO 80201 USA.
RP Roth, DJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
NR 17
TC 6
Z9 6
U1 0
U2 3
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 SEP
PY 2011
VL 69
IS 9
BP 1090
EP 1098
PG 9
WC Materials Science, Characterization & Testing
SC Materials Science
GA 831EE
UT WOS:000295710700010
ER
PT J
AU Pearson, JC
Drouin, BJ
Maestrini, A
Mehdi, I
Ward, J
Lin, RH
Yu, SS
Gill, JJ
Thomas, B
Lee, C
Chattopadhyay, G
Schlecht, E
Maiwald, FW
Goldsmith, PF
Siegel, P
AF Pearson, John C.
Drouin, Brian J.
Maestrini, Alain
Mehdi, Imran
Ward, John
Lin, Robert H.
Yu, Shanshan
Gill, John J.
Thomas, Bertrand
Lee, Choonsup
Chattopadhyay, Goutam
Schlecht, Erich
Maiwald, Frank W.
Goldsmith, Paul F.
Siegel, Peter
TI Demonstration of a room temperature 2.48-2.75 THz coherent spectroscopy
source
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
DE carbon compounds; frequency multipliers; organic compounds; oscillators;
power amplifiers; terahertz spectroscopy; terahertz wave spectra; water
ID ROTATIONAL TRANSITION FREQUENCIES; QUANTUM CASCADE LASER; LAMB-DIP
SPECTRUM; LOCAL OSCILLATOR; BAND; SPECTROMETER; POWER; HD; PARAMETERS;
DATABASE
AB We report the first demonstration of a continuous wave coherent source covering 2.48-2.75 THz, with greater than 10% instantaneous tuning bandwidth and having 1-14 mu W of output power at room temperature. This source is based on a 91.8-101.8 GHz synthesizer followed by a power amplifier and three cascaded frequency triplers. It demonstrates for the first time that purely electronic solid-state sources can generate a useful amount of power in a region of the electromagnetic spectrum where lasers (solid state or gas) were previously the only available coherent sources. The bandwidth, agility, and operability of this THz source have enabled wideband, high resolution spectroscopic measurements of water, methanol, and carbon monoxide with a resolution and signal-to-noise ratio unmatched by any other existing system, providing new insight in the physics of these molecules. Furthermore, the power and optical beam quality are high enough to observe the Lamb-dip effect in water. The source frequency has an absolute accuracy better than 1 part in 10(12) and the spectrometer achieves sub-Doppler frequency resolution better than 1 part in 10(8). The harmonic purity is better than 25 dB. This source can serve as a coherent signal for absorption spectroscopy, a local oscillator for a variety of heterodyne systems and can be used as a method for precision control of more powerful but much less frequency agile quantum mechanical terahertz sources. (C) 2011 American Institute of Physics. [doi:10.1063/1.3617420]
C1 [Pearson, John C.; Drouin, Brian J.; Mehdi, Imran; Ward, John; Lin, Robert H.; Yu, Shanshan; Gill, John J.; Thomas, Bertrand; Lee, Choonsup; Chattopadhyay, Goutam; Schlecht, Erich; Maiwald, Frank W.; Goldsmith, Paul F.; Siegel, Peter] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Maestrini, Alain] Univ Paris 06, Lab Etud Rayonnement & Matiere, Observ Paris, F-75014 Paris, France.
RP Pearson, JC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM John.C.Pearson@jpl.nasa.gov
RI Yu, Shanshan/D-8733-2016; Goldsmith, Paul/H-3159-2016
FU National Aeronautics and Space Administration; Centre National d'Etudes
Spatiales; European Space Agency
FX A part of research was performed at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration. Funding from the NASA Astrophysics
Research and Analysis Program (APRA) is gratefully acknowledged. This
work was performed in part at the Observatoire de Paris, LERMA. Funding
of the Centre National d'Etudes Spatiales and the European Space Agency
is gratefully acknowledged. Thanks to Dr. G. Moruzzi for providing the
FTIR methanol spectrum and Dr. H.-W. Hubers for providing the QCL
methanol spectrum.
NR 57
TC 42
Z9 43
U1 1
U2 19
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0034-6748
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD SEP
PY 2011
VL 82
IS 9
AR 093105
DI 10.1063/1.3617420
PG 9
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA 829XX
UT WOS:000295621100006
PM 21974571
ER
PT J
AU Sinha, MP
Neidholdt, EL
Hurowitz, J
Sturhahn, W
Beard, B
Hecht, MH
AF Sinha, M. P.
Neidholdt, E. L.
Hurowitz, J.
Sturhahn, W.
Beard, B.
Hecht, M. H.
TI Laser ablation-miniature mass spectrometer for elemental and isotopic
analysis of rocks
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
DE geochemistry; geochronology; geophysical equipment; geophysical
techniques; mass spectrometers; minerals; rocks
ID INDUCTIVELY-COUPLED PLASMA; MARTIAN METEORITES; RB-SR; GEOLOGICAL
SAMPLES; ICP-MS; MARS; CONSTRAINTS; SYSTEMATICS; MICROPROBE; CHRONOLOGY
AB A laser ablation-miniature mass spectrometer (LA-MMS) for the chemical and isotopic measurement of rocks and minerals is described. In the LA-MMS method, neutral atoms ablated by a pulsed laser are led into an electron impact ionization source, where they are ionized by a 70 eV electron beam. This results in a secondary ion pulse typically 10-100 mu s wide, compared to the original 5-10 ns laser pulse duration. Ions of different masses are then spatially dispersed along the focal plane of the magnetic sector of the miniature mass spectrometer (MMS) and measured in parallel by a modified CCD array detector capable of detecting ions directly. Compared to conventional scanning techniques, simultaneous measurement of the ion pulse along the focal plane effectively offers a 100% duty cycle over a wide mass range. LA-MMS offers a more quantitative assessment of elemental composition than techniques that detect ions directly generated by the ablation process because the latter can be strongly influenced by matrix effects that vary with the structure and geometry of the surface, the wavelength of the laser beam, and the not well characterized ionization efficiencies of the elements in the process. The above problems attendant to the direct ion analysis has been minimized in the LA-MMS by analyzing the ablated neutral species after their post-ionization by electron impaction. These neutral species are much more abundant than the directly ablated ions in the ablated vapor plume and are, therefore, expected to be characteristic of the chemical composition of the solid. Also, the electron impact ionization of elements is well studied and their ionization cross sections are known and easy to find in databases. Currently, the LA-MMS limit of detection is 0.4 wt.%. Here we describe LA-MMS elemental composition measurements of various minerals including microcline, lepidolite, anorthoclase, and USGS BCR-2G samples. The measurements of high precision isotopic ratios including (41)K/(39)K (0.077 +/- 0.004) and (29)Si/(28)Si (0.052 +/- 0.006) in these minerals by LA-MMS are also described. The LA-MMS has been developed as a prototype instrument system for space applications for geochemical and geochronological measurements on the surface of extraterrestrial bodies. (C) 2011 American Institute of Physics. [doi:10.1063/1.3626794]
C1 [Sinha, M. P.; Neidholdt, E. L.; Hurowitz, J.; Sturhahn, W.; Hecht, M. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Beard, B.] Univ Wisconsin, Dept Geol & Geophys, Madison, WI 53706 USA.
[Sinha, M. P.; Beard, B.] NASA Astrobiol Inst, Washington, DC USA.
RP Sinha, MP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Mahadeva.p.sinha@jpl.nasa.gov
FU National Aeronautics and Space Administration; NASA Astrobiology
Institute (NAI)
FX The authors thank Shannon Jackson for technical support in the design
and implementation of some of the electronics for the LA-MMS. The
development of LA-MMS was performed at the Jet Propulsion Laboratory
(JPL), California Institute of Technology and was supported by grants
from the National Aeronautics and Space Administration. The research
work described in this paper was, in part, supported by the NASA
Astrobiology Institute (NAI).
NR 37
TC 11
Z9 11
U1 2
U2 17
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0034-6748
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD SEP
PY 2011
VL 82
IS 9
AR 094102
DI 10.1063/1.3626794
PG 7
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA 829XX
UT WOS:000295621100036
PM 21974601
ER
PT J
AU Weatherford, BR
Foster, JE
Kamhawi, H
AF Weatherford, B. R.
Foster, J. E.
Kamhawi, H.
TI Electron current extraction from a permanent magnet waveguide plasma
cathode
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
DE anodes; cathodes; circular waveguides; electron sources; Langmuir
probes; permanent magnets; plasma radiofrequency heating; plasma sources
ID MICROWAVE PLASMA; DISK SOURCE; ION-SOURCE; POWER
AB An electron cyclotron resonance plasma produced in a cylindrical waveguide with external permanent magnets was investigated as a possible plasma cathode electron source. The configuration is desirable in that it eliminates the need for a physical antenna inserted into the plasma, the erosion of which limits operating lifetime. Plasma bulk density was found to be overdense in the source. Extraction currents over 4 A were achieved with the device. Measurements of extracted electron currents were similar to calculated currents, which were estimated using Langmuir probe measurements at the plasma cathode orifice and along the length of the external plume. The influence of facility effects and trace ionization in the anode-cathode gap are also discussed. (C) 2011 American Institute of Physics. [doi:10.1063/1.3642662]
C1 [Weatherford, B. R.; Foster, J. E.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Kamhawi, H.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Weatherford, BR (reprint author), Univ Michigan, Ann Arbor, MI 48109 USA.
EM brweathe@umich.edu
NR 23
TC 2
Z9 2
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 0034-6748
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD SEP
PY 2011
VL 82
IS 9
AR 093507
DI 10.1063/1.3642662
PG 9
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA 829XX
UT WOS:000295621100022
PM 21974587
ER
PT J
AU Cornejo-Garrido, H
Kibanova, D
Nieto-Camacho, A
Guzman, J
Ramirez-Apan, T
Fernandez-Lomelin, P
Garduno, ML
Cervini-Silva, J
AF Cornejo-Garrido, Hilda
Kibanova, Daria
Nieto-Camacho, Antonio
Guzman, Jose
Ramirez-Apan, Teresa
Fernandez-Lomelin, Pilar
Laura Garduno, Maria
Cervini-Silva, Javiera
TI Oxidative stress, cytoxicity, and cell mortality induced by nano-sized
lead in aqueous suspensions
SO CHEMOSPHERE
LA English
DT Article
DE Water-stable; Stable nanoparticles; Lipid peroxidation; Lead
nanoparticles; Biological activity
ID LIPID-PEROXIDATION; RAT-BRAIN; HYDROXAMATE SIDEROPHORES; BRINE SHRIMP;
NITRIC-OXIDE; IRON; DISSOLUTION; ADSORPTION; PB(II); GROWTH
AB This paper reports on the effect of aqueous and nano-particulated Pb on oxidative stress (lipid peroxidation), cytoxicity, and cell mortality. As determined by the Thiobarbituric Acid Reactive Substances (TBARS) method, only 6 h after incubation aqueous suspensions bearing nano-sized PbO2, soluble Pb(II), and brain-homogenate only suspensions, were determined to contain as much as ca. 7, 5, and 1 nmol TBARS mg protein(-1), respectively. Exposure of human cells (central nervous system, prostate, leukemia, colon, breast, lung cells) to nano-PbO2 led to cell-growth inhibition values (%) Ca. <= 18.7%. Finally, as estimated by the Artemia sauna test, cell mortality values were found to show high-survival larvae rates. Microscopic observations revealed that Pb particles were swallowed, but caused no mortality, however. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Cornejo-Garrido, Hilda; Kibanova, Daria; Laura Garduno, Maria; Cervini-Silva, Javiera] Univ Autonoma Metropolitana Cuajimalpa, Dept Proc & Tecnol, Mexico City, DF, Mexico.
[Cornejo-Garrido, Hilda] Univ Nacl Autonoma Mexico, Posgrado Ciencias Tierra, Mexico City 04510, DF, Mexico.
[Nieto-Camacho, Antonio; Ramirez-Apan, Teresa] Univ Nacl Autonoma Mexico, Lab Ciencias Biolog, Inst Quim, Mexico City 04510, DF, Mexico.
[Guzman, Jose] Cent Invest Ciencia Aplicada & Tecnol Avanzada, Unidad Legaria, Mexico City, DF, Mexico.
[Fernandez-Lomelin, Pilar] Univ Nacl Autonoma Mexico, Inst Geog, Mexico City 04510, DF, Mexico.
[Cervini-Silva, Javiera] NASA, Astrobiol Inst, Washington, DC USA.
[Cervini-Silva, Javiera] Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA USA.
RP Cervini-Silva, J (reprint author), Univ Autonoma Metropolitana Cuajimalpa, Dept Proc & Tecnol, Artificios 40,6 Piso Col Miguel Hidalgo, Mexico City, DF, Mexico.
EM jcervini@correo.cua.uam.mx
FU Universidad Autifinoma Metropolitana Unidad Cuajimalpa; ECACORE
(SEMARNAT CONACYT) [23496]
FX HC-G gratefully acknowledges the support of an undergraduate fellowship
from DGAPA-UNAM. The authors are most grateful to Drs. Ben Gilbert and
Zhao Hao (LBNL) for technical assistance. The authors would like to
express their sincere appreciation to Dr. Rebecca Sutton (Environmental
Working Group, Oakland, CA) who provided insightful comments and helpful
suggestions which have substantially improved this manuscript. The
authors thank Lic. Maria del Rocio Galindo Ortega (UAM-Cuajimalpa), and
M. in Sc. Claudia Rivera Cerecedo and Hector Malagon Rivera (Bioterio,
lnstituto de Fisiologia Celular, UNAM) for technical assistance. This
project was supported in part by Universidad Autifinoma Metropolitana
Unidad Cuajimalpa and ECACORE 2020 (SEMARNAT CONACYT 23496).
NR 61
TC 15
Z9 18
U1 2
U2 15
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0045-6535
J9 CHEMOSPHERE
JI Chemosphere
PD SEP
PY 2011
VL 84
IS 10
BP 1329
EP 1335
DI 10.1016/j.chemosphere.2011.05.018
PG 7
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA 828YX
UT WOS:000295542400004
PM 21640370
ER
PT J
AU Ramp, SR
Lermusiaux, PFJ
Shulman, I
Chao, Y
Wolf, RE
Bahr, FL
AF Ramp, Steven R.
Lermusiaux, Pierre F. J.
Shulman, Igor
Chao, Yi
Wolf, Rebecca E.
Bahr, Frederick L.
TI Oceanographic and atmospheric conditions on the continental shelf north
of the Monterey Bay during August 2006
SO DYNAMICS OF ATMOSPHERES AND OCEANS
LA English
DT Article
DE Coastal circulation; Air/sea interaction; Upwelling; Ocean modeling and
prediction; USA/West Coast/California/Monterey Bay
ID OCEAN DYNAMICS EXPERIMENT; CENTRAL CALIFORNIA; SEA-LEVEL; WEST-COAST;
MOORED OBSERVATIONS; BOUNDARY-LAYER; UPPER SLOPE; TEMPERATURE;
VARIABILITY; CURRENTS
AB A comprehensive data set from the ocean and atmosphere was obtained just north of the Monterey Bay as part of the Monterey Bay 2006 (MB06) field experiment. The wind stress, heat fluxes, and sea surface temperature were sampled by the Naval Postgraduate School's TWIN OTTER research aircraft. In situ data were collected using ships, moorings, gliders and AUVs. Four data-assimilating numerical models were additionally run, including the Coupled Ocean/Atmosphere Mesoscale Prediction System (COAMPS(R)) model for the atmosphere and the Harvard Ocean Prediction System (HOPS), the Regional Ocean Modeling System (ROMS), and the Navy Coastal Ocean Model (NCOM) for the ocean.
The scientific focus of the Adaptive Sampling and Prediction Experiment (ASAP) was on the upwelling/relaxation cycle and the resulting three-dimensional coastal circulation near a coastal promontory, in this case Point Ano Nuevo, CA. The emphasis of this study is on the circulation over the continental shelf as estimated from the wind forcing, two ADCP moorings, and model outputs. The wind stress during August 2006 consisted of 3-10 day upwelling favorable events separated by brief 1-3 day relaxations. During the first two weeks there was some correlation between local winds and currents and the three models' capability to reproduce the events. During the last two weeks, largely equatorward surface wind stress forced the sea surface and barotropic poleward flow occurred over the shelf, reducing model skill at predicting the circulation. The poleward flow was apparently remotely forced by mesoscale eddies and alongshore pressure gradients, which were not well simulated by the models. The small, high-resolution model domains were highly reliant on correct open boundary conditions to drive these larger-scale poleward flows. Multiply-nested models were no more effective than well-initialized local models in this respect. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Ramp, Steven R.] Soliton Ocean Serv Inc, Carmel Valley, CA 93924 USA.
[Lermusiaux, Pierre F. J.] MIT, Cambridge, MA 02139 USA.
[Shulman, Igor] USN, Res Lab, Stennis Space Ctr, MS 39529 USA.
[Chao, Yi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wolf, Rebecca E.] USN, Postgrad Sch, Monterey, CA 93943 USA.
[Bahr, Frederick L.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA.
RP Ramp, SR (reprint author), Soliton Ocean Serv Inc, Carmel Valley, CA 93924 USA.
EM sramp@solitonocean.com
RI Lermusiaux, Pierre/H-6003-2011
FU National Aeronautics and Space Administration; Office of Naval Research
FX Joe Rice (Navel Postgraduate School) arranged and installed the
real-time data transmission via the Seaweb network. Marla Stone expertly
prepared, deployed, and recovered the moorings. The crew at the NPS
Center for Interdisciplinary Remotely-Piloted Aircraft Studies (CIRPAS),
under the direction of Bob Bluth and Haf Jonsson, expertly piloted and
maintained the TWIN OTrER aircraft. Todd Anderson (NPS) went on every
flight to operate the scientific instrumentation package on board. PFJL
thanks P.J. Haley and W.G. Leslie for discussions and collaborations. IS
thanks S. Anderson and P. Sakalaukus for programming and computer
support. This research was carried out in part by the Jet Propulsion
Laboratory (JPL), California Institute of Technology, under contract
with the National Aeronautics and Space Administration. The authors
thank the whole MB06 team for their close collaborations over several
years. We thank the Office of Naval Research for support under the
MURI-ASAP grants.
NR 45
TC 12
Z9 12
U1 0
U2 10
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0377-0265
J9 DYNAM ATMOS OCEANS
JI Dyn. Atmos. Oceans
PD SEP
PY 2011
VL 52
IS 1-2
SI SI
BP 192
EP 223
DI 10.1016/j.dynatmoce.2011.04.005
PG 32
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences;
Oceanography
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences;
Oceanography
GA 828KD
UT WOS:000295499000011
ER
PT J
AU Caruso, T
Chan, YK
Lacap, DC
Lau, MCY
Mckay, CP
Pointing, SB
AF Caruso, Tancredi
Chan, Yuki
Lacap, Donnabella C.
Lau, Maggie C. Y.
McKay, Christopher P.
Pointing, Stephen B.
TI Stochastic and deterministic processes interact in the assembly of
desert microbial communities on a global scale
SO ISME JOURNAL
LA English
DT Article
ID NULL MODEL ANALYSIS; NEUTRAL THEORY; ENVIRONMENTAL GRADIENTS; SPECIES
ABUNDANCE; CHINA HOT; LONG-TERM; DIVERSITY; ECOLOGY; NICHE; BIODIVERSITY
AB Extreme arid regions in the worlds' major deserts are typified by quartz pavement terrain. Cryptic hypolithic communities colonize the ventral surface of quartz rocks and this habitat is characterized by a relative lack of environmental and trophic complexity. Combined with readily identifiable major environmental stressors this provides a tractable model system for determining the relative role of stochastic and deterministic drivers in community assembly. Through analyzing an original, worldwide data set of 16S rRNA-gene defined bacterial communities from the most extreme deserts on the Earth, we show that functional assemblages within the communities were subject to different assembly influences. Null models applied to the photosynthetic assemblage revealed that stochastic processes exerted most effect on the assemblage, although the level of community dissimilarity varied between continents in a manner not always consistent with neutral models. The heterotrophic assemblages displayed signatures of niche processes across four continents, whereas in other cases they conformed to neutral predictions. Importantly, for continents where neutrality was either rejected or accepted, assembly drivers differed between the two functional groups. This study demonstrates that multi-trophic microbial systems may not be fully described by a single set of niche or neutral assembly rules and that stochasticity is likely a major determinant of such systems, with significant variation in the influence of these determinants on a global scale. The ISME Journal (2011) 5, 1406-1413; doi:10.1038/ismej.2011.21; published online 3 March 2011
C1 [Caruso, Tancredi] Free Univ Berlin, Inst Biol, D-14195 Berlin, Germany.
[Chan, Yuki; Lacap, Donnabella C.; Lau, Maggie C. Y.; Pointing, Stephen B.] Univ Hong Kong, Sch Biol Sci, Hong Kong, Hong Kong, Peoples R China.
[McKay, Christopher P.] NASA, Ames Res Ctr, Mountain View, CA USA.
RP Caruso, T (reprint author), Free Univ Berlin, Inst Biol, Altensteinstr 6, D-14195 Berlin, Germany.
EM tancredi.caruso@fu-berlin.de; pointing.steve@gmail.com
RI Caruso, Tancredi/H-1103-2012;
OI Caruso, Tancredi/0000-0002-3607-9609; Chan, Yuki/0000-0002-9570-5462
FU United States National Science Foundation; NASA Astrobiology Science and
Technology for Exploring Planets (ASTEP) Programme; Hong Kong Research
Grants Council [HKU7733/08M, HKU7763/10]; EBESA [452]; SCAR; Italian
PNRA (Programma Nazionale di Ricerche in Antartide); Freie Universitat
Berlin; Humboldt Foundation
FX This research was supported by the United States National Science
Foundation, NASA Astrobiology Science and Technology for Exploring
Planets (ASTEP) Programme, and the Hong Kong Research Grants Council
(HKU7733/08M and HKU7763/10). T. Caruso was supported by EBESA IPY
project no 452, SCAR EBA Programs, the Italian PNRA (Programma Nazionale
di Ricerche in Antartide), Freie Universitat Berlin and the Humboldt
Foundation. The authors thank Professor Yuwadee Peerapornpisal (Chiang
Mai University, Thailand) for providing tropical hypolith samples. We
thank Jeff R Powell for commenting on the manuscript.
NR 47
TC 78
Z9 79
U1 13
U2 85
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1751-7362
J9 ISME J
JI ISME J.
PD SEP
PY 2011
VL 5
IS 9
BP 1406
EP 1413
DI 10.1038/ismej.2011.21
PG 8
WC Ecology; Microbiology
SC Environmental Sciences & Ecology; Microbiology
GA 832DU
UT WOS:000295782900002
PM 21368908
ER
PT J
AU Nielsen, K
Nedoluha, GE
Chandran, A
Chang, LC
Barker-Tvedtnes, J
Taylor, MJ
Mitchell, NJ
Lambert, A
Schwartz, MJ
Russell, JM
AF Nielsen, Kim
Nedoluha, Gerald E.
Chandran, Amal
Chang, Loren C.
Barker-Tvedtnes, Jodie
Taylor, Michael J.
Mitchell, Nick J.
Lambert, Alyn
Schwartz, Michael J.
Russell, James M., III
TI On the origin of mid-latitude mesospheric clouds: The July 2009 cloud
outbreak
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article; Proceedings Paper
CT 9th International Workshop on Layered Phenomena in theMesospause Region
(LPMR)
CY JUL 14, 2009
CL Stockholm Univ, Dept Meteorol, Stockholm, SWEDEN
SP Int Commission Middle Atmosphere (ICMA), Int Meteorol Inst, Swedish Natl Space Board, Esrange Space Ctr
HO Stockholm Univ, Dept Meteorol
DE Mesospheric clouds; Planetary waves; Mesosphere
ID NOCTILUCENT CLOUDS; PLANETARY-WAVES; ICE; NLC
AB Mid-latitude mesospheric clouds (MCs) are a rare phenomenon and their existence is not well understood, as the mesosphere at these latitudes is, in general, too warm for clouds to form. During the 2009 northern hemisphere summer season an unusually high number of these clouds were reported over both central and southern Europe, and the western contiguous United States. In this paper we investigate the mesospheric temperature field utilizing data from the Microwave Limb Sounder (MLS) instrument. We find that the temperature occasionally is near the frost point temperature and that the presence of planetary waves with periods of 2-, 5-, and 16-days combine to provide temperature anomalies of 1-1.5 K, lowering the temperature below the frost point for cloud formation and growth. Observed MCs are found to occur in close proximity to the 5-day wave anomaly. Model results show that the growth time to achieve visible particle sizes under the observed temperature and water vapor mixing ratio conditions are greater than similar to 20 h. Combined with climatological winds from a mid-latitude site, our study suggests that these clouds occur due to a combination of advection from higher and colder latitudes, and in situ wave growth. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Nielsen, Kim] Computat Phys Inc, Boulder, CO USA.
[Chandran, Amal] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Chang, Loren C.] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA.
[Barker-Tvedtnes, Jodie; Taylor, Michael J.] Utah State Univ, Ctr Atmospher & Space Sci, Logan, UT 84322 USA.
[Mitchell, Nick J.] Univ Bath, Ctr Space Atmospher & Ocean Sci, Bath BA2 7AY, Avon, England.
[Lambert, Alyn; Schwartz, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Russell, James M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
RP Nielsen, K (reprint author), Computat Phys Inc, Boulder, CO USA.
EM knielsen@cpi.com
RI Chang, Loren/G-3722-2015; Schwartz, Michael/F-5172-2016
OI Schwartz, Michael/0000-0001-6169-5094
NR 29
TC 3
Z9 3
U1 1
U2 7
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 SEP
PY 2011
VL 73
IS 14-15
SI SI
BP 2118
EP 2124
DI 10.1016/j.jastp.2010.10.015
PG 7
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 829BT
UT WOS:000295551000009
ER
PT J
AU Schubert, S
Wang, HL
Suarez, M
AF Schubert, Siegfried
Wang, Hailan
Suarez, Max
TI Warm Season Subseasonal Variability and Climate Extremes in the Northern
Hemisphere: The Role of Stationary Rossby Waves
SO JOURNAL OF CLIMATE
LA English
DT Article
ID SUMMER HEAT-WAVE; UNITED-STATES; 1988 DROUGHT; INTRASEASONAL
TELECONNECTION; SOIL-MOISTURE; 1993 FLOODS; PRECIPITATION; PROPAGATION;
AMERICA; CYCLE
AB This study examines the nature of boreal summer subseasonal atmospheric variability based on the new NASA Modern-Era Retrospective Analysis for Research and Applications (MERRA) for the period 1979-2010. An analysis of the June, July, and August subseasonal 250-hPa meridional nu-wind anomalies shows distinct Rossby wave-like structures that appear to be guided by the mean jets. On monthly subseasonal time scales, the leading waves [ the first 10 rotated empirical orthogonal functions (REOFs) of the 250-hPa nu wind] explain about 50% of the Northern Hemisphere nu-wind variability and account for more than 30% (60%) of the precipitation (surface temperature) variability over a number of regions of the northern middle and high latitudes, including the U. S. northern Great Plains, parts of Canada, Europe, and Russia. The first REOF in particular consists of a Rossby wave that extends across northern Eurasia where it is a dominant contributor to monthly surface temperature and precipitation variability and played an important role in the 2003 European and 2010 Russian heat waves. While primarily subseasonal in nature, the Rossby waves can at times have a substantial seasonal mean component. This is exemplified by REOF 4, which played a major role in the development of the most intense anomalies of the U. S. 1988 drought (during June) and the 1993 flooding (during July), though differed in the latter event by also making an important contribution to the seasonal mean anomalies. A stationary wave model (SWM) is used to reproduce some of the basic features of the observed waves and provide insight into the nature of the forcing. In particular, the responses to a set of idealized forcing functions are used to map the optimal forcing patterns of the leading waves. Also, experiments to reproduce the observed waves with the SWM using MERRA-based estimates of the forcing indicate that the wave forcing is dominated by submonthly vorticity transients.
C1 [Schubert, Siegfried; Wang, Hailan; Suarez, Max] NASA GSFC, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Wang, Hailan] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
RP Schubert, S (reprint author), NASA GSFC, Global Modeling & Assimilat Off, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM siegfried.d.schubert@nasa.gov
FU NASA; NOAA
FX Support for this project was provided by the NASA Modeling, Analysis and
Prediction (MAP) Program, and the NOAA Climate Prediction Program for
the Americas (CPPA).
NR 37
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U1 1
U2 25
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 SEP
PY 2011
VL 24
IS 18
BP 4773
EP 4792
DI 10.1175/JCLI-D-10-05035.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 823WN
UT WOS:000295158100001
ER
PT J
AU Wang, JQ
Pawson, S
Tian, BJ
Liang, MC
Shia, RL
Yung, YL
Jiang, X
AF Wang, Jingqian
Pawson, Steven
Tian, Baijun
Liang, Mao-Chang
Shia, Run-Lie
Yung, Yuk L.
Jiang, Xun
TI El Nino-Southern Oscillation in Tropical and Midlatitude Column Ozone
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID QUASI-BIENNIAL OSCILLATION; SEA-SURFACE TEMPERATURE; INTERANNUAL
VARIABILITY; TROPOPAUSE PRESSURE; TROPOSPHERIC OZONE; SPATIAL-PATTERNS;
TRANSPORT MODEL; GLOBAL QBO; TRENDS; STRATOSPHERE
AB The impacts of El Nino-Southern Oscillation (ENSO) on the tropical total column ozone, the tropical tropopause pressure, and the 3.5-yr ozone signal in the midlatitude total column ozone were examined using the Goddard Earth Observing System Chemistry-Climate Model (GEOS CCM). Observed monthly mean sea surface temperature and sea ice between 1951 and 2004 were used as boundary conditions for the model. Since the model includes no solar cycle, quasi-biennial oscillation, or volcanic forcing, the ENSO signal was found to dominate the tropical total column ozone variability. Principal component analysis was applied to the detrended, deseasonalized, and low-pass filtered model outputs. The first mode of model total column ozone captured 63.8% of the total variance. The spatial pattern of this mode was similar to that in Total Ozone Mapping Spectrometer (TOMS) observations. There was also a clear ENSO signal in the tropical tropopause pressure in the GEOS CCM, which is related to the ENSO signal in the total column ozone. The regression coefficient between the model total column ozone and the model tropopause pressure was 0.71 Dobson units (DU) hPa(-1). The GEOS CCM was also used to investigate a possible mechanism for the 3.5-yr signal observed in the midlatitude total column ozone. The 3.5-yr signal in the GEOS CCM column ozone is similar to that in the observations, which suggests that a model with realistic ENSO can reproduce the 3.5-yr signal. Hence, it is likely that the 3.5-yr signal was caused by ENSO.
C1 [Wang, Jingqian; Jiang, Xun] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA.
[Pawson, Steven] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Tian, Baijun] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Liang, Mao-Chang] Acad Sinica, Res Ctr Environm Changes, Taipei 115, Taiwan.
[Liang, Mao-Chang] Natl Cent Univ, Grad Inst Astron, Jhongli, Taiwan.
[Liang, Mao-Chang; Shia, Run-Lie; Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Wang, JQ (reprint author), Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA.
EM jwang3@mail.uh.edu
RI Tian, Baijun/A-1141-2007; Pawson, Steven/I-1865-2014
OI Tian, Baijun/0000-0001-9369-2373; Pawson, Steven/0000-0003-0200-717X
FU National Aeronautics and Space Administration
FX We thank Bernhard Rappenglueck, Barry Lefer, Mimi Gerstell, and three
anonymous reviewers for useful inputs and helpful comments. We thank the
World Ozone and Ultraviolet Radiation Data Centre for providing the
ozone observation data. Dr. Tian's research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 44
TC 7
Z9 7
U1 1
U2 9
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD SEP
PY 2011
VL 68
IS 9
BP 1911
EP 1921
DI 10.1175/JAS-D-11-045.1
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 823WF
UT WOS:000295157100006
ER
PT J
AU Kahn, BH
Teixeira, J
Fetzer, EJ
Gettelman, A
Hristova-Veleva, SM
Huang, XL
Kochanski, AK
Kohler, M
Krueger, SK
Wood, R
Zhao, M
AF Kahn, B. H.
Teixeira, J.
Fetzer, E. J.
Gettelman, A.
Hristova-Veleva, S. M.
Huang, X. L.
Kochanski, A. K.
Koehler, M.
Krueger, S. K.
Wood, R.
Zhao, M.
TI Temperature and Water Vapor Variance Scaling in Global Models:
Comparisons to Satellite and Aircraft Data
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID ATMOSPHERIC ENERGY-SPECTRUM; SOUTHEAST PACIFIC STRATOCUMULUS;
QUASI-GEOSTROPHIC MODEL; BOUNDARY-LAYER; CLOUD SCHEME; TURBULENCE;
CLIMATE; SIMULATION; VARIABILITY; CONVECTION
AB Observations of the scale dependence of height-resolved temperature T and water vapor q variability are valuable for improved subgrid-scale climate model parameterizations and model evaluation. Variance spectral benchmarks for T and q obtained from the Atmospheric Infrared Sounder (AIRS) are compared to those generated by state-of-the-art numerical weather prediction "analyses'' and "free-running'' climate model simulations with spatial resolution comparable to AIRS. The T and q spectra from both types of models are generally too steep, with small-scale variance up to several factors smaller than AIRS. However, the two model analyses more closely resemble AIRS than the two free-running model simulations. Scaling exponents obtained for AIRS column water vapor (CWV) and height-resolved layers of q are also compared to the superparameterized Community Atmospheric Model (SP-CAM), highlighting large differences in the magnitude of CWV variance and the relative flatness of height-resolved q scaling in SP-CAM. Height-resolved q spectra obtained from aircraft observations during the Variability of the American Monsoon Systems Ocean-Cloud-Atmosphere-Land Study Regional Experiment (VOCALS-REx) demonstrate changes in scaling exponents that depend on the observations' proximity to the base of the subsidence inversion with scale breaks that occur at approximately the dominant cloud scale (similar to 10-30 km). This suggests that finer spatial resolution requirements must be considered for future satellite observations of T and q than those currently planned for infrared and microwave satellite sounders.
C1 [Kahn, B. H.; Teixeira, J.; Fetzer, E. J.; Hristova-Veleva, S. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gettelman, A.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Huang, X. L.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Kochanski, A. K.; Krueger, S. K.] Univ Utah, Dept Atmospher Sci, Salt Lake City, UT USA.
[Koehler, M.] Deutsch Wetterdienst, Offenbach, Germany.
[Wood, R.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Zhao, M.] Geophys Fluid Dynam Lab, Princeton, NJ USA.
RP Kahn, BH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 169-237, Pasadena, CA 91109 USA.
EM brian.h.kahn@jpl.nasa.gov
RI Huang, Xianglei/G-6127-2011; Wood, Robert/A-2989-2008; Zhao,
Ming/C-6928-2014
OI Huang, Xianglei/0000-0002-7129-614X; Wood, Robert/0000-0002-1401-3828;
FU NASA; AIRS; Office of Naval Research [N0001408IP20064]; NOAA MAPPCPO;
NSF [ATM0755310]; VOCALS NSF [ATM-0745702]
FX Support from the JPL Internal Research and Technology Development
Program, NASA's Making Earth Science Data Records for Use in Research
Environments (MEaSUREs) program, and the AIRS Project at JPL is
acknowledged. JT acknowledges the support provided by the Office of
Naval Research, Marine Meteorology Program under award N0001408IP20064,
the NASA MAP Program, and the NOAA MAPPCPO Program. The work of X.L.
Huang is partly supported by NSF Grant ATM0755310. RW acknowledges the
support of VOCALS NSF Award ATM-0745702. AIRS data were obtained through
the Goddard Earth Sciences Data and Information Services Center
(http:/daac.gsfc.nasa.gov/). ECMWF data are provided in coordination
with the Year of Coordinated Observing Modeling and Forecasting Tropical
Convection project (http:/data-portal. ecmwf. intdatadyotc_od/). MERRA
data are provided by the Global Modeling and Assimilation Office
(http:/gmao.gsfc.nasa.gov/). This material is partly based on work
supported by the National Science Foundation Science and Technology
Center for Multi-Scale Modeling of Atmospheric Processes, managed by
Colorado State University under cooperative agreement ATM-0425247. Roger
Marchand provided the SP-CAM output. The MMF model runs were performed
at theDepartment of Energy Pacific Northwest National Laboratory (PNNL)
and the San Diego Supercomputing Center (SDSC). The authors thank
Stephen Eckermann, Jon Petch, Kyle Pressel, Richard Rood, Allen Schanot,
Ka-Kit Tung, and the anonymous reviewers for insightful discussions and
suggestions. This research was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
NASA.
NR 57
TC 17
Z9 17
U1 0
U2 9
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 SEP
PY 2011
VL 68
IS 9
BP 2156
EP 2168
DI 10.1175/2011JAS3737.1
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 823WF
UT WOS:000295157100020
ER
PT J
AU Kauffmann, J
Bertoldi, F
Bourke, TL
Myers, PC
Lee, CW
Huard, TL
AF Kauffmann, J.
Bertoldi, F.
Bourke, T. L.
Myers, P. C.
Lee, C. W.
Huard, T. L.
TI Confirmation of the VeLLO L1148-IRS: star formation at very low (column)
density
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE brown dwarfs; stars: formation; stars: low-mass; ISM: individual
objects: L1148; ISM: jets and outflows; infrared: stars
ID SPITZER C2D SURVEY; YOUNG STELLAR OBJECTS; BIPOLAR MOLECULAR OUTFLOW;
LOW-LUMINOSITY OBJECT; 1ST HYDROSTATIC CORE; PRE-MAIN-SEQUENCE; LOW-MASS
STARS; INFALL MOTIONS; EVOLUTIONARY MODELS; SMALL CLOUDS
AB We report the detection of a compact (similar to 5 arcsec; about 1800 au projected size) CO outflow from L1148-IRS. This confirms that this Spitzer source is physically associated with the nearby (approximate to 325 pc) L1148 dense core. Radiative transfer modelling suggests an internal luminosity of 0.08 to 0.13 L-circle dot. This validates L1148-IRS as a Very Low Luminosity Object (VeLLO; L = 0.1 L-circle dot). The L1148 dense core has unusually low densities and column densities for a star-forming core. It is difficult to understand how L1148-IRS might have formed under these conditions. Independent of the exact final mass of this VeLLO (which is likely <0.24 M-circle dot), L1148-IRS and similar VeLLOs might hold some clues about the isolated formation of brown dwarfs.
C1 [Kauffmann, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bertoldi, F.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Bourke, T. L.; Myers, P. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lee, C. W.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Huard, T. L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Kauffmann, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jens.kauffmann@jpl.nasa.gov
FU NASA [1279198, 1288806, 1407]; National Research Foundation of Korea;
Ministry of Education, Science and Technology [2010-0011605]
FX We are indebted to our local IRAM contacts, Arancha Castro-Carrizo and
Frederic Gueth, who changed their busy schedule to simplify our travel
arrangements for a data reduction visit. We thank Endrik Krugel for
providing us with a custom-modified dust radiative transfer code. Mike
Dunham was so kind to check our VeLLO catalogue (Table 2, Section 5.2)
against his notes. JK is deeply indebted to FB, Karl Menten, Malcolm
Walmsley, Johannes Schmid-Burgk and TP. This work would have been
impossible without their continuous and unconditional support. He also
thanks Di Li and Paul Goldsmith, his hosts at JPL, for making this
research possible. This project was supported by an appointment of JK to
the NASA Postdoctoral Program at the Jet Propulsion Laboratory,
administered by Oak Ridge Associated Universities through a contract
with NASA. His research was executed at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Air and Space Administration. Partial support for TLB was provided by
NASA through contracts 1279198 and 1288806 issued by the Jet Propulsion
Laboratory, California Institute of Technology, under NASA contract
1407. CWL acknowledges the support by Basic Science Research Program
through the National Research Foundation of Korea funded by the Ministry
of Education, Science and Technology (2010-0011605).
NR 86
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U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2011
VL 416
IS 3
BP 2341
EP 2358
DI 10.1111/j.1365-2966.2011.19205.x
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 826TQ
UT WOS:000295378100055
ER
PT J
AU Ashby, MLN
Mahajan, S
Smith, HA
Willner, SP
Fazio, GG
Raychaudhury, S
Zezas, A
Barmby, P
Bonfini, P
Cao, C
Gonzalez-Alfonso, E
Ishihara, D
Kaneda, H
Lyttle, V
Madden, S
Papovich, C
Sturm, E
Surace, J
Wu, H
Zhu, YN
AF Ashby, M. L. N.
Mahajan, S.
Smith, H. A.
Willner, S. P.
Fazio, G. G.
Raychaudhury, S.
Zezas, A.
Barmby, P.
Bonfini, P.
Cao, C.
Gonzalez-Alfonso, E.
Ishihara, D.
Kaneda, H.
Lyttle, V.
Madden, S.
Papovich, C.
Sturm, E.
Surace, J.
Wu, H.
Zhu, Y. -N.
TI The Star Formation Reference Survey. I. Survey Description and Basic
Data
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID SPECTRAL ENERGY-DISTRIBUTIONS; ACTIVE GALACTIC NUCLEI; TELESCOPE KEY
PROJECT; DIGITAL SKY SURVEY; FORMATION HISTORY; SPACE-TELESCOPE; NEARBY
GALAXIES; FORMATION RATES; INFRARED PROPERTIES; STARBURST GALAXIES
AB Star formation is arguably the most important physical process in the cosmos. It is a fundamental driver of galaxy evolution and the ultimate source of most of the energy emitted by galaxies in the local universe. A correct interpretation of star formation rate (SFR) measures is therefore essential to our understanding of galaxy formation and evolution. Unfortunately, however, no single SFR estimator is universally available or even applicable in all circumstances: the numerous galaxies found in deep surveys are often too faint (or too distant) to yield significant detections with most standard SFR measures, and until now there have been no global multiband observations of nearby galaxies that span all the conditions under which star formation is taking place. To address this need in a systematic way, we have undertaken a multiband survey of all types of star-forming galaxies in the local universe. This project, the Star Formation Reference Survey (SFRS), is based on a statistically valid sample of 369 nearby galaxies that span all existing combinations of dust temperature, SFR, and specific SFR. Furthermore, because the SFRS is blind with respect to AGN fraction and environment, it serves as a means to assess the influence of these factors on SFR. Our panchromatic global flux measurements (including GALEX FUV + NUV, SDSS ugriz, 2MASS JHK(s), Spitzer 3-8 mu m, and others) furnish uniform SFR measures and the context in which their reliability can be assessed. This article describes the SFRS survey strategy, defines the sample, and presents the multiband photometry collected to date.
C1 [Ashby, M. L. N.; Mahajan, S.; Smith, H. A.; Willner, S. P.; Fazio, G. G.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mahajan, S.; Raychaudhury, S.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Zezas, A.; Bonfini, P.] Univ Crete, Dept Phys, Iraklion, Greece.
[Barmby, P.; Lyttle, V.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Cao, C.] Shandong Univ, Sch Space Sci & Phys, Weihai 264209, Shandong, Peoples R China.
[Gonzalez-Alfonso, E.] Univ Alcala de Henares, Dept Fis, E-28871 Madrid, Spain.
[Ishihara, D.; Kaneda, H.] Nagoya Univ, Grad Sch Sci, Chikusa Ku, Aichi 4648602, Japan.
[Madden, S.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Papovich, C.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
[Sturm, E.] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany.
[Surace, J.] CALTECH, Jet Prop Lab, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Wu, H.; Zhu, Y. -N.] Chinese Acad Sci, Key Lab Opt Astron, Natl Astron Observ, Beijing 100012, Peoples R China.
RP Ashby, MLN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mashby@cfa.harvard.edu
RI Mahajan, Smriti/D-8902-2013; Barmby, Pauline/I-7194-2016; Zezas,
Andreas/C-7543-2011
OI Barmby, Pauline/0000-0003-2767-0090; Zezas, Andreas/0000-0001-8952-676X
FU National Aeronautics and Space Administration [NNX07AH49G, NNX10AD83G];
National Science Foundation of China [10833006, 10773014]; 973 Program
[2007CB815406]; Natural Sciences and Engineering Research Council of
Canada; Smithsonian Institution; Marie-Curie International Reintegration
Grant [224878]; European Union [206469]
FX The authors gratefully acknowledge the assistance of R. Brent Tully, who
generously supplied quality distances for many of our sample galaxies.
This research has made use of the NASA/IPAC Extragalactic Database
(NED), which is operated by the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration. This work is based in part on observations
made with Spitzer, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. Support
for this work was provided by NASA. The VLA is operated by the National
Radio Astronomy Observatory, which is a facility of the National Science
Foundation operated under cooperative agreement by Associated
Universities, Inc. H. Wu is supported by National Science Foundation of
China grants 10833006 and 10773014 and the 973 Program grant
2007CB815406. P. Barmby acknowledges research support through a
Discovery Grant from the Natural Sciences and Engineering Research
Council of Canada. S. Mahajan acknowledges support from a Smithsonian
Institution Endowment Grant. A. Zezas and P. Bonfini acknowledge support
by Marie-Curie International Reintegration Grant 224878 and European
Union grant 206469. H. Smith acknowledges support from NASA grants
NNX07AH49G and NNX10AD83G.
NR 80
TC 3
Z9 3
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD SEP
PY 2011
VL 123
IS 907
BP 1011
EP 1029
DI 10.1086/661920
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 829ON
UT WOS:000295593300001
ER
PT J
AU Abramowski, A
Acero, F
Aharonian, F
Akhperjanian, AG
Anton, G
Barnacka, A
de Almeida, UB
Bazer-Bachi, AR
Becherini, Y
Becker, J
Behera, B
Bernlohr, K
Bochow, A
Boisson, C
Bolmont, J
Bordas, P
Borrel, V
Brucker, J
Brun, F
Brun, P
Bulik, T
Busching, I
Casanova, S
Cerruti, M
Chadwick, PM
Charbonnier, A
Chaves, RCG
Cheesebrough, A
Chounet, LM
Clapson, AC
Coignet, G
Conrad, J
Dalton, M
Daniel, MK
Davids, ID
Degrange, B
Deil, C
Dickinson, HJ
Djannati-Atai, A
Domainko, W
Drury, LO
Dubois, F
Dubus, G
Dyks, J
Dyrda, M
Egberts, K
Eger, P
Espigat, P
Fallon, L
Farnier, C
Fegan, S
Feinstein, F
Fernandes, MV
Fiasson, A
Fontaine, G
Forster, A
Fussling, M
Gabici, S
Gallant, YA
Gast, H
Gerard, L
Gerbig, D
Giebels, B
Glicenstein, JF
Gluck, B
Goret, P
Goring, D
Hague, JD
Hampf, D
Hauser, M
Heinz, S
Heinzelmann, G
Henri, G
Hermann, G
Hinton, JA
Hoffmann, A
Hofmann, W
Hofverberg, P
Horns, D
Jacholkowska, A
de Jager, OC
Jahn, C
Jamrozy, M
Jung, I
Kastendieck, MA
Katarzynski, K
Katz, U
Kaufmann, S
Keogh, D
Kerschhaggl, M
Khangulyan, D
Khelifi, B
Klochkov, D
Kluzniak, W
Kneiske, T
Komin, N
Kosack, K
Kossakowski, R
Laffon, H
Lamanna, G
Lenain, JP
Lennarz, D
Lohse, T
Lopatin, A
Lu, CC
Marandon, V
Marcowith, A
Masbou, J
Maurin, D
Maxted, N
McComb, TJL
Medina, MC
Mehault, J
Nguyen, N
Moderski, R
Moulin, E
Naumann-Godo, M
de Naurois, M
Nedbal, D
Nekrassov, D
Nicholas, B
Niemiec, J
Nolan, SJ
Ohm, S
Olive, JF
Wilhelmi, ED
Opitz, B
Ostrowski, M
Panter, M
Arribas, MP
Pedaletti, G
Pelletier, G
Petrucci, PO
Pita, S
Puhlhofer, G
Punch, M
Quirrenbach, A
Raue, M
Rayner, SM
Reimer, A
Reimer, O
Renaud, M
de los Reyes, R
Rieger, F
Ripken, J
Rob, L
Rosier-Lees, S
Rowell, G
Rudak, B
Rulten, CB
Ruppel, J
Ryde, F
Sahakian, V
Santangelo, A
Schlickeiser, R
Schock, FM
Schonwald, A
Schwanke, U
Schwarzburg, S
Schwemmer, S
Shalchi, A
Sikora, M
Skilton, JL
Sol, H
Spengler, G
Stawarz, L
Steenkamp, R
Stegmann, C
Stinzing, F
Sushch, I
Szostek, A
Tam, PH
Tavernet, JP
Terrier, R
Tibolla, O
Tluczykont, M
Valerius, K
van Eldik, C
Vasileiadis, G
Venter, C
Vialle, JP
Viana, A
Vincent, P
Vivier, M
Volk, HJ
Volpe, F
Vorobiov, S
Vorster, M
Wagner, SJ
Ward, M
Wierzcholska, A
Zajczyk, A
Zdziarski, AA
Zech, A
Zechlin, HS
Abdo, AA
Ackermann, M
Ajello, M
Baldini, L
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Thayer, J. G.
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Torres, D. F.
Tosti, G.
Tramacere, A.
Troja, E.
Uehara, T.
Usher, T. L.
Vandenbroucke, J.
Vianello, G.
Vilchez, N.
Vitale, V.
Waite, A. P.
Wang, P.
Winer, B. L.
Wood, K. S.
Yang, Z.
Ylinen, T.
Ziegler, M.
CA HESS Collaboration
Fermi LAT Collaboration
TI Simultaneous multi-wavelength campaign on PKS 2005-489 in a high state
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; BL Lacertae objects: individual: PKS 2005-489
ID LARGE-AREA TELESCOPE; INFRARED OBSERVATIONS; BACKGROUND-RADIATION; HOST
GALAXIES; GAMMA-RAYS; EGRET DATA; BLAZAR; SWIFT; FLARE; PKS-2005-489
AB The high-frequency peaked BL Lac object PKS 2005-489 was the target of a multi-wavelength campaign with simultaneous observations in the TeV gamma-ray (H.E.S.S.), GeV gamma-ray (Fermi/LAT), X-ray (RXTE, Swift), UV (Swift) and optical (ATOM, Swift) bands. This campaign was carried out during a high flux state in the synchrotron regime. The flux in the optical and X-ray bands reached the level of the historical maxima. The hard GeV spectrum observed with Fermi/LAT connects well to the very high energy (VHE, E > 100 GeV) spectrum measured with H.E.S.S. with a peak energy between similar to 5 and 500 GeV. Compared to observations with contemporaneous coverage in the VHE and X-ray bands in 2004, the X-ray flux was similar to 50 times higher during the 2009 campaign while the TeV gamma-ray flux shows marginal variation over the years. The spectral energy distribution during this multi-wavelength campaign was fit by a one zone synchrotron self-Compton model with a well determined cutoff in X-rays. The parameters of a one zone SSC model are inconsistent with variability time scales. The variability behaviour over years with the large changes in synchrotron emission and small changes in the inverse Compton emission does not warrant an interpretation within a one-zone SSC model despite an apparently satisfying fit to the broadband data in 2009.
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[Chekhtman, A.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Chekhtman, A.; Makeev, A.] George Mason Univ, Dept Computat & Data Sci, Fairfax, VA 22030 USA.
[Dumora, D.; Escande, L.; Lott, B.] Univ Bordeaux 1, CNRS IN2p3, Ctr Etudes Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Escande, L.] Ctr Etudes Nucl Bordeaux Gradignan, CNRS IN2P3, UMR 5797, F-33175 Gradignan, France.
[Rieger, F.] MPG, Paris, France.
[Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[Frailis, M.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy.
[Fukazawa, Y.; Katagiri, H.; Mizuno, T.; Nishino, S.; Uehara, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Hughes, R. E.; Sander, A.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Kataoka, J.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knoedlseder, J.; Vilchez, N.] CNRS UPS, Ctr Etude Spatiale Rayonnements, F-31028 Toulouse 4, France.
[McConville, W.; McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McConville, W.; McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Okumura, A.; Ozaki, M.; Takahashi, T.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Kanagawa 2525210, Japan.
[Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Parent, D.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Sadrozinski, H. F-W; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Sadrozinski, H. F-W; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Tramacere, A.] CIFS, I-10133 Turin, Italy.
[Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Troja, E.] NASA, Postdoctoral Program, Greenbelt, MD 20771 USA.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, S-39182 Kalmar, Sweden.
RP Abramowski, A (reprint author), Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany.
EM S.Kaufmann@lsw.uni-heidelberg.de; fortin@llr.in2p3.fr; wmcconvi@umd.edu
RI Daniel, Michael/A-2903-2010; Komin, Nukri/J-6781-2015; Moskalenko,
Igor/A-1301-2007; Wang, Pengfei/M-8060-2013; Mazziotta, Mario
/O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016;
Orlando, E/R-5594-2016; Drury, Luke/B-1916-2017; Moulin,
Emmanuel/B-5959-2017; Tjus, Julia/G-8145-2012; Rando,
Riccardo/M-7179-2013; Fontaine, Gerard/D-6420-2014; Hays,
Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Venter,
Christo/E-6884-2011; Katarzynski, Krzysztof/G-4528-2014; Jamrozy,
Marek/F-4507-2015; Casanova, Sabrina/J-8935-2013; Anton,
Gisela/C-4840-2013; Johannesson, Gudlaugur/O-8741-2015; Loparco,
Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Morselli,
Aldo/G-6769-2011; Thompson, David/D-2939-2012; Gehrels,
Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012;
lubrano, pasquale/F-7269-2012; Kuss, Michael/H-8959-2012; giglietto,
nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; van Eldik,
Christopher/C-3901-2013; Katz, Uli/E-1925-2013; Tosti, Gino/E-9976-2013;
Ozaki, Masanobu/K-1165-2013
OI Tramacere, Andrea/0000-0002-8186-3793; Rowell,
Gavin/0000-0002-9516-1581; Baldini, Luca/0000-0002-9785-7726; Lenain,
Jean-Philippe/0000-0001-7284-9220; Maxted, Nigel/0000-0003-2762-8378;
Punch, Michael/0000-0002-4710-2165; Sushch, Iurii/0000-0002-2814-1257;
Bordas, Pol/0000-0002-0266-8536; Cutini, Sara/0000-0002-1271-2924;
Gasparrini, Dario/0000-0002-5064-9495; de Ona Wilhelmi,
Emma/0000-0002-5401-0744; Frailis, Marco/0000-0002-7400-2135; Daniel,
Michael/0000-0002-8053-7910; de los Reyes Lopez,
Raquel/0000-0003-0485-9552; Caraveo, Patrizia/0000-0003-2478-8018;
Komin, Nukri/0000-0003-3280-0582; Sgro', Carmelo/0000-0001-5676-6214;
SPINELLI, Paolo/0000-0001-6688-8864; Rando,
Riccardo/0000-0001-6992-818X; Bastieri, Denis/0000-0002-6954-8862;
Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins,
Melissa/0000-0003-1790-8018; Giroletti, Marcello/0000-0002-8657-8852;
Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario
/0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Drury,
Luke/0000-0002-9257-2270; Moulin, Emmanuel/0000-0003-4007-0145;
Chadwick, Paula/0000-0002-1468-2685; giommi, paolo/0000-0002-2265-5003;
Kneiske, Tanja M./0000-0002-3210-6200; Venter,
Christo/0000-0002-2666-4812; Casanova, Sabrina/0000-0002-6144-9122;
Anton, Gisela/0000-0003-2039-4724; Johannesson,
Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673;
Gargano, Fabio/0000-0002-5055-6395; Morselli, Aldo/0000-0002-7704-9553;
Thompson, David/0000-0001-5217-9135; lubrano,
pasquale/0000-0003-0221-4806; giglietto, nicola/0000-0002-9021-2888;
Reimer, Olaf/0000-0001-6953-1385; van Eldik,
Christopher/0000-0001-9669-645X; Katz, Uli/0000-0002-7063-4418;
FU CAPES Foundation, Ministry of Education of Brazil; Namibian authorities;
University of Namibia; German Ministry for Education and Research (BMBF)
[DLR 50OR0906]; Max Planck Society; French Ministry for Research;
CNRS-IN2P3; CNRS; UK Science and Technology Facilities Council (STFC);
IPNP of the Charles University; Polish Ministry of Science and Higher
Education; South African Department of Science and Technology; National
Research Foundation; Istituto Nazionale di Astrofisica in Italy; Centre
National d'Etudes Spatiales in France; RXTE
FX Supported by CAPES Foundation, Ministry of Education of Brazil.; The
support of the Namibian authorities and of the University of Namibia in
facilitating the construction and operation of H.E.S.S. is gratefully
acknowledged, as is the support by the German Ministry for Education and
Research (BMBF), the Max Planck Society, the French Ministry for
Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary
Programme of the CNRS, the UK Science and Technology Facilities Council
(STFC), the IPNP of the Charles University, the Polish Ministry of
Science and Higher Education, the South African Department of Science
and Technology and National Research Foundation, and by the University
of Namibia. We appreciate the excellent work of the technical support
staff in Berlin, Durham, Hamburg, Heidelberg, Palaiseau, Paris, Saclay,
and in Namibia in the construction and operation of the equipment.;
Additional support for science analysis during the operations phase is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National d'Etudes Spatiales in France.; The authors
acknowledge the support by the RXTE and Swift teams for providing ToO
observations and the use of the public HEASARC software packages. S.K.
and S.W. acknowledge support from the BMBF through grant DLR 50OR0906.
NR 43
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2011
VL 533
AR A110
DI 10.1051/0004-6361/201016170
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100110
ER
PT J
AU Bock, M
Grinberg, V
Pottschmidt, K
Hanke, M
Nowak, MA
Markoff, SB
Uttley, P
Rodriguez, J
Pooley, GG
Suchy, S
Rothschild, RE
Wilms, J
AF Boeck, M.
Grinberg, V.
Pottschmidt, K.
Hanke, M.
Nowak, M. A.
Markoff, S. B.
Uttley, P.
Rodriguez, J.
Pooley, G. G.
Suchy, S.
Rothschild, R. E.
Wilms, J.
TI Spectro-timing analysis of Cygnus X-1 during a fast state transition
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays: binaries; X-rays: individuals: CygX-1
ID X-RAY BINARIES; BROAD-BAND SPECTRUM; LONG-TERM VARIABILITY; BLACK-HOLE
CANDIDATES; ALL-SKY MONITOR; HARD STATE; LOW/HARD STATE; RADIO-EMISSION;
EXPLORER OBSERVATION; POWER SPECTRA
AB We present the analysis of two long, quasi-uninterrupted RXTE observations of Cygnus X-1 that span several days within a 10 d interval. The spectral characteristics during this observation cover the region where previous observations have shown the source to be most dynamic. Despite that the source behavior on time scales of hours and days is remarkably similar to that on year time scales. This includes a variety of spectral/temporal correlations that previously had only been observed over CygX-1's long-term evolution. Furthermore, we observe a full transition from a hard to a soft spectral state that occurs within less than 2.5 h - shorter than previously reported for any other similar CygX-1 transition. We describe the spectra with a phenomenological model dominated by a broken power law, and we fit the X-ray variability power spectra with a combination of a cutoff power law and Lorentzian components. The spectral and timing properties are correlated: the power spectrum Lorentzian components have an energy-dependent amplitude, and their peak frequencies increase with photon spectral index. Averaged over 3.2-10 Hz, the time lag between the variability in the 4.5-5.7 keV and 9.5-15 keV bands increases with decreasing hardness when the variability is dominated by the Lorentzian components during the hard state. The lag is small when there is a large power law noise contribution, shortly after the transition to the soft state. Interestingly, the soft state not only shows the shortest lags, but also the longest lags when the spectrum is at its softest and faintest. We discuss our results in terms of emission models for black hole binaries.
C1 [Boeck, M.; Grinberg, V.; Hanke, M.; Wilms, J.] Univ Erlangen Nurnberg, Astron Inst, Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany.
[Boeck, M.; Grinberg, V.; Hanke, M.; Wilms, J.] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany.
[Grinberg, V.] Univ Munich, Univ Sternwarte, D-81679 Munich, Germany.
[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.
[Nowak, M. A.] MIT CXC, Cambridge, MA 02139 USA.
[Markoff, S. B.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands.
[Uttley, P.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Rodriguez, J.] Univ Paris Diderot, Lab AIM, CEA, CNRS,INSU,CEA DSM,IRFU,SAp,Ctr Saclay,IRFU, F-91191 Gif Sur Yvette, France.
[Pooley, G. G.] Cavevdish Lab, Cambridge CB3 0HE, England.
[Suchy, S.; Rothschild, R. E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
RP Bock, M (reprint author), Univ Erlangen Nurnberg, Astron Inst, Dr Karl Remeis Sternwarte, Sternwartstr 7, D-96049 Bamberg, Germany.
EM Moritz.Boeck@sternwarte.uni-erlangen.de
RI Wilms, Joern/C-8116-2013;
OI Wilms, Joern/0000-0003-2065-5410; Rodriguez, Jerome/0000-0002-4151-4468
FU Bundesministerium fur Wirtschaft und Technologie through the Deutsches
Zentrum fur Luft-und Raumfahrt [50OR0701]; NASA [SV3-73016]; European
Community [FP7/2007-2013, ITN 215212]; International Space Science
Institute, Berne, Switzerland [116]
FX We acknowledge funding from the Bundesministerium fur Wirtschaft und
Technologie through the Deutsches Zentrum fur Luft-und Raumfahrt under
contract 50OR0701. M.A.N. was supported by NASA Grant SV3-73016. J.R.
acknowledges partial funding from the European Community's Seventh
Framework Programme (FP7/2007-2013) under grant agreement number ITN
215212 "Black Hole Universe". We thank the International Space Science
Institute, Berne, Switzerland for supporting team 116 and the X-ray
group at the Center for Astrophysics and Space Sciences of the
University of California at San Diego for their hospitality during the
initial stages of this project.
NR 65
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PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
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SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2011
VL 533
AR A8
DI 10.1051/0004-6361/201117159
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100008
ER
PT J
AU Bulbul, GE
Hasler, N
Bonamente, M
Joy, M
Marrone, D
Miller, A
Mroczkowski, T
AF Bulbul, G. E.
Hasler, N.
Bonamente, M.
Joy, M.
Marrone, D.
Miller, A.
Mroczkowski, T.
TI The effect of helium sedimentation on galaxy cluster masses and scaling
relations
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: clusters: general
ID X-RAY MEASUREMENTS; BREMSSTRAHLUNG GAUNT FACTOR; HUBBLE CONSTANT; CL
0016+16; CONSTRAINTS; DIFFUSION; ELEMENTS; PLASMA; GAS
AB Context. Recent theoretical studies predict that the inner regions of galaxy clusters may have an enhanced helium abundance due to sedimentation over the cluster lifetime. If sedimentation is not suppressed (e.g., by tangled magnetic fields), this may significantly affect the cluster mass estimates.
Aims. We use Chandra X-ray observations of eight relaxed galaxy clusters to investigate the upper limits to the effect of helium sedimentation on the measurement of cluster masses and the best-fit slopes of the Y(X) - M(500) and Y(X) -M(2500) scaling relations.
Methods. We calculated gas mass and total mass in two limiting cases: a uniform, unenhanced abundance distribution and a radial distribution from numerical simulations of helium sedimentation on a timescale of 11 Gyr.
Results. The assumed helium sedimentation model, on average, produces a negligible increase in the gas mass inferred within large radii (r < r(500)) (1.3 +/- 1.2%) and a 10.2 +/- 5.5% mean decrease in the total mass inferred within r < r(500). Significantly stronger effects in the gas mass (10.5 +/- 0.8%) and total mass (25.1 +/- 1.1%) are seen at small radii owing to a larger variance in helium abundance in the inner region, r <= 0.1 r(500).
Conclusions. We find that the slope of the Y(X) - M(500) scaling relation is not significantly affected by helium sedimentation.
C1 [Bulbul, G. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bulbul, G. E.; Hasler, N.; Bonamente, M.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Bonamente, M.; Joy, M.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Marrone, D.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Miller, A.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Mroczkowski, T.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
RP Bulbul, GE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM bonamem@email.uah.edu
OI Marrone, Daniel/0000-0002-2367-1080; Mroczkowski,
Tony/0000-0003-3816-5372
NR 31
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SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2011
VL 533
AR A6
DI 10.1051/0004-6361/201016407
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100006
ER
PT J
AU Dehaes, S
Bauwens, E
Decin, L
Eriksson, K
Raskin, G
Butler, B
Dowell, CD
Ali, B
Blommaert, JADL
AF Dehaes, S.
Bauwens, E.
Decin, L.
Eriksson, K.
Raskin, G.
Butler, B.
Dowell, C. D.
Ali, B.
Blommaert, J. A. D. L.
TI Structure of the outer layers of cool standard stars
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: chromospheres; stars: late-type; stars: winds, outflows; radio
continuum: stars
ID ISO-SWS CALIBRATION; SPECTRAL IRRADIANCE CALIBRATION; RADIO-CONTINUUM
EMISSION; OXYGEN-RICH GIANTS; CARBON-MONOXIDE; MODEL ATMOSPHERES;
CORONAL GRAVEYARD; SOLAR ATMOSPHERE; DIVIDING LINES; BRIGHT GIANTS
AB Context. Among late-type red giants, an interesting change occurs in the structure of the outer atmospheric layers as one moves to later spectral types in the Hertzsprung-Russell diagram: a chromosphere is always present, but the coronal emission diminishes and a cool massive wind steps in.
Aims. Where most studies have focussed on short-wavelength observations, this article explores the influence of the chromosphere and the wind on long-wavelength photometric measurements. The goal of this study is to assess wether a set of standard near-infrared calibration sources are fiducial calibrators in the far-infrared, beyond 50 mu m.
Methods. The observational spectral energy distributions were compared with the theoretical model predictions for a sample of nine K- and M-giants. The discrepancies found are explained using basic models for flux emission originating in a chromosphere or an ionised wind.
Results. For seven out of nine sample stars, a clear flux excess is detected at (sub)millimetre and/or centimetre wavelengths, while only observational upper limits are obtained for the other two. The precise start of the excess depends upon the star under consideration. For six sources the flux excess starts beyond 210 mu m and they can be considered as fiducial calibrators for Herschel/PACS (60-210 mu m). Out of this sample, four sources show no flux excess in the Herschel/SPIRE wavelength range (200-670 mu m) and are good calibration sources for this instrument as well. The flux at wavelengths shorter than similar to 1 mm is most likely dominated by an optically thick chromosphere, where an optically thick ionised wind is the main flux contributor at longer wavelengths.
Conclusions. Although the optical to mid-infrared spectrum of the studied K- and M-type infrared standard stars is represented well by a radiative equilibrium atmospheric model, a chromosphere and/or ionised stellar wind at higher altitudes dominates the spectrum in the (sub)millimetre and centimetre wavelength ranges. The presence of a flux excess has implications on the role of the stars as fiducial spectrophotometric calibrators in these wavelength ranges.
C1 [Dehaes, S.; Bauwens, E.; Decin, L.; Raskin, G.; Blommaert, J. A. D. L.] Katholieke Univ Leuven, Inst Sterrenkunde, Dept Phys & Astron, B-3001 Louvain, Belgium.
[Decin, L.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 Amsterdam, Netherlands.
[Eriksson, K.] Uppsala Univ, Dept Astron & Space Phys, S-75120 Uppsala, Sweden.
[Butler, B.] NRAO, Socorro, NM 87801 USA.
[Dowell, C. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ali, B.] CALTECH, IPAC, Pasadena, CA 91125 USA.
RP Dehaes, S (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Dept Phys & Astron, Celestijnenlaan 200D, B-3001 Louvain, Belgium.
EM Leen.Decin@ster.kuleuven.be
FU Fund for Scientific Research, Flanders; National Science Foundation
[AST-0540882]; Fund for Scientific Research Flanders (Belgium)
FX Postdoctoral Fellow of the Fund for Scientific Research, Flanders.; This
work is based on observations collected at the European Southern
Observatory, La Silla, Chile within program ESO 71.D-0600 and on
observations collected with the IRAM 30 m telescope within project
038_03. We would like to thank R. Zylka and S. Leon for their support
for the data reduction. The research at the Caltech Submillimetre
Observatory is supported by grant AST-0540882 from the National Science
Foundation. S.D. and L.D. acknowledge financial support from the Fund
for Scientific Research Flanders (Belgium). We thank B. Vandenbussche
for fruitful discussions.
NR 59
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2011
VL 533
AR A107
DI 10.1051/0004-6361/200912442
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100107
ER
PT J
AU Duro, R
Dauser, T
Wilms, J
Pottschmidt, K
Nowak, MA
Fritz, S
Kendziorra, E
Kirsch, MGF
Reynolds, CS
Staubert, R
AF Duro, R.
Dauser, T.
Wilms, J.
Pottschmidt, K.
Nowak, M. A.
Fritz, S.
Kendziorra, E.
Kirsch, M. G. F.
Reynolds, C. S.
Staubert, R.
TI The broad iron K alpha line of Cygnus X-1 as seen by XMM-Newton in the
EPIC-pn modified timing mode
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays: binaries; black hole physics; gravitation
ID X-RAY SPECTROSCOPY; BLACK-HOLE; EMISSION; STATE; VARIABILITY; EVOLUTION;
EXPLORER; CHANDRA; SYSTEM; ORBIT
AB We present the analysis of the broadened, flourescent iron K alpha line in simultaneous XMM-Newton and RXTE data from the black hole Cygnus X-1. The XMM-Newton data were taken in a modified version of the timing mode of the EPIC-pn camera. In this mode the lower energy threshold of the instrument is increased to 2.8 keV to avoid telemetry drop outs due to the brightness of the source, while at the same time preserving the signal-to-noise ratio in the FeK alpha band. We find that the best-fit spectrum consists of the sum of an exponentially cutoff power-law and relativistically smeared, ionized reflection. The shape of the broadened FeKa feature is due to strong Compton broadening combined with relativistic broadening. Assuming a standard, thin accretion disk, the black hole is close to rotating maximally.
C1 [Duro, R.; Dauser, T.; Wilms, J.; Fritz, S.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, D-96049 Bamberg, Germany.
[Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Pottschmidt, K.] CRESST, Greenbelt, MD 20771 USA.
[Pottschmidt, K.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Nowak, M. A.] MIT, Kavli Inst Astrophys, Cambridge, MA 02139 USA.
[Fritz, S.; Kendziorra, E.; Staubert, R.] Univ Tubingen, Inst Astron & Astrophys, D-72074 Tubingen, Germany.
[Kirsch, M. G. F.] European Space Agcy, European Space Operat Ctr, D-64293 Darmstadt, Germany.
[Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Reynolds, C. S.] Univ Maryland, Maryland Astron Ctr Theory & Computat, College Pk, MD 20742 USA.
RP Duro, R (reprint author), Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, Sternwartstr 7, D-96049 Bamberg, Germany.
RI Wilms, Joern/C-8116-2013
OI Wilms, Joern/0000-0003-2065-5410
FU European Commission [ITN215212]; Bundesministerium fur Wirtschaft and
Technologie under Deutsches Zentrum fur Luft- und Raumfahrt [50OR0701,
50OR1001]; ESA member states; NASA
FX This work was partly supported by the European Commission under contract
ITN215212 "Black Hole Universe" and by the Bundesministerium fur
Wirtschaft and Technologie under Deutsches Zentrum fur Luft- und
Raumfahrt grants 50OR0701 and 50OR1001. This paper is based on
observations obtained with XMM-Newton, an ESA science mission with
instruments and contributions directly funded by ESA member states and
NASA. We thank Norbert Schartel and the XMM-Newton operations team for
agreeing to perform observations in a new and untested mode, Maria
Diaz-Trigo for many useful discussions on CTE and pile-up effects in the
EPIC-pn camera, Manfred Hanke for his significant input concerning the
data analysis and interpretation for black hole X-ray data, and Jerome
Rodriguez for his many insightful comments.
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J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2011
VL 533
AR L3
DI 10.1051/0004-6361/201117446
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100150
ER
PT J
AU Elbaz, D
Dickinson, M
Hwang, HS
Diaz-Santos, T
Magdis, G
Magnelli, B
Le Borgne, D
Galliano, F
Pannella, M
Chanial, P
Armus, L
Charmandaris, V
Daddi, E
Aussel, H
Popesso, P
Kartaltepe, J
Altieri, B
Valtchanov, I
Coia, D
Dannerbauer, H
Dasyra, K
Leiton, R
Mazzarella, J
Alexander, DM
Buat, V
Burgarella, D
Chary, RR
Gilli, R
Ivison, RJ
Juneau, S
Le Floc'h, E
Lutz, D
Morrison, GE
Mullaney, JR
Murphy, E
Pope, A
Scott, D
Brodwin, M
Calzetti, D
Cesarsky, C
Charlot, S
Dole, H
Eisenhardt, P
Ferguson, HC
Schreiber, NF
Frayer, D
Giavalisco, M
Huynh, M
Koekemoer, AM
Papovich, C
Reddy, N
Surace, C
Teplitz, H
Yun, MS
Wilson, G
AF Elbaz, D.
Dickinson, M.
Hwang, H. S.
Diaz-Santos, T.
Magdis, G.
Magnelli, B.
Le Borgne, D.
Galliano, F.
Pannella, M.
Chanial, P.
Armus, L.
Charmandaris, V.
Daddi, E.
Aussel, H.
Popesso, P.
Kartaltepe, J.
Altieri, B.
Valtchanov, I.
Coia, D.
Dannerbauer, H.
Dasyra, K.
Leiton, R.
Mazzarella, J.
Alexander, D. M.
Buat, V.
Burgarella, D.
Chary, R-R
Gilli, R.
Ivison, R. J.
Juneau, S.
Le Floc'h, E.
Lutz, D.
Morrison, G. E.
Mullaney, J. R.
Murphy, E.
Pope, A.
Scott, D.
Brodwin, M.
Calzetti, D.
Cesarsky, C.
Charlot, S.
Dole, H.
Eisenhardt, P.
Ferguson, H. C.
Schreiber, N. Foerster
Frayer, D.
Giavalisco, M.
Huynh, M.
Koekemoer, A. M.
Papovich, C.
Reddy, N.
Surace, C.
Teplitz, H.
Yun, M. S.
Wilson, G.
TI GOODS-Herschel: an infrared main sequence for star-forming galaxies
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; infrared: galaxies; galaxies: evolution; galaxies:
starburst
ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTION; DEEP-FIELD-SOUTH;
POLYCYCLIC AROMATIC-HYDROCARBONS; HIGH-REDSHIFT GALAXIES; SIMILAR-TO 3;
MIDINFRARED SPECTROSCOPY; SUBMILLIMETER GALAXIES; FORMATION HISTORY;
MASSIVE GALAXIES
AB We present the deepest 100 to 500 mu m far-infrared observations obtained with the Herschel Space Observatory as part of the GOODS-Herschel key program, and examine the infrared (IR) 3-500 mu m spectral energy distributions (SEDs) of galaxies at 0 < z < 2.5, supplemented by a local reference sample from IRAS, ISO, Spitzer, and AKARI data. We determine the projected star formation densities of local galaxies from their radio and mid-IR continuum sizes.
We find that the ratio of total IR luminosity to rest-frame 8 mu m luminosity, IR8 ( L-IR(tot)/L-8), follows a Gaussian distribution centered on IR8 = 4 (sigma = 1.6) and defines an IR main sequence for star-forming galaxies independent of redshift and luminosity. Outliers from this main sequence produce a tail skewed toward higher values of IR8. This minority population (< 20%) is shown to consist of starbursts with compact projected star formation densities. IR8 can be used to separate galaxies with normal and extended modes of star formation from compact starbursts with high-IR8, high projected IR surface brightness (Sigma(IR) > 3 x 10(10) L-circle dot kpc(-2)) and a high specific star formation rate (i.e., starbursts). The rest-frame, UV-2700 angstrom size of these distant starbursts is typically half that of main sequence galaxies, supporting the correlation between star formation density and starburst activity that is measured for the local sample.
Locally, luminous and ultraluminous IR galaxies, (U) LIRGs (L-IR(tot) >= 10(11) L-circle dot), are systematically in the starburst mode, whereas most distant (U) LIRGs form stars in the "normal" main sequence mode. This confusion between two modes of star formation is the cause of the so-called "mid-IR excess" population of galaxies found at z > 1.5 by previous studies. Main sequence galaxies have strong polycyclic aromatic hydrocarbon (PAH) emission line features, a broad far-IR bump resulting from a combination of dust temperatures (T-dust similar to 15-50 K), and an effective T-dust similar to 31 K, as derived from the peak wavelength of their infrared SED. Galaxies in the starburst regime instead exhibit weak PAH equivalent widths and a sharper far-IR bump with an effective T-dust similar to 40 K. Finally, we present evidence that the mid-to-far IR emission of X-ray active galactic nuclei (AGN) is predominantly produced by star formation and that candidate dusty AGNs with a power-law emission in the mid-IR systematically occur in compact, dusty starbursts. After correcting for the effect of starbursts on IR8, we identify new candidates for extremely obscured AGNs.
C1 [Elbaz, D.; Hwang, H. S.; Magdis, G.; Galliano, F.; Pannella, M.; Chanial, P.; Daddi, E.; Aussel, H.; Dannerbauer, H.; Dasyra, K.; Leiton, R.; Le Floc'h, E.; Mullaney, J. R.; Cesarsky, C.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA DSM Irfu, CNRS, F-91191 Gif Sur Yvette, France.
[Dickinson, M.; Kartaltepe, J.; Brodwin, M.; Reddy, N.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Diaz-Santos, T.; Charmandaris, V.] Univ Crete, Dept Phys, Iraklion 71003, Greece.
[Diaz-Santos, T.; Charmandaris, V.] Univ Crete, Inst Theoret & Computat Phys, Iraklion 71003, Greece.
[Magnelli, B.; Popesso, P.; Lutz, D.; Schreiber, N. Foerster] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany.
[Le Borgne, D.; Charlot, S.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Armus, L.; Chary, R-R; Murphy, E.; Huynh, M.; Teplitz, H.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Charmandaris, V.] IESL Fdn Res & Technol, Iraklion 71110, Greece.
[Charmandaris, V.] Observ Paris, F-75014 Paris, France.
[Altieri, B.; Valtchanov, I.; Coia, D.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain.
[Leiton, R.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Mazzarella, J.] CALTECH, IPAC, Pasadena, CA 91125 USA.
[Alexander, D. M.] Univ Durham, Dept Phys & Astron, Durham DH1 3LE, England.
[Buat, V.; Burgarella, D.; Surace, C.] Univ Aix Marseille, CNRS, Lab Astrophys Marseille, OAMP, F-13388 Marseille 13, France.
[Gilli, R.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Juneau, S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Morrison, G. E.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Morrison, G. E.] Canada France Hawaii Telescope, Kamuela, HI 96743 USA.
[Pope, A.; Calzetti, D.; Giavalisco, M.; Yun, M. S.; Wilson, G.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Dole, H.] Univ Paris 11, IAS, F-91405 Orsay, France.
[Dole, H.] CNRS, UMR 8617, F-91405 Orsay, France.
[Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ferguson, H. C.; Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21228 USA.
[Frayer, D.] Natl Radio Astron Observ, Green Bank, WV 24944 USA.
[Papovich, C.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77845 USA.
[Papovich, C.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77845 USA.
RP Elbaz, D (reprint author), Univ Paris Diderot, Lab AIM Paris Saclay, CEA DSM Irfu, CNRS, Pt Courrier 131, F-91191 Gif Sur Yvette, France.
EM delbaz@cea.fr
RI Charmandaris, Vassilis/A-7196-2008; Leiton, Roger/A-9221-2012; Daddi,
Emanuele/D-1649-2012; Magdis, Georgios/C-7295-2014; Ivison,
R./G-4450-2011;
OI Alexander, David/0000-0002-5896-6313; Koekemoer,
Anton/0000-0002-6610-2048; Altieri, Bruno/0000-0003-3936-0284;
Charmandaris, Vassilis/0000-0002-2688-1956; Daddi,
Emanuele/0000-0002-3331-9590; Magdis, Georgios/0000-0002-4872-2294;
Ivison, R./0000-0001-5118-1313; Dasyra, Kalliopi/0000-0002-1482-2203;
Leiton, Roger/0000-0002-0744-489X; Scott, Douglas/0000-0002-6878-9840;
Mazzarella, Joseph/0000-0002-8204-8619
FU Centre National d'Etudes Spatiales (CNES); French National Agency for
Research (ANR) [ANR-09-BLAN-0224]; EU ToK [39965, FP7-REGPOT 206469];
NASA; BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR
(Germany); ASI/INAF (Italy); CICYT/MCYT (Spain); CSA (Canada); NAOC
(China); CEA; CNRS (France); ASI (Italy); MCINN (Spain); Stockholm
Observatory (Sweden); STFC (UK); NASA (USA)
FX We wish to thank R.Gobat for generating the three color images of the
GOODS fields and our referee Kai Noeske for his constructive comments
that helped improving the paper. D. Elbaz and H. S. Hwang thank the
Centre National d'Etudes Spatiales (CNES) for their support. D. Elbaz
wishes to thank the French National Agency for Research (ANR) for their
support (ANR-09-BLAN-0224). V.C. would like to acknowledge partial
support from the EU ToK grant 39965 and FP7-REGPOT 206469. Support for
this work was also provided by NASA through an award issued by
JPL/Caltech. PACS has been developed by a consortium of institutes led
by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC
(Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/OAA/OAP/OAT,
LENS, SISSA (Italy); IAC (Spain). This development has been supported by
the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES
(France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE
has been developed by a consortium of institutes led by Cardiff
University (UK) and including Univ. Lethbridge (Canada); NAOC (China);
CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm
Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC,
Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This
development has been supported by national funding agencies: CSA
(Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN
(Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA).
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JI Astron. Astrophys.
PD SEP
PY 2011
VL 533
AR A119
DI 10.1051/0004-6361/201117239
PG 26
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SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100119
ER
PT J
AU Gruber, D
Lachowicz, P
Bissaldi, E
Briggs, MS
Connaughton, V
Greiner, J
van der Horst, AJ
Kanbach, G
Rau, A
Bhat, PN
Diehl, R
von Kienlin, A
Kippen, RM
Meegan, CA
Paciesas, WS
Preece, RD
Wilson-Hodge, C
AF Gruber, D.
Lachowicz, P.
Bissaldi, E.
Briggs, M. S.
Connaughton, V.
Greiner, J.
van der Horst, A. J.
Kanbach, G.
Rau, A.
Bhat, P. N.
Diehl, R.
von Kienlin, A.
Kippen, R. M.
Meegan, C. A.
Paciesas, W. S.
Preece, R. D.
Wilson-Hodge, C.
TI Quasi-periodic pulsations in solar flares: new clues from the Fermi
Gamma-Ray Burst Monitor
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: flares; methods: statistical; methods: data analysis; methods:
observational
ID MAGNETOHYDRODYNAMIC OSCILLATIONS; SPECTRAL-ANALYSIS; POWER SPECTRA;
SPACED DATA; EMISSION; 090709A; GRB; SIGNALS; MISSION; ORIGIN
AB Aims. In the past four decades, it has been observed that solar flares display quasi-periodic pulsations (QPPs) from the lowest, i.e. radio, to the highest, i.e. gamma-ray, frequencies in the electromagnetic spectrum. It remains unclear which mechanism creates these QPPs. In this paper, we analyze four bright solar flares that display compelling signatures of quasi-periodic behavior and were observed with the Gamma-Ray Burst Monitor (GBM) onboard the Fermi satellite. Because GBM covers over three decades in energy (8 keV to 40 MeV), it is regarded as a key instrument in our attempt to understand the physical processes that drive solar flares.
Methods. We tested for periodicity in the time series of the solar flares observed by GBM by applying a classical periodogram analysis. However, in contrast to previous authors, we did not detrend the raw light curve before creating the power spectral density (PSD) spectrum. To assess the significance of the frequencies, we used a method that is commonly applied to X-ray binaries and Seyfert galaxies. This technique takes into account the underlying continuum of the PSD, which for all of these sources has a P(f) similar to f (-alpha) dependence and is typically labeled red-noise.
Results. We checked the reliability of this technique by applying it to observations of a solar flare that had been observed by the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI). These data contain, besides any potential periodicity from the Sun, a 4 s rotational period caused by the rotation of the spacecraft about its axis. We were unable to identify any intrinsic solar quasi-periodic pulsation but we did manage to reproduce the instrumental periodicity. Moreover, with the method adopted here, we do not detect significant QPPs in the four bright solar flares observed by GBM. We stress that for this kind of analyses it is of utmost importance to account appropriately for the red-noise component in the PSD of these astrophysical sources.
C1 [Gruber, D.; Greiner, J.; Kanbach, G.; Rau, A.; Diehl, R.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Lachowicz, P.] Green Cross Capital Pty Ltd, Ultimo, NSW 2007, Australia.
[Bissaldi, E.] Univ Innsbruck, Inst Astro & Particle Phys, A-6176 Innsbruck, Austria.
[Briggs, M. S.; Connaughton, V.; van der Horst, A. J.; Bhat, P. N.; Paciesas, W. S.; Preece, R. D.] Univ Alabama, NSSTC, Huntsville, AL 35805 USA.
[Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Meegan, C. A.] Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA.
[Wilson-Hodge, C.] NASA, Space Sci Off, Marshall Space Flight Ctr Huntsville, Huntsville, AL 35812 USA.
RP Gruber, D (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr,Postfach 1312, D-85748 Garching, Germany.
EM dgruber@mpe.mpg.de
RI Bissaldi, Elisabetta/K-7911-2016;
OI Bissaldi, Elisabetta/0000-0001-9935-8106; Preece,
Robert/0000-0003-1626-7335
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SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2011
VL 533
AR A61
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SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100061
ER
PT J
AU Kumar, MSN
Sharma, S
Davis, CJ
Borissova, J
Grave, JMC
AF Kumar, M. S. N.
Sharma, S.
Davis, C. J. .
Borissova, J.
Grave, J. M. C.
TI H-2 flows in the Corona Australis cloud and their driving sources
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: formation; ISM: jets and outflows; stars: variables: T Tauri,
Herbig Ae/Be; Herbig-Haro objects
ID YOUNG STELLAR OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; HERBIG-HARO
OBJECTS; MOLECULAR CLOUD; R-CRA; OUTFLOWS; EVOLUTION; REGION; NGC-1333;
TAURUS
AB Aims. We uncover the H-2 flows in the Corona Australis molecular cloud and in particular identify the flows from the Coronet cluster.
Methods. A deep, near-infrared H-2 upsilon = 1-0 S(1), 2.122 mu m-line, narrow-band imaging survey of the R CrA cloud core was carried out. The nature of all candidate-driving sources in the region was evaluated using data available from the literature and also by fitting the spectral energy distributions (SED) of each source either with an extincted photosphere or YSO model. Archival Spitzer-IRAC and MIPS data was used to obtain photometry, which was combined with USNO, 2MASS catalogs and millimeter photometry from the literature, to build the SEDs. We identify the best candidate-driving source for each outflow by comparing the flow properties, available proper motions, and the known/estimated properties of the driving sources. We also adopted the thumbrule of outflow power as proportional to source luminosity and inversely proportional to the source age to reach a consensus.
Results. Continuum-subtracted, narrow-band images reveal several new Molecular Hydrogen emission-line Objects (MHOs). Together with previously known MHOs and Herbig-Haro objects we catalog at least 14 individual flow components of which 11 appear to be driven by the R CrA aggregate members. The flows originating in the Coronet cluster have lengths of similar to 0.1-0.2 pc. Eight out of nine submillimeter cores mapped in the Coronet cluster region display embedded stars driving an outflow component. Roughly 80% of the youngest objects in the Coronet are associated with outflows. The MHO flows to the west of the Coronet display lobes moving to the west and vice-versa, resulting in nondetections of the counter lobe in our deep imaging. We speculate that these counter flows may be experiencing a stunting effect in penetrating the dense central core.
Conclusions. Although this work has reduced the ambiguities for many flows in the Coronet region, one of the brightest H-2 feature (MHO2014) and a few fainter features in the region remain unassociated with a clear driving source. The flows from Coronet, therefore, continue to be interesting targets for future studies.
C1 [Kumar, M. S. N.; Grave, J. M. C.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Sharma, S.; Borissova, J.] Univ Valparaiso, Fac Ciencias, Dept Fis & Astron, Valparaiso, Chile.
[Davis, C. J. .] Joint Astron Ctr, Hilo, HI 96720 USA.
[Davis, C. J. .] NASA Headquarters, Sci Miss Directorate, Washington, DC 20546 USA.
[Sharma, S.] Aryabhatta Res Inst Observat Sci, Naini Tal 263129, India.
RP Kumar, MSN (reprint author), Univ Porto, Ctr Astrofis, Rua Estrelas, P-4150762 Oporto, Portugal.
EM nanda@astro.up.pt
RI Kumar, Nanda/I-4183-2013;
OI Grave, Jorge/0000-0003-4897-4595
FU Ciencia contract; FCT/MCTES (Portugal); POPH/FSE (EC); FONDECYT
[1080086]; Ministry for the Economy, Development, and Tourism; Center of
Excellence in Astrophysics and Associated Technologies [BASAL CATA
PFB-06]; JPL/Caltech
FX We thank Christopher Groppi for providing the CO data for overplotting
in Fig. 3. Kumar is supported by a Ciencia 2007 contract, funded by
FCT/MCTES (Portugal) and POPH/FSE (EC). S.S. and J.B. are supported by
FONDECYT No. 1080086, by the Ministry for the Economy, Development, and
Tourism's Programa Inicativa Cientifica Milenio through grant P07-021-F,
awarded to The Milky Way Millennium Nucleus and from Comitee Mixto
ESO-GOBIERNO DE CHILE. S.S. received partial support from Center of
Excellence in Astrophysics and Associated Technologies BASAL CATA
PFB-06. This work is based in part on archival data obtained with the
Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA. Support for this work was provided by an award issued by
JPL/Caltech.
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SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2011
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SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100137
ER
PT J
AU Mahy, L
Martins, F
Machado, C
Donati, JF
Bouret, JC
AF Mahy, L.
Martins, F.
Machado, C.
Donati, J. -F.
Bouret, J. -C.
TI The two components of the evolved massive binary LZ Cephei Testing the
effects of binarity on stellar evolution
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: early-type; binaries: general; stars: fundamental parameters;
stars: winds, outflows
ID O-TYPE STARS; UPPER MAIN-SEQUENCE; CLOSE BINARIES; SPECTROSCOPIC
BINARIES; RADIAL-VELOCITIES; NORTHERN STARS; CLASSIFICATION; MODELS;
SYSTEM; ASSOCIATIONS
AB Aims. We present an in-depth study of the two components of the binary system LZCep to constrain the effects of binarity on the evolution of massive stars.
Methods. We analyzed a set of high-resolution, high signal-to-noise ratio optical spectra obtained over the orbital period of the system to perform a spectroscopic disentangling and derive an orbital solution. We subsequently determine the stellar properties of each component by means of an analysis with the CMFGEN atmosphere code. Finally, with the derived stellar parameters, we model the Hipparcos photometric light curve using the program NIGHTFALL to obtain the orbit inclination and the stellar masses.
Results. LZCep is a O9III+ON 9.7V binary. It is as a semi-detached system in which either the primary or the secondary star almost fills up its Roche lobe. The dynamical masses are about 16.0 M(circle dot) (primary) and 6.5 M(circle dot) (secondary). The latter is lower than the typical mass of late-type O stars. The secondary component is chemically more evolved than the primary (which barely shows any sign of CNO processing), with strong helium and nitrogen enhancements as well as carbon and oxygen depletions. These properties (surface abundances and mass) are typical of Wolf-Rayet stars, although the spectral type is ON 9.7V. The luminosity of the secondary is consistent with that of core He-burning objects. The preferred, tentative evolutionary scenario to explain the observed properties involves mass transfer from the secondary - which was initially more massive-towards the primary. The secondary is now almost a core He-burning object, probably with only a thin envelope of H-rich and CNO processed material. A very inefficient mass transfer is necessary to explain the chemical appearance of the primary. Alternative scenarios are discussed but they are affected by greater uncertainties.
C1 [Mahy, L.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Martins, F.; Machado, C.] Univ Montpellier 2, F-34095 Montpellier 05, France.
[Martins, F.; Machado, C.] CNRS, UMR 5299, LUPM, F-34095 Montpellier 05, France.
[Donati, J. -F.] Univ Toulouse, F-31400 Toulouse, France.
[Donati, J. -F.] CNRS, UMR 5277, IRAP, F-31400 Toulouse, France.
[Bouret, J. -C.] Univ Aix Marseille 1, F-13388 Marseille 13, France.
[Bouret, J. -C.] CNRS, UMR 6110, LAM, F-13388 Marseille 13, France.
[Bouret, J. -C.] NASA, GSFC, Greenbelt, MD 20771 USA.
RP Mahy, L (reprint author), Univ Liege, Inst Astrophys & Geophys, Bat B5C,Allee 6 Aout 17, B-4000 Liege, Belgium.
EM mahy@astro.ulg.ac.be
FU PRODEX XMM (Belspo); Communaute francaise de Belgique - Action de
recherche concertee - ARC - Academie Wallonie-Europe
FX We thank the anonymous referee for valuable comments that helped us to
improve the presentation of the paper and the discussion of our results.
L.M. thanks the PRODEX XMM/Integral contract (Belspo) and the Communaute
francaise de Belgique - Action de recherche concertee - ARC - Academie
Wallonie-Europe for their support. We thank John Hillier for making his
code CMFGEN available and for constant support with its use.
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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 SEP
PY 2011
VL 533
AR A9
DI 10.1051/0004-6361/201116993
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100009
ER
PT J
AU Mucciarelli, P
Preibisch, T
Zinnecker, H
AF Mucciarelli, P.
Preibisch, T.
Zinnecker, H.
TI Revealing the "missing" low-mass stars in the S254-S258 star forming
region by deep X-ray imaging
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: formation; stars: pre-main sequence; open clusters and
associations: individual: S254-S258; X-rays: stars
ID ORION ULTRADEEP PROJECT; YOUNG STELLAR OBJECTS; METHANOL MASERS;
PARAMETER-ESTIMATION; INTERSTELLAR-MEDIUM; NEBULA CLUSTER; CARINA
COMPLEX; RCW 120; CHANDRA; EMISSION
AB Context. X-ray observations provide a very good way to reveal the population of young stars in star forming regions avoiding the biases introduced when selecting samples based on infrared excess.
Aims. The aim of this study was to find an explanation for the remarkable morphology of the central part of the S254-S258 star forming complex, where a dense embedded cluster of very young stellar objects (S255-IR) is sandwiched between the two H II regions S255 and S257. This interesting configuration had led to different speculations such as dynamical ejection of the B-stars from the central cluster or triggered star formation in a cloud that was swept up in the collision zone between the two expanding H II regions. The presence or absence, and the spatial distribution of low-mass stars associated with these B-stars can discriminate between the possible scenarios.
Methods. We performed a deep Chandra X-ray observation of the S254-S258 region in order to efficiently discriminate young stars (with and without circumstellar matter) from the numerous older field stars in the area.
Results. We detected 364 X-ray point sources in a 17' x 17' field (approximate to 8x8 pc). This X-ray catalog provides, for the first time, a complete sample of all young stars in the region down to similar to 0.5 M(circle dot). A clustering analysis identifies three significant clusters: the central embedded cluster S255-IR and two smaller clusterings in S256 and S258. Sixty-four X-ray sources can be classified as members in one of these clusters. After accounting for X-ray background contaminants, this implies that about 250 X-ray sources constitute a widely scattered population of young stars, distributed over the full field-of-view of our X-ray image. This distributed young stellar population is considerably larger than the previously known number of non-clustered young stars selected by infrared excesses. Comparison of the X-ray luminosity function with that of the Orion Nebula Cluster suggests a total population of similar to 2000 young stars in the observed part of the S254-S258 region.
Conclusions. The observed number of similar to 250 X-ray detected distributed young stars agrees well with the expectation for the low-mass population associated to the B-stars in S255 and S257 as predicted by an IMF extrapolation. These results are consistent with the scenario that these two B-stars represent an earlier stellar population and that their expanding H II regions have swept up the central cloud and trigger star formation (i.e. the central embedded cluster S255-IR) therein.
C1 [Mucciarelli, P.; Preibisch, T.] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Mucciarelli, P.] Exzellenzcluster Universe, D-85748 Garching, Germany.
[Zinnecker, H.] Astrophys Inst Potsdam, D-14482 Potsdam, Germany.
[Zinnecker, H.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany.
[Zinnecker, H.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Mucciarelli, P (reprint author), Univ Munich, Univ Sternwarte Munchen, Scheinerstr 1, D-81679 Munich, Germany.
EM pmuccia@usm.uni-muenchen.de; preibisch@usm.uni-muenchen.de
FU National Aeronautics Space Administration (NASA) [NAS8-03060]; Munich
Cluster of Excellence: "Origin and Structure of the Universe"; National
Science Foundation
FX We would like to thank the referee for several suggestions that helped
to improve this paper. This work is based on observations obtained with
the Chandra X-ray Observatory, which is operated by the Smithsonian
Astrophysical Observatory for and on behalf of the National Aeronautics
Space Administration (NASA) under contract NAS8-03060. Our analysis
presented in this paper was supported by the Munich Cluster of
Excellence: "Origin and Structure of the Universe". This publication
makes use of data products from the Two Micron All Sky Survey, which is
a joint project of the University of Massachusetts and the Infrared
Processing and Analysis Center/California Institute of Technology,
funded by the National Aeronautics and Space Administration and the
National Science Foundation, and of observations made with the Spitzer
Space Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with NASA.
NR 69
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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 SEP
PY 2011
VL 533
AR A121
DI 10.1051/0004-6361/201117074
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100121
ER
PT J
AU Ore, CMD
Fulchignoni, M
Cruikshank, DP
Barucci, MA
Brunetto, R
Campins, H
de Bergh, C
Debes, JH
Dotto, E
Emery, JP
Grundy, WM
Jones, AP
Mennella, V
Orthous-Daunay, FR
Owen, T
Pascucci, I
Pendleton, YJ
Pinilla-Alonso, N
Quirico, E
Strazzulla, G
AF Ore, C. M. Dalle
Fulchignoni, M.
Cruikshank, D. P.
Barucci, M. A.
Brunetto, R.
Campins, H.
de Bergh, C.
Debes, J. H.
Dotto, E.
Emery, J. P.
Grundy, W. M.
Jones, A. P.
Mennella, V.
Orthous-Daunay, F. R.
Owen, T.
Pascucci, I.
Pendleton, Y. J.
Pinilla-Alonso, N.
Quirico, E.
Strazzulla, G.
TI Organic materials in planetary and protoplanetary systems: nature or
nurture?
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE planets and satellites: composition; comets: general; circumstellar
matter; Kuiper belt: general; dust, extinction
ID HYDROGENATED AMORPHOUS-CARBON; DIFFUSE INTERSTELLAR-MEDIUM; KUIPER-BELT
OBJECTS; AROMATIC-HYDROCARBON MOLECULES; INTERPLANETARY DUST PARTICLES;
YOUNG CIRCUMSTELLAR DISKS; TRANS-NEPTUNIAN OBJECTS; OUTER SOLAR-SYSTEM;
H-ATOM IRRADIATION; COMET 81P/WILD 2
AB Aims. The objective of this work is to summarize the discussion of a workshop aimed at investigating the properties, origins, and evolution of the materials that are responsible for the red coloration of the small objects in the outer parts of the solar system. Because of limitations or inconsistencies in the observations and, until recently, the limited availability of laboratory data, there are still many questions on the subject. Our goal is to approach two of the main questions in a systematic way:
- Is coloring an original signature of materials that are presolar in origin ("nature") or stems from post-formational chemical alteration, or weathering ("nurture")?
- What is the chemical signature of the material that causes spectra to be sloped towards the red in the visible? We examine evidence available both from the laboratory and from observations sampling different parts of the solar system and circumstellar regions (disks).
Methods. We present a compilation of brief summaries gathered during the workshop and describe the evidence towards a primordial vs. evolutionary origin for the material that reddens the small objects in the outer parts of our, as well as in other, planetary systems. We proceed by first summarizing laboratory results followed by observational data collected at various distances from the Sun.
Results. While laboratory experiments show clear evidence of irradiation effects, particularly from ion bombardment, the first obstacle often resides in the ability to unequivocally identify the organic material in the observations. The lack of extended spectral data of good quality and resolution is at the base of this problem. Furthermore, that both mechanisms, weathering and presolar, act on the icy materials in a spectroscopically indistinguishable way makes our goal of defining the impact of each mechanism challenging.
Conclusions. Through a review of some of the workshop presentations and discussions, encompassing laboratory experiments as well as observational data, we infer that both "nature" and "nurture" are instrumental in the coloration of small objects in the outer parts of the solar system. While in the case of some observations it is clear that the organic reddening material originated before the solar nebula (i.e. presolar grains found in meteorites), for many other cases pointers are not as clear and indicate a concurrence of both processes.
C1 [Ore, C. M. Dalle] Observ Paris, Ctr Int Ateliers Sci, F-75014 Paris, France.
[Ore, C. M. Dalle] SETI Inst, Mountain View, CA 94043 USA.
[Pinilla-Alonso, N.] NASA, Nasa Postdoctoral Program, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Fulchignoni, M.; Barucci, M. A.] Observ Paris, LESIA, F-92195 Meudon, France.
[Brunetto, R.; Jones, A. P.] Univ Paris 11, Inst Astrophys Spatiale IAS, F-91405 Orsay, France.
[Brunetto, R.; Jones, A. P.] CNRS, F-91405 Orsay, France.
[Campins, H.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA.
[Dotto, E.] INAF Osservatorio Astron Roma, I-00040 Rome, Italy.
[Emery, J. P.] Univ Tennessee, Earth & Planetary Sci Dept, Knoxville, TN 37919 USA.
[Grundy, W. M.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Mennella, V.] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy.
[Orthous-Daunay, F. R.; Quirico, E.] UJF Grenoble 1, CNRS INSU, Inst Planetol & Astrophys Grenoble IPAG UMR 5274, F-38041 Grenoble, France.
[Owen, T.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Pascucci, I.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Pascucci, I.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Pendleton, Y. J.] NASA, Lunar Sci Inst, Moffett Field, CA 94035 USA.
[Strazzulla, G.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy.
[Debes, J. H.] NASA, Postdoctoral Program, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Ore, CMD (reprint author), Observ Paris, Ctr Int Ateliers Sci, F-75014 Paris, France.
EM Cristina.M.DalleOre@nasa.gov; marcello.fulchignoni@obspm.fr;
Dale.P.Cruikshank@nasa.gov; Antonella.Barucci@obspm.fr;
Catherine.deBergh@obspm.fr; Dotto@mporzio.astro.it; JEmery2@utk.edu;
W.Grundy@lowell.edu; owen@ifa.hawaii.edu; Pascucci@stsci.edu;
noemi.pinilla-alonso@nasa.gov; Gianni@oact.inaf.it
RI quirico, eric/K-9650-2013;
OI quirico, eric/0000-0003-2768-0694; Dotto,
Elisabetta/0000-0002-9335-1656; Strazzulla, Giovanni/0000-0003-1412-4023
FU Centre International d'Ateliers Scientifiques de l'Observatoire de
Paris; NASA at Ames Research Center; NASA
FX This paper is based on the conclusions of the workshop "Organic material
in planetary system: "nature" or "nurture"?" held on May 27-29, 2010 at
the Centre International d'Ateliers Scientifiques de l'Observatoire de
Paris with the participation of all the authors. C.M.D.O. aknowledges
support from the Centre International d'Ateliers Scientifiques de
l'Observatoire de Paris. N.P.A. acknowledges support from the NASA
postdoctoral program at Ames Research Center administered by Oak Ridge
Associated Universities through a contract with NASA.
NR 140
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U1 1
U2 13
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 SEP
PY 2011
VL 533
AR A98
DI 10.1051/0004-6361/201116599
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100098
ER
PT J
AU Wirstrom, ES
Geppert, WD
Hjalmarson, A
Persson, CM
Black, JH
Bergman, P
Millar, TJ
Hamberg, M
Vigren, E
AF Wirstrom, E. S.
Geppert, W. D.
Hjalmarson, A.
Persson, C. M.
Black, J. H.
Bergman, P.
Millar, T. J.
Hamberg, M.
Vigren, E.
TI Observational tests of interstellar methanol formation
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: molecules; astrochemistry; radio lines: ISM
ID MILLIMETER-WAVE OBSERVATIONS; SPITZER SPECTROSCOPIC SURVEY; NUCLEAR-SPIN
TEMPERATURES; YOUNG STELLAR OBJECTS; ICY GRAIN MANTLES; MOLECULAR
CLOUDS; ROTATIONAL-EXCITATION; SURFACE-REACTIONS; DENSE CLOUDS; NGC 7538
AB Context. It has been established that the classical gas-phase production of interstellar methanol (CH3OH) cannot explain observed abundances. Instead it is now generally thought that the main formation path has to be by successive hydrogenation of solid CO on interstellar grain surfaces.
Aims. While theoretical models and laboratory experiments show that methanol is efficiently formed from CO on cold grains, our aim is to test this scenario by astronomical observations of gas associated with young stellar objects (YSOs).
Methods. We have observed the rotational transition quartets J = 2(K) - 1(K) of (CH3OH)-C-12 and (CH3OH)-C-13 at 96.7 and 94.4 GHz, respectively, towards a sample of massive YSOs in different stages of evolution. In addition, the J = 1-0 transitions of (CO)-C-12-O-18 and (CO)-C-13-O-18 were observed towards some of these sources. We use the C-12/C-13 ratio to discriminate between gas-phase and grain surface origin: If methanol is formed from CO on grains, the ratios should be similar in CH3OH and CO. If not, the ratio should be higher in CH3OH due to C-13 fractionation in cold CO gas. We also estimate the abundance ratios between the nuclear spin types of methanol (E and A). If methanol is formed on grains, this ratio is likely to have been thermalized at the low physical temperature of the grain, and therefore show a relative over-abundance of A-methanol.
Results. We show that the C-12/C-13 isotopic ratio is very similar in gas-phase CH3OH and (CO)-O-18, on the spatial scale of about 40 '', towards four YSOs. For two of our sources we find an overabundance of A-methanol as compared to E-methanol, corresponding to nuclear spin temperatures of 10 and 16 K. For the remaining five sources, the methanol E/A ratio is less than unity.
Conclusions. While the C-12/C-13 ratio test is consistent with methanol formation from hydrogenation of CO on grain surfaces, the result of the E/A ratio test is inconclusive.
C1 [Wirstrom, E. S.] NASA, Astrochem Lab, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
[Wirstrom, E. S.] NASA, Goddard Ctr Astrobiol, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
[Wirstrom, E. S.; Hjalmarson, A.; Persson, C. M.; Black, J. H.; Bergman, P.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden.
[Geppert, W. D.; Hamberg, M.; Vigren, E.] Stockholm Univ, Dept Phys, S-10691 Stockholm, Sweden.
[Millar, T. J.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
RP Wirstrom, ES (reprint author), NASA, Astrochem Lab, Goddard Space Flight Ctr, Mailstop 691, Greenbelt, MD 20770 USA.
EM eva.s.wirstrom@nasa.gov
OI Millar, Tom/0000-0001-5178-3656; Wirstrom, Eva/0000-0002-0656-876X;
Black, John/0000-0001-7221-7207
FU Swedish Research Council (VR); Swedish National Space Board; NASA; STFC
FX This work was supported in part by the Swedish Research Council (VR) and
the Swedish National Space Board. In addition, E.S.W. was partially
supported by NASA's Exobiology Program. Astrophysics at QUB is supported
by a grant from the STFC. The authors appreciate constructive comments
from the anonymous referee.
NR 60
TC 26
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U1 0
U2 9
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 SEP
PY 2011
VL 533
AR A24
DI 10.1051/0004-6361/201116525
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100024
ER
PT J
AU Zwintz, K
Lenz, P
Breger, M
Pamyatnykh, AA
Zdravkov, T
Kuschnig, R
Matthews, JM
Guenther, DB
Moffat, AFJ
Rowe, JF
Rucinski, SM
Sasselov, D
Weiss, WW
AF Zwintz, K.
Lenz, P.
Breger, M.
Pamyatnykh, A. A.
Zdravkov, T.
Kuschnig, R.
Matthews, J. M.
Guenther, D. B.
Moffat, A. F. J.
Rowe, J. F.
Rucinski, S. M.
Sasselov, D.
Weiss, W. W.
TI Regular frequency patterns in the classical delta Scuti star HD 144277
observed by the MOST satellite
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: oscillations; techniques: photometric; asteroseismology; stars:
variables: delta Scuti; stars: individual: HD 144277
ID RAPIDLY ROTATING STARS; SPACE; OPACITIES; PHOTOMETRY; PULSATION;
VARIABLES; SPECTRA; CLUSTER; MODES
AB Context. We present high-precision time-series photometry of the classical delta Scuti star HD 144277 obtained with the MOST (Microvariability and Oscillations of STars) satellite in two consecutive years. The observed regular frequency patterns are investigated asteroseismologically.
Aims. HD 144277 is a hot A-type star that is located on the blue border of the classical instability strip. While we mostly observe low radial order modes in classical delta Scuti stars, HD 144277 presents a different case. Its high observed frequencies, i.e., between 59.9 d(-1) (693.9 mu Hz) and 71.1 d(-1) (822.8 mu Hz), suggest higher radial orders. We examine the progression of the regular frequency spacings from the low radial order to the asymptotic frequency region.
Methods. Frequency analysis was performed using Period04 and SigSpec. The results from the MOST observing runs in 2009 and 2010 were compared to each other. The resulting frequencies were submitted to asteroseismic analysis.
Results. HD 144277 was discovered to be a delta Scuti star using the time-series photometry observed by the MOST satellite. Twelve independent pulsation frequencies lying in four distinct groups were identified. Two additional frequencies were found to be combination frequencies. The typical spacing of 3.6 d(-1) corresponds to the spacing between subsequent radial and dipole modes, therefore the spacing between radial modes is twice this value, 7.2 d(-1). Based on the assumption of slow rotation, we find evidence that the two radial modes are the sixth and seventh overtones, and the frequency with the highest amplitude can be identified as a dipole mode.
Conclusions. The models required to fit the observed instability range need slightly less metallicity and a moderate enhancement of the helium abundance compared to the standard chemical composition. Our asteroseismic models suggest that HD 144277 is a delta Scuti star close to the ZAMS with a mass of 1.66 M(circle dot).
C1 [Zwintz, K.; Breger, M.; Pamyatnykh, A. A.; Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Lenz, P.; Pamyatnykh, A. A.; Zdravkov, T.] Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Breger, M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Pamyatnykh, A. A.] Russian Acad Sci, Inst Astron, Moscow 109017, Russia.
[Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Rowe, J. F.] NASA, Moffett Field, CA 94035 USA.
[Rucinski, S. M.] Univ Toronto, David Dunlap Observ, Richmond Hill, ON L4C 4Y6, Canada.
[Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Zwintz, K (reprint author), Univ Vienna, Inst Astron, Turkenschanzstr 17, A-1180 Vienna, Austria.
EM konstanze.zwintz@univie.ac.at
OI Zwintz, Konstanze/0000-0001-9229-8315
FU Polish MNiSW [N N203 379 636]; Austrian Fonds zur Forderung der
wissenschaftlichen Forschung [P21830-N16, P22691-N16]; Austrian Academy
of Sciences at the Institute of Astronomy of the University of Vienna
FX We are grateful to Gerald Handler, who obtained the Stroemgren
photometry for HD 144277 for us at the SAAO 50 cm telescope. K.Z. is
recipient of an APART fellowship of the Austrian Academy of Sciences at
the Institute of Astronomy of the University of Vienna. P.L.,A.A.P., and
T.Z. acknowledge partial financial support from the Polish MNiSW grant
No. N N203 379 636. M.B. and W.W.W. acknowledge support by the Austrian
Fonds zur Forderung der wissenschaftlichen Forschung (MB: project
P21830-N16; WWW: project P22691-N16).
NR 27
TC 5
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U1 0
U2 4
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2011
VL 533
AR A133
DI 10.1051/0004-6361/201117272
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100133
ER
PT J
AU Dobrokhodov, V
Kaminer, I
Kitsios, I
Xargay, E
Hovakimyan, N
Cao, CY
Gregory, IM
Valavani, L
AF Dobrokhodov, Vladimir
Kaminer, Isaac
Kitsios, Ioannis
Xargay, Enric
Hovakimyan, Naira
Cao, Chengyu
Gregory, Irene M.
Valavani, Lena
TI Experimental Validation of L-1 Adaptive Control: The Rohrs
Counterexample in Flight
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article; Proceedings Paper
CT AIAA Guidance, Navigation, and Control Conference
CY AUG 10-13, 2009
CL Chicago, IL
SP Amer Inst Aeronaut & Astronaut (AIAA)
ID OUTPUT-FEEDBACK CONTROLLER; SYSTEMS; ROBUSTNESS; DYNAMICS;
STABILIZATION; EXCITATION
AB This paper presents flight-test results that examine the performance and robustness properties of an L-1 control augmentation loop implemented onboard a small unmanned aerial vehicle. The framework used for in-flight control evaluation is based on the Rohrs counterexample, a benchmark problem presented in the early 1980s, to show the limitations of adaptive controllers developed at that time. Hardware-in-the-loop simulations and flight-test results confirm the ability of the L-1 flight control system to maintain stability and predictable performance of the closed-loop adaptive system in the presence of general (artificially injected) unmodeled dynamics. The results demonstrate the advantages of L-1 control as a robust adaptive control architecture with the potential of facilitating the transition of adaptive control into advanced flight control systems.
C1 [Dobrokhodov, Vladimir; Kitsios, Ioannis] USN, Postgrad Sch, Dept Mech & Aerosp Engn, Cpt HAF, Monterey, CA 93943 USA.
[Xargay, Enric; Hovakimyan, Naira] Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA.
[Cao, Chengyu] Univ Connecticut, Dept Mech Engn, Storrs, CT 06269 USA.
[Gregory, Irene M.] NASA Langley Res Ctr, Dynam Syst & Controls Branch, Hampton, VA 23681 USA.
[Valavani, Lena] Hellen Space Syst SA, Athens 15451, Greece.
RP Dobrokhodov, V (reprint author), USN, Postgrad Sch, Dept Mech & Aerosp Engn, Cpt HAF, Monterey, CA 93943 USA.
EM vldobr@nps.edu; kaminer@nps.edu; ikitsios@nps.edu; xargay@illinois.edu;
nhovakim@illinois.edu; ccao@engr.uconn.edu; irene.m.gregory@nasa.gov;
valavani@mit.edu
RI Dobrokhodov, Vladimir/C-3443-2009
NR 35
TC 10
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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 SEP-OCT
PY 2011
VL 34
IS 5
BP 1311
EP 1328
DI 10.2514/1.50683
PG 18
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 825BZ
UT WOS:000295247200003
ER
PT J
AU Butler, EJ
Wang, HO
Burken, JJ
AF Butler, Evan J.
Wang, Hua O.
Burken, John J.
TI Takagi-Sugeno Fuzzy Model-Based Flight Control and Failure Stabilization
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article; Proceedings Paper
CT AIAA Guidance, Navigation, and Control Conference
CY AUG 02-05, 2010
CL Toronto, CANADA
SP Amer Inst Aeronaut & Astronaut (AIAA)
ID CONTROL-SYSTEMS; DESIGN
AB This paper presents a Takagi-Sugeno fuzzy model-based approach to modeling, controlling, and stabilizing an aircraft in both normal and damaged conditions. The major contributions of this paper are as follows. First, it introduces the Takagi-Sugeno modeling and the parallel distributed compensation control approach. Then, it demonstrates how the approach can be applied to aircraft in a systematic manner. Finally, the approach is applied to the modified NASA F-15 number 837 nonlinear model, and preliminary simulation results are presented. The benefits of using a Takagi-Sugeno model-based parallel distributed compensation control approach include a systematic controller design procedure, mathematical proof of stability for classes of failures, and intuitive insight into damage effects on an aircraft. This work is the first to present this control approach as applied to aircraft.
C1 [Butler, Evan J.] Sterling Point Res, Winchester, MA 01890 USA.
[Wang, Hua O.] Boston Univ, Dept Mech Engn, Boston, MA 02215 USA.
[Burken, John J.] NASA Dryden Flight Res Ctr, Edwards AFB, CA 93523 USA.
RP Butler, EJ (reprint author), Sterling Point Res, Winchester, MA 01890 USA.
EM Evan.Butler@sterlingpointresearch.com; wangh@bu.edu;
John.J.Burken@nasa.gov
NR 29
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U1 0
U2 2
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 SEP-OCT
PY 2011
VL 34
IS 5
BP 1543
EP 1555
DI 10.2514/1.52509
PG 13
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 825BZ
UT WOS:000295247200021
ER
PT J
AU Sridhar, B
Ng, HK
Chen, NY
AF Sridhar, Banavar
Ng, Hok K.
Chen, Neil Y.
TI Aircraft Trajectory Optimization and Contrails Avoidance in the Presence
of Winds
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article; Proceedings Paper
CT 10th AIAA Aviation Technology, Integration, and Operations (ATIO)
Conference
CY SEP 13-15, 2010
CL Ft Worth, TX
SP AIAA, Universidad Politecnica de Madrid
ID UNITED-STATES; COVERAGE
C1 [Sridhar, Banavar; Chen, Neil Y.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ng, Hok K.] Univ Calif Santa Cruz, Moffett Field, CA 94035 USA.
RP Sridhar, B (reprint author), Air Transportat Syst, Aviat Syst Div, Moffett Field, CA 94035 USA.
NR 19
TC 11
Z9 11
U1 0
U2 1
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 SEP-OCT
PY 2011
VL 34
IS 5
BP 1577
EP 1583
DI 10.2514/1.53378
PG 7
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 825BZ
UT WOS:000295247200026
ER
PT J
AU Zwally, HJ
Giovinetto, MB
AF Zwally, H. Jay
Giovinetto, Mario B.
TI Overview and Assessment of Antarctic Ice-Sheet Mass Balance Estimates:
1992-2009
SO SURVEYS IN GEOPHYSICS
LA English
DT Review
DE Antarctica; Ice sheet; Mass balance; ERS; GRACE; ICESat; Input output
fluxes
ID SEA-LEVEL RISE; GLACIAL ISOSTATIC-ADJUSTMENT; GREENLAND; SNOWFALL;
ACCUMULATION
AB Mass balance estimates for the Antarctic Ice Sheet (AIS) in the 2007 report by the Intergovernmental Panel on Climate Change and in more recent reports lie between approximately +50 to -250 Gt/year for 1992 to 2009. The 300 Gt/year range is approximately 15% of the annual mass input and 0.8 mm/year Sea Level Equivalent (SLE). Two estimates from radar altimeter measurements of elevation change by European Remote-sensing Satellites (ERS) (+28 and -31 Gt/year) lie in the upper part, whereas estimates from the Input-minus-Output Method (IOM) and the Gravity Recovery and Climate Experiment (GRACE) lie in the lower part (-40 to -246 Gt/year). We compare the various estimates, discuss the methodology used, and critically assess the results. We also modify the IOM estimate using (1) an alternate extrapolation to estimate the discharge from the non-observed 15% of the periphery, and (2) substitution of input from a field data compilation for input from an atmospheric model in 6% of area. The modified IOM estimate reduces the loss from 136 Gt/year to 13 Gt/year. Two ERS-based estimates, the modified IOM, and a GRACE-based estimate for observations within 1992-2005 lie in a narrowed range of +27 to -40 Gt/year, which is about 3% of the annual mass input and only 0.2 mm/year SLE. Our preferred estimate for 1992-2001 is -47 Gt/year for West Antarctica, +16 Gt/year for East Antarctica, and -31 Gt/year overall (+0.1 mm/year SLE), not including part of the Antarctic Peninsula (1.07% of the AIS area). Although recent reports of large and increasing rates of mass loss with time from GRACE-based studies cite agreement with IOM results, our evaluation does not support that conclusion.
C1 [Zwally, H. Jay; Giovinetto, Mario B.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch Code 614 1, SGT Inc, Greenbelt, MD 20771 USA.
RP Zwally, HJ (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Branch Code 614 1, SGT Inc, Greenbelt, MD 20771 USA.
EM zwally@icesat2.gsfc.nasa.gov
FU NASA
FX This research was supported by NASA's ICESat Project Science funding. We
thank Scott Luthcke for providing his insights on GRACE methodology,
issues, and developments, and two anonymous reviewers for helpful
suggestions and corrections.
NR 38
TC 39
Z9 39
U1 2
U2 38
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0169-3298
EI 1573-0956
J9 SURV GEOPHYS
JI Surv. Geophys.
PD SEP
PY 2011
VL 32
IS 4-5
SI SI
BP 351
EP 376
DI 10.1007/s10712-011-9123-5
PG 26
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 826DY
UT WOS:000295332800004
ER
PT J
AU Van den Broeke, MR
Bamber, J
Lenaerts, J
Rignot, E
AF Van den Broeke, Michiel R.
Bamber, Jonathan
Lenaerts, Jan
Rignot, Eric
TI Ice Sheets and Sea Level: Thinking Outside the Box
SO SURVEYS IN GEOPHYSICS
LA English
DT Review
DE Greenland; Antarctica; Mass balance; Sea level
ID SURFACE MASS-BALANCE; ACCUMULATION VARIABILITY; CLIMATE MODEL;
GREENLAND; RISE; ACCELERATION; ANTARCTICA; ALTIMETRY; GLACIERS; SNOWFALL
AB Until quite recently, the mass balance (MB) of the great ice sheets of Greenland and Antarctica was poorly known and often treated as a residual in the budget of oceanic mass and sea level change. Recent developments in regional climate modelling and remote sensing, especially altimetry, gravimetry and InSAR feature tracking, have enabled us to specifically resolve the ice sheet mass balance components at a near-annual timescale. The results reveal significant mass losses for both ice sheets, caused by the acceleration of marine-terminating glaciers in southeast, west and northwest Greenland and coastal West Antarctica, and increased run-off in Greenland. At the same time, the data show that interannual variability is very significant, masking the underlying trends.
C1 [Van den Broeke, Michiel R.; Lenaerts, Jan] Univ Utrecht, Inst Marine & Atmospher Res, Utrecht, Netherlands.
[Bamber, Jonathan] Univ Bristol, Bristol Glaciol Ctr, Sch Geog Sci, Bristol, Avon, England.
[Rignot, Eric] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Rignot, Eric] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Van den Broeke, MR (reprint author), Univ Utrecht, Inst Marine & Atmospher Res, Utrecht, Netherlands.
EM m.r.vandenbroeke@uu.nl; j.bamber@bristol.ac.uk; j.lenaerts@uu.nl;
erignot@uci.edu
RI Bamber, Jonathan/C-7608-2011; Van den Broeke, Michiel/F-7867-2011;
Rignot, Eric/A-4560-2014; Lenaerts, Jan/D-9423-2012
OI Bamber, Jonathan/0000-0002-2280-2819; Van den Broeke,
Michiel/0000-0003-4662-7565; Rignot, Eric/0000-0002-3366-0481; Lenaerts,
Jan/0000-0003-4309-4011
NR 60
TC 30
Z9 30
U1 2
U2 39
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0169-3298
EI 1573-0956
J9 SURV GEOPHYS
JI Surv. Geophys.
PD SEP
PY 2011
VL 32
IS 4-5
SI SI
BP 495
EP 505
DI 10.1007/s10712-011-9137-z
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 826DY
UT WOS:000295332800012
ER
PT J
AU Dehlinger, J
Lutz, RR
AF Dehlinger, Josh
Lutz, Robyn R.
TI Gaia-PL: A Product Line Engineering Approach for Efficiently Designing
Multiagent Systems
SO ACM TRANSACTIONS ON SOFTWARE ENGINEERING AND METHODOLOGY
LA English
DT Article
DE Design; Documentation; Agent-oriented software engineering; software
product line engineering
ID REQUIREMENTS; METHODOLOGY; REUSE; EVOLUTION; TROPOS
AB Agent-oriented software engineering (AOSE) has provided powerful and natural, high-level abstractions in which software developers can understand, model and develop complex, distributed systems. Yet, the realization of AOSE partially depends on whether agent-based software systems can achieve reductions in development time and cost similar to other reuse-conscious development methods. Specifically, AOSE does not adequately address requirements specifications as reusable assets. Software product line engineering is a reuse technology that supports the systematic development of a set of similar software systems through understanding, controlling, and managing their common, core characteristics and their differing variation points. In this article, we present an extension to the Gaia AOSE methodology, named Gaia-PL (Gaia-Product Line), for agent-based distributed software systems that enables requirements specifications to be easily reused. We show how our methodology uses a product line perspective to promote reuse in agent-based software systems early in the development life cycle so that software assets can be reused throughout system development and evolution. We also present results from an application to show how Gaia-PL provided reuse that reduced the design and development effort for a large, multiagent system.
C1 [Dehlinger, Josh] Towson Univ, Dept Comp & Informat Sci, Towson, MD 21252 USA.
[Lutz, Robyn R.] Iowa State Univ, Dept Comp Sci, Ames, IA 50011 USA.
[Lutz, Robyn R.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Dehlinger, J (reprint author), Towson Univ, Dept Comp & Informat Sci, Towson, MD 21252 USA.
EM jdehlinger@towson.edu; rlutz@cs.iastate.edu
FU National Science Foundation [0204139, 0205588, 0541163]; Iowa Space
Consortium
FX This research was supported by the National Science Foundation grants
0204139, 0205588, and 0541163 and by an Iowa Space Consortium grant.
NR 45
TC 4
Z9 4
U1 1
U2 5
PU ASSOC COMPUTING MACHINERY
PI NEW YORK
PA 2 PENN PLAZA, STE 701, NEW YORK, NY 10121-0701 USA
SN 1049-331X
EI 1557-7392
J9 ACM T SOFTW ENG METH
JI ACM Trans. Softw. Eng. Methodol.
PD SEP
PY 2011
VL 20
IS 4
AR 17
DI 10.1145/2000799.2000803
PG 27
WC Computer Science, Software Engineering
SC Computer Science
GA 824QN
UT WOS:000295217200004
ER
PT J
AU Bathel, BF
Danehy, PM
Inman, JA
Jones, SB
Ivey, CB
Goyne, CP
AF Bathel, Brett F.
Danehy, Paul M.
Inman, Jennifer A.
Jones, Stephen B.
Ivey, Christopher B.
Goyne, Christopher P.
TI Velocity Profile Measurements in Hypersonic Flows Using Sequentially
Imaged Fluorescence-Based Molecular Tagging
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT 48th AIAA Aerospace Sciences Meeting and Exhibit Including the New
Horizons Forum and Aerospace Exposition
CY JAN 04-08, 2010
CL Orlando, FL
SP AIAA, Vinnova, Maritime Competence Ctr Lighthouse, Swedish Armed Forces, Swedish Def Mat Agcy, NASA Langley Res Ctr, NASA Dryden Flight Res Ctr
ID LASER-INDUCED PHOSPHORESCENCE; UNDEREXPANDED JET FLOWFIELD;
SUPERSONIC-FLOW; NITRIC-OXIDE; VELOCIMETRY MTV; PHOTODISSOCIATION;
THERMOMETRY; PHOTOLYSIS; TUBE; WAKE
AB Nitric-oxide planar laser-induced fluorescence was used to perform velocity measurements in hypersonic flows by generating multiple tagged lines that fluoresce as they convect downstream. Determination of axial velocity was made by application of a cross-correlation analysis of the horizontal shift of individual tagged lines. A single interline, progressive scan-intensified charge-coupled device camera was used to obtain two sequential images of the nitric-oxide molecules that had been tagged by the laser. The charge-coupled device allowed for submicrosecond acquisition of both images, resulting in submicrosecond temporal resolution as well as submillimeter spatial resolution (0.5 mm horizontal, 03 mm vertical). Quantification of systematic errors, the contribution of gating/exposure duration errors, and the influence of collision rate on temporal uncertainty were made. This velocity measurement technique has been demonstrated for two hypersonic flow experiments: 1) a reaction control system jet on an Orion crew exploration vehicle wind-tunnel model and 2) a 10 deg half-angle wedge with a 2-mm-tall 4-mm-wide cylindrical boundary-layer trip. Mean-velocity uncertainties below 30 m/s (2.7% of the measured average velocity) and single-shot uncertainties below 100 m/s (9.7% of the measured average velocity) have been obtained in regions with optimal signal intensities using this technique.
C1 [Bathel, Brett F.] Univ Virginia, Natl Inst Aerosp, Hampton, VA 23681 USA.
[Bathel, Brett F.; Danehy, Paul M.; Inman, Jennifer A.; Jones, Stephen B.] NASA, Langley Res Ctr, Adv Sensing & Optic Measurement Branch, Hampton, VA 23681 USA.
[Ivey, Christopher B.] Stanford Univ, Stanford, CA 94305 USA.
[Goyne, Christopher P.] Univ Virginia, Aerosp Res Lab, Charlottesville, VA 22904 USA.
RP Bathel, BF (reprint author), Univ Virginia, Natl Inst Aerosp, Mail Stop 493, Hampton, VA 23681 USA.
RI Ivey, Christopher/I-8642-2012
OI Ivey, Christopher/0000-0003-0008-7532
NR 44
TC 12
Z9 12
U1 1
U2 10
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD SEP
PY 2011
VL 49
IS 9
BP 1883
EP 1896
DI 10.2514/1.J050722
PG 14
WC Engineering, Aerospace
SC Engineering
GA 824MX
UT WOS:000295207100006
ER
PT J
AU Bennett, SA
Statham, PJ
Green, DRH
Le Bris, N
McDermott, JM
Prado, F
Rouxel, OJ
Von Damm, K
German, CR
AF Bennett, Sarah A.
Statham, Peter J.
Green, Darryl R. H.
Le Bris, Nadine
McDermott, Jill M.
Prado, Florencia
Rouxel, Olivier J.
Von Damm, Karen
German, Christopher R.
TI Dissolved and particulate organic carbon in hydrothermal plumes from the
East Pacific Rise, 9 degrees 50 ' N
SO DEEP-SEA RESEARCH PART I-OCEANOGRAPHIC RESEARCH PAPERS
LA English
DT Article
DE Hydrothermal; Dissolved organic carbon; Particulate organic carbon; East
Pacific Rise
ID MID-ATLANTIC RIDGE; DE-FUCA RIDGE; VOLCANIC-ERUPTION; GORDA RIDGE;
GEOCHEMICAL CONSTRAINTS; AMMONIA OXIDATION; MIDOCEAN RIDGE;
PARTICLE-FLUX; EVENT PLUMES; WATER COLUMN
AB Chemoautotrophic production in seafloor hydrothermal systems has the potential to provide an important source of organic carbon that is exported to the surrounding deep-ocean. While hydrothermal plumes may export carbon, entrained from chimney walls and biologically rich diffuse flow areas, away from sites of venting they also have the potential to provide an environment for in-situ carbon fixation. In this study, we have followed the fate of dissolved and particulate organic carbon (DOC and POC) as it is dispersed through and settles beneath a hydrothermal plume system at 9 degrees 50'N on the East Pacific Rise. Concentrations of both DOC and POC are elevated in buoyant plume samples that were collected directly above sites of active venting using both DSV Alvin and a CTD-rosette. Similar levels of POC enrichment are also observed in the dispersing non-buoyant plume, similar to 500 m downstream from the vent-site. Further, sediment-trap samples collected beneath the same dispersing plume system, show evidence for a close coupling between organic carbon and Fe oxyhydroxide fluxes. We propose, therefore, a process that concentrates POC into hydrothermal plumes as they disperse through the deep-ocean. This is most probably the result of some combination of preferential adsorption of organic carbon onto Fe-oxyhydroxides and/or microbial activity that preferentially concentrates organic carbon in association with Fe-oxyhydroxides (e.g. through the microbial oxidation of Fe(II) and Fe sulfides). This potential for biological production and consumption within hydrothermal plumes highlights the importance of a multidisciplinary approach to understanding the role of the carbon cycle in deep-sea hydrothermal systems as well as the role that hydrothermal systems may play in regulating global deep-ocean carbon budgets. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Bennett, Sarah A.; Statham, Peter J.] Natl Oceanog Ctr, Sch Ocean & Earth Sci, Southampton SO14 3ZH, Hants, England.
[Green, Darryl R. H.] Natl Oceanog Ctr, Natl Environm Res Council, Southampton SO14 3ZH, Hants, England.
[Le Bris, Nadine] Univ Paris 06, CNRS, UPMC, FRE3350,LECOB, F-66650 Banyuls Sur Mer, France.
[McDermott, Jill M.; Prado, Florencia; Von Damm, Karen] Univ New Hampshire, Durham, NH 03824 USA.
[Rouxel, Olivier J.; German, Christopher R.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
[Rouxel, Olivier J.] Univ Europeenne Bretagne, European Inst Marine Studies IUEM, F-29280 Plouzane, France.
RP Bennett, SA (reprint author), NASA, Jet Prop Lab, CALTECH, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Sarah.A.Bennett@jpl.nasa.gov
RI Bennett, Sarah/F-9831-2011; Le Bris, Nadine/E-1381-2014; Rouxel,
Olivier/F-3954-2014
OI Bennett, Sarah/0000-0002-9811-4764; Le Bris, Nadine/0000-0002-0142-4847;
FU NERC [NER/S/A/2004/12631]; [OCE-0327126]; [OCE-0647948]
FX We would like to thank Andy Gooday, Michael Bacon and three anonymous
reviewers for their constructive comments. We thank the captain, crew
and scientists on board AT15-6, AT15-12, AT15-13 and AT15-14 who
contributed to the success of this work and to Chief Scientist, Jim
Ledwell, who enabled SAB to participate in AT15-14 (as part of the
LADDER project), as well as Lauren Mullineaux the LADDER project
coordinator who invited NLB to this cruise. We also thank Ryan Jackson
for creation of the location map and to Tim Fischer for work up of the
L-ADCP data. We thank Robert Head and Xi Pan for POC and DOC
measurements and Steven Manganini, Maureen Auro and Scot Birdwhistell
for sediment trap sample analysis. Support for vent fluid analysis was
supported by the OCE-0327126, originally awarded to Karen Von Damm and
subsequently managed by Julie Bryce. Support for sediment trap analysis
was funded by OCE-0647948, awarded to CRG and OJR. SAB was funded by a
NERC PhD studentship, NER/S/A/2004/12631.
NR 69
TC 18
Z9 18
U1 2
U2 41
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0637
J9 DEEP-SEA RES PT I
JI Deep-Sea Res. Part I-Oceanogr. Res. Pap.
PD SEP
PY 2011
VL 58
IS 9
BP 922
EP 931
DI 10.1016/j.dsr.2011.06.010
PG 10
WC Oceanography
SC Oceanography
GA 824EV
UT WOS:000295186100002
ER
PT J
AU Yamada, Y
Ziegler, B
Newman, JC
AF Yamada, Y.
Ziegler, B.
Newman, J. C., Jr.
TI Application of a strip-yield model to predict crack growth under
variable-amplitude and spectrum loading - Part 1: Compact specimens
SO ENGINEERING FRACTURE MECHANICS
LA English
DT Article
DE Cracks; Fatigue-crack growth; Aluminum alloy; Crack closure;
Stress-intensity factor; Plasticity
ID ALUMINUM-ALLOYS; CONSTANT; CLOSURE; RATES
AB Fatigue-crack-growth tests were conducted on compact, C(T), specimens made of D16Cz (clad) aluminum alloy under constant-amplitude loading, a single spike overload, and simulated aircraft spectrum loading. Constant-amplitude tests were conducted to generate crack-growth-rate data from threshold to near fracture over a wide range of stress ratios (R = P(min)/P(max) = 0.1-0.75) using the new compression pre-cracking test methods. Comparisons were made between test data generated on the C(T) specimens with test data from the literature on middle-crack-tension, M(T), specimens machined from the same sheet. A crack-closure analysis was used to collapse the rate data from both specimen types into a narrow band over many orders of magnitude in rates using proper constraint factors. The constraint factors were established from constant-amplitude (CA) and single-spike overload tests. The life-prediction code, FASTRAN, which is based on the strip-yield model concept, was used to calculate crack-length-against-cycles under CA loading and a single-spike overload (OL) test, and to predict crack growth under simulated aircraft spectrum loading tests on C(T) specimens. The calculated crack-growth lives under CA loading were generally within about +/- 25% of the test results, but slower crack growth under the double-shear fatigue mode, unlike the single-shear mode (45 degrees slant crack growth), may be the reason for some of the larger differences. The predicted results under the single-spike overload and the Mini-Falstaff+ spectrum were within 10% of the test data. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Ziegler, B.; Newman, J. C., Jr.] Mississippi State Univ, Mississippi State, MS 39762 USA.
[Yamada, Y.] NASA Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA.
RP Newman, JC (reprint author), Mississippi State Univ, Mississippi State, MS 39762 USA.
EM j.c.newman@ae.msstate.edu
FU US Army through Georgia Tech
FX The authors thank Professors M. Skorupa, T. Machniewicz and J. Schijve
for providing the D16Cz alloy and the test data on the M(T) specimens.
The US Army under a sub-contract through Georgia Tech (Dr. A. Makeev) to
Mississippi State University (MSU) sponsored this study. Special thanks
to Dr. Dy Le, US Army (formally US Federal Aviation Administration), for
continuing to support development of the compression pre-cracking
testing procedures used in this study; and to Dr. Keith Donald, Fracture
Technology Associates, for his valuable advise on his steady-state and
variable-amplitude fatigue-crack-growth software.
NR 24
TC 14
Z9 16
U1 0
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0013-7944
J9 ENG FRACT MECH
JI Eng. Fract. Mech.
PD SEP
PY 2011
VL 78
IS 14
BP 2597
EP 2608
DI 10.1016/j.engfracmech.2011.06.015
PG 12
WC Mechanics
SC Mechanics
GA 825BK
UT WOS:000295245700004
ER
PT J
AU Ziegler, B
Yamada, Y
Newman, JC
AF Ziegler, B.
Yamada, Y.
Newman, J. C., Jr.
TI Application of a strip-yield model to predict crack growth under
variable-amplitude and spectrum loading - Part 2: Middle-crack-tension
specimens
SO ENGINEERING FRACTURE MECHANICS
LA English
DT Article
DE Cracks; Fatigue-crack growth; Aluminum alloy; Crack closure;
Stress-intensity factor; Plasticity
ID ALUMINUM-ALLOY; CONSTANT
AB In previous work, fatigue-crack-growth tests were conducted on middle-crack tension. M(T), and compact, C(T), specimens made from the same D16Cz (clad) aluminum alloy sheet. These tests were conducted over a wide range of stress ratios (R = P(min)/P(max) = -0.5 to 0.75) to generate crack-growth-rate data from threshold to near fracture. These tests were used to generate the effective stress-intensity factor range (Delta K(eff)) against rate curve using a crack-closure model. The analyses collapsed the rate data from both specimen types into a fairly narrow band over many orders of magnitude in rates using proper constraint factors. Constraint factors were established from single-spike overload and the constant-amplitude tests. Herein, the life-prediction code. FASTRAN, which is based on the strip-yield model concept, was used to calculate the crack-length-against-cycles under constant-amplitude (CA) loading and the single-spike overload (OL) tests; and to predict crack growth under variable-amplitude (VA) loading and simulated aircraft loading spectrum tests on the M(T) specimens. The calculated crack-growth lives under CA and an OL tests were generally within +/- 20% of the test results, but slower crack growth under the double-shear fatigue mode, rather than single shear, may be the reason for some of the larger differences. The predicted crack-growth lives for the VA and Mini-Falstaff spectrum tests were also short by 25-45%. A modified model with some assumed notch constraint effects matched the spectrum tests quite well. Issues on the crack-starter-notch effects under spectrum loading are discussed, and recommendations are suggested on avoiding these notch effects. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Ziegler, B.; Newman, J. C., Jr.] Mississippi State Univ, Mississippi State, MS 39762 USA.
[Yamada, Y.] NASA Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA.
RP Newman, JC (reprint author), Mississippi State Univ, Mississippi State, MS 39762 USA.
EM j.c.newman@ae.msstate.edu
FU US Army through Georgia Tech
FX The authors thank Professors M. Skorupa and T. Machniewicz, University
of Science and Technology, Krakow, Poland, and Professor J. Schijve,
Delft University of Technology, Delft, Netherlands, for providing the
D16Cz alloy material and the test data on the M(T) specimens. The US
Army under a sub-contract through Georgia Tech (Dr. A. Makeev) to
Mississippi State University (MSU) sponsored this study.
NR 20
TC 10
Z9 13
U1 0
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0013-7944
J9 ENG FRACT MECH
JI Eng. Fract. Mech.
PD SEP
PY 2011
VL 78
IS 14
BP 2609
EP 2619
DI 10.1016/j.engfracmech.2011.06.018
PG 11
WC Mechanics
SC Mechanics
GA 825BK
UT WOS:000295245700005
ER
PT J
AU Gouesbet, G
Xu, F
Han, YP
AF Gouesbet, G.
Xu, F.
Han, Y. P.
TI Expanded description of electromagnetic arbitrary shaped beams in
spheroidal coordinates, for use in light scattering theories: A review
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Review
DE Generalized Lorenz-Mie theories; Spheroids; Beam shape coefficients
ID LORENZ-MIE THEORY; LOCATED SPHERICAL INCLUSION; GAUSSIAN-BEAM; LOCALIZED
APPROXIMATION; INFINITE CYLINDER; NEAR-SURFACE; EXPANSION COEFFICIENTS;
RIGOROUS JUSTIFICATION; BROMWICH FORMULATION; ELLIPTIC CYLINDERS
AB During the last decade, a strong effort has been devoted to the development of a generalized Lorenz-Mie theory for spheroids illuminated by Gaussian beams, and more generally by arbitrary shaped beams. An important issue in such a framework concerns the expanded description of the illuminating beam, and particularly the evaluation of beam shape coefficients. Unfortunately, the effort in this field is located at the bridge of three streams, each one with different conventions and notations, making the access to the literature inconveniently difficult. The aim of the present paper is to review the different approaches published, and to establish in a clear way the relationships between them. Beside being a help to the newcomer, this paper also aims to set milestones for future works, particularly concerning the development, under current investigation, of a localized beam model in spheroidal coordinates. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Gouesbet, G.; Xu, F.] Univ Rouen, LESP, CNRS, UMR 6614, F-76821 Mont St Aignan, France.
[Gouesbet, G.; Xu, F.] INSA Rouen, F-76801 St Etienne, France.
[Xu, F.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
[Han, Y. P.] Xidian Univ, Sch Sci, Xian, Peoples R China.
RP Gouesbet, G (reprint author), Univ Rouen, LESP, CNRS, UMR 6614, CORIA, F-76821 Mont St Aignan, France.
EM Gouesbet@coria.fr
RI Xu, Feng/G-3673-2013
NR 69
TC 19
Z9 19
U1 2
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 SEP
PY 2011
VL 112
IS 14
BP 2249
EP 2267
DI 10.1016/j.jqsrt.2011.05.012
PG 19
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 823FW
UT WOS:000295108900001
ER
PT J
AU Gordon, IE
Rothman, LS
Toon, GC
AF Gordon, Iouli E.
Rothman, Laurence S.
Toon, Geoffrey C.
TI Revision of spectral parameters for the B- and gamma-bands of oxygen and
their validation against atmospheric spectra
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE HITRAN; Oxygen spectroscopy; B-band; gamma-Band
ID MOLECULAR SPECTROSCOPIC DATABASE; O-2 A-BAND; SELF-BROADENING
COEFFICIENTS; RING-DOWN SPECTROSCOPY; ABSORPTION-SPECTROSCOPY; INTENSITY
MEASUREMENTS; LINE PARAMETERS; RESOLUTION; PRESSURE; O-16(2)
AB Until recently the B (b(1)Sigma(+)(g) (nu=1)-X-3 Sigma(-)(g) (nu=0)) and gamma (b(1)Sigma(+)(g) (nu=2)-X-3 Sigma(-)(g) (nu=0)) bands of oxygen in the visible region had not been used extensively in satellite remote sensing of the atmosphere. These bands roughly cover the regions around 14,527 and 15,904 cm(-1), respectively (0.69 and 0.63 mu m). However, these bands (in particular the B-band) are now being increasingly considered for future satellite missions. In this light, it is important to make sure that the reference spectroscopic parameters allow accurate retrieval of important physical characteristics from the atmospheric spectra. The spectroscopic parameters currently given for these bands in the HITRAN2008 spectroscopic database were tested against high-resolution atmospheric spectra measured with solar-pointing Fourier transform spectrometers at Park Falls, Wisconsin (B-band) and Kitt Peak, Arizona (gamma-band). It was found that the current HITRAN parameters cannot produce satisfactory fits of the observed spectra. In order to improve the database we have collected the best available measured line positions that involve the b(1)E(g)(+) (nu=1 and nu=2) states for the three most abundant isotopologues of oxygen and performed a combined fit to obtain a consistent set of spectroscopic constants. These constants were then used to calculate the line positions. A careful review of the available intensity and line-shape measurements was also carried out, and new parameters were derived based on that review. In particular, line shift parameters, that were not previously available, were introduced. The new data have been validated using the high-resolution atmospheric spectra measured with the Fourier transform spectrometers at Park Falls, Wisconsin (B-band) and Kitt Peak, Arizona (gamma-band) and have yielded substantial improvement. In addition, we report the first direct observation and analysis of the (OO)-O-16-O-18 lines in the gamma-band. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Gordon, Iouli E.; Rothman, Laurence S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
[Toon, Geoffrey C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gordon, IE (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA.
EM igordon@cfa.harvard.edu
OI Gordon, Iouli/0000-0003-4763-2841
FU NASA [NAG5-13534]
FX We would like to thank Joseph Hodges and Daniel Lisak for providing us
with unpublished line position measurements of five transitions in the
B-band. Helpful discussions with Linda Brown and Caroline Nowlan are
much appreciated. The work carried out at the Harvard-Smithsonian Center
for Astrophysics was supported by NASA through the Earth Observing
System (EOS) under grant NAG5-13534. Part of this work was performed at
the Jet Propulsion Laboratory, California Institute of Technology, under
contract with NASA We thank the Kitt Peak National Observatory, and the
Total Column Carbon Observing Network (TCCON) for providing the
atmospheric spectra used to validate the new line lists.
NR 44
TC 20
Z9 20
U1 0
U2 11
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 SEP
PY 2011
VL 112
IS 14
BP 2310
EP 2322
DI 10.1016/j.jqsrt.2011.05.007
PG 13
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 823FW
UT WOS:000295108900007
ER
PT J
AU Jones, SM
Flynn, G
AF Jones, Steven M.
Flynn, George
TI Hypervelocity capture of meteoritic particles in nonsilica aerogels
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID COHERENT EXPANDED AEROGELS
AB The Stardust mission captured particles from the comet 81P/Wild 2 in gradient density silica aerogel and returned the collected samples to earth in 2006. The analyses of these particles have revealed several new insights into the formation of our solar system. However, since the aerogel used as the capture material was silica, the elemental analyses of the silica-rich particles were made more complicated in certain ways due to the mixing of the silicon of the particles and that of the aerogel. By using a nonsilica aerogel, future elemental analyses of silica-rich particles captured in aerogel could be made more straightforward. Resorcinol/formaldehyde (RF), alumina, and zirconia aerogels were impact tested with meteoritic fragments and the captured fragments were mapped with synchrotron-based X-ray microprobe (XRM) and the particles were analyzed with X-ray fluorescence (XRF). The resorcinol/formaldehyde aerogel proved to be the best capture material, in that it could be keystoned and XRF could be used to locate and analyze particles that were less than 10 mu m.
C1 [Jones, Steven M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Flynn, George] SUNY Coll Plattsburgh, Dept Phys, Plattsburgh, NY 12901 USA.
RP Jones, SM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 125-109, Pasadena, CA 91109 USA.
EM Steven.M.Jones@jpl.nasa.gov
FU Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration;
Department of Energy (DOE) Geosciences [DE-FG02-92ER14244]; DOE-Office
of Biological and Environmental Research, Environmental Remediation
Sciences Div. [DE-FC09-96-SR18546]; DOE [DE-AC02-98CH10886]
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. (C) 2011 California Institute of
Technology. Government sponsorship is acknowledged.; Portions of this
work were performed at Beamline X26A, National Synchrotron Light Source
(NSLS), Brookhaven National Laboratory. X26A is supported by the
Department of Energy (DOE) Geosciences (DE-FG02-92ER14244 to The
University of Chicago-CARS) and DOE-Office of Biological and
Environmental Research, Environmental Remediation Sciences Div.
(DE-FC09-96-SR18546 to the University of Kentucky). Use of the NSLS was
supported by DOE under Contract No. DE-AC02-98CH10886.
NR 13
TC 2
Z9 2
U1 0
U2 1
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2011
VL 46
IS 9
BP 1253
EP 1264
DI 10.1111/j.1945-5100.2011.01223.x
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 822MY
UT WOS:000295053300002
ER
PT J
AU Hui, HJ
Peslier, AH
Lapen, TJ
Shafer, JT
Brandon, AD
Irving, AJ
AF Hui, Hejiu
Peslier, Anne H.
Lapen, Thomas J.
Shafer, John T.
Brandon, Alan D.
Irving, Anthony J.
TI Petrogenesis of basaltic shergottite Northwest Africa 5298:
Closed-system crystallization of an oxidized mafic melt
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID RARE-EARTH-ELEMENTS; MARTIAN BASALTS; OXYGEN FUGACITY; TRACE-ELEMENT;
OXIDATION-STATE; SILICATE MELTS; UPPER-MANTLE; REDOX STATE; LOS-ANGELES;
LAVA FLOWS
AB Northwest Africa (NWA) 5298 is an evolved basaltic shergottite that has bulk characteristics and mineral compositions consistent with derivation from an oxidized reservoir in Mars. Chemically zoned clinopyroxene (64.5%, augite and pigeonite), with interstitial lath-shaped plagioclase (29.4%, An(40) to An(55)), constitutes the bulk of this meteorite. The plagioclase has been converted by shock to both isotropic maskelynite and spherulitic, birefringent feldspar representing a quenched vesicular melt. The remainder of the rock consists of minor amounts of Fe-Ti oxides (ilmenite and titanomagnetite), phosphates (merrillite and apatite), silica polymorph, fayalite, pyrrhotite, baddeleyite, and minor hot desert weathering products (calcite and barite). Oxygen fugacity derived from Fe-Ti oxide thermobarometry is close to the quartz-fayalite-magnetite (QFM) buffer indicating that the late stage evolution of this magma occurred under more oxidizing condition than those recorded in most other shergottites. Merrillite contains the largest abundances of rare earth elements (REE) of all phases, thereby controlling the REE budget in NWA 5298. The calculated bulk rock REE pattern normalized to CI chondrite is relatively flat. The evolution of the normalized REE patterns of the bulk rock, clinopyroxene, plagioclase, and phosphate in NWA 5298 is consistent with closed-system chemical behavior with no evidence of crustal contamination or postcrystallization disturbance of the REE contents of these phases.
C1 [Hui, Hejiu] USRA Houston, Lunar & Planetary Inst, Houston, TX 77058 USA.
[Peslier, Anne H.] ESCG, Houston, TX 77058 USA.
[Peslier, Anne H.] NASA Johnson Space Ctr, ARES, Houston, TX 77058 USA.
[Lapen, Thomas J.; Shafer, John T.; Brandon, Alan D.] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA.
[Irving, Anthony J.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.
RP Hui, HJ (reprint author), Univ Notre Dame, Dept Civil Engn & Geol Sci, Notre Dame, IN 46556 USA.
EM hhui@nd.edu
RI Hui, Hejiu/D-2912-2011; Peslier, Anne/F-3956-2010
OI Hui, Hejiu/0000-0003-2733-5794;
FU NASA; Lunar and Planetary Institute
FX The Mars Meteorite Compendium edited by C. Meyer was very helpful for
literature review. G.-A. Robinson and A. Wittmann are thanked for their
help with the SEM at NASA-JSC. We are grateful to S. Kuehner for
microprobe analyses obtained at the University of Washington, and to T.
Bunch for optical photomicrographs. A NASA Cosmochemistry award to T. J.
L. is acknowledged for financial support for the laser ablation
analyses. H. H. was supported on a Lunar and Planetary Institute
postdoctoral fellowship during this work. We greatly appreciate the
constructive comments by associate editor A. Yamaguchi, and reviewers A.
Riches and J. Barrat.
NR 81
TC 16
Z9 16
U1 2
U2 22
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2011
VL 46
IS 9
BP 1313
EP 1328
DI 10.1111/j.1945-5100.2011.01231.x
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 822MY
UT WOS:000295053300006
ER
PT J
AU De Gregorio, BT
Stroud, RM
Cody, GD
Nittler, LR
Kilcoyne, ALD
Wirick, S
AF De Gregorio, Bradley T.
Stroud, Rhonda M.
Cody, George D.
Nittler, Larry R.
Kilcoyne, A. L. David
Wirick, Sue
TI Correlated microanalysis of cometary organic grains returned by Stardust
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID X-RAY SPECTROMICROSCOPY; TRANSMISSION ELECTRON-MICROSCOPY;
INTERPLANETARY DUST PARTICLES; MOLECULAR-CLOUD MATERIAL; INNER-SHELL
EXCITATION; ISOTOPIC COMPOSITIONS; 81P/WILD 2; INFRARED-SPECTROSCOPY;
HYPERVELOCITY CAPTURE; CORE EXCITATION
AB Carbonaceous matter in Stardust samples returned from comet 81P/Wild 2 is observed to contain a wide variety of organic functional chemistry. However, some of this chemical variety may be due to contamination or alteration during particle capture in aerogel. We investigated six carbonaceous Stardust samples that had been previously analyzed and six new samples from Stardust Track 80 using correlated transmission electron microscopy (TEM), X-ray absorption near-edge structure spectroscopy (XANES), and secondary ion mass spectroscopy (SIMS). TEM revealed that samples from Track 35 containing abundant aliphatic XANES signatures were predominantly composed of cometary organic matter infilling densified silica aerogel. Aliphatic organic matter from Track 16 was also observed to be soluble in the epoxy embedding medium. The nitrogen-rich samples in this study (from Track 22 and Track 80) both contained metal oxide nanoparticles, and are likely contaminants. Only two types of cometary organic matter appear to be relatively unaltered during particle capture. These are (1) polyaromatic carbonyl-containing organic matter, similar to that observed in insoluble organic matter (IOM) from primitive meteorites, interplanetary dust particles (IDPs), and in other carbonaceous Stardust samples, and (2) highly aromatic refractory organic matter, which primarily constitutes nanoglobule-like features. Anomalous isotopic compositions in some of these samples also confirm their cometary heritage. There also appears to be a significant labile aliphatic component of Wild 2 organic matter, but this material could not be clearly distinguished from carbonaceous contaminants known to be present in the Stardust aerogel collector.
C1 [De Gregorio, Bradley T.; Stroud, Rhonda M.] USN, Mat Sci & Technol Div, Res Lab, Washington, DC USA.
[De Gregorio, Bradley T.] NASA Johnson Space Ctr, ESCG, Houston, TX USA.
[Cody, George D.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA.
[Nittler, Larry R.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Kilcoyne, A. L. David] Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA USA.
[Wirick, Sue] Brookhaven Natl Lab, Natl Synchrotron Light Source, Upton, NY 11973 USA.
RP De Gregorio, BT (reprint author), USN, Mat Sci & Technol Div, Res Lab, Washington, DC USA.
EM brad.degregorio@gmail.com
RI De Gregorio, Bradley/B-8465-2008; Kilcoyne, David/I-1465-2013; Stroud,
Rhonda/C-5503-2008
OI De Gregorio, Bradley/0000-0001-9096-3545; Stroud,
Rhonda/0000-0001-5242-8015
FU Office of Naval Research; NASA; NASA Astrobiology Institute; U.S.
Department of Energy; Natural Sciences and Engineering Research Council
of Canada; National Research Council Canada; Canadian Institutes of
Health Research; Province of Saskatchewan; Western Economic
Diversification Canada; University of Saskatchewan
FX This work was funded by the Office of Naval Research, NASA Discovery
Data Analysis and Origins of Solar Systems Program, and NASA
Astrobiology Institute. This research was conducted while the primary
author held a National Research Council Research Associateship at the
U.S. Naval Research Laboratory. Use of the Advanced Light Source and the
National Synchrotron Light Source was supported by the U.S. Department
of Energy. Use of the Canadian Light Source was supported by the Natural
Sciences and Engineering Research Council of Canada, the National
Research Council Canada, the Canadian Institutes of Health Research, the
Province of Saskatchewan, Western Economic Diversification Canada, and
the University of Saskatchewan. The authors gratefully acknowledge the
support of Thomas Zega and Nabil Bassim with the acquisition of STXM
data.
NR 85
TC 16
Z9 16
U1 1
U2 26
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2011
VL 46
IS 9
BP 1376
EP 1396
DI 10.1111/j.1945-5100.2011.01237.x
PG 21
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 822MY
UT WOS:000295053300010
ER
PT J
AU Smith, DJB
Dunne, L
Maddox, SJ
Eales, S
Bonfield, DG
Jarvis, MJ
Sutherland, W
Fleuren, S
Rigby, EE
Thompson, MA
Baldry, IK
Bamford, S
Buttiglione, S
Cava, A
Clements, DL
Cooray, A
Croom, S
Dariush, A
de Zotti, G
Driver, SP
Dunlop, JS
Fritz, J
Hill, DT
Hopkins, A
Hopwood, R
Ibar, E
Ivison, RJ
Jones, DH
Kelvin, L
Leeuw, L
Liske, J
Loveday, J
Madore, BF
Norberg, P
Panuzzo, P
Pascale, E
Pohlen, M
Popescu, CC
Prescott, M
Robotham, A
Rodighiero, G
Scott, D
Seibert, M
Sharp, R
Temi, P
Tuffs, RJ
van der Werf, P
van Kampen, E
AF Smith, D. J. B.
Dunne, L.
Maddox, S. J.
Eales, S.
Bonfield, D. G.
Jarvis, M. J.
Sutherland, W.
Fleuren, S.
Rigby, E. E.
Thompson, M. A.
Baldry, I. K.
Bamford, S.
Buttiglione, S.
Cava, A.
Clements, D. L.
Cooray, A.
Croom, S.
Dariush, A.
de Zotti, G.
Driver, S. P.
Dunlop, J. S.
Fritz, J.
Hill, D. T.
Hopkins, A.
Hopwood, R.
Ibar, E.
Ivison, R. J.
Jones, D. H.
Kelvin, L.
Leeuw, L.
Liske, J.
Loveday, J.
Madore, B. F.
Norberg, P.
Panuzzo, P.
Pascale, E.
Pohlen, M.
Popescu, C. C.
Prescott, M.
Robotham, A.
Rodighiero, G.
Scott, D.
Seibert, M.
Sharp, R.
Temi, P.
Tuffs, R. J.
van der Werf, P.
van Kampen, E.
TI Herschel-ATLAS: counterparts from the ultraviolet-near-infrared in the
science demonstration phase catalogue
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: statistical; submillimetre: galaxies
ID DIGITAL SKY SURVEY; DEEP-FIELD-SOUTH; MASS ASSEMBLY GAMA; SUBMILLIMETER
GALAXIES; REDSHIFT SURVEY; MIDINFRARED COUNTERPARTS; IRAS GALAXIES;
RADIO GALAXY; 2DF-SDSS LRG; MU-M
AB We present a technique to identify optical counterparts of 250-mu m-selected sources from the Herschel-ATLAS survey. Of the 6621 250 mu m > 32-mJy sources in our science demonstration catalogue we find that similar to 60 per cent have counterparts brighter than r = 22.4 mag in the Sloan Digital Sky Survey. Applying a likelihood ratio technique we are able to identify 2423 of the counterparts with a reliability R > 0.8. This is approximately 37 per cent of the full 250-mu m catalogue. We have estimated photometric redshifts for each of these 2423 reliable counterparts, while 1099 also have spectroscopic redshifts collated from several different sources, including the GAMA survey. We estimate the completeness of identifying counterparts as a function of redshift, and present evidence that 250-mu m-selected Herschel-ATLAS galaxies have a bimodal redshift distribution. Those with reliable optical identifications have a redshift distribution peaking at z approximate to 0.25 +/- 0.05, while submillimetre colours suggest that a significant fraction with no counterpart above the r-band limit have z > 1. We also suggest a method for selecting populations of strongly lensed high-redshift galaxies. Our identifications are matched to UV-NIR photometry from the GAMA survey, and these data are available as part of the Herschel-ATLAS public data release.
C1 [Smith, D. J. B.; Dunne, L.; Maddox, S. J.; Rigby, E. E.; Bamford, S.] Univ Nottingham, Sch Phys & Astron, Ctr Astron & Particle Theory, Nottingham NG7 1HR, England.
[Smith, D. J. B.; Bonfield, D. G.; Jarvis, M. J.; Thompson, M. A.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Eales, S.; Dariush, A.; Pascale, E.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Sutherland, W.; Fleuren, S.] Univ London, Sch Math Sci, London E1 4NS, England.
[Baldry, I. K.; Prescott, M.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Buttiglione, S.; de Zotti, G.; Rodighiero, G.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy.
[Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain.
[Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England.
[Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Croom, S.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[de Zotti, G.] SISSA, I-34136 Trieste, Italy.
[Driver, S. P.; Hill, D. T.; Kelvin, L.; Robotham, A.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Driver, S. P.] Univ Western Australia, Int Ctr Radio Astron Res, Perth, WA 6009, Australia.
[Dunlop, J. S.; Ivison, R. J.; Norberg, P.; van der Werf, P.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Hopkins, A.; Jones, D. H.; Sharp, R.] Anglo Australian Observ, Epping, NSW 1710, Australia.
[Hopwood, R.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[Ibar, E.; Ivison, R. J.] Royal Observ, Uk Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Leeuw, L.] SETI Inst, Mountain View, CA 94043 USA.
[Liske, J.; van Kampen, E.] European So Observ, D-85748 Garching, Germany.
[Loveday, J.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Madore, B. F.; Seibert, M.] Observ Carnegie Inst, Pasadena, CA 91101 USA.
[Panuzzo, P.] CEA, Lab AIM, Irfu SAp, F-91191 Gif Sur Yvette, France.
[Popescu, C. C.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA.
[Tuffs, R. J.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Smith, DJB (reprint author), Univ Nottingham, Sch Phys & Astron, Ctr Astron & Particle Theory, Univ Pk Campus, Nottingham NG7 1HR, England.
EM daniel.j.b.smith@gmail.com
RI Robotham, Aaron/H-5733-2014; Driver, Simon/H-9115-2014; Ivison,
R./G-4450-2011; Bamford, Steven/E-8702-2010; Cava, Antonio/C-5274-2017;
OI Robotham, Aaron/0000-0003-0429-3579; Driver, Simon/0000-0001-9491-7327;
Ivison, R./0000-0001-5118-1313; Bamford, Steven/0000-0001-7821-7195;
Cava, Antonio/0000-0002-4821-1275; Scott, Douglas/0000-0002-6878-9840;
Maddox, Stephen/0000-0001-5549-195X; Smith, Daniel/0000-0001-9708-253X;
Rodighiero, Giulia/0000-0002-9415-2296; Liske,
Jochen/0000-0001-7542-2927; Baldry, Ivan/0000-0003-0719-9385
FU NASA; Alfred P. Sloan Foundation; National Science Foundation; US
Department of Energy; National Aeronautics and Space Administration;
Japanese Monbukagakusho; Max Planck Society; Higher Education Funding
Council for England; ASI [I/009/10/0 'COFIS']
FX Herschel is an ESA space observatory with science instruments provided
by European-led Principal Investigator consortia with significant
participation from NASA. US participants in Herschel-ATLAS acknowledge
support provided by NASA through a contract issued from JPL. GAMA is a
joint European-Australasian project based around a spectroscopic
campaign using the Anglo-Australian Telescope. The GAMA input catalogue
is based on data taken from the SDSS and the UKIRT Infrared Deep Sky
Survey. Complementary imaging of the GAMA regions is being obtained by a
number of independent survey programmes including GALEX MIS, VST KIDS,
VISTA VIKING, WISE, Herschel-ATLAS, GMRT and ASKAP providing UV to radio
coverage. The GAMA website is: http://www.gama-survey.org/. This work
used data from the UKIDSS DR5 and the SDSS DR7. The UKIDSS project is
defined in Lawrence et al. (2007) and uses the UKIRT Wide Field Camera
(WFCAM; Casali et al. 2007). Funding for the SDSS and SDSS-II has been
provided by the Alfred P. Sloan Foundation, the Participating
Institutions, The National Science Foundation, the US Department of
Energy, the National Aeronautics and Space Administration, the Japanese
Monbukagakusho, the Max Planck Society and the Higher Education Funding
Council for England. The Italian group acknowledges partial financial
support from ASI contract I/009/10/0 'COFIS'.
NR 69
TC 66
Z9 67
U1 1
U2 6
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 SEP
PY 2011
VL 416
IS 2
BP 857
EP 872
DI 10.1111/j.1365-2966.2011.18827.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823KA
UT WOS:000295119900004
ER
PT J
AU Davies, B
Hoare, MG
Lumsden, SL
Hosokawa, T
Oudmaijer, RD
Urquhart, JS
Mottram, JC
Stead, J
AF Davies, Ben
Hoare, Melvin G.
Lumsden, Stuart L.
Hosokawa, Takashi
Oudmaijer, Rene D.
Urquhart, James S.
Mottram, Joseph C.
Stead, Joseph
TI The Red MSX Source survey: critical tests of accretion models for the
formation of massive stars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: formation; stars: massive; stars: pre-main-sequence; stars:
protostars
ID YOUNG STELLAR OBJECTS; GALACTIC-O-STARS; H-II REGIONS; RMS SURVEY;
GRAVITATIONAL COLLAPSE; (CO)-C-13 OBSERVATIONS; SOUTHERN-HEMISPHERE;
CLUSTER; YSOS; EXTINCTION
AB There is currently no accepted theoretical framework for the formation of the most massive stars, and the manner in which protostars continue to accrete and grow in mass beyond similar to 10M(circle dot) is still a controversial topic. In this study we use several prescriptions of stellar accretion and a description of the Galactic gas distribution to simulate the luminosities and spatial distribution of massive protostellar population of the Galaxy. We then compare the observables of each simulation to the results of the Red MSX Source (RMS) survey, a recently compiled data base of massive young stellar objects (YSO). We find that the observations are best matched by accretion rates which increase as the protostar grows in mass, such as those predicted by the turbulent core and competitive accretion (i.e. Bondi-Hoyle) models. These 'accelerating accretion' models provide very good qualitative and quantitative fits to the data, though we are unable to distinguish between these two models on our simulations alone. We rule out models with accretion rates which are constant with time, and those which are initially very high and which fall away with time, as these produce results which are quantitatively and/or qualitatively incompatible with the observations. To simultaneously match the low- and high-luminosity YSO distribution we require the inclusion of a 'swollen-star' pre-main-sequence phase, the length of which is well-described by the Kelvin-Helmholz time-scale. Our results suggest that the lifetime of the YSO phase is similar to 10(5) yr, whereas the compact HII region phase lasts between similar to 2 and 4 x 10(5) yr depending on the final mass of the star. Finally, the absolute numbers of YSOs are best matched by a globally averaged star formation rate for the Galaxy of 1.5-2M(circle dot).
C1 [Davies, Ben] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Davies, Ben; Hoare, Melvin G.; Lumsden, Stuart L.; Oudmaijer, Rene D.; Stead, Joseph] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Hosokawa, Takashi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hosokawa, Takashi] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan.
[Urquhart, James S.] CSIRO, Australia Telescope Natl Facil, Sydney, NSW 2052, Australia.
[Mottram, Joseph C.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
RP Davies, B (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
EM bdavies@ast.cam.ac.uk
RI Davies, Ben/K-3996-2012;
OI Davies, Ben/0000-0002-2010-2122
FU Royal Astronomical Society
FX We would like to thank the anonymous referee for several comments and
suggestions that helped improve our paper. We thank Jonathan Tan and
Willem-Jan de Wit for many useful discussions during the course of this
work. BD is funded by a fellowship from the Royal Astronomical Society.
NR 71
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U1 8
U2 58
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 SEP
PY 2011
VL 416
IS 2
BP 972
EP 990
DI 10.1111/j.1365-2966.2011.19095.x
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823KA
UT WOS:000295119900013
ER
PT J
AU Zdziarski, AA
Skinner, GK
Pooley, GG
Lubinski, P
AF Zdziarski, Andrzej A.
Skinner, Gerald K.
Pooley, Guy G.
Lubinski, Piotr
TI X-ray variability patterns and radio/X-ray correlations in Cyg X-1
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; stars: individual: Cyg X-1; stars:
individual: HDE 226868; radio continuum: stars; X-rays: binaries;
X-rays: stars
ID ACCRETING BLACK-HOLES; TRANSIENT SOURCE EXPERIMENT; BROAD-BAND SPECTRUM;
ALL-SKY MONITOR; GX 339-4; LOW/HARD-STATE; ORBITAL MODULATION;
RELATIVISTIC JETS; TERM VARIABILITY; TIMING EXPLORER
AB We have studied the X-ray variability patterns and correlations of the radio and X-ray fluxes in all spectral states of Cyg X-1 using X-ray data from the All-Sky Monitor onboard the Rossi X-ray Timing Explorer, Burst And Transient Source Experiment onboard the Compton Gamma Ray Observatory and the Burst Alert Telescope onboard Swift. In the hard state, the dominant spectral variability is a changing of normalization with a fixed spectral shape, while in the intermediate state, the slope changes, with a pivot point around 10 keV. In the soft state, the low-energy X-ray emission dominates the bolometric flux which is only loosely correlated with the high-energy emission. In black hole binaries in the hard state, the radio flux is generally found to depend on a power of the X-ray flux, F-R proportional to F-X(p). We confirm this for Cyg X-1. Our new finding is that this correlation extends to the intermediate and soft states, provided the broad-band X-ray flux in the Comptonization part of the spectrum (excluding the blackbody component) is considered instead of a narrow-band medium-energy X-ray flux. We find an index p similar or equal to 1.7 +/- 0.1 for 15-GHz radio emission, decreasing to p similar or equal to 1.5 +/- 0.1 at 2.25 GHz. We conclude that the higher value at 15 GHz is due to the effect of free-free absorption in the wind from the companion. The intrinsic correlation index remains uncertain. However, based on a theoretical model of the wind in Cyg X-1, it may to be close to similar or equal to 1.3, which, in the framework of accretion/jet models, would imply that the accretion flow in Cyg X-1 is radiatively efficient. The correlation with the flux due to Comptonization emission indicates that the radio jet is launched by the hot electrons in the accretion flow in all spectral states of Cyg X-1. On the other hand, we are able to rule out the X-ray jet model. Finally, we find that the index of the correlation, when measured using the X-ray flux in a narrow energy band, strongly depends on the band chosen and is, in general, different from that for either the bolometric flux or the flux in the hot-electron emission.
C1 [Zdziarski, Andrzej A.] Ctr Astron M Kopernika, PL-00716 Warsaw, Poland.
[Skinner, Gerald K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Skinner, Gerald K.] CRESST, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Skinner, Gerald K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Pooley, Guy G.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England.
[Lubinski, Piotr] Ctr Astron M Kopernika, PL-87100 Torun, Poland.
RP Zdziarski, AA (reprint author), Ctr Astron M Kopernika, Bartycka 18, PL-00716 Warsaw, Poland.
EM aaz@camk.edu.pl
FU Polish MNiSW [N N203 581240, N N203 404939, 362/1/N-INTEGRAL/2008/09/0];
STFC; NASA
FX We thank T. Belloni, S. Corbel, R. Narayan, M. Ostrowski, A. R. Rao and
F. Yuan for valuable discussions. We also thank M. Coriat for providing
us with the data used in Fig. 11 and the referee for valuable
suggestions. This research has been supported in part by the Polish
MNiSW grants N N203 581240, N N203 404939 and
362/1/N-INTEGRAL/2008/09/0. The AMI Large Arrays are operated by the
University of Cambridge and supported by the STFC. The GBI is a facility
of the National Science Foundation operated by the NRAO in support of
NASA High Energy Astrophysics programmes. We acknowledge the use of data
provided by the RXTE-ASM and Swift-BAT teams.
NR 79
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U1 0
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2011
VL 416
IS 2
BP 1324
EP 1339
DI 10.1111/j.1365-2966.2011.19127.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823KA
UT WOS:000295119900040
ER
PT J
AU Townsend, LJ
Coe, MJ
Corbet, RHD
Hill, AB
AF Townsend, L. J.
Coe, M. J.
Corbet, R. H. D.
Hill, A. B.
TI On the orbital parameters of Be/X-ray binaries in the Small Magellanic
Cloud
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE ephemerides; stars: emission-line, Be; Magellanic Clouds; X-rays:
binaries
ID X-RAY; ACCRETING PULSAR; SUPERGIANT SYSTEM; TIMING-EXPLORER; GRO
J1750-27; NEUTRON-STAR; II OUTBURST; SPIN-UP; MASS; DISCOVERY
AB The orbital motion of a neutron star about its optical companion presents a window through which we can study the orbital parameters of that binary system. This has been used extensively in the Milky Way to calculate these parameters for several high-mass X-ray binaries. Using several years of Rossi X-ray Timing Explorer Proportional Counter Array data, we derive the orbital parameters of four Be/X-ray binary systems in the Small Magellanic Cloud (SMC), increasing the number of systems with orbital solutions by a factor of 3. We find one new orbital period, confirm a second and discuss the parameters with comparison to the Galactic systems. Despite the low metallicity in the SMC, these binary systems sit amongst the Galactic distribution of orbital periods and eccentricities, suggesting that metallicity may not play an important role in the evolution of high-mass X-ray binary systems. A plot of orbital period against eccentricity shows that the supergiant, Be and low-eccentricity OB transient systems occupy separate regions of the parameter space; akin to the separated regions on the Corbet diagram. Using a Spearman's rank correlation test, we also find a possible correlation between the two parameters. The mass functions, inclinations and orbital semimajor axes are derived for the SMC systems based on the binary parameters and the spectral classification of the optical counterpart. As a by-product of our work, we present a catalogue of the orbital parameters for every high-mass X-ray binary in the Galaxy and Magellanic Clouds for which they are known.
C1 [Townsend, L. J.; Coe, M. J.; Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Corbet, R. H. D.] Univ Maryland Baltimore Cty, Xray Astrophys Lab, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Townsend, LJ (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
EM ljt203@soton.ac.uk
OI Hill, Adam/0000-0003-3470-4834
FU University of Southampton
FX LJT is supported by a Mayflower scholarship from the University of
Southampton. We would like to thank the anonymous referee for their
helpful and constructive comments.
NR 89
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U1 0
U2 0
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 SEP
PY 2011
VL 416
IS 2
BP 1556
EP 1565
DI 10.1111/j.1365-2966.2011.19153.x
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823KA
UT WOS:000295119900060
ER
PT J
AU Oliker, L
Nishtala, R
Biswas, R
AF Oliker, Leonid
Nishtala, Rajesh
Biswas, Rupak
TI Emerging programming paradigms for large-scale scientific computing
SO PARALLEL COMPUTING
LA English
DT Editorial Material
C1 [Oliker, Leonid] Univ Calif Berkeley, Lawrence Berkeley Lab, Computat Res Div, NERSC, Berkeley, CA 94720 USA.
[Nishtala, Rajesh] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA.
[Biswas, Rupak] NASA, Ames Res Ctr, NAS Div, Moffett Field, CA 94035 USA.
RP Oliker, L (reprint author), Univ Calif Berkeley, Lawrence Berkeley Lab, Computat Res Div, NERSC, Berkeley, CA 94720 USA.
EM rupak.biswas@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0167-8191
J9 PARALLEL COMPUT
JI Parallel Comput.
PD SEP
PY 2011
VL 37
IS 9
SI SI
BP 499
EP 500
DI 10.1016/j.parco.2011.07.002
PG 2
WC Computer Science, Theory & Methods
SC Computer Science
GA 823TW
UT WOS:000295150400001
ER
PT J
AU Jin, HQ
Jespersen, D
Mehrotra, P
Biswas, R
Huang, L
Chapman, B
AF Jin, Haoqiang
Jespersen, Dennis
Mehrotra, Piyush
Biswas, Rupak
Huang, Lei
Chapman, Barbara
TI High performance computing using MPI and OpenMP on multi-core parallel
systems
SO PARALLEL COMPUTING
LA English
DT Article
DE Hybrid MPI plus OpenMP programming; Multi-core Systems; OpenMP
Extensions; Data Locality
ID CHAPEL
AB The rapidly increasing number of cores in modern microprocessors is pushing the current high performance computing (HPC) systems into the petascale and exascale era. The hybrid nature of these systems - distributed memory across nodes and shared memory with non-uniform memory access within each node - poses a challenge to application developers. In this paper, we study a hybrid approach to programming such systems - a combination of two traditional programming models, MPI and OpenMP. We present the performance of standard benchmarks from the multi-zone NAS Parallel Benchmarks and two full applications using this approach on several multi-core based systems including an SGI Altix 4700, an IBM p575+ and an SGI Altix ICE 8200EX. We also present new data locality extensions to OpenMP to better match the hierarchical memory structure of multi-core architectures. Published by Elsevier B.V.
C1 [Jin, Haoqiang; Jespersen, Dennis; Mehrotra, Piyush; Biswas, Rupak] NASA, Ames Res Ctr, NAS Div, Moffett Field, CA 94035 USA.
[Huang, Lei; Chapman, Barbara] Univ Houston, Dept Comp Sci, Houston, TX 77004 USA.
RP Jin, HQ (reprint author), NASA, Ames Res Ctr, NAS Div, Moffett Field, CA 94035 USA.
EM haoqiang.jin@nasa.gov
FU National Science Foundation [CCF-0702775]; University of Houston
FX The authors thank Jahed Djomehri for providing the CART3D results
presented here, Johnny Chang and Robert Hood for their valuable
discussion and comments, the NAS HECC staff for their support in
conducting these performance measurements on the NAS systems, and
anonymous reviewers for their valuable comments on the manuscript. The
work was partially supported by the National Science Foundation grant
CCF-0702775 with the University of Houston.
NR 32
TC 45
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U1 1
U2 25
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0167-8191
J9 PARALLEL COMPUT
JI Parallel Comput.
PD SEP
PY 2011
VL 37
IS 9
SI SI
BP 562
EP 575
DI 10.1016/j.parco.2011.02.002
PG 14
WC Computer Science, Theory & Methods
SC Computer Science
GA 823TW
UT WOS:000295150400006
ER
PT J
AU Grant, JA
Golombek, MP
Grotzinger, JP
Wilson, SA
Watkins, MM
Vasavada, AR
Griffes, JL
Parker, TJ
AF Grant, John A.
Golombek, Matthew P.
Grotzinger, John P.
Wilson, Sharon A.
Watkins, Michael M.
Vasavada, Ashwin R.
Griffes, Jennifer L.
Parker, Timothy J.
TI The science process for selecting the landing site for the 2011 Mars
Science Laboratory
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mars; Landing sites
ID MERIDIANI-PLANUM; VALLES-MARINERIS; LAYERED DEPOSITS; TERRA MERIDIANI;
MAWRTH-VALLIS; CLAY-MINERALS; HOLDEN CRATER; MELAS-CHASMA; ART.;
EVOLUTION
AB The process of identifying the landing site for NASA's 2011 Mars Science Laboratory (MSL) began in 2005 by defining science objectives, related to evaluating the potential habitability of a location on Mars, and engineering parameters, such as elevation, latitude, winds, and rock abundance, to determine acceptable surface and atmospheric characteristics. Nearly 60 candidate sites were considered at a series of open workshops in the years leading up to the launch. During that period, iteration between evolving engineering constraints and the relative science potential of candidate sites led to consensus on four final sites. The final site will be selected in the Spring of 2011 by NASA's Associate Administrator for the Science Mission Directorate. This paper serves as a record of landing site selection activities related primarily to science, an inventory of the number and variety of sites proposed, and a summary of the science potential of the highest ranking sites. Published by Elsevier Ltd.
C1 [Grant, John A.; Wilson, Sharon A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
[Golombek, Matthew P.; Watkins, Michael M.; Vasavada, Ashwin R.; Parker, Timothy J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grotzinger, John P.; Griffes, Jennifer L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Grant, JA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, 6th & Independence SW, Washington, DC 20560 USA.
EM grantj@si.edu
FU NASA MDAP [NNX09AI65G]
FX Reviews by Nicolas Mangold and an anonymous reviewer improved the
manuscript. Work supported by NASA MDAP Grant NNX09AI65G.
NR 75
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U1 2
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD SEP
PY 2011
VL 59
IS 11-12
SI SI
BP 1114
EP 1127
DI 10.1016/j.pss.2010.06.016
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 822TS
UT WOS:000295073100002
ER
PT J
AU Compher, EM
Gupta, MC
Wilson, WC
Madaras, EI
AF Compher, Eric M.
Gupta, Moo C.
Wilson, William C.
Madaras, Eric I.
TI Solar powered micrometeorite sensors using indoor ambient light for the
International Space Station
SO SOLAR ENERGY
LA English
DT Article
DE Solar cell; Sensor; Space station; Micrometeriote; Photovoltaics;
Ambient light
ID NETWORK
AB Sensors for detecting micrometeorite impact locations and magnitudes as well as pressure vessel leaks have been under investigation for some time by the NASA Langley Research Center and other related entities. NASA has been investigating the use of the Distribution Impact Detection System (DIDS) for use on the International Space Station (ISS). However, the DIDS currently requires thionyl chloride lithium batteries which pose explosion and toxicity hazards, and replacing batteries is tedious and utilizes scarce man-hours. Carrying replacement batteries into space is also expensive. To hardwire new sensing devices into the ISS while in orbit would be time consuming. To overcome this problem, high efficiency GaAs solar cells have been studied under low light conditions comparable to those found inside the ISS. The cells were also studied for temperature dependence. Solar concentrators were investigated for possible use with ambient lighting. The power generated by the cells was stored in a large 300 F supercapacitor. A DC to DC boost regulator was modified to produce an output voltage of 3.55 V that is required by the DIDS. The successful operation of the DIDS with ambient light power, supercapacitor energy storage, and boost regulation was demonstrated. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Compher, Eric M.; Gupta, Moo C.] Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA.
[Wilson, William C.; Madaras, Eric I.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Gupta, MC (reprint author), Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA.
EM mgupta@virginia.edu
FU NASA Langley Research Center's Nondestructive Evaluative Sciences Branch
(NESB)
FX Thanks to Dr. William Winfree of NASA Langley Research Center's
Nondestructive Evaluative Sciences Branch (NESB) for his support of this
project.
NR 14
TC 0
Z9 0
U1 3
U2 12
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0038-092X
J9 SOL ENERGY
JI Sol. Energy
PD SEP
PY 2011
VL 85
IS 9
BP 1899
EP 1905
DI 10.1016/j.solener.2011.04.029
PG 7
WC Energy & Fuels
SC Energy & Fuels
GA 824WT
UT WOS:000295233600017
ER
PT J
AU Dominguez, A
Kleissl, J
Luvall, JC
AF Dominguez, Anthony
Kleissl, Jan
Luvall, Jeffrey C.
TI Effects of solar photovoltaic panels on roof heat transfer
SO SOLAR ENERGY
LA English
DT Article
DE Building energy use; Cooling load; Photovoltaic; Roof heat flux; Thermal
infrared camera
ID COOLING ENERGY SAVINGS; PEAK POWER; SYSTEMS; MODEL
AB Indirect benefits of rooftop photovoltaic (PV) systems for building insulation are quantified through measurements and modeling. Measurements of the thermal conditions throughout a roof profile on a building partially covered by solar photovoltaic (PV) panels were conducted in San Diego, California. Thermal infrared imagery on a clear April day demonstrated that daytime ceiling temperatures under the PV arrays were up to 2.5 K cooler than under the exposed roof. Heat flux modeling showed a significant reduction in daytime roof heat flux under the PV array. At night the conditions reversed and the ceiling under the PV arrays was warmer than for the exposed roof indicating insulating properties of PV. Simulations showed no benefit (but also no disadvantage) of the PV covered roof for the annual heating load, but a 5.9 kWh m(-2) (or 38%) reduction in annual cooling load. The reduced daily variability in rooftop surface temperature under the PV array reduces thermal stresses on the roof and leads to energy savings and/or human comfort benefits especially for rooftop PV on older warehouse buildings. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Dominguez, Anthony; Kleissl, Jan] Univ Calif San Diego, Dept Mech & Aerosp Engn, La Jolla, CA 92093 USA.
[Luvall, Jeffrey C.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Kleissl, J (reprint author), Univ Calif San Diego, Dept Mech & Aerosp Engn, 9500 Gilman Dr,EBUII 580, La Jolla, CA 92093 USA.
EM jkleissl@ucsd.edu
FU NASA; NSF; Hellman Foundation
FX Anthony Dominguez was funded by the NASA graduate student researchers
program. Kleissl acknowledges funding from a NSF CAREER award and the
Hellman Foundation. The following UCSD undergraduate students were
instrumental in the data collection: Avneet Singh, Kevin Chivatakarn,
Thomas Minor, Jeremiah Farinella. We thank Ronnen Levinson for
contributing his expertise and the Powell Structural Systems Laboratory
building staff, especially Andrew Gunthardt, for being supportive of our
work and allowing access to the building for the measurements.
NR 17
TC 16
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U1 0
U2 16
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0038-092X
J9 SOL ENERGY
JI Sol. Energy
PD SEP
PY 2011
VL 85
IS 9
BP 2244
EP 2255
DI 10.1016/j.solener.2011.06.010
PG 12
WC Energy & Fuels
SC Energy & Fuels
GA 824WT
UT WOS:000295233600050
ER
PT J
AU Pinilla-Alonso, N
Roush, TL
Marzo, GA
Cruikshank, DP
Ore, CMD
AF Pinilla-Alonso, Noemi
Roush, Ted L.
Marzo, Giuseppe A.
Cruikshank, Dale P.
Ore, Cristina M. Dalle
TI Iapetus surface variability revealed from statistical clustering of a
VIMS mosaic: The distribution of CO2
SO ICARUS
LA English
DT Article
DE Iapetus; Ices; Spectroscopy; Satellites, Composition; Satellites,
Surfaces
ID NEAR-INFRARED SPECTROSCOPY; CASSINI-VIMS; CARBON-DIOXIDE; ICY
SATELLITES; DARK MATERIAL; MU-M; HYDROCARBONS; MIXTURES; SPECTRA
AB We present a detailed study of an Iapetus mosaic of VIMS data with high spatial resolution (0.5 x 0.5 degrees or similar to 6.4 km/pixel). The spectra were taken in August 2007 and provide the highest VIMS spatial resolution data for this object during Cassini's primary mission. We analyze this set of data using a statistical clustering approach to reduce the analysis of a large number of data (similar to 10(4) spectra from 0.35 to 5.10 mu m) to the study of seven representative groups accounting for 99.6% of the surface covered by the original sample. We analyze the spectral absorption bands in the spectra of the different clusters indicative of different composition over the observed surface. We find coherence between the distribution of the clusters and the geographical features on the surface. We give special attention to the study of the water ice and CO2 bands. We find that CO2 is widespread over the entire surface being studied, including the bright and dark areas on Iapetus' surface, and is probably trapped at the molecular level with other materials. The strength of the CO2 band in the areas where both, H2O- and carbon-bearing materials exist, gives support to the hypothesis that this volatile is formed on the surface of Iapetus as a product of irradiation of these two components. Finally, we also compare the Iapetus CO2 with that on other satellites confirming, that there are evident differences on the center, depth and width of the band on Iapetus and Phoebe, where CO2 has been suggested to be endogenous. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Pinilla-Alonso, Noemi] NASA, Ames Res Ctr, NASA Postdoctoral Program, Moffett Field, CA 94035 USA.
[Marzo, Giuseppe A.] ENEA, CR Casaccia, I-00123 Rome, Italy.
[Ore, Cristina M. Dalle] SETI Inst, Mountain View, CA 94043 USA.
RP Pinilla-Alonso, N (reprint author), NASA, Ames Res Ctr, NASA Postdoctoral Program, Mail Stop 245-6, Moffett Field, CA 94035 USA.
EM npinilla@seti.org
RI Marzo, Giuseppe/A-9765-2015
FU NASA
FX N.P.A. acknowledges the support from NASA Postdoctoral Program
administered by Oak Ridge Associated Universities through a contract
with NASA. T.L.R. and G.A.M. acknowledge NASA's Planetary Geology &
Geophysics program for supporting part of this research. We appreciate
the thorough reviews of this manuscript given by G.R. Filacchione and an
anonymous referee.
NR 40
TC 14
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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 SEP
PY 2011
VL 215
IS 1
BP 75
EP 82
DI 10.1016/j.icarus.2011.07.004
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821NJ
UT WOS:000294981400008
ER
PT J
AU Morishima, R
Spilker, L
Ohtsuki, K
AF Morishima, Ryuji
Spilker, Linda
Ohtsuki, Keiji
TI A multilayer model for thermal infrared emission of Saturn's rings. III:
Thermal inertia inferred from Cassini CIRS
SO ICARUS
LA English
DT Article
DE Saturn, Rings; Infrared observations; Radiative transfer; Regoliths
ID PARTICLE-SIZE DISTRIBUTIONS; DENSE PLANETARY RINGS; SELF-GRAVITY WAKES;
NUMERICAL SIMULATIONS; STELLAR OCCULTATION; MAIN RINGS; B-RING; C-RING;
ROTATION; CONDUCTIVITY
AB The thermal inertia values of Saturn's main rings (the A, B, and C rings and the Cassini division) are derived by applying our thermal model to azimuthally scanned spectra taken by the Cassini Composite Infrared Spectrometer (CIRS). Model fits show the thermal inertia of ring particles to be 16, 13, 20, and 11 J m(-2) K-1 s(-1/2) for the A, B, and C rings, and the Cassini division, respectively. However, there are systematic deviations between modeled and observed temperatures in Saturn's shadow depending on solar phase angle, and these deviations indicate that the apparent thermal inertia increases with solar phase angle. This dependence is likely to be explained if large slowly spinning particles have lower thermal inertia values than those for small fast spinning particles because the thermal emission of slow rotators is relatively stronger than that of fast rotators at low phase and vise versa. Additional parameter fits, which assume that slow and fast rotators have different thermal inertia values, show the derived thermal inertia values of slow (fast) rotators to be 8 (77), 8 (27), 9 (34), 5 (55) J m(-2) K-1 s(-1/2) for the A, B, and C rings, and the Cassini division, respectively. The values for fast rotators are still much smaller than those for solid ice with no porosity. Thus, fast rotators are likely to have surface regolith layers, but these may not be as fluffy as those for slow rotators, probably because the capability of holding regolith particles is limited for fast rotators due to the strong centrifugal force on surfaces of fast rotators. Other additional parameter fits, in which radii of fast rotators are varied, indicate that particles less than similar to 1 cm should not occupy more than roughly a half of the cross section for the A, B, and C rings. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Morishima, Ryuji; Spilker, Linda] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morishima, Ryuji] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Morishima, Ryuji; Ohtsuki, Keiji] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Ohtsuki, Keiji] Kobe Univ, Dept Earth & Planetary Sci, Kobe, Hyogo 6578501, Japan.
[Ohtsuki, Keiji] Kobe Univ, Ctr Planetary Sci, Kobe, Hyogo 6578501, Japan.
RP Morishima, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Ryuji.Morishima@jpl.nasa.gov
FU Cassini project; NASA; JSPS [22340125]
FX We thank Cedric Leyrat and an anonymous reviewer for their comments,
which improved our manuscript. We are grateful for the support by the
Cassini project and the NASA's OPR and PGG Programs. K.O. is also
grateful for the support by JSPS KAKENHI (22340125). We thank Nicholas
Altobelli and Stu Pilorz for developing the CIRS database, Scott
Edington, Shawn Brooks and Mark Showalter for designing the CIRS ring
observations. R.M. thanks the UVIS ring team in LASP for fruitful
discussions. Numerical simulations were carried out with the
supercomputers, Nebula and Galaxy, at JPL.
NR 52
TC 12
Z9 12
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
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP
PY 2011
VL 215
IS 1
BP 107
EP 127
DI 10.1016/j.icarus.2011.06.042
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821NJ
UT WOS:000294981400011
ER
PT J
AU Jockers, K
Szutowicz, S
Villanueva, G
Bonev, T
Hartogh, P
AF Jockers, K.
Szutowicz, S.
Villanueva, G.
Bonev, T.
Hartogh, P.
TI HCN and CN in Comet 2P/Encke: Models of the non-isotropic,
rotation-modulated coma and CN parent life time
SO ICARUS
LA English
DT Article
DE Comets, Coma; Data reduction techniques
ID SOUTHERN SPECTROPHOTOMETRIC STANDARDS; DIRECT STATISTICAL SIMULATION;
CHIRP TRANSFORM SPECTROMETER; NEAR-SURFACE LAYERS; O1 HALE-BOPP;
PHYSICAL-PROPERTIES; C/1995 O1; OUTGASSING ASYMMETRY; RADIO TELESCOPES;
GAS JETS
AB Axisymmetric models of the outgassing of a cometary nucleus have been constructed. Such models can be used to describe a nucleus with a single active region. The models may include a solar zenith angle dependence of the outgassing. They retrieve the outgassing flux at distances from the nucleus where collisions between molecules are unimportant, as function of the angle with respect to the outgassing axis. The observed emissions must be optically thin. Furthermore the models assume that the outflow speed at large distance from the nucleus does not depend on direction. The value of the outflow speed is retrieved. The models are applied to CN images and HCN spectra of Comet 2P/Encke, obtained nearly simultaneously in November 2003 with the 2 m optical telescope on Mount Rozhen, Bulgaria, and with the 10 m Heinrich Hertz Submillimeter Telescope on Mount Graham, Arizona, USA. According to Sekanina (1988), Astron. J. 95, 911-924, at that time a single outgassing source was active. Input parameters to the models like the rotation period of the nucleus and a small correction to Sekanina's rotation axis are determined from a simpler jet position angle model. The rotation is prograde with a sideric period of 11.056 +/- 0.024 h, in agreement with literature values. The best fit model has an outflow speed of 0.95 +/- 0.04 km s(-1). The same value has been derived from the corkscrew appearing in the CN images. The location of the outgassing axis is at colatitude delta(a) = 7.4 degrees +/- 2.9 degrees and longitude lambda(a) = 235 degrees +/- 17 degrees (a definition of zero longitude is provided). Comet Encke's outgassing corresponds approximately to the longitudinally averaged solar input on a spherical nucleus (i.e. very likely comes from deeper layers) but with some deficiency of outgassing at mid-latitudes and non-zero outgassing from the dark polar cap. The presence of gas flow from the dark polar cap is explained as evidence of gas flow across the terminator. The models rely mostly on the CN images. The HCN spectra are more noisy. They provide information how to determine the best fit outflow velocity and the sense of rotation. The model HCN spectra are distinctly non-Gaussian. Within error limits they are consistent with the observations. Models based solely on the HCN spectra are also presented but, because of the lower quality of the data and the unfavorable observing geometry, yield inferior results. As a by-product we determine the CN parent life time from our CN observations. The solar EUV and Ly alpha radiation field at the time of our observations is taken into account. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Jockers, K.; Villanueva, G.; Hartogh, P.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Szutowicz, S.] Polish Acad Sci, Space Res Ctr, PL-00716 Warsaw, Poland.
[Villanueva, G.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Bonev, T.] Inst Astron, Sofia 1784, Bulgaria.
RP Jockers, K (reprint author), Max Planck Inst Sonnensyst Forsch, Max Planck Str 2, D-37191 Katlenburg Lindau, Germany.
EM jockers@mps.mpg.de; slawka@cbk.waw.pl; geronimo.villanueva@nasa.gov;
tbonev@astro.bas.bg; Hartogh@mps.mpg.de
FU Max-Planck Society; Polish Ministry of Education and Science
[181/N-HSO/2008/0]
FX K. Jockers enjoyed the hospitality of the Polish Institute of Space
Science in summer 2004. He is grateful to the directorate of the
Max-Planck-Institut fur Sonnensystemforschung for allowing him to use
the institute facilities to complete this work after his retirement. He
enjoyed stimulating discussions with M. Drahus, L Paganini and J.-B.
Vincent. S. Szutowicz acknowledges partial support by grants of the
Max-Planck Society in the early stage of this work, and later by the
Polish Ministry of Education and Science (Grant No. 181/N-HSO/2008/0).
Kent Tobiska provided free access to the SOLAR2000 system of Space
Environment Technologies. This research has made use of the SAO/NASA
Astrophysics Data System. The comments of M. Drahus and an unknown
referee are very much appreciated, as they have significantly helped us
to improve this difficult manuscript.
NR 82
TC 5
Z9 5
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
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP
PY 2011
VL 215
IS 1
BP 153
EP 185
DI 10.1016/j.icarus.2011.06.038
PG 33
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821NJ
UT WOS:000294981400013
ER
PT J
AU Hand, KP
Carlson, RW
AF Hand, Kevin P.
Carlson, Robert W.
TI H2O2 production by high-energy electrons on icy satellites as a function
of surface temperature and electron flux
SO ICARUS
LA English
DT Article
DE Ices; Europa; Enceladus; Experimental techniques; Satellites,
Composition; Ices, IR Spectroscopy
ID HYDROGEN-PEROXIDE; WATER ICE; INFRARED SPECTROSCOPY; GALILEAN
SATELLITES; OPTICAL-CONSTANTS; ION IRRADIATION; EUROPA; ENCELADUS;
RELEVANT; SPECTRA
AB Chemistry on the icy surface of Europa is heavily influenced by the incident energetic particle flux from the jovian magnetosphere. The majority (>75%) of this energy is in the form of high energy electrons (extending to >10 MeV). We have simulated the electron irradiation environment of Europa with a vacuum system containing a high-energy electron gun for irradiation of ice samples formed on a gold mirror cooled with a cryostat. Pure water films of similar to 2.6 mu m thickness were grown at 100 K and then either cooled (to 80 K), warmed (to 120 K) or left at 100 K and subsequently irradiated with 10 key electrons. The production of hydrogen peroxide (H2O2) was monitored by observation of the 2850 cm(-1) (3.5 mu m) band. Equilibrium concentrations of H2O2, in units of percent by number H2O2 relative to water, were found to be 0.043% (80 K), 0.029% (100 K), and 0.0063% (120 K). These values are 33%, 22%, and 5%, respectively, that of the reported surface concentration on the leading hemisphere of Europa (Carlson, R.W., Anderson, M.S., Johnson, R.E., Smythe, W.D., Hendrix, A.R., Barth, C.A., et al. [1999]. Science 283(5410), 2062-2064) and less than the equilibrium concentrations formed by ion irradiation. In addition to the ice film temperature, the current of electrons was varied between different experiments to determine the production and destruction of H2O2 as a function of both electron flux and ice temperature. Variation in current was found to have little effect on the results other than accelerating arrival at radiolytic equilibrium. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Hand, Kevin P.; Carlson, Robert W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Hand, KP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM khand@jpl.nasa.gov
FU National Aeronautics and Space Administration; internal Research and
Technology Development program; Exobiology program; NASA Astrobiology
Institute
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration and funded in part through the
internal Research and Technology Development program. R.W.C. and K.P.H.
acknowledge support from the Exobiology program, and K.P.H. acknowledges
support from the NASA Astrobiology Institute, through the 'Astrobiology
of Icy Worlds' node at JPL. We thank R. Beyer, D. O'Brien, P. Withers,
and G. Bart for their work on the LaTex template for Icarus.
NR 37
TC 13
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U1 1
U2 19
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 SEP
PY 2011
VL 215
IS 1
BP 226
EP 233
DI 10.1016/j.icarus.2011.06.031
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821NJ
UT WOS:000294981400018
ER
PT J
AU Williams, KE
Pappalardo, RT
AF Williams, K. E.
Pappalardo, R. T.
TI Variability in the small crater population on Callisto
SO ICARUS
LA English
DT Article
DE Callisto; Cratering; Small crater population
ID GALILEAN SATELLITES; MORPHOLOGY; RATES
AB Previous analyses of Galileo images showed the small (approximate to 1 km and smaller) crater population on Callisto to be lower than had been expected (Moore, J.M. et al. [1999]. Icarus 140, 294-312; Bierhaus E.B. et al. [2000]. Lunar Planet. Sci. 31. Abstract #1996). In this paper we examine the small crater population using high-resolution imagery from Callisto flybys during Galileo orbits C3, C10, C21, and C30, including several C30 regions not previously analyzed. Our findings confirm that most small craters are depleted relative to a presumed equilibrium of R = 0.22, and we find that there is significant variability in the small crater counts. While some of the variability in the small crater population on Callisto can be attributed to secondary cratering, some variability also may be explained by resetting of portions of Callisto's surface by larger impactors. This is expected where the differential size frequency distribution of the crater production population b < 3 (where b represents the exponent of a differential power-law crater-size distribution), such that large impacts affect a greater planetary surface area than smaller craters. (C) 2011 Elsevier Inc. All rights reserved.
C1 NASA Ames, Moffett Field, CA 94035 USA.
[Pappalardo, R. T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Williams, KE (reprint author), NASA Ames, Mail Stop 245-3, Moffett Field, CA 94035 USA.
EM Kaj.williams@gmail.com; Robert.Pappalar-do@jpl.nasa.gov
FU NASA
FX We thank Roland Wagner (DLR) and David Williams (Arizona State
University) for constructing the beautiful rectified images and image
mosaics used in this study. We also thank Roland Wagner and especially
Beau Bierhaus for their extremely helpful review comments. K.E.W. was
partially supported by the NASA Postdoctoral Program for this research.
The portion of this work performed by R.T.P. was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 17
TC 0
Z9 0
U1 0
U2 1
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP
PY 2011
VL 215
IS 1
BP 253
EP 259
DI 10.1016/j.icarus.2011.06.028
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821NJ
UT WOS:000294981400021
ER
PT J
AU Loeffler, MJ
Hudson, RL
Moore, MH
Carlson, RW
AF Loeffler, M. J.
Hudson, R. L.
Moore, M. H.
Carlson, R. W.
TI Radiolysis of sulfuric acid, sulfuric acid monohydrate, and sulfuric
acid tetrahydrate and its relevance to Europa
SO ICARUS
LA English
DT Article
DE Europa; Ices, IR spectroscopy; Jupiter, Satellites; Impact processes;
Cosmic rays
ID HYDRATED SALT MINERALS; COBALT GAMMA-RAYS; WATER ICE; GALILEAN
SATELLITES; HYDROGEN-PEROXIDE; ION IRRADIATION; PROTON-IRRADIATION;
INFRARED-SPECTRA; LOW-TEMPERATURES; OZONE SYNTHESIS
AB We report laboratory studies on the 0.8 MeV proton irradiation of ices composed of sulfuric acid (H(2)SO(4)), sulfuric acid monohydrate (H(2)SO(4)center dot H(2)O), and sulfuric acid tetrahydrate (H(2)SO(4)center dot 4H(2)O) between 10 and 180 K. Using infrared spectroscopy, we identify the main radiation products as H(2)O, SO(2), (S(2)O(3)), H(3)O(+), HSO(4)(-), and SO(4)(2-). At high radiation doses, we find that H(2)SO(4) molecules are destroyed completely and that H(2)SO(4)center dot H(2)O is formed on subsequent warming. This hydrate is significantly more stable to radiolytic destruction than pure H(2)SO(4), falling to an equilibrium relative abundance of 50% of its original value on prolonged irradiation. Unlike either pure H(2)SO(4) or H(2)SO(4)center dot H(2)O, the loss of H(2)SO(4)center dot 4H(2)O exhibits a strong temperature dependence, as the tetrahydrate is essentially unchanged at the highest irradiation temperatures and completely destroyed at the lowest ones, which we speculate is due to a combination of radiolytic destruction and amorphization. Furthermore, at the lower temperatures it is clear that irradiation causes the tetrahydrate spectrum to transition to one that closely resembles the monohydrate spectrum. Extrapolating our results to Europa's surface, we speculate that the variations in SO(2) concentrations observed in the chaotic terrains are a result of radiation processing of lower hydration states of sulfuric acid and that the monohydrate will remain stable on the surface over geological times, while the tetrahydrate will remain stable in the warmer regions but be destroyed in the colder regions, unless it can be reformed by other processes, such as thermal reactions induced by diurnal cycling. Published by Elsevier Inc.
C1 [Loeffler, M. J.; Hudson, R. L.; Moore, M. H.] NASA, Astrochem Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Carlson, R. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Loeffler, MJ (reprint author), NASA, Astrochem Lab, Goddard Space Flight Ctr, Mail Code 691, Greenbelt, MD 20771 USA.
EM mark.loeffler@nasa.gov
RI Loeffler, Mark/C-9477-2012; Hudson, Reggie/E-2335-2012
FU NASA; NASA Astrobiology Institute's Goddard Center for Astrobiology
FX This work was funded by NASA's Planetary Geology and Geophysics program.
R.L.H. and M.H.M. also received support through the NASA Astrobiology
Institute's Goddard Center for Astrobiology. Steve Brown, Tom Ward, and
Eugene Gerashchenko, members of the Radiation Laboratory at NASA
Goddard, are thanked for operation and maintenance of the Van de Graaff
accelerator.
NR 72
TC 9
Z9 9
U1 0
U2 14
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 SEP
PY 2011
VL 215
IS 1
BP 370
EP 380
DI 10.1016/j.icarus.2011.06.008
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821NJ
UT WOS:000294981400029
ER
PT J
AU Davies, AG
Ennis, ME
AF Davies, Ashley Gerard
Ennis, Megan Elizabeth
TI The variability of volcanic activity at Zamama, Culann, and Tupan Patera
on Io as seen by the Galileo Near Infrared Mapping Spectrometer
SO ICARUS
LA English
DT Article
DE Io; Volcanism; Jupiter, Satellites; Satellites, Surfaces
ID JUPITERS MOON IO; PHOTOPOLARIMETER-RADIOMETER; THERMAL SIGNATURE; MOUNT
EREBUS; LAVA FLOWS; HEAT-FLOW; NIMS DATA; MU-M; ERUPTION; SSI
AB Zamama, Culann, and Tupan Patera are three large, persistent volcanic centers on the jovian moon Io. As part of an ongoing project to quantify contributions from individual volcanic centers to Io's thermal budget, we have quantified the radiant flux from all suitable observations made by the Galileo Near Infrared Mapping Spectrometer (NIMS) of these volcanoes, in some cases filling omissions in previous analyses. At Zamama, after a long period of cooling, we see a peak in thermal emission that corresponds with new plume activity. Subsequently, toward the end of the Galileo epoch, thermal emission from Zamama drops off in a manner consistent with a greatly reduced eruption rate and the cooling of emplaced flows. Culann exhibits possible episodic activity. We present the full Tupan Patera NIMS dataset and derive new estimates of thermal output and temporal behavior. Eruption rates at these three volcanoes are on the order of 30 m(3) s(-1), consistent with a previous analysis of NIMS observations of Prometheus, and nearly an order of magnitude greater than Kilauea volcano, Hawai'i, Earth's most active volcano. We propose that future missions to the jovian system could better constrain activity at these volcanoes and others where similar styles of activity are taking place by obtaining data on a time scale of, ideally, at least one observation per day. Observations at similar or even shorter timescales are desirable during initial waxing phases of eruption episodes. These eruptions are identifiable from their characteristic spectral signatures and temporal behavior. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Davies, Ashley Gerard] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ennis, Megan Elizabeth] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
RP Davies, AG (reprint author), CALTECH, Jet Prop Lab, Ms 183-401,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Ashley.Davies@jpi.nasa.gov
FU NASA; Planetary Geology and Geophysics Undergraduate Research Program
FX This work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under contract to NASA. AGD is supported by a
grant from the NASA Outer Planets Research Program. MEE was supported by
a Planetary Geology and Geophysics Undergraduate Research Program grant.
We thank David Williams, Arizona State University, for SSI images and
discussions of volcanic activity in the Zamama region. We thank David
Williams and Jani Radebaugh for their reviews of the manuscript. (C)
Caltech 2011. All rights reserved.
NR 62
TC 8
Z9 8
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 SEP
PY 2011
VL 215
IS 1
BP 401
EP 416
DI 10.1016/j.icarus.2011.06.003
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821NJ
UT WOS:000294981400032
ER
PT J
AU Pinty, B
Taberner, M
Haemmerle, VR
Paradise, SR
Vermote, E
Verstraete, MM
Gobron, N
Widlowski, JL
AF Pinty, Bernard
Taberner, Malcolm
Haemmerle, Vance R.
Paradise, Susan R.
Vermote, Eric
Verstraete, Michel M.
Gobron, Nadine
Widlowski, Jean-Luc
TI Biogeophysical effects of land use on climate: Model simulations of
radiative forcing and large-scale temperature changes (vol 142, pg 216,
2007)
SO JOURNAL OF CLIMATE
LA English
DT Correction
C1 [Pinty, Bernard; Verstraete, Michel M.; Gobron, Nadine; Widlowski, Jean-Luc] Commiss European Communities, DG Joint Res Ctr, Inst Environm & Sustainabil, Global Environm Monitoring Unit, I-21027 Ispra, Italy.
[Taberner, Malcolm] Plymouth Marine Lab, Remote Sensing Grp, Plymouth, Devon, England.
[Haemmerle, Vance R.; Paradise, Susan R.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Vermote, Eric] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Vermote, Eric] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Pinty, Bernard] ESA ESRIN, Earth Observat Directorate, Frascati, Italy.
RP Pinty, B (reprint author), Commiss European Communities, DG Joint Res Ctr, Inst Environm & Sustainabil, Global Environm Monitoring Unit, TP 272,Via Enrico Fermi 2749, I-21027 Ispra, Italy.
EM bernard.pinty@jrc.ec.europa.eu
RI Vermote, Eric/K-3733-2012
NR 3
TC 0
Z9 0
U1 1
U2 8
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 SEP
PY 2011
VL 24
IS 17
BP 4769
EP 4769
DI 10.1175/JCLI-D-11-00126.1
PG 1
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 821SD
UT WOS:000294993800018
ER
PT J
AU Snyder, JE
Hamid, Q
Wang, C
Chang, R
Emami, K
Wu, H
Sun, W
AF Snyder, J. E.
Hamid, Q.
Wang, C.
Chang, R.
Emami, K.
Wu, H.
Sun, W.
TI Bioprinting cell-laden matrigel for radioprotection study of liver by
pro-drug conversion in a dual-tissue microfluidic chip
SO BIOFABRICATION
LA English
DT Article
ID IN-VITRO; CULTURE; MODEL
AB The objective of this paper is to introduce a novel cell printing and microfluidic system to serve as a portable ground model for the study of drug conversion and radiation protection of living liver tissue analogs. The system is applied to study behavior in ground models of space stress, particularly radiation. A microfluidic environment is engineered by two cell types to prepare an improved higher fidelity in vitro micro-liver tissue analog. Cell-laden Matrigel printing and microfluidic chips were used to test radiation shielding to liver cells by the pro-drug amifostine. In this work, the sealed microfluidic chip regulates three variables of interest: radiation exposure, anti-radiation drug treatment and single-or dual-tissue culture environments. This application is intended to obtain a scientific understanding of the response of the multi-cellular biological system for long-term manned space exploration, disease models and biosensors.
C1 [Snyder, J. E.; Hamid, Q.; Wang, C.; Chang, R.; Sun, W.] Drexel Univ, Dept Mech Engn, Philadelphia, PA 19104 USA.
[Emami, K.; Wu, H.] NASA Johnson Space Ctr, Radiat Biophys Lab, Houston, TX 77586 USA.
[Sun, W.] Tsinghua Univ, Dept Mech Engn, Beijing 100084, Peoples R China.
RP Snyder, JE (reprint author), Drexel Univ, Dept Mech Engn, Philadelphia, PA 19104 USA.
EM sunwei@drexel.edu
FU NASA USRA [09940-008]; National Space Biomedical Research Institute
FX Support was provided from NASA USRA subcontract grant no. 09940-008 and
the National Space Biomedical Research Institute Summer Intern Program
funded this research.
NR 24
TC 36
Z9 38
U1 7
U2 50
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1758-5082
J9 BIOFABRICATION
JI Biofabrication
PD SEP
PY 2011
VL 3
IS 3
SI SI
AR 034112
DI 10.1088/1758-5082/3/3/034112
PG 9
WC Engineering, Biomedical; Materials Science, Biomaterials
SC Engineering; Materials Science
GA 821DO
UT WOS:000294955200014
PM 21881168
ER
PT J
AU Stoklosa, AM
Weiss, I
Bugbee, B
Perchonok, MH
Mauer, LJ
AF Stoklosa, Adam M.
Weiss, Ilan
Bugbee, Bruce
Perchonok, Michele H.
Mauer, Lisa J.
TI COMPOSITION AND FUNCTIONAL PROPERTIES OF APOGEE AND PERIGEE COMPARED TO
COMMON TERRESTRIAL WHEAT CULTIVARS
SO INTERNATIONAL JOURNAL OF FOOD PROPERTIES
LA English
DT Article
DE Apogee; Perigee; Wheat; Characterization; Hydroponic
ID QUALITY; STARCH; FLOUR; ANTIOXIDANTS
AB Long duration space missions may include dwarf wheat cultivars to meet closed-loop food system constraints. Composition and functional properties of dwarf wheats (Apogee, Perigee) were characterized and compared to terrestrial cultivars (Parshall, Yecora Rojo, Yavaros 79). Proximate composition was determined using standard methods, and functional attributes were evaluated by mixograph and pasting profiles. Additional analyses measured antioxidant capacity, protein profiles, non-protein nitrogen, lipid oxidation, and starch damage. Apogee and Perigee were compositionally and functionally different from traditional cultivars, having higher protein (18-20%), ash (2-2.4%), and antioxidant (Perigee had 23.7 mu mol Trolox equivalent/g), and lipid oxidation levels but lower protein quality indicators. There was significant correlation (R(2) = 0.84) between ash content and lipid oxidation. Apogee is a better candidate crop than Perigee for a self sustaining environment, but both dwarf varieties could be used for tailored food applications.
C1 [Stoklosa, Adam M.; Weiss, Ilan; Mauer, Lisa J.] Purdue Univ, Dept Food Sci, W Lafayette, IN 47907 USA.
[Bugbee, Bruce] Utah State Univ, Dept Plants Soils & Biometeorol, Logan, UT 84322 USA.
[Perchonok, Michele H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Mauer, LJ (reprint author), 745 Agr Mall Dr, W Lafayette, IN 47907 USA.
EM mauer@purdue.edu
RI bugbee, bruce/I-5008-2012
FU NASA [NAG5-12686]
FX This research was partially funded by NASA grant NAG5-12686. The authors
wish to acknowledge Dr. Cary Mitchell and Dr. Gioia Massa at Purdue
University for their assistance in cultivating these crops.
NR 27
TC 1
Z9 1
U1 0
U2 5
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA
SN 1094-2912
J9 INT J FOOD PROP
JI Int. J. Food Prop.
PD SEP-OCT
PY 2011
VL 14
IS 5
BP 996
EP 1006
DI 10.1080/10942910903556447
PG 11
WC Food Science & Technology
SC Food Science & Technology
GA 819AC
UT WOS:000294796800006
ER
PT J
AU Matheou, G
Chung, D
Nuijens, L
Stevens, B
Teixeira, J
AF Matheou, Georgios
Chung, Daniel
Nuijens, Louise
Stevens, Bjorn
Teixeira, Joao
TI On the Fidelity of Large-Eddy Simulation of Shallow Precipitating
Cumulus Convection
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID FINITE-DIFFERENCE APPROXIMATIONS; TRADE-WIND CUMULUS; BOUNDARY-LAYER;
INCOMPRESSIBLE-FLOW; MOIST CONVECTION; CLOUDS; PARAMETERIZATION;
RESOLUTION; TURBULENCE; MODELS
AB The present study considers the impact of various choices pertaining to the numerical solution of the governing equations on large-eddy simulation (LES) prediction and the association of these choices with flow physics. These include the effect of dissipative versus nondissipative advection discretizations, different implementations of the constant-coefficient Smagorinsky subgrid-scale model, and grid resolution. Simulations corresponding to the trade wind precipitating shallow cumulus composite case of the Rain in Cumulus over the Ocean (RICO) field experiment were carried out. Global boundary layer quantities such as cloud cover, liquid water path, surface precipitation rate, power spectra, and the overall convection structure were used to compare the effects of different discretization implementations. The different discretization implementations were found to exert a significant impact on the LES prediction even for the cases where the process of precipitation was not included. Increasing numerical dissipation decreases cloud cover and surface precipitation rates. For nonprecipitating cases, grid convergence is achieved for grid spacings of 20 m. Cloud cover was found to be particularly sensitive, exhibiting variations between different resolution runs even when the mean liquid water profile had converged.
C1 [Matheou, Georgios; Chung, Daniel; Teixeira, Joao] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Nuijens, Louise; Stevens, Bjorn] Max Planck Inst Meteorol, Hamburg, Germany.
[Nuijens, Louise; Stevens, Bjorn] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
RP Matheou, G (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM georgios.matheou@jpl.nasa.gov
RI Stevens, Bjorn/A-1757-2013; Chung, Daniel/F-4468-2016
OI Stevens, Bjorn/0000-0003-3795-0475; Chung, Daniel/0000-0003-3732-364X
FU Office of Naval Research [N0001408IP20064]; NASA; NSF [EIA-0079871];
AFOSR [FA9550-07-1-0091]; National Aeronautics and Space Administration
FX We would like to acknowledge many fruitful discussions with Paul
Dimotakis and Pier Siebesma. JT and GM acknowledge the support provided
by the Office of Naval Research, Marine Meteorology Program under Award
N0001408IP20064, and by the NASA MAP Program. Resources supporting this
work were provided by the NASA High-End Computing (HEC) Program through
the NASA Advanced Supercomputing (NAS) Division at Ames Research Center.
Simulations were also performed on the Shared Heterogeneous Cluster at
the Center for Advanced Computing Research (CACR) at Caltech developed
with cofunding by NSF MRI Grant EIA-0079871 and AFOSR Grant
FA9550-07-1-0091 as part of a larger research effort on turbulent
mixing. This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 66
TC 36
Z9 36
U1 0
U2 11
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 SEP
PY 2011
VL 139
IS 9
BP 2918
EP 2939
DI 10.1175/2011MWR3599.1
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 820UR
UT WOS:000294932100014
ER
PT J
AU Castro, SL
Nelman-Gonzalez, M
Nickerson, CA
Ott, CM
AF Castro, Sarah L.
Nelman-Gonzalez, Mayra
Nickerson, Cheryl A.
Ott, C. Mark
TI Induction of Attachment-Independent Biofilm Formation and Repression of
hfq Expression by Low-Fluid-Shear Culture of Staphylococcus aureus
SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY
LA English
DT Article
ID INVASIVE ESCHERICHIA-COLI; MODELED REDUCED GRAVITY; GENE-EXPRESSION;
METHICILLIN-RESISTANT; GASTROINTESTINAL CARRIAGE; SIMULATED
MICROGRAVITY; HOSPITALIZED-PATIENTS; MICROBIAL BIOFILMS; SIGMA(B)
REGULON; GLOBAL REGULATOR
AB The opportunistic pathogen Staphylococcus aureus encounters a wide variety of fluid shear levels within the human host, and they may play a key role in dictating whether this organism adopts a commensal interaction with the host or transitions to cause disease. By using rotating-wall vessel bioreactors to create a physiologically relevant, low-fluid-shear environment, S. aureus was evaluated for cellular responses that could impact its colonization and virulence. S. aureus cells grown in a low-fluid-shear environment initiated a novel attachment-independent biofilm phenotype and were completely encased in extracellular polymeric substances. Compared to controls, low-shear-cultured cells displayed slower growth and repressed virulence characteristics, including decreased carotenoid production, increased susceptibility to oxidative stress, and reduced survival in whole blood. Transcriptional whole-genome microarray profiling suggested alterations in metabolic pathways. Further genetic expression analysis revealed downregulation of the RNA chaperone Hfq, which parallels low-fluid-shear responses of certain Gram-negative organisms. This is the first study to report an Hfq association with fluid shear in a Gram-positive organism, suggesting an evolutionarily conserved response to fluid shear among structurally diverse prokaryotes. Collectively, our results suggest S. aureus responds to a low-fluid-shear environment by initiating a biofilm/colonization phenotype with diminished virulence characteristics, which could lead to insight into key factors influencing the divergence between infection and colonization during the initial host-pathogen interaction.
C1 [Castro, Sarah L.] Univ Texas Med Branch, Dept Microbiol & Immunol, Galveston, TX 77555 USA.
[Nelman-Gonzalez, Mayra] Human Adaptat & Countermeasures Div, Houston, TX 77058 USA.
[Nickerson, Cheryl A.] Arizona State Univ, Biodesign Inst, Ctr Infect Dis & Vaccinol, Tempe, AZ 85287 USA.
[Ott, C. Mark] NASA, Lyndon B Johnson Space Ctr, Habitabil & Environm Factors Div, Houston, TX 77058 USA.
RP Ott, CM (reprint author), 2101 NASA Pkwy,Mail Code SF24, Houston, TX 77058 USA.
EM c.m.ott@nasa.gov
FU NASA [NNX07AM16G]
FX This work was supported by NASA Human Research Program student grant
NNX07AM16G.
NR 74
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U1 0
U2 30
PU AMER SOC MICROBIOLOGY
PI WASHINGTON
PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA
SN 0099-2240
J9 APPL ENVIRON MICROB
JI Appl. Environ. Microbiol.
PD SEP
PY 2011
VL 77
IS 18
BP 6368
EP 6378
DI 10.1128/AEM.00175-11
PG 11
WC Biotechnology & Applied Microbiology; Microbiology
SC Biotechnology & Applied Microbiology; Microbiology
GA 817RJ
UT WOS:000294691400007
PM 21803898
ER
PT J
AU Chu, YH
Su, KYL
Bilikova, J
Gruendl, RA
De Marco, O
Guerrero, MA
Updike, AC
Volk, K
Rauch, T
AF Chu, You-Hua
Su, Kate Y. L.
Bilikova, Jana
Gruendl, Robert A.
De Marco, Orsola
Guerrero, Martin A.
Updike, Adria C.
Volk, Kevin
Rauch, Thomas
TI SPITZER 24 mu m SURVEY FOR DUST DISKS AROUND HOT WHITE DWARFS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared: stars; planetary nebulae: general; white
dwarfs
ID MULTIBAND IMAGING PHOTOMETER; EXCESS INFRARED RADIATION;
PLANETARY-NEBULAE; DEBRIS DISKS; SPACE-TELESCOPE; SPECTRAL-ANALYSIS; OLD
PLANETARIES; CENTRAL STARS; ABSOLUTE CALIBRATION; EVOLUTION
AB Two types of dust disks around white dwarfs (WDs) have been reported: small dust disks around cool metal-rich WDs consisting of tidally disrupted asteroids and a large dust disk around the hot central WD of the Helix planetary nebula (PN) possibly produced by collisions among Kuiper-Belt-like objects. To search for more dust disks of the latter type, we have conducted a Spitzer MIPS 24 mu m survey of 71 hot WDs or pre-WDs, among which 35 are central stars of PNe (CSPNs). Nine of these evolved stars are detected and their 24 mu m flux densities are at least two orders of magnitude higher than their expected photospheric emission. Considering the bias against the detection of distant objects, the 24 mu m detection rate for the sample is greater than or similar to 15%. It is striking that seven, or similar to 20%, of the WD and pre-WDs in known PNe exhibit 24 mu m excesses, while two, or 5%-6%, of the WDs not in PNe show 24 mu m excesses and they have the lowest 24 mu m flux densities. We have obtained follow-up Spitzer Infrared Spectrograph spectra for five objects. Four show clear continuum emission at 24 mu m, and one is overwhelmed by a bright neighboring star but still shows a hint of continuum emission. In the cases of WD 0950+139 and CSPN K 1-22, a late-type companion is present, making it difficult to determine whether the excess 24 mu m emission is associated with the WD or its red companion. High-resolution images in the mid-infrared are needed to establish unambiguously the stars responsible for the 24 mu m excesses.
C1 [Chu, You-Hua; Bilikova, Jana; Gruendl, Robert A.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Su, Kate Y. L.] Univ Arizona, Stewart Observ, Tucson, AZ 85721 USA.
[De Marco, Orsola] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia.
[Guerrero, Martin A.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain.
[Updike, Adria C.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA.
[Updike, Adria C.] NASA, Observat Cosmol Lab, GSFC, Greenbelt, MD 20771 USA.
[Updike, Adria C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Updike, Adria C.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA.
[Volk, Kevin] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Rauch, Thomas] Abt Astron, IAAT, D-72076 Tubingen, Germany.
RP Chu, YH (reprint author), Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
EM yhchu@illinois.edu
FU NASA [JPL 1319342, 1343946, NAS 5-26555]; SAO [GO8-9026]; Spanish
Ministerio de Ciencia e Innovacion (MICINN) [AYA2008-01934]; U.S.
Government [NAG W-2166]; National Aeronautics and Space Administration
FX This research was supported by the NASA grants JPL 1319342 and 1343946
and SAO GO8-9026. M. A. G. acknowledges support from the Spanish
Ministerio de Ciencia e Innovacion (MICINN) through grant AYA2008-01934.
We thank George Rieke for useful discussion, Adam Myers for advice on
the SDSS photometry, Adeline Caulet and Ian McNabb for assisting in the
preliminary IRS data reduction, and the anonymous referee and Jay Farihi
for suggestions that improved the paper. The Digitized Sky Survey images
used were produced at the Space Telescope Science Institute under U.S.
Government grant NAG W-2166. The images of these surveys are based on
photographic data obtained using the UK Schmidt Telescope. The plates
were processed into the present compressed digital form with the
permission of these institutions. Images from the NASA/ESA Hubble Space
Telescope were obtained from the data archive at the Space Telescope
Science Institute. STScI is operated by the Association of Universities
for Research in Astronomy, Inc., under NASA contract NAS 5-26555. This
research has made use of the SIMBAD database, operated at CDS,
Strasbourg, France. This research has also made use of the NASA/IPAC
Infrared Science Archive, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration.
NR 66
TC 20
Z9 20
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD SEP
PY 2011
VL 142
IS 3
AR 75
DI 10.1088/0004-6256/142/3/75
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 817JY
UT WOS:000294669700009
ER
PT J
AU Eisenstein, DJ
Weinberg, DH
Agol, E
Aihara, H
Prieto, CA
Anderson, SF
Arns, JA
Aubourg, E
Bailey, S
Balbinot, E
Barkhouser, R
Beers, TC
Berlind, AA
Bickerton, SJ
Bizyaev, D
Blanton, MR
Bochanski, JJ
Bolton, AS
Bosman, CT
Bovy, J
Brandt, WN
Breslauer, B
Brewington, HJ
Brinkmann, J
Brown, PJ
Brownstein, JR
Burger, D
Busca, NG
Campbell, H
Cargile, PA
Carithers, WC
Carlberg, JK
Carr, MA
Chang, L
Chen, YM
Chiappini, C
Comparat, J
Connolly, N
Cortes, M
Croft, RAC
Cunha, K
da Costa, LN
Davenport, JRA
Dawson, K
De Lee, N
de Mello, GFP
de Simoni, F
Dean, J
Dhital, S
Ealet, A
Ebelke, GL
Edmondson, EM
Eiting, JM
Escoffier, S
Esposito, M
Evans, ML
Fan, XH
Castella, BF
Ferreira, LD
Fitzgerald, G
Fleming, SW
Font-Ribera, A
Ford, EB
Frinchaboy, PM
Perez, AEG
Gaudi, BS
Ge, J
Ghezzi, L
Gillespie, BA
Gilmore, G
Girardi, L
Gott, JR
Gould, A
Grebel, EK
Gunn, JE
Hamilton, JC
Harding, P
Harris, DW
Hawley, SL
Hearty, FR
Hennawi, JF
Hernandez, JIG
Ho, S
Hogg, DW
Holtzman, JA
Honscheid, K
Inada, N
Ivans, II
Jiang, LH
Jiang, P
Johnson, JA
Jordan, C
Jordan, WP
Kauffmann, G
Kazin, E
Kirkby, D
Klaene, MA
Knapp, GR
Kneib, JP
Kochanek, CS
Koesterke, L
Kollmeier, JA
Kron, RG
Lampeitl, H
Lang, D
Lawler, JE
Le Goff, JM
Lee, BL
Lee, YS
Leisenring, JM
Lin, YT
Liu, J
Long, DC
Loomis, CP
Lucatello, S
Lundgren, B
Lupton, RH
Ma, B
Ma, ZB
MacDonald, N
Mack, C
Mahadevan, S
Maia, MAG
Majewski, SR
Makler, M
Malanushenko, E
Malanushenko, V
Mandelbaum, R
Maraston, C
Margala, D
Maseman, P
Masters, KL
McBride, CK
McDonald, P
McGreer, ID
McMahon, RG
Requejo, OM
Menard, B
Miralda-Escude, J
Morrison, HL
Mullally, F
Muna, D
Murayama, H
Myers, AD
Naugle, T
Neto, AF
Nguyen, DC
Nichol, RC
Nidever, DL
O'Connell, RW
Ogando, RLC
Olmstead, MD
Oravetz, DJ
Padmanabhan, N
Paegert, M
Palanque-Delabrouille, N
Pan, KK
Pandey, P
Parejko, JK
Paris, I
Pellegrini, P
Pepper, J
Percival, WJ
Petitjean, P
Pfaffenberger, R
Pforr, J
Phleps, S
Pichon, C
Pieri, MM
Prada, F
Price-Whelan, AM
Raddick, MJ
Ramos, BHF
Reid, IN
Reyle, C
Rich, J
Richards, GT
Rieke, GH
Rieke, MJ
Rix, HW
Robin, AC
Rocha-Pinto, HJ
Rockosi, CM
Roe, NA
Rollinde, E
Ross, AJ
Ross, NP
Rossetto, B
Sanchez, AG
Santiago, B
Sayres, C
Schiavon, R
Schlegel, DJ
Schlesinger, KJ
Schmidt, SJ
Schneider, DP
Sellgren, K
Shelden, A
Sheldon, E
Shetrone, M
Shu, YP
Silverman, JD
Simmerer, J
Simmons, AE
Sivarani, T
Skrutskie, MF
Slosar, A
Smee, S
Smith, VV
Snedden, SA
Stassun, KG
Steele, O
Steinmetz, M
Stockett, MH
Stollberg, T
Strauss, MA
Szalay, AS
Tanaka, M
Thakar, AR
Thomas, D
Tinker, JL
Tofflemire, BM
Tojeiro, R
Tremonti, CA
Magana, MV
Verde, L
Vogt, NP
Wake, DA
Wan, XK
Wang, J
Weaver, BA
White, M
White, SDM
Wilson, JC
Wisniewski, JP
Wood-Vasey, WM
Yanny, B
Yasuda, N
Yeche, C
York, DG
Young, E
Zasowski, G
Zehavi, I
Zhao, B
AF Eisenstein, Daniel J.
Weinberg, David H.
Agol, Eric
Aihara, Hiroaki
Allende Prieto, Carlos
Anderson, Scott F.
Arns, James A.
Aubourg, Eric
Bailey, Stephen
Balbinot, Eduardo
Barkhouser, Robert
Beers, Timothy C.
Berlind, Andreas A.
Bickerton, Steven J.
Bizyaev, Dmitry
Blanton, Michael R.
Bochanski, John J.
Bolton, Adam S.
Bosman, Casey T.
Bovy, Jo
Brandt, W. N.
Breslauer, Ben
Brewington, Howard J.
Brinkmann, J.
Brown, Peter J.
Brownstein, Joel R.
Burger, Dan
Busca, Nicolas G.
Campbell, Heather
Cargile, Phillip A.
Carithers, William C.
Carlberg, Joleen K.
Carr, Michael A.
Chang, Liang
Chen, Yanmei
Chiappini, Cristina
Comparat, Johan
Connolly, Natalia
Cortes, Marina
Croft, Rupert A. C.
Cunha, Katia
da Costa, Luiz N.
Davenport, James R. A.
Dawson, Kyle
De Lee, Nathan
de Mello, Gustavo F. Porto
de Simoni, Fernando
Dean, Janice
Dhital, Saurav
Ealet, Anne
Ebelke, Garrett L.
Edmondson, Edward M.
Eiting, Jacob M.
Escoffier, Stephanie
Esposito, Massimiliano
Evans, Michael L.
Fan, Xiaohui
Femenia Castella, Bruno
Ferreira, Leticia Dutra
Fitzgerald, Greg
Fleming, Scott W.
Font-Ribera, Andreu
Ford, Eric B.
Frinchaboy, Peter M.
Perez, Ana Elia Garcia
Gaudi, B. Scott
Ge, Jian
Ghezzi, Luan
Gillespie, Bruce A.
Gilmore, G.
Girardi, Leo
Gott, J. Richard
Gould, Andrew
Grebel, Eva K.
Gunn, James E.
Hamilton, Jean-Christophe
Harding, Paul
Harris, David W.
Hawley, Suzanne L.
Hearty, Frederick R.
Hennawi, Joseph F.
Gonzalez Hernandez, Jonay I.
Ho, Shirley
Hogg, David W.
Holtzman, Jon A.
Honscheid, Klaus
Inada, Naohisa
Ivans, Inese I.
Jiang, Linhua
Jiang, Peng
Johnson, Jennifer A.
Jordan, Cathy
Jordan, Wendell P.
Kauffmann, Guinevere
Kazin, Eyal
Kirkby, David
Klaene, Mark A.
Knapp, G. R.
Kneib, Jean-Paul
Kochanek, C. S.
Koesterke, Lars
Kollmeier, Juna A.
Kron, Richard G.
Lampeitl, Hubert
Lang, Dustin
Lawler, James E.
Le Goff, Jean-Marc
Lee, Brian L.
Lee, Young Sun
Leisenring, Jarron M.
Lin, Yen-Ting
Liu, Jian
Long, Daniel C.
Loomis, Craig P.
Lucatello, Sara
Lundgren, Britt
Lupton, Robert H.
Ma, Bo
Ma, Zhibo
MacDonald, Nicholas
Mack, Claude
Mahadevan, Suvrath
Maia, Marcio A. G.
Majewski, Steven R.
Makler, Martin
Malanushenko, Elena
Malanushenko, Viktor
Mandelbaum, Rachel
Maraston, Claudia
Margala, Daniel
Maseman, Paul
Masters, Karen L.
McBride, Cameron K.
McDonald, Patrick
McGreer, Ian D.
McMahon, Richard G.
Mena Requejo, Olga
Menard, Brice
Miralda-Escude, Jordi
Morrison, Heather L.
Mullally, Fergal
Muna, Demitri
Murayama, Hitoshi
Myers, Adam D.
Naugle, Tracy
Fausti Neto, Angelo
Duy Cuong Nguyen
Nichol, Robert C.
Nidever, David L.
O'Connell, Robert W.
Ogando, Ricardo L. C.
Olmstead, Matthew D.
Oravetz, Daniel J.
Padmanabhan, Nikhil
Paegert, Martin
Palanque-Delabrouille, Nathalie
Pan, Kaike
Pandey, Parul
Parejko, John K.
Paris, Isabelle
Pellegrini, Paulo
Pepper, Joshua
Percival, Will J.
Petitjean, Patrick
Pfaffenberger, Robert
Pforr, Janine
Phleps, Stefanie
Pichon, Christophe
Pieri, Matthew M.
Prada, Francisco
Price-Whelan, Adrian M.
Raddick, M. Jordan
Ramos, Beatriz H. F.
Reid, I. Neill
Reyle, Celine
Rich, James
Richards, Gordon T.
Rieke, George H.
Rieke, Marcia J.
Rix, Hans-Walter
Robin, Annie C.
Rocha-Pinto, Helio J.
Rockosi, Constance M.
Roe, Natalie A.
Rollinde, Emmanuel
Ross, Ashley J.
Ross, Nicholas P.
Rossetto, Bruno
Sanchez, Ariel G.
Santiago, Basilio
Sayres, Conor
Schiavon, Ricardo
Schlegel, David J.
Schlesinger, Katharine J.
Schmidt, Sarah J.
Schneider, Donald P.
Sellgren, Kris
Shelden, Alaina
Sheldon, Erin
Shetrone, Matthew
Shu, Yiping
Silverman, John D.
Simmerer, Jennifer
Simmons, Audrey E.
Sivarani, Thirupathi
Skrutskie, M. F.
Slosar, Anze
Smee, Stephen
Smith, Verne V.
Snedden, Stephanie A.
Stassun, Keivan G.
Steele, Oliver
Steinmetz, Matthias
Stockett, Mark H.
Stollberg, Todd
Strauss, Michael A.
Szalay, Alexander S.
Tanaka, Masayuki
Thakar, Aniruddha R.
Thomas, Daniel
Tinker, Jeremy L.
Tofflemire, Benjamin M.
Tojeiro, Rita
Tremonti, Christy A.
Magana, Mariana Vargas
Verde, Licia
Vogt, Nicole P.
Wake, David A.
Wan, Xiaoke
Wang, Ji
Weaver, Benjamin A.
White, Martin
White, Simon D. M.
Wilson, John C.
Wisniewski, John P.
Wood-Vasey, W. Michael
Yanny, Brian
Yasuda, Naoki
Yeche, Christophe
York, Donald G.
Young, Erick
Zasowski, Gail
Zehavi, Idit
Zhao, Bo
TI SDSS-III: MASSIVE SPECTROSCOPIC SURVEYS OF THE DISTANT UNIVERSE, THE
MILKY WAY, AND EXTRA-SOLAR PLANETARY SYSTEMS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE cosmology: observations; Galaxy: evolution; planets and satellites:
detection; surveys
ID DIGITAL SKY SURVEY; BARYON ACOUSTIC-OSCILLATIONS; SURVEY COMMISSIONING
DATA; LUMINOUS RED GALAXIES; LENS ACS SURVEY; STELLAR ATMOSPHERIC
PARAMETERS; SAGITTARIUS DWARF GALAXY; VELOCITY EXPERIMENT RAVE;
ULTRACOOL WHITE-DWARFS; INFRARED CAII TRIPLET
AB Building on the legacy of the Sloan Digital Sky Survey (SDSS-I and II), SDSS-III is a program of four spectroscopic surveys on three scientific themes: dark energy and cosmological parameters, the history and structure of the Milky Way, and the population of giant planets around other stars. In keeping with SDSS tradition, SDSS-III will provide regular public releases of all its data, beginning with SDSS Data Release 8 (DR8), which was made public in 2011 January and includes SDSS-I and SDSS-II images and spectra reprocessed with the latest pipelines and calibrations produced for the SDSS-III investigations. This paper presents an overview of the four surveys that comprise SDSS-III. The Baryon Oscillation Spectroscopic Survey will measure redshifts of 1.5 million massive galaxies and Ly alpha forest spectra of 150,000 quasars, using the baryon acoustic oscillation feature of large-scale structure to obtain percent-level determinations of the distance scale and Hubble expansion rate at z < 0.7 and at z approximate to 2.5. SEGUE-2, an already completed SDSS-III survey that is the continuation of the SDSS-II Sloan Extension for Galactic Understanding and Exploration (SEGUE), measured medium-resolution (R = lambda/lambda Delta approximate to 1800) optical spectra of 118,000 stars in a variety of target categories, probing chemical evolution, stellar kinematics and substructure, and the mass profile of the dark matter halo from the solar neighborhood to distances of 100 kpc. APOGEE, the Apache Point Observatory Galactic Evolution Experiment, will obtain high-resolution (R approximate to 30,000), high signal-to-noise ratio (S/N >= 100 per resolution element), H-band (1.51 mu m < lambda < 1.70 mu m) spectra of 105 evolved, late-type stars, measuring separate abundances for similar to 15 elements per star and creating the first high-precision spectroscopic survey of all Galactic stellar populations (bulge, bar, disks, halo) with a uniform set of stellar tracers and spectral diagnostics. The Multi-object APO Radial Velocity Exoplanet Large-area Survey (MARVELS) will monitor radial velocities of more than 8000 FGK stars with the sensitivity and cadence (10-40 ms(-1), similar to 24 visits per star) needed to detect giant planets with periods up to two years, providing an unprecedented data set for understanding the formation and dynamical evolution of giant planet systems. As of 2011 January, SDSS-III has obtained spectra of more than 240,000 galaxies, 29,000 z >= 2.2 quasars, and 140,000 stars, including 74,000 velocity measurements of 2580 stars for MARVELS.
C1 [Eisenstein, Daniel J.; Fan, Xiaohui; Jiang, Linhua; Maseman, Paul; McGreer, Ian D.; Rieke, George H.; Rieke, Marcia J.; Young, Erick] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Eisenstein, Daniel J.] Harvard Coll Observ, Cambridge, MA 02138 USA.
[Weinberg, David H.; Gaudi, B. Scott; Gould, Andrew; Johnson, Jennifer A.; Kochanek, C. S.; Pieri, Matthew M.; Schlesinger, Katharine J.; Sellgren, Kris] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Weinberg, David H.; Honscheid, Klaus; Johnson, Jennifer A.; Kochanek, C. S.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Agol, Eric; Anderson, Scott F.; Davenport, James R. A.; Evans, Michael L.; Hawley, Suzanne L.; MacDonald, Nicholas; Sayres, Conor; Schmidt, Sarah J.; Tofflemire, Benjamin M.; Wisniewski, John P.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Aihara, Hiroaki; Lin, Yen-Ting; Murayama, Hitoshi; Silverman, John D.; Tanaka, Masayuki; Yasuda, Naoki] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan.
[Allende Prieto, Carlos; Esposito, Massimiliano; Femenia Castella, Bruno; Gonzalez Hernandez, Jonay I.] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Allende Prieto, Carlos; Esposito, Massimiliano; Femenia Castella, Bruno] Univ La Laguna, Dept Astron, E-38206 Tenerife, Spain.
[Arns, James A.] Kaiser Opt Syst, Ann Arbor, MI 48103 USA.
[Aubourg, Eric; Busca, Nicolas G.; Hamilton, Jean-Christophe; Magana, Mariana Vargas] Univ Paris Diderot, F-75205 Paris 13, France.
[Aubourg, Eric; Le Goff, Jean-Marc; Palanque-Delabrouille, Nathalie; Rich, James; Yeche, Christophe] CEA, Ctr Saclay, Irfu SPP, F-91191 Gif Sur Yvette, France.
[Bailey, Stephen; Carithers, William C.; Cortes, Marina; Ho, Shirley; McDonald, Patrick; Roe, Natalie A.; Ross, Nicholas P.; Schlegel, David J.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
[Balbinot, Eduardo; Fausti Neto, Angelo; Santiago, Basilio] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501970 Porto Alegre, RS, Brazil.
[Balbinot, Eduardo; Chiappini, Cristina; da Costa, Luiz N.; de Mello, Gustavo F. Porto; de Simoni, Fernando; Ferreira, Leticia Dutra; Ghezzi, Luan; Girardi, Leo; Maia, Marcio A. G.; Makler, Martin; Fausti Neto, Angelo; Ogando, Ricardo L. C.; Pellegrini, Paulo; Ramos, Beatriz H. F.; Rocha-Pinto, Helio J.; Rossetto, Bruno; Santiago, Basilio] Lab Interinst E Astron LIneA, BR-20921400 Rio De Janeiro, Brazil.
[Barkhouser, Robert; Menard, Brice; Raddick, M. Jordan; Smee, Stephen; Szalay, Alexander S.; Thakar, Aniruddha R.] Johns Hopkins Univ, Dept Phys & Astron, Ctr Astrophys Sci, Baltimore, MD 21218 USA.
[Beers, Timothy C.; Lee, Young Sun] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Beers, Timothy C.; Lee, Young Sun] Michigan State Univ, JINA Joint Inst Nucl Astrophys, E Lansing, MI 48824 USA.
[Berlind, Andreas A.; Burger, Dan; Cargile, Phillip A.; Dhital, Saurav; Mack, Claude; McBride, Cameron K.; Paegert, Martin; Pepper, Joshua; Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Bickerton, Steven J.; Carr, Michael A.; Gott, J. Richard; Gunn, James E.; Knapp, G. R.; Lang, Dustin; Loomis, Craig P.; Lupton, Robert H.; Mandelbaum, Rachel; Mullally, Fergal; Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Bizyaev, Dmitry; Brewington, Howard J.; Brinkmann, J.; Ebelke, Garrett L.; Gillespie, Bruce A.; Jordan, Cathy; Jordan, Wendell P.; Klaene, Mark A.; Long, Daniel C.; Malanushenko, Elena; Malanushenko, Viktor; Naugle, Tracy; Oravetz, Daniel J.; Pan, Kaike; Shelden, Alaina; Simmons, Audrey E.; Snedden, Stephanie A.] Apache Point Observ, Sunspot, NM 88349 USA.
[Blanton, Michael R.; Bovy, Jo; Hogg, David W.; Kazin, Eyal; Muna, Demitri; Price-Whelan, Adrian M.; Tinker, Jeremy L.; Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
[Bochanski, John J.; Brandt, W. N.; Mahadevan, Suvrath; Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Bolton, Adam S.; Brown, Peter J.; Brownstein, Joel R.; Dawson, Kyle; Harris, David W.; Ivans, Inese I.; Olmstead, Matthew D.; Pandey, Parul; Shu, Yiping; Simmerer, Jennifer] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Bosman, Casey T.; Chang, Liang; De Lee, Nathan; Fleming, Scott W.; Ford, Eric B.; Ge, Jian; Jiang, Peng; Lee, Brian L.; Liu, Jian; Ma, Bo; Duy Cuong Nguyen; Sivarani, Thirupathi; Wan, Xiaoke; Wang, Ji; Zhao, Bo] Univ Florida, Dept Astron, Bryant Space Sci Ctr, Gainesville, FL 32611 USA.
[Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Breslauer, Ben; Carlberg, Joleen K.; Dean, Janice; Perez, Ana Elia Garcia; Hearty, Frederick R.; Leisenring, Jarron M.; Majewski, Steven R.; Maseman, Paul; Nidever, David L.; O'Connell, Robert W.; Skrutskie, M. F.; Wilson, John C.; Zasowski, Gail] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Campbell, Heather; Edmondson, Edward M.; Lampeitl, Hubert; Maraston, Claudia; Masters, Karen L.; Nichol, Robert C.; Percival, Will J.; Pforr, Janine; Ross, Ashley J.; Steele, Oliver; Thomas, Daniel; Tojeiro, Rita] Univ Portsmouth, ICG, Portsmouth PO1 3FX, Hants, England.
[Chang, Liang] Chinese Acad Sci, Yunnan Astron Observ, Beijing 100864, Yunnan, Peoples R China.
[Chen, Yanmei; Tremonti, Christy A.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Chiappini, Cristina; Steinmetz, Matthias] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany.
[Chiappini, Cristina] 3 Ist Nazl Astrofis OATrieste, I-34143 Trieste, Italy.
[Comparat, Johan; Kneib, Jean-Paul] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France.
[Connolly, Natalia] Hamilton Coll, Dept Phys, Clinton, NY 13323 USA.
[Croft, Rupert A. C.] Carnegie Mellon Univ, Bruce & Astrid McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.
[da Costa, Luiz N.; de Simoni, Fernando; Ghezzi, Luan; Maia, Marcio A. G.; Ogando, Ricardo L. C.; Ramos, Beatriz H. F.] Observ Nacl, BR-20921400 Rio De Janeiro, Brazil.
[de Mello, Gustavo F. Porto; Ferreira, Leticia Dutra; Rocha-Pinto, Helio J.; Rossetto, Bruno] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio De Janeiro, Brazil.
[Ealet, Anne; Escoffier, Stephanie] Aix Marseille Univ, CNRS, IN2P3, Ctr Phys Particules Marseille, Marseille, France.
[Ebelke, Garrett L.; Holtzman, Jon A.; Jordan, Wendell P.; Pfaffenberger, Robert; Vogt, Nicole P.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Eiting, Jacob M.; Honscheid, Klaus] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Fitzgerald, Greg; Stollberg, Todd] New England Opt Syst, Marlborough, MA 01752 USA.
[Font-Ribera, Andreu] CSIC, IEEC, Inst Ciencies Espai, Barcelona 08193, Spain.
[Frinchaboy, Peter M.] Texas Christian Univ, Dept Phys & Astron, Ft Worth, TX 76129 USA.
[Gilmore, G.; McMahon, Richard G.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Girardi, Leo; Lucatello, Sara] Osservatorio Astron Padova INAF, I-35122 Padua, Italy.
[Grebel, Eva K.] Univ Heidelberg, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany.
[Harding, Paul; Ma, Zhibo; Morrison, Heather L.; Zehavi, Idit] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA.
[Hennawi, Joseph F.; Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Inada, Naohisa] Univ Tokyo, Grad Sch Sci, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan.
[Jiang, Peng] Chinese Acad Sci, Univ Sci & Technol China, Key Lab Res Galaxies & Cosmol, Hefei 230026, Anhui, Peoples R China.
[Kauffmann, Guinevere; White, Simon D. M.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Kirkby, David; Margala, Daniel] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Koesterke, Lars] Univ Texas Austin, Texas Adv Comp Ctr, Austin, TX 78758 USA.
[Kollmeier, Juna A.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Kron, Richard G.; Yanny, Brian] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Kron, Richard G.; York, Donald G.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Lawler, James E.; Stockett, Mark H.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Lin, Yen-Ting] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Lundgren, Britt; Padmanabhan, Nikhil; Parejko, John K.; Wake, David A.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
[Mahadevan, Suvrath; Schneider, Donald P.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Makler, Martin] ICRA Ctr Brasileiro Pesquisas Fis, BR-22290180 Rio De Janeiro, Brazil.
[Mena Requejo, Olga] Univ Valencia, CSIC, Inst Fis Corpuscular IFIC, Valencia, Spain.
[Menard, Brice] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada.
[Miralda-Escude, Jordi; Verde, Licia] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain.
[Miralda-Escude, Jordi; Verde, Licia] Univ Barcelona, IEEC, Inst Ciencies Cosmos, E-08028 Barcelona, Spain.
[Mullally, Fergal] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Myers, Adam D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Paris, Isabelle; Petitjean, Patrick; Pichon, Christophe; Rollinde, Emmanuel] Univ Paris 06, UMR7095, CNRS, Inst Astrophys Paris, F-75014 Paris, France.
[Phleps, Stefanie; Sanchez, Ariel G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Prada, Francisco] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain.
[Pieri, Matthew M.] Univ Colorado, CASA, Boulder, CO 80309 USA.
[Reid, I. Neill] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Reyle, Celine; Robin, Annie C.] Univ Franche Comte, Observ Besancon, Inst Utinam, F-25010 Besancon, France.
[Richards, Gordon T.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA.
[Rockosi, Constance M.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Schiavon, Ricardo] Gemini Observ, Hilo, HI 96720 USA.
[Shetrone, Matthew] Univ Texas Austin, McDonald Observ, Ft Davis, TX 79734 USA.
[Sivarani, Thirupathi] Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
[Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN USA.
[White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Wood-Vasey, W. Michael] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[York, Donald G.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Young, Erick] NASA, SOFIA Sci Ctr, USRA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[McDonald, Patrick; Sheldon, Erin; Slosar, Anze] Brookhaven Natl Lab, Dept Phys, Upton, NY 11973 USA.
[Cunha, Katia; Smith, Verne V.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
RP Eisenstein, DJ (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RI Kneib, Jean-Paul/A-7919-2015; Pforr, Janine/J-3967-2015; White,
Martin/I-3880-2015; Brandt, William/N-2844-2015; Rocha-Pinto,
Helio/C-2719-2008; Jiang, Linhua/H-5485-2016; Croft, Rupert/N-8707-2014;
Padmanabhan, Nikhil/A-2094-2012; Roe, Natalie/A-8798-2012; Yasuda,
Naoki/A-4355-2011; Makler, Martin/G-2639-2012; Gaudi,
Bernard/I-7732-2012; Aihara, Hiroaki/F-3854-2010; Agol,
Eric/B-8775-2013; Murayama, Hitoshi/A-4286-2011; Le Goff,
Jean-Marc/E-7629-2013; Gonzalez Hernandez, Jonay I./L-3556-2014; Ogando,
Ricardo/A-1747-2010; Mandelbaum, Rachel/N-8955-2014; Balbinot,
Eduardo/E-8019-2015
OI Stockett, Mark/0000-0003-4603-5172; McDonald,
Patrick/0000-0001-8346-8394; Miralda-Escude, Jordi/0000-0002-2316-8370;
Schmidt, Sarah/0000-0002-7224-7702; Bovy, Jo/0000-0001-6855-442X; Verde,
Licia/0000-0003-2601-8770; McMahon, Richard/0000-0001-8447-8869;
/0000-0002-1891-3794; Masters, Karen/0000-0003-0846-9578; Hogg,
David/0000-0003-2866-9403; Davenport, James/0000-0002-0637-835X;
/0000-0001-6545-639X; Pepper, Joshua/0000-0002-3827-8417; Kneib,
Jean-Paul/0000-0002-4616-4989; Pforr, Janine/0000-0002-3414-8391; White,
Martin/0000-0001-9912-5070; Brandt, William/0000-0002-0167-2453; Jiang,
Linhua/0000-0003-4176-6486; Croft, Rupert/0000-0003-0697-2583; Cortes,
Marina/0000-0003-0485-3767; Escoffier, Stephanie/0000-0002-2847-7498;
Kirkby, David/0000-0002-8828-5463; Fleming, Scott/0000-0003-0556-027X;
Makler, Martin/0000-0003-2206-2651; Aihara, Hiroaki/0000-0002-1907-5964;
Agol, Eric/0000-0002-0802-9145; Gonzalez Hernandez, Jonay
I./0000-0002-0264-7356; Ogando, Ricardo/0000-0003-2120-1154; Mandelbaum,
Rachel/0000-0003-2271-1527; Balbinot, Eduardo/0000-0002-1322-3153
FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department
of Energy Office of Science; University of Arizona; Brazilian
Participation Group; Brookhaven National Laboratory; University of
Cambridge; Carnegie Mellon University; University of Florida; French
Participation Group; German Participation Group; Harvard University;
Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA
Participation Group; Johns Hopkins University; Lawrence Berkeley
National Laboratory; Max Planck Institute for Astrophysics; New Mexico
State University; New York University; Ohio State University;
Pennsylvania State University; University of Portsmouth; Princeton
University; Spanish Participation Group; University of Tokyo; University
of Utah; Vanderbilt University; University of Virginia; University of
Washington; Yale University
FX Funding for SDSS-III has been provided by the Alfred P. Sloan
Foundation, the Participating Institutions, the National Science
Foundation, and the U.S. Department of Energy Office of Science. The
SDSS-III Web site is http://www.sdss3.org/.; SDSS-III is managed by the
Astrophysical Research Consortium for the Participating Institutions of
the SDSS-III Collaboration including the University of Arizona, the
Brazilian Participation Group, Brookhaven National Laboratory,
University of Cambridge, Carnegie Mellon University, University of
Florida, the French Participation Group, the German Participation Group,
Harvard University, the Instituto de Astrofisica de Canarias, the
Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins
University, Lawrence Berkeley National Laboratory, Max Planck Institute
for Astrophysics, New Mexico State University, New York University, Ohio
State University, Pennsylvania State University, University of
Portsmouth, Princeton University, the Spanish Participation Group,
University of Tokyo, University of Utah, Vanderbilt University,
University of Virginia, University of Washington, and Yale University.
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 817JY
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ER
PT J
AU Petrov, L
Taylor, GB
AF Petrov, L.
Taylor, G. B.
TI PRECISE ABSOLUTE ASTROMETRY FROM THE VLBA IMAGING AND POLARIMETRY SURVEY
AT 5 GHz
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE astrometry; catalogs; surveys
ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; CALIBRATOR SURVEY; BLAZARS;
JETS
AB We present accurate positions for 857 sources derived from the astrometric analysis of 16 eleven-hour experiments from the Very Long Baseline Array imaging and polarimetry survey at 5 GHz (VIPS). Among the observed sources, positions of 430 objects were not previously determined at milliarcsecond-level accuracy. For 95% of the sources the uncertainty of their positions ranges from 0.3 to 0.9 mas, with a median value of 0.5 mas. This estimate of accuracy is substantiated by the comparison of positions of 386 sources that were previously observed in astrometric programs simultaneously at 2.3/8.6 GHz. Surprisingly, the ionosphere contribution to group delay was adequately modeled with the use of the total electron content maps derived from GPS observations and only marginally affected estimates of source coordinates.
C1 [Petrov, L.] NASA, ADNET Syst Inc, GSFC, Greenbelt, MD 20771 USA.
[Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
RP Petrov, L (reprint author), NASA, ADNET Syst Inc, GSFC, Greenbelt, MD 20771 USA.
EM Leonid.Petrov@lpetrov.net; gbtaylor@unm.edu
FU Associated Universities, Inc.
FX We thank an anonymous referee for constructive suggestions. The National
Radio Astronomy Observatory is a facility of the National Science
Foundation operated under cooperative agreement by Associated
Universities, Inc.
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SC Astronomy & Astrophysics
GA 817JY
UT WOS:000294669700023
ER
PT J
AU Thomas, CA
Trilling, DE
Emery, JP
Mueller, M
Hora, JL
Benner, LAM
Bhattacharya, B
Bottke, WF
Chesley, S
Delbo, M
Fazio, G
Harris, AW
Mainzer, A
Mommert, M
Morbidelli, A
Penprase, B
Smith, HA
Spahr, TB
Stansberry, JA
AF Thomas, C. A.
Trilling, D. E.
Emery, J. P.
Mueller, M.
Hora, J. L.
Benner, L. A. M.
Bhattacharya, B.
Bottke, W. F.
Chesley, S.
Delbo, M.
Fazio, G.
Harris, A. W.
Mainzer, A.
Mommert, M.
Morbidelli, A.
Penprase, B.
Smith, H. A.
Spahr, T. B.
Stansberry, J. A.
TI ExploreNEOs. V. AVERAGE ALBEDO BY TAXONOMIC COMPLEX IN THE NEAR-EARTH
ASTEROID POPULATION
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE minor planets, asteroids: general; surveys
ID THERMAL INFRARED SPECTROPHOTOMETRY; SPITZER-SPACE-TELESCOPE; 10302 1989
ML; SPECTROSCOPIC SURVEY; MAIN-BELT; PHYSICAL-CHARACTERIZATION; SPECTRAL
PROPERTIES; OPTICAL-PROPERTIES; OBJECT SURVEY; PHASE-II
AB Examining the albedo distribution of the near-Earth object (NEO) population allows for a better understanding of the relationship between absolute (H) magnitude and size, which impacts calculations of the size frequency distribution and impact hazards. Examining NEO albedos also sheds light on the differences between the NEO and Main Belt populations. We combine albedo results from the ExploreNEOs Warm Spitzer Exploration Science program with taxonomic classifications from the literature, publicly available data sets, and new observations from our concurrent spectral survey to derive the average albedos for C-, D-, Q-, S-, V-, and X-complex NEOs. Using a sample size of 118 NEOs, we calculate average albedos of 0.29(-0.04)(+0.05), 0.26(-0.03)(+0.04), and 0.42(-0.11)(+0.13) for the Q-, S-, and V-complexes, respectively. The averages for the C-and D-complexes are 0.13(-0.05)(+0.06) and 0.02(-0.01)(+0.02), but these averages are based on a small number of objects (five and two, respectively) and will improve with additional observations. We use albedos to assign X-complex asteroids to one of the E-, M-, or P-types. Our results demonstrate that the average albedos for the C-, S-, V-, and X-complexes are higher for NEOs than the corresponding averages observed in the Main Belt.
C1 [Thomas, C. A.; Trilling, D. E.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86001 USA.
[Emery, J. P.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Mueller, M.; Delbo, M.; Morbidelli, A.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice 4, France.
[Hora, J. L.; Fazio, G.; Smith, H. A.; Spahr, T. B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Benner, L. A. M.; Chesley, S.; Mainzer, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bhattacharya, B.] Claremont Mckenna Coll, Joint Sci Dept, Claremont, CA 91711 USA.
[Bhattacharya, B.] Pitzer Coll, Joint Sci Dept, Claremont, CA 91711 USA.
[Bhattacharya, B.] Scripps Coll, Joint Sci Dept, Claremont, CA 91711 USA.
[Bottke, W. F.] SW Res Inst, Boulder, CO 80302 USA.
[Harris, A. W.; Mommert, M.] DLR Inst Planetary Res, D-12489 Berlin, Germany.
[Penprase, B.] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA.
[Stansberry, J. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Thomas, CA (reprint author), No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86001 USA.
EM cristina.thomas@nau.edu
OI Mueller, Michael/0000-0003-3217-5385; Hora, Joseph/0000-0002-5599-4650;
Thomas, Cristina/0000-0003-3091-5757
FU NASA; National Aeronautics and Space Administration, Office of Space
Science, Planetary Astronomy Program [NCC 5-538, NNX-08AE38A]; National
Science Foundation [0506716]
FX This work is based in part on observations made with the Spitzer Space
Telescope, which is operated by JPL/Caltech under a contract with NASA.
Support for this work was provided by NASA through an award issued by
JPL/Caltech.; Some of this work was performed at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration (NASA). This material is
based in part upon work supported by NASA under the Science Mission
Directorate Research and Analysis Programs.; Part of the data utilized
in this publication were obtained and made available by the MIT-UH-IRTF
Joint Campaign for NEO Reconnaissance. The IRTF is operated by the
University of Hawaii under Cooperative Agreement no. NCC 5-538 with the
National Aeronautics and Space Administration, Office of Space Science,
Planetary Astronomy Program. The MIT component of this work is supported
by the National Science Foundation under Grant 0506716.; Visiting
Astronomer at the Infrared Telescope Facility, which is operated by the
University of Hawaii under Cooperative Agreement no. NNX-08AE38A with
the National Aeronautics and Space Administration, Science Mission
Directorate, Planetary Astronomy Program.
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DI 10.1088/0004-6256/142/3/85
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 817JY
UT WOS:000294669700019
ER
PT J
AU Hurley, K
Briggs, MS
Kippen, RM
Kouveliotou, C
Fishman, G
Meegan, C
Cline, T
Trombka, J
McClanahan, T
Boynton, W
Starr, R
McNutt, R
Boer, M
AF Hurley, K.
Briggs, M. S.
Kippen, R. M.
Kouveliotou, C.
Fishman, G.
Meegan, C.
Cline, T.
Trombka, J.
McClanahan, T.
Boynton, W.
Starr, R.
McNutt, R.
Boer, M.
TI THE INTERPLANETARY NETWORK SUPPLEMENT TO THE BURST AND TRANSIENT SOURCE
EXPERIMENT 5B CATALOG OF COSMIC GAMMA-RAY BURSTS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; gamma-ray burst: general
AB We present Interplanetary Network localization information for 343 gamma-ray bursts observed by the Burst and Transient Source Experiment (BATSE) between the end of the 4th BATSE catalog and the end of the Compton Gamma-Ray Observatory (CGRO) mission, obtained by analyzing the arrival times of these bursts at the Ulysses, Near Earth Asteroid Rendezvous (NEAR), and CGRO spacecraft. For any given burst observed by CGRO and one other spacecraft, arrival time analysis (or "triangulation") results in an annulus of possible arrival directions whose half-width varies between 11 arcsec and 21 degrees, depending on the intensity, time history, and arrival direction of the burst, as well as the distance between the spacecraft. This annulus generally intersects the BATSE error circle, resulting in an average reduction of the area of a factor of 20. When all three spacecraft observe a burst, the result is an error box whose area varies between 1 and 48,000 arcmin(2), resulting in an average reduction of the BATSE error circle area of a factor of 87.
C1 [Hurley, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Briggs, M. S.] Univ Alabama, NSSTC, Huntsville, AL 35805 USA.
[Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Kouveliotou, C.; Fishman, G.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
[Meegan, C.] Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA.
[Cline, T.; Trombka, J.; McClanahan, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Boynton, W.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Starr, R.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[McNutt, R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Boer, M.] CNRS, Observ Haute Provence, F-04870 St Michel lObservatoire, France.
RP Hurley, K (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM khurley@ssl.berkeley.edu
RI McClanahan, Timothy/C-8164-2012; McNutt, Ralph/E-8006-2010
OI McNutt, Ralph/0000-0002-4722-9166
FU JPL [958056]; NASA [NAG 5-1560, NAG5-9701, NAG 5-3500, NAG 5-9503]
FX Support for the Ulysses GRB experiment was provided by JPL Contract
958056. Joint analysis of Ulysses and BATSE data was supported by NASA
Grants NAG 5-1560 and NAG5-9701. NEAR data analysis was supported under
NASA Grants NAG 5-3500 and NAG 5-9503. We are also grateful to the NEAR
team for their modifications to the XGRS experiment which made gamma-ray
burst detection possible.
NR 45
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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 SEP
PY 2011
VL 196
IS 1
AR UNSP 1
DI 10.1088/0067-0049/196/1/1
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818RT
UT WOS:000294773400001
ER
PT J
AU Levine, AM
Bradt, HV
Chakrabarty, D
Corbet, RHD
Harris, RJ
AF Levine, Alan M.
Bradt, Hale V.
Chakrabarty, Deepto
Corbet, Robin H. D.
Harris, Robert J.
TI AN EXTENDED AND MORE SENSITIVE SEARCH FOR PERIODICITIES IN ROSSI X-RAY
TIMING EXPLORER/ALL-SKY MONITOR X-RAY LIGHT CURVES
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE binaries: general; X-rays: stars
ID ORBITAL PERIOD; BLACK-HOLE; NEUTRON-STAR; INTEGRAL OBSERVATIONS; PULSAR
EXO-1722-363; COMPACT OBJECT; GRO J1008-57; TIME-SERIES; 4TH EDITION; 4U
1746-371
AB We present the results of a systematic search in similar to 14 years of Rossi X-ray Timing Explorer All-Sky Monitor (ASM) data for evidence of periodicities. Two variations of the commonly used Fourier analysis search method have been employed to significantly improve upon the sensitivity achieved by Wen et al. in 2006, who also searched for periodicities in ASM data. In addition, the present search is comprehensive in terms of sources studied and frequency range covered, and has yielded the detection of the signatures of the orbital periods of eight low-mass X-ray binary systems and of ten high-mass X-ray binaries not listed in the tables of Wen et al. Orbital periods, epochs, signal amplitudes, modulation fractions, and folded light curves are given for each of these systems. Seven of the orbital periods are the most precise reported to date. In the course of this work, the 18.545 day orbital period of IGR J18483-0311 was co-discovered, and the first detections in X-rays were made of the similar to 3.9 day orbital period of LMC X-1 and the similar to 3.79 hr orbital period of 4U 1636-536. The results inform future searches for orbital and other periodicities in X-ray binaries.
C1 [Levine, Alan M.; Bradt, Hale V.; Chakrabarty, Deepto] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Bradt, Hale V.; Chakrabarty, Deepto] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Corbet, Robin H. D.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
[Corbet, Robin H. D.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Harris, Robert J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Levine, AM (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM aml@space.mit.edu; hale@space.mit.edu; deepto@mit.edu;
robin.corbet@nasa.gov; rjharris@cfa.harvard.edu
FU NASA [NAS 5-30612 (MIT)]
FX We gratefully acknowledge the efforts of the RXTE/ASM science teams at
MIT and NASA/GSFC, and the RXTE mission support groups at GSFC. We thank
Alex Camacho for computing the upper limits presented in Table 3. We
also want to acknowledge an anonymous referee for helpful comments. This
work was supported by NASA through Contract NAS 5-30612 (MIT).
NR 81
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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 SEP
PY 2011
VL 196
IS 1
AR UNSP 6
DI 10.1088/0067-0049/196/1/6
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818RT
UT WOS:000294773400006
ER
PT J
AU Mangina, RS
Ajello, JM
West, RA
Dziczek, D
AF Mangina, Rao S.
Ajello, Joseph M.
West, Robert A.
Dziczek, Dariusz
TI HIGH-RESOLUTION ELECTRON-IMPACT EMISSION SPECTRA AND VIBRATIONAL
EMISSION CROSS SECTIONS FROM 330-1100 nm FOR N-2
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE atomic data; line: identification; molecular data; radiation mechanisms:
general; techniques: imaging spectroscopy; ultraviolet: general
ID FIRST NEGATIVE BAND; ULTRAVIOLET IMAGING SPECTROGRAPH; MEINEL BAND;
NITROGEN MOLECULES; TRANSITION PROBABILITIES; SIMULTANEOUS IONIZATION;
ROTATIONAL TEMPERATURE; UPPER-ATMOSPHERE; POSITIVE BANDS; EXCITATION
AB Electron-impact emission cross sections for N-2 were measured in the wavelength range of 330-1100 nm at 25 eV and 100 eV impact energies. Cross sections of several molecular emission bands of the first positive band system B (3)Pi(+)(g)(nu') -> A (3)Sigma(+)(g)(nu '') and the second positive band system C (3)Pi(u)(nu') -> B (3)Pi(g)(nu '') of N-2, the first negative band (1NB) system B (2)Sigma(+)(u)(nu') -> X (2)Sigma(+)(g)(nu '') and Meinel band system A (2)Pi(u)(nu') -> X (2)Sigma(+)(g)(nu '') of N-2(+) ions as well as line emissions of N (N I) and N+ (N II) in the visible-optical-near-IR wavelength range reported in this work were measured for the first time in a single experimental setup at high spectral resolving power (lambda/Delta lambda approximate to 10000) under single-collision-scattering geometry and optically thin conditions. Rotational emission lines of N-2 and N-2(+) were observed for strong emission bands at a gas temperature of about 300 K. The absolute cross section of the strongest (0,0) vibrational band at 391.43 nm of 1NB was determined using the standard H-alpha emission cross sections of H-2 by electron impact at both 25 eV and 100 eV electron-impact energies, and the cross sections for the remainder of the emissions were determined using (0,0) 1NB value. A comparison of the present emission cross sections with the earlier published data from both electron energy loss and electron-impact-induced fluorescence emission is discussed.
C1 [Mangina, Rao S.; Ajello, Joseph M.; West, Robert A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dziczek, Dariusz] Nicholas Copernicus Univ, Inst Phys, Torun, Poland.
RP Mangina, RS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RI Dziczek, Dariusz/G-3620-2014
FU NASA Planetary Atmospheres Program Office; NASA Cassini Data Analysis
Program Office; NASA Space Astrophysics Research Program Office; NASA
Outer Planets Research Analysis Program Office; Geospace Program Office;
National Science Foundation
FX The laboratory measurements described in this text were carried out at
the Jet Propulsion Laboratory, California Institute of Technology. The
work was supported by the NASA Planetary Atmospheres Program Office,
NASA Cassini Data Analysis Program Office, NASA Space Astrophysics
Research Program Office, NASA Outer Planets Research Analysis Program
Office, the Geospace Program Office, and the Aeronomy Program of the
National Science Foundation. We thank Ronald Cummings for his technical
assistance.
NR 97
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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 SEP
PY 2011
VL 196
IS 1
AR UNSP 13
DI 10.1088/0067-0049/196/1/13
PG 34
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818RT
UT WOS:000294773400013
ER
PT J
AU Rebull, LM
Koenig, XP
Padgett, DL
Terebey, S
McGehee, PM
Hillenbrand, LA
Knapp, GR
Leisawitz, D
Liu, W
Noriega-Crespo, A
Ressler, ME
Stapelfeldt, KR
Fajardo-Acosta, S
Mainzer, A
AF Rebull, L. M.
Koenig, X. P.
Padgett, D. L.
Terebey, S.
McGehee, P. M.
Hillenbrand, L. A.
Knapp, G. R.
Leisawitz, D.
Liu, W.
Noriega-Crespo, A.
Ressler, M. E.
Stapelfeldt, K. R.
Fajardo-Acosta, S.
Mainzer, A.
TI NEW YOUNG STAR CANDIDATES IN THE TAURUS-AURIGA REGION AS SELECTED FROM
THE WIDE-FIELD INFRARED SURVEY EXPLORER
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE circumstellar matter; infrared: stars; stars: formation; stars: pre-main
sequence
AB The Taurus Molecular Cloud subtends a large solid angle on the sky, in excess of 250 deg(2). The search for legitimate Taurus members to date has been limited by sky coverage as well as the challenge of distinguishing members from field interlopers. The Wide-field Infrared Survey Explorer has recently observed the entire sky, and we take advantage of the opportunity to search for young stellar object (YSO) candidate Taurus members from a similar to 260 deg(2) region designed to encompass previously identified Taurus members. We use near-and mid-infrared colors to select objects with apparent infrared excesses and incorporate other catalogs of ancillary data to present a list of rediscovered Taurus YSOs with infrared excesses (taken to be due to circumstellar disks), a list of rejected YSO candidates (largely galaxies), and a list of 94 surviving candidate new YSO-like Taurus members. There is likely to be contamination lingering in this candidate list, and follow-up spectra are warranted.
C1 [Rebull, L. M.; Padgett, D. L.; Noriega-Crespo, A.] CALTECH, SSC, Pasadena, CA 91125 USA.
[Koenig, X. P.; Leisawitz, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Terebey, S.] Calif State Univ Los Angeles, Dept Phys & Astron, Los Angeles, CA 90032 USA.
[McGehee, P. M.; Liu, W.; Fajardo-Acosta, S.] CALTECH, IPAC, Pasadena, CA 91125 USA.
[Knapp, G. R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Ressler, M. E.; Stapelfeldt, K. R.; Mainzer, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Rebull, LM (reprint author), CALTECH, SSC, M-S 220-6,1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM rebull@ipac.caltech.edu; xavier.p.koenig@nasa.gov;
Deborah.L.Padgett@nasa.gov; sterebe@calstatela.edu;
peregrin@ipac.caltech.edu; lah@astro.caltech.edu;
gk@astro.princeton.edu; david.t.leisawitz@nasa.gov;
wliu@ipac.caltech.edu; alberto@ipac.caltech.edu;
michael.e.ressler@jpl.nasa.gov; karl.r.stapelfeldt@nasa.gov;
fajardo@ipac.caltech.edu; amainzer@jpl.nasa.gov
OI Koenig, Xavier/0000-0002-9478-4170; Rebull, Luisa/0000-0001-6381-515X
FU National Aeronautics and Space Administration
FX The research described in this paper was partially carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration.
NR 31
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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 SEP
PY 2011
VL 196
IS 1
AR UNSP 4
DI 10.1088/0067-0049/196/1/4
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818RT
UT WOS:000294773400004
ER
PT J
AU Shang, ZH
Brotherton, MS
Wills, BJ
Wills, D
Cales, SL
Dale, DA
Green, RF
Runnoe, JC
Nemmen, RS
Gallagher, SC
Ganguly, R
Hines, DC
Kelly, BJ
Kriss, GA
Li, J
Tang, BT
Xie, YX
AF Shang, Zhaohui
Brotherton, Michael S.
Wills, Beverley J.
Wills, D.
Cales, Sabrina L.
Dale, Daniel A.
Green, Richard F.
Runnoe, Jessie C.
Nemmen, Rodrigo S.
Gallagher, Sarah C.
Ganguly, Rajib
Hines, Dean C.
Kelly, Benjamin J.
Kriss, Gerard A.
Li, Jun
Tang, Baitian
Xie, Yanxia
TI THE NEXT GENERATION ATLAS OF QUASAR SPECTRAL ENERGY DISTRIBUTIONS FROM
RADIO TO X-RAYS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE atlases; galaxies: active; infrared: galaxies; quasars: general; radio
continuum: galaxies; ultraviolet: galaxies; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; SPITZER-SPACE-TELESCOPE; HIGH-RESOLUTION
SPECTROSCOPY; OPTICALLY SELECTED QUASARS; MOLONGLO REFERENCE CATALOG;
XMM-NEWTON OBSERVATIONS; ROSAT DETECTED QUASARS; DIGITAL SKY SURVEY;
QUIET QUASARS; HOST GALAXIES
AB We have produced the next generation of quasar spectral energy distributions (SEDs), essentially updating the work of Elvis et al. by using high-quality data obtained with several space-and ground-based telescopes, including NASA's Great Observatories. We present an atlas of SEDs of 85 optically bright, non-blazar quasars over the electromagnetic spectrum from radio to X-rays. The heterogeneous sample includes 27 radio-quiet and 58 radio-loud quasars. Most objects have quasi-simultaneous ultraviolet-optical spectroscopic data, supplemented with some far-ultraviolet spectra, and more than half also have Spitzer mid-infrared Infrared Spectrograph spectra. The X-ray spectral parameters are collected from the literature where available. The radio, far-infrared, and near-infrared photometric data are also obtained from either the literature or new observations. We construct composite SEDs for radio-loud and radio-quiet objects and compare these to those of Elvis et al., finding that ours have similar overall shapes, but our improved spectral resolution reveals more detailed features, especially in the mid-and near-infrared.
C1 [Shang, Zhaohui; Li, Jun; Xie, Yanxia] Tianjin Normal Univ, Dept Phys, Tianjin 300387, Peoples R China.
[Shang, Zhaohui; Brotherton, Michael S.; Cales, Sabrina L.; Dale, Daniel A.; Runnoe, Jessie C.; Kelly, Benjamin J.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA.
[Wills, Beverley J.; Wills, D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Green, Richard F.] Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA.
[Nemmen, Rodrigo S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gallagher, Sarah C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Ganguly, Rajib] Univ Michigan, Dept Comp Sci Engn & Phys, Flint, MI 48502 USA.
[Hines, Dean C.] Space Sci Inst, Boulder, CO 80301 USA.
[Kriss, Gerard A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Kelly, Benjamin J.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Tang, Baitian] Washington State Univ, Dept Phys, Pullman, WA 99164 USA.
[Tang, Baitian] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China.
[Xie, Yanxia] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China.
RP Shang, ZH (reprint author), Tianjin Normal Univ, Dept Phys, Tianjin 300387, Peoples R China.
EM zshang@gmail.com
RI Nemmen, Rodrigo/O-6841-2014
FU National Natural Science Foundation of China [10773006]; Chinese 973
Program [2007CB815405]; NASA [HST-GO-10717.01-A, NAG5-3431,
GO-2578.01.87A, GO-4504, GO-5441, GO-06781]; Space Telescope Science
Institute [AR-5820]; Association of Universities for Research in
Astronomy, Inc., under NASA [NAS5-26555]; US National Science Foundation
[AST-0206261, AST-8794137, AST-0507781]; [Spitzer-GO-20084];
[NNG05GD03G]
FX This work has been supported by the National Natural Science Foundation
of China through Grant No. 10773006 and Chinese 973 Program
2007CB815405. We are also grateful for support by NASA through grant
HST-GO-10717.01-A, Spitzer-GO-20084, and Grant No. NNG05GD03G. B.J.W.
acknowledges financial support by NASA through LTSA grant NAG5-3431 and
HST grant GO-2578.01.87A, GO-4504, GO-5441, GO-06781, and AR-5820 from
the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS5-26555. We are also grateful for support from the US
National Science Foundation, through grants AST-0206261, AST-8794137
(B.J.W.), and AST-0507781 (M.S.B.).
NR 92
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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 SEP
PY 2011
VL 196
IS 1
AR UNSP 2
DI 10.1088/0067-0049/196/1/2
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818RT
UT WOS:000294773400002
ER
PT J
AU Witthoeft, MC
Bautista, MA
Garcia, J
Kallman, TR
Mendoza, C
Palmeri, P
Quinet, P
AF Witthoeft, M. C.
Bautista, M. A.
Garcia, J.
Kallman, T. R.
Mendoza, C.
Palmeri, P.
Quinet, P.
TI K-SHELL PHOTOIONIZATION OF NICKEL IONS USING R-MATRIX
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE atomic data; atomic processes; line: formation; X-rays: general
AB We present R-matrix calculations of photoabsorption and photoionization cross sections across the K edge of the Li-like to Ca-like ion stages of Ni. Level-resolved, Breit-Pauli calculations were performed for the Li-like to Na-like stages. Term-resolved calculations, which include the mass-velocity and Darwin relativistic corrections, were performed for the Mg-like to Ca-like ion stages. This data set is extended up to Fe-like Ni using the distorted wave approximation as implemented by autostructure. The R-matrix calculations include the effects of radiative and Auger dampings by means of an optical potential. The damping processes affect the absorption resonances converging to the K thresholds causing them to display symmetric profiles of constant width that smear the otherwise sharp edge at the K-shell photoionization threshold. These data are important for the modeling of features found in photoionized plasmas.
C1 [Witthoeft, M. C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Witthoeft, M. C.; Garcia, J.; Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bautista, M. A.; Garcia, J.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA.
[Mendoza, C.] Inst Venezolano Invest Cient, Ctr Fis, Caracas, Venezuela.
[Palmeri, P.; Quinet, P.] Univ Mons UMONS, B-7000 Mons, Belgium.
[Quinet, P.] Univ Liege, INPAS, B-4000 Liege, Belgium.
RP Witthoeft, MC (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
FU NASA; Belgian F.R.S.-FNRS
FX Support for this research was provided in part by a grant from the NASA
Astronomy and Physics Research program. P.P. and P.Q. are, respectively,
Research Associate and Senior Research Associate of the Belgian
F.R.S.-FNRS. Financial support from this organization is acknowledged.
NR 43
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Z9 8
U1 0
U2 7
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 SEP
PY 2011
VL 196
IS 1
AR UNSP 7
DI 10.1088/0067-0049/196/1/7
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818RT
UT WOS:000294773400007
ER
PT J
AU Duerr, RE
Downs, RR
Tilmes, C
Barkstrom, B
Lenhardt, WC
Glassy, J
Bermudez, LE
Slaughter, P
AF Duerr, Ruth E.
Downs, Robert R.
Tilmes, Curt
Barkstrom, Bruce
Lenhardt, W. Christopher
Glassy, Joseph
Bermudez, Luis E.
Slaughter, Peter
TI On the utility of identification schemes for digital earth science data:
an assessment and recommendations
SO EARTH SCIENCE INFORMATICS
LA English
DT Review
DE Digital identifiers; Unique Identifiers; Permanent identifiers; Global
unique persistent identifiers
ID INFORMATION; SYSTEM
AB In recent years, a number of data identification technologies have been developed which purport to permanently identify digital objects. In this paper, nine technologies and systems for assigning persistent identifiers are assessed for their applicability to Earth science data (ARKs, DOIs, XRIs, Handles, LSIDs, OIDs, PURLs, URIs/URNs/URLs, and UUIDs). The evaluation used four use cases that focused on the suitability of each scheme to provide Unique Identifiers for Earth science data objects, to provide Unique Locators for the objects, to serve as Citable Locators, and to uniquely identify the scientific contents of data objects if the data were reformatted. Of all the identifier schemes assessed, the one that most closely meets all of the requirements for an Unique Identifier is the UUID scheme. Any of the URL/URI/IRI-based identifier schemes assessed could be used for Unique Locators. Since there are currently no strong market leaders to help make the choice among them, the decision must be based on secondary criteria. While most publications now allow the use of URLs in citations, so that all of the URL/URI/IRI based identification schemes discussed in this paper could potentially be used as a Citable Locator, DOIs are the identification scheme currently adopted by most commercial publishers. None of the identifier schemes assessed here even minimally address identification of scientifically identical numerical data sets under reformatting.
C1 [Duerr, Ruth E.] Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA.
[Downs, Robert R.] Columbia Univ, CIESIN, Palisades, NY 10964 USA.
[Tilmes, Curt] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bermudez, Luis E.] OGC, Herndon, VA 20170 USA.
[Slaughter, Peter] Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA.
[Barkstrom, Bruce] NASA NOAA, Asheville, NC 28804 USA.
[Lenhardt, W. Christopher] Oak Ridge Natl Lab, Oak Ridge, TN USA.
[Glassy, Joseph] Lupine Log Inc, R&D, Missoula, MT 59802 USA.
RP Duerr, RE (reprint author), Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA.
EM rduerr@nsidc.org; rdowns@ciesin.columbia.edu; Curt.Tilmes@nasa.gov;
brbarkstrom@gmail.com; ledhardtc@ornl.gov; jglassy@lupinelogic.com;
lbermudez@opengeospatial.org; peter@eri.ucsb.edu
RI Tilmes, Curt/D-5637-2012; Downs, Robert/B-4153-2013; Lenhardt, W
Christopher/H-3257-2016;
OI Downs, Robert/0000-0002-8595-5134; Lenhardt, W
Christopher/0000-0001-9677-784X; Slaughter, Peter/0000-0002-2192-403X;
Tilmes, Curt/0000-0002-6512-0287; Duerr, Ruth/0000-0003-4808-4736
FU National Aeronautics and Space Administration (NASA) [NNG08HZ11C,
NNG08HZ07C, NNX08AN99A, NNX10AE07A]; National Science Foundation [ARC
0946625]
FX The authors are grateful for the support received from the National
Aeronautics and Space Administration (NASA), including support received
for Robert Downs under contract NNG08HZ11C and the support for Ruth
Duerr received under contract NNG08HZ07C and grants NNX08AN99A and
NNX10AE07A. The authors are also grateful for the support received from
the National Science Foundation under grant ARC 0946625. Lastly, the
authors are grateful to the members of NASA's TIWG and the ESIP
Stewardship Cluster who materially contributed to the results of the
paper through many discussions during monthly teleconferences, list
serve discussions and twice yearly meetings.
NR 102
TC 9
Z9 9
U1 2
U2 10
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1865-0473
EI 1865-0481
J9 EARTH SCI INFORM
JI Earth Sci. Inform.
PD SEP
PY 2011
VL 4
IS 3
BP 139
EP 160
DI 10.1007/s12145-011-0083-6
PG 22
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA 818VT
UT WOS:000294784700004
ER
PT J
AU Fassett, CI
Head, JW
Smith, DE
Zuber, MT
Neumann, GA
AF Fassett, Caleb I.
Head, James W.
Smith, David E.
Zuber, Maria T.
Neumann, Gregory A.
TI Thickness of proximal ejecta from the Orientale Basin from Lunar Orbiter
Laser Altimeter (LOLA) data: Implications for multi-ring basin formation
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID IMPACT BASINS; CRATER EJECTA; DEPOSITS; MOON
AB Quantifying the ejecta distribution around large lunar basins is important to understanding the origin of basin rings, the volume of the transient cavity, the depth of sampling, and the nature of the basin formation processes. We have used newly obtained altimetry data of the Moon from the Lunar Orbiter Laser Altimeter (LOLA) instrument to estimate the thickness of ejecta in the region surrounding the Orientale impact basin, the youngest and best preserved large basin on the Moon. Our measurements yield ejecta thicknesses of similar to 2900 m near the Cordillera Mountains, the topographic rim of Orientale, decaying to similar to 1 km in thickness at a range of 215 km. These measurements imply a volume of ejecta in the region from the Cordillera ring to a radial range of one basin diameter of similar to 2.9 x 10(6) km(3) and permit the derivation of an ejecta-thickness decay model, which can be compared with estimates for the volume of excavation and the size of the transient cavity. These data are consistent with the Outer Rook Mountains as the approximate location of the transient cavity's rim crest and suggest a volume of similar to 4.8 x 106 km(3) for the total amount of basin ejecta exterior to this location. Citation: Fassett, C. I., J. W. Head, D. E. Smith, M. T. Zuber, and G. A. Neumann (2011), Thickness of proximal ejecta from the Orientale Basin from Lunar Orbiter Laser Altimeter (LOLA) data: Implications for multi- ring basin formation, Geophys. Res. Lett., 38, L17201, doi: 10.1029/2011GL048502.
C1 [Fassett, Caleb I.; Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Smith, David E.; Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
RP Fassett, CI (reprint author), Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
EM Caleb_Fassett@brown.edu
RI Neumann, Gregory/I-5591-2013;
OI Neumann, Gregory/0000-0003-0644-9944; Fassett, Caleb/0000-0001-9155-3804
NR 32
TC 25
Z9 25
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 1
PY 2011
VL 38
AR L17201
DI 10.1029/2011GL048502
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 816PZ
UT WOS:000294615900002
ER
PT J
AU Le Vine, DM
Jackson, TJ
Kim, EJ
Lang, RH
AF Le Vine, David M.
Jackson, Thomas J.
Kim, Edward J.
Lang, Roger H.
TI Foreword to the Special Issue on the 11th Specialist Meeting on
Microwave Radiometry and Remote Sensing Applications (MicroRad 2010)
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Editorial Material
C1 [Le Vine, David M.; Kim, Edward J.] NASA, Goddard Space Flight Ctr, Lab Hydrospher & Biospher Sci, Greenbelt, MD 20771 USA.
[Jackson, Thomas J.] ARS, USDA, Beltsville, MD 20705 USA.
[Lang, Roger H.] George Washington Univ, Washington, DC 20052 USA.
RP Le Vine, DM (reprint author), NASA, Goddard Space Flight Ctr, Lab Hydrospher & Biospher Sci, Greenbelt, MD 20771 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD SEP
PY 2011
VL 49
IS 9
SI SI
BP 3143
EP 3145
DI 10.1109/TGRS.2011.2161843
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 815PE
UT WOS:000294536700001
ER
PT J
AU Kurum, M
Lang, RH
O'Neill, PE
Joseph, AT
Jackson, TJ
Cosh, MH
AF Kurum, Mehmet
Lang, Roger H.
O'Neill, Peggy E.
Joseph, Alicia T.
Jackson, Thomas J.
Cosh, Michael H.
TI A First-Order Radiative Transfer Model for Microwave Radiometry of
Forest Canopies at L-Band
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article; Proceedings Paper
CT 11th Specialist Meeting on Microwave Radiometry and Remote Sensing
Applications (MicroRad 2010)
CY MAR 01-04, 2010
CL Washington, DC
SP IEEE Geosci & Remote Soc, Int Radio Sci
DE Emission; microwave radiometry; scattering; soil; vegetation
ID DIELECTRIC DISKS; EMISSION; SCATTERING; VEGETATION; BACKSCATTERING;
FIELDS; SOILS
AB In this study, a first-order radiative transfer (RT) model is developed to more accurately account for vegetation canopy scattering by modifying the basic tau-omega model (the zero-order RT solution). In order to optimally utilize microwave radiometric data in soil moisture (SM) retrievals over vegetated landscapes, a quantitative understanding of the relationship between scattering mechanisms within vegetation canopies and the microwave brightness temperature is desirable. The first-order RT model is used to investigate this relationship and to perform a physical analysis of the scattered and emitted radiation from vegetated terrain. This model is based on an iterative solution (successive orders of scattering) of the RT equations up to the first order. This formulation adds a new scattering term to the tau-omega model. The additional term represents emission by particles (vegetation components) in the vegetation layer and emission by the ground that is scattered once by particles in the layer. The model is tested against 1.4-GHz brightness temperature measurements acquired over deciduous trees by a truck-mounted microwave instrument system called ComRAD in 2007. The model predictions are in good agreement with the data, and they give quantitative understanding for the influence of first-order scattering within the canopy on the brightness temperature. The model results show that the scattering term is significant for trees and modifications are necessary to the tau-omega model when applied to dense vegetation. Numerical simulations also indicate that the scattering term has a negligible dependence on SM and is mainly a function of the incidence angle and polarization of the microwave observation.
C1 [Kurum, Mehmet; O'Neill, Peggy E.; Joseph, Alicia T.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Lang, Roger H.] George Washington Univ, Dept Elect & Comp Engn, Washington, DC 20052 USA.
[Joseph, Alicia T.] Univ Maryland, College Pk, MD 20742 USA.
[Jackson, Thomas J.; Cosh, Michael H.] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA.
RP Kurum, M (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA.
EM mehmet.kurum@nasa.gov; lang@gwu.edu; peggy.e.oneill@nasa.gov;
Alicia.T.Joseph@nasa.gov; tom.jackson@ars.usda.gov;
Michael.Cosh@ars.usda.gov
RI Cosh, MIchael/A-8858-2015
OI Cosh, MIchael/0000-0003-4776-1918
NR 37
TC 24
Z9 26
U1 0
U2 10
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD SEP
PY 2011
VL 49
IS 9
SI SI
BP 3167
EP 3179
DI 10.1109/TGRS.2010.2091139
PG 13
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 815PE
UT WOS:000294536700004
ER
PT J
AU Le Vine, DM
Dinnat, EP
Abraham, S
de Matthaeis, P
Wentz, FJ
AF Le Vine, David M.
Dinnat, Emmanuel P.
Abraham, Saji
de Matthaeis, Paolo
Wentz, Frank J.
TI The Aquarius Simulator and Cold-Sky Calibration
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article; Proceedings Paper
CT 11th Specialist Meeting on Microwave Radiometry and Remote Sensing
Applications (MicroRad 2010)
CY MAR 01-04, 2010
CL Washington, DC
SP IEEE Geosci & Remote Soc, Int Radio Sci
DE Microwave radiometry; microwave remote sensing; sea surface salinity;
simulation
ID SEA-SURFACE SALINITY; L-BAND; MICROWAVE-FREQUENCIES; ANTENNA PATTERN;
SPACE; WATER; IONOSPHERE; ABSORPTION; RADIOMETER; IMPACT
AB A numerical simulator has been developed to study remote sensing from space in the spectral window at 1.413 GHz (L-band), and it has been used to optimize the cold-sky calibration (CSC) for the Aquarius radiometers. The celestial sky is a common cold reference in microwave radiometry. It is currently being used by the Soil Moisture and Ocean Salinity satellite, and it is planned that, after launch, the Aquarius/SAC-D observatory will periodically rotate to view "cold sky" as part of the calibration plan. Although radiation from the celestial sky is stable and relatively well known, it varies with location. In addition, radiation from the Earth below contributes to the measured signal through the antenna back lobes and also varies along the orbit. Both effects must be taken into account for a careful calibration. The numerical simulator has been used with the Aquarius configuration (antennas and orbit) to investigate these issues and determine optimum conditions for performing a CSC. This paper provides an overview of the simulator and the analysis leading to the selection of the optimum locations for a CSC.
C1 [Le Vine, David M.; Dinnat, Emmanuel P.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Dinnat, Emmanuel P.] Chapman Univ, Sch Earth & Environm Sci, Orange, CA 92866 USA.
[Abraham, Saji] NASA, Goddard Space Flight Ctr, Wyle Informat Syst, Greenbelt, MD 20771 USA.
[Wentz, Frank J.] Remote Sensing Syst, Santa Rosa, CA 95401 USA.
RP Le Vine, DM (reprint author), NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA.
EM david.m.levine@nasa.gov; emmanuel.dinnat@nasa.gov;
Saji.Abraham-1@nasa.gov; paolo.dematthaeis@nasa.gov;
frank.wentz@remss.com
RI Dinnat, Emmanuel/D-7064-2012
OI Dinnat, Emmanuel/0000-0001-9003-1182
NR 33
TC 17
Z9 17
U1 1
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD SEP
PY 2011
VL 49
IS 9
SI SI
BP 3198
EP 3210
DI 10.1109/TGRS.2011.2161481
PG 13
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 815PE
UT WOS:000294536700007
ER
PT J
AU Sahoo, S
Reising, SC
Padmanabhan, S
Vivekanandan, J
Iturbide-Sanchez, F
Pierdicca, N
Pichelli, E
Cimini, D
AF Sahoo, Swaroop
Reising, Steven C.
Padmanabhan, Sharmila
Vivekanandan, Jothiram
Iturbide-Sanchez, Flavio
Pierdicca, Nazzareno
Pichelli, Emanuela
Cimini, Domenico
TI Three-Dimensional Humidity Retrieval Using a Network of Compact
Microwave Radiometers to Correct for Variations in Wet Tropospheric Path
Delay in Spaceborne Interferometric SAR Imagery
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article; Proceedings Paper
CT 11th Specialist Meeting on Microwave Radiometry and Remote Sensing
Applications (MicroRad 2010)
CY MAR 01-04, 2010
CL Washington, DC
SP IEEE Geosci & Remote Soc, Int Radio Sci
DE Digital elevation models; humidity measurement; microwave radiometry;
moisture; remote sensing
ID WATER-VAPOR; SPECTROMETER; ABSORPTION; SURFACE; LINE
AB Spaceborne interferometric synthetic aperture radar (SAR) (InSAR) imaging has been used for over a decade to monitor tectonic movements and landslides, as well as to improve digital elevation models. However, InSAR is affected by variations in round-trip propagation delay due to changes in ionospheric total electron content and in tropospheric humidity and temperature along the signal path. One of the largest sources of uncertainty in estimates of tropospheric path delay is the spatial and temporal variability of water vapor density, which currently limits the quality of InSAR products. This problem can be partially addressed by using a number of SAR interferograms from subsequent satellite overpasses to reduce the degradation in the images or by analyzing a long time series of interferometric phases from permanent scatterers. However, if there is a sudden deformation of the Earth's surface, the detection of which is one of the principal objectives of InSAR measurements over land, the effect of water vapor variations cannot be removed, reducing the quality of the interferometric products. In those cases, high-resolution information on the atmospheric water vapor content and its variation with time can be crucial to mitigate the effect of wet-tropospheric path delay variations. This paper describes the use of a ground-based microwave radiometer network to retrieve 3-D water vapor density with fine spatial and temporal resolution, which can be used to reduce InSAR ambiguities due to changes in wet-tropospheric path delay. Retrieval results and comparisons between the integrated water vapor measured by the radiometer network and satellite data are presented.
C1 [Sahoo, Swaroop; Reising, Steven C.] Colorado State Univ, Microwave Syst Lab, Dept Elect & Comp Engn, Ft Collins, CO 80523 USA.
[Padmanabhan, Sharmila] NASA, CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Vivekanandan, Jothiram] Natl Ctr Atmospher Res, Boulder, CO 80301 USA.
[Iturbide-Sanchez, Flavio] Natl Environm Satellite Data & Informat Serv, Natl Ocean & Atmospher Adm, IM Syst Grp, Ctr Satellite Applicat & Res, Camp Springs, MD 20746 USA.
[Pierdicca, Nazzareno] Univ Roma La Sapienza, Dept Informat Elect & Telecommun Engn, I-00184 Rome, Italy.
[Pichelli, Emanuela] Univ Aquila, Dept Phys, Ctr Excellence Remote Sensing & Modeling Severe W, I-67010 Coppito, Italy.
[Cimini, Domenico] Italian Natl Res Council IMAA CNR, Inst Methodol Environm Anal, I-85100 Potenza, Italy.
RP Sahoo, S (reprint author), Colorado State Univ, Microwave Syst Lab, Dept Elect & Comp Engn, Ft Collins, CO 80523 USA.
EM Swaroop.Sahoo@ColoState.edu; Steven.Reising@ColoState.edu;
sharmila.padmanabhan@jpl.nasa.gov; vivek@ucar.edu;
Flavio.Iturbide@noaa.gov; nazzareno.pierdicca@uniroma1.it;
emanuela.pichelli@aquila.infn.it; nico.cimini@aquila.infn.it
RI Iturbide-Sanchez, Flavio/F-9186-2014; Cimini, Domenico/M-8707-2013;
Pichelli, Emanuela/G-7723-2015
OI Iturbide-Sanchez, Flavio/0000-0002-8539-0073; Cimini,
Domenico/0000-0002-5962-223X;
NR 16
TC 5
Z9 5
U1 0
U2 12
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD SEP
PY 2011
VL 49
IS 9
SI SI
BP 3281
EP 3290
DI 10.1109/TGRS.2011.2119400
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 815PE
UT WOS:000294536700013
ER
PT J
AU Brown, ST
Lambrigtsen, B
Denning, RF
Gaier, T
Kangaslahti, P
Lim, BH
Tanabe, JM
Tanner, AB
AF Brown, Shannon T.
Lambrigtsen, Bjorn
Denning, Richard F.
Gaier, Todd
Kangaslahti, Pekka
Lim, Boon H.
Tanabe, Jordan M.
Tanner, Alan B.
TI The High-Altitude MMIC Sounding Radiometer for the Global Hawk Unmanned
Aerial Vehicle: Instrument Description and Performance
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article; Proceedings Paper
CT 11th Specialist Meeting on Microwave Radiometry and Remote Sensing
Applications (MicroRad 2010)
CY MAR 01-04, 2010
CL Washington, DC
SP IEEE Geosci & Remote Soc, Int Radio Sci
DE Airborne remote sensing; microwave sounder; tropical cyclone; unmanned
aerial vehicle
ID UNIT AMSU; MICROWAVE; SATELLITE; TEMPERATURE; RETRIEVALS
AB The Jet Propulsion Laboratory's High-Altitude Monolithic Microwave Integrated Circuit (MMIC) Sounding Radiometer (HAMSR) is a 25-channel cross-track scanning microwave sounder with channels near the 60- and 118-GHz oxygen lines and the 183-GHz water-vapor line. It has previously participated in three hurricane field campaigns, namely, CAMEX-4 (2001), Tropical Cloud Systems and Processes (2005), and NASA African Monsoon Multidisciplinary Analyses (2006). The HAMSR instrument was recently extensively upgraded for the deployment on the Global Hawk (GH) unmanned aerial vehicle platform. One of the major upgrades is the addition of a front-end low-noise amplifier, developed by JPL, to the 183-GHz channel which reduces the noise in this channel to less than 0.1 K at the sensor resolution (similar to 2 km). This will enable HAMSR to observe much smaller scale water-vapor features. Another major upgrade is an enhanced data system that provides onboard science processing capability and real-time data access. HAMSR has been well characterized, including passband characterization, along-scan bias characterization, and calibrated noise-performance characterization. The absolute calibration is determined in-flight and has been estimated to be better than 1.5 K from previous campaigns. In 2010, HAMSR participated in the NASA Genesis and Rapid Intensification Processes campaign on the GH to study tropical cyclone genesis and rapid intensification. HAMSR-derived products include observations of the atmospheric state through retrievals of temperature, water-vapor, and cloud-liquid-water profiles. Other products include convective intensity, precipitation content, and 3-D storm structure.
C1 [Brown, Shannon T.; Lambrigtsen, Bjorn; Denning, Richard F.; Gaier, Todd; Kangaslahti, Pekka; Lim, Boon H.; Tanabe, Jordan M.; Tanner, Alan B.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Brown, ST (reprint author), CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
EM Shannon.T.Brown@jpl.nasa.gov; bjorn.lambrigtsen@jpl.nasa.gov;
richard.denning@jpl.nasa.gov; Todd.gaier@jpl.nasa.gov;
pekka.kangaslahti@jpl.nasa.gov; Boon.Lim@jpl.nasa.gov;
jordan.tanabe@jpl.nasa.gov; Alan.Tanner@jpl.nasa.gov
NR 14
TC 21
Z9 21
U1 1
U2 13
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD SEP
PY 2011
VL 49
IS 9
SI SI
BP 3291
EP 3301
DI 10.1109/TGRS.2011.2125973
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 815PE
UT WOS:000294536700014
ER
PT J
AU Park, J
Johnson, JT
Majurec, N
Niamsuwan, N
Piepmeier, JR
Mohammed, PN
Ruf, CS
Misra, S
Yueh, SH
Dinardo, SJ
AF Park, James
Johnson, J. T.
Majurec, Ninoslav
Niamsuwan, Noppasin
Piepmeier, Jeffrey R.
Mohammed, Priscilla N.
Ruf, Christopher S.
Misra, Sidharth
Yueh, Simon H.
Dinardo, Steve J.
TI Airborne L-Band Radio Frequency Interference Observations From the
SMAPVEX08 Campaign and Associated Flights
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Microwave radiometry; radio frequency interference
ID MICROWAVE RADIOMETRY; RFI; MITIGATION; DETECTOR; MISSION
AB Statistics of radio frequency interference (RFI) observed in the band 1398-1422 MHz during an airborne campaign in the United States are reported for use in analysis and forecasting of L-band RFI for microwave radiometry. The observations were conducted from September to October 2008, and included approximately 92 h of flight time, of which approximately 20 h of "transit" or dedicated RFI observing flights are used in compiling the statistics presented. The observations used include outbound and return flights from Colorado to Maryland, as well as RFI surveys over large cities. The Passive Active L-Band Sensor (PALS) radiometer of NASA Jet Propulsion Laboratory augmented by three dedicated RFI observing systems was used in these observations. The complete system as well as the associated RFI characterization approaches are described, along with the resulting RFI statistical information and examinations of specific RFI sources. The results show that RFI in the protected L-band spectrum is common over North America, although the resulting interference when extrapolated to satellite observations will appear as "low-level" corruption that will be difficult to detect for traditional radiometer systems.
C1 [Park, James; Johnson, J. T.; Majurec, Ninoslav; Niamsuwan, Noppasin] Ohio State Univ, Dept Elect & Comp Engn, Columbus, OH 43210 USA.
[Piepmeier, Jeffrey R.; Mohammed, Priscilla N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ruf, Christopher S.; Misra, Sidharth] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Yueh, Simon H.; Dinardo, Steve J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Park, J (reprint author), Ohio State Univ, Dept Elect & Comp Engn, Columbus, OH 43210 USA.
EM park.918@osu.edu; johnson@ece.osu.edu; majurec.1@osu.edu;
niamsuwan.1@osu.edu; jeffrey.r.piepmeier@nasa.gov;
Priscilla.N.Mohammed@nasa.gov; tgrs-editor@ieee.org; samisra@umich.edu;
simon.h.yueh@jpl.nasa.gov; Steve.Dinardo@jpl.nasa.gov
RI Ruf, Christopher/I-9463-2012
FU National Aeronautics and Space Administration; NASA/JPL [1335558]
FX This project was carried out under a contract with the National
Aeronautics and Space Administration. The work performed by the
University of Michigan was supported in part by NASA/JPL Award Reference
Number 1335558.
NR 22
TC 10
Z9 10
U1 0
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD SEP
PY 2011
VL 49
IS 9
SI SI
BP 3359
EP 3370
DI 10.1109/TGRS.2011.2107560
PG 12
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 815PE
UT WOS:000294536700020
ER
PT J
AU van Zyl, JJ
Arii, M
Kim, Y
AF van Zyl, Jakob J.
Arii, Motofumi
Kim, Yunjin
TI Model-Based Decomposition of Polarimetric SAR Covariance Matrices
Constrained for Nonnegative Eigenvalues
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Model-based decomposition; nonnegative eigenvalue decomposition (NNED);
radar polarimetry
AB Model-based decomposition of polarimetric radar covariance matrices holds the promise that specific scattering mechanisms can be isolated for further quantitative analysis. In this paper, we show that current algorithms suffer from a fatal flaw in that some of the scattering components result in negative powers. We propose a simple modification that ensures that all covariance matrices in the decomposition will have nonnegative eigenvalues. We further combine our nonnegative eigenvalue decomposition with eigenvector decomposition to remove additional assumptions that have to be made before the current algorithms can be used to estimate all the scattering components. Our results are illustrated using Airborne Synthetic Aperture Radar data and show that current algorithms typically overestimate the canopy scattering contribution by 10%-20%.
C1 [van Zyl, Jakob J.; Kim, Yunjin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Arii, Motofumi] Mitsubishi Space Software Co Ltd, Kamakura, Kanagawa 2470065, Japan.
RP van Zyl, JJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jakob.vanzyl@jpl.nasa.gov; motofumi@gmail.com; yunjin.kim@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX Part of this work was performed at the Jet Propulsion Laboratory under a
contract with the National Aeronautics and Space Administration.
NR 10
TC 101
Z9 101
U1 0
U2 9
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD SEP
PY 2011
VL 49
IS 9
SI SI
BP 3452
EP 3459
DI 10.1109/TGRS.2011.2128325
PG 8
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 815PE
UT WOS:000294536700029
ER
PT J
AU Huang, B
Rodriguez, M
Li, M
Bernstein, JB
Smidts, CS
AF Huang, Bing
Rodriguez, Manuel
Li, Ming
Bernstein, Joseph B.
Smidts, Carol S.
TI Hardware Error Likelihood Induced by the Operation of Software
SO IEEE TRANSACTIONS ON RELIABILITY
LA English
DT Article
DE Circuit simulation; embedded systems; failure propagation;
hardware-software interaction; permanent hardware failures
ID DEGRADATION; MOSFETS; SILICON
AB The influence of the software, and its interaction and interdependency with the hardware in the creation and propagation of hardware failures, are usually neglected in reliability analyses of safety critical systems. The software operation is responsible for the usage of semiconductor devices along the system lifetime. This usage consists of voltage changes and current flows that steadily degrade the materials of circuit devices until the degradation becomes permanent, and the device can no longer perform its intended function. At the circuit level, these failures manifest as stuck-at values, signal delays, or circuit functional changes. These failures are permanent in nature. Due to the extremely high scaling of complementary metal-oxide-semiconductor (CMOS) technology into deep submicron regimes, permanent hardware failures are a key concern, and can no longer be neglected compared to transient failures in radiation-intense applications. Our work proposes a methodology for the reliability analysis of permanent failure manifestations of hardware devices due to the usage induced by the execution of embedded software applications. The methodology is illustrated with a case study based on a safety critical application.
C1 [Huang, Bing] Everspin Technol Inc, Chandler, AZ 85224 USA.
[Rodriguez, Manuel; Smidts, Carol S.] Ohio State Univ, Columbus, OH 43210 USA.
[Li, Ming] NASA, Goddard Space Flight Ctr, Mantech Int Corp, Greenbelt, MD 20771 USA.
[Bernstein, Joseph B.] Bar Ilan Univ, IL-52100 Ramat Gan, Israel.
RP Huang, B (reprint author), Everspin Technol Inc, Chandler, AZ 85224 USA.
EM bing.huang@everspin.com; rodriguez-moreno.1@osu.edu; ming.li-1@nasa.gov;
bernstj@macs.biu.ac.il; smidts.1@osu.edu
FU Space Vehicle Technology Institute [NCC3-989]; NASA; DOD within the NASA
Constellation University Institutes; Claudia Meyer; NASA's Office of
Safety and Mission Assurance; NASA IV&V facility under NASA [NAG511952];
Air Force Office of Scientific Research [AFOSR FA9550-08-1-0139]
FX Manuscript received August 16, 2009; revised August 23, 2010; accepted
November 24, 2010. Date of publication July 22, 2011; date of current
version August 31, 2011. This research was funded in part by the Space
Vehicle Technology Institute under Grant NCC3-989 (jointly funded by
NASA and DOD within the NASA Constellation University Institutes
Project, with Claudia Meyer as the project manager), NASA's Office of
Safety and Mission Assurance through the NASA SARP program managed by
the NASA IV&V facility under NASA Grant NAG511952 and the Air Force
Office of Scientific Research under Grant Number AFOSR FA9550-08-1-0139.
Associate Editor: J. C. Lu.
NR 50
TC 3
Z9 3
U1 0
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9529
EI 1558-1721
J9 IEEE T RELIAB
JI IEEE Trans. Reliab.
PD SEP
PY 2011
VL 60
IS 3
BP 622
EP 639
DI 10.1109/TR.2011.2161699
PG 18
WC Computer Science, Hardware & Architecture; Computer Science, Software
Engineering; Engineering, Electrical & Electronic
SC Computer Science; Engineering
GA 815RB
UT WOS:000294543800011
ER
PT J
AU Hunter, GW
Xu, JC
Biaggi-Labiosa, AM
Laskowski, D
Dutta, PK
Mondal, SP
Ward, BJ
Makel, DB
Liu, CC
Chang, CW
Dweik, RA
AF Hunter, G. W.
Xu, J. C.
Biaggi-Labiosa, A. M.
Laskowski, D.
Dutta, P. K.
Mondal, S. P.
Ward, B. J.
Makel, D. B.
Liu, C. C.
Chang, C. W.
Dweik, R. A.
TI Smart sensor systems for human health breath monitoring applications
SO JOURNAL OF BREATH RESEARCH
LA English
DT Article
ID EXHALED NITRIC-OXIDE; INDUCED ASTHMATIC RESPONSE; LEUKOTRIENE B-4;
SPECTROMETRY ANALYSIS; LUNG-FUNCTION; VALIDATION; CONDENSATE; DIAGNOSIS;
8-ISOPROSTANE; CHILDREN
AB Breath analysis techniques offer a potential revolution in health care diagnostics, especially if these techniques can be brought into standard use in the clinic and at home. The advent of microsensors combined with smart sensor system technology enables a new generation of sensor systems with significantly enhanced capabilities and minimal size, weight and power consumption. This paper discusses the microsensor/smart sensor system approach and provides a summary of efforts to migrate this technology into human health breath monitoring applications. First, the basic capability of this approach to measure exhaled breath associated with exercise physiology is demonstrated. Building from this foundation, the development of a system for a portable asthma home health care system is described. A solid-state nitric oxide (NO) sensor for asthma monitoring has been identified, and efforts are underway to miniaturize this NO sensor technology and integrate it into a smart sensor system. It is concluded that base platform microsensor technology combined with smart sensor systems can address the needs of a range of breath monitoring applications and enable new capabilities for healthcare.
C1 [Hunter, G. W.; Xu, J. C.; Biaggi-Labiosa, A. M.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Laskowski, D.; Dweik, R. A.] Cleveland Clin, Cleveland, OH 44106 USA.
[Dutta, P. K.; Mondal, S. P.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA.
[Ward, B. J.; Makel, D. B.] Makel Engn Inc, Cleveland, OH USA.
[Liu, C. C.] Case Western Reserve Univ, Cleveland, OH 44106 USA.
[Chang, C. W.] ASRC Aerosp NASA Glenn Res Ctr, Cleveland, OH USA.
RP Hunter, GW (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
EM ghunter@grc.nasa.gov; DWEIKR@ccf.org
NR 43
TC 15
Z9 15
U1 2
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1752-7155
J9 J BREATH RES
JI J. Breath Res.
PD SEP
PY 2011
VL 5
IS 3
SI SI
AR 037111
DI 10.1088/1752-7155/5/3/037111
PG 11
WC Biochemical Research Methods; Respiratory System
SC Biochemistry & Molecular Biology; Respiratory System
GA 817KI
UT WOS:000294671000014
PM 21896970
ER
PT J
AU Sun, WB
Lin, B
Hu, YX
Lukashin, C
Kato, S
Liu, ZY
AF Sun, Wenbo
Lin, Bing
Hu, Yongxiang
Lukashin, Constantine
Kato, Seiji
Liu, Zhaoyan
TI On the consistency of CERES longwave flux and AIRS temperature and
humidity profiles
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID UNIFIED SATELLITE CLIMATOLOGY; CLOUDS; MODIS; AEROSOL; MISSION; TERRA;
MISR
AB In this paper, the temperature and humidity profiles from the Atmospheric Infrared Sounder (AIRS) are evaluated with outgoing longwave radiation (OLR) from the Clouds and the Earth's Radiant Energy System (CERES) measurements. Using collocated CERES and AIRS measurements from A-train observations, the temperature and humidity profiles from the AIRS are evaluated by using them in a radiative transfer model and comparing the modeled OLR with that from the CERES. Both the Moderate Resolution Imaging Spectroradiometer (MODIS) and the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) measurements are used to ensure a strict clear-sky condition over the CERES fields-of-view (FOVs) in the evaluation. The paper shows that model-computed OLRs using the AIRS temperature and humidity profiles and surface skin temperature agree well with CERES data for daytime oceans, indicating good accuracies of both the AIRS and the CERES products. However, it is found that a certain discrepancy exists between OLR from the modeling with the AIRS atmospheric profiles and that from the CERES measurements. For nighttime oceans, the AIRS temperature and humidity profiles and surface skin temperature likely have significant bias errors in tropical and subtropical areas that are due to undetected thin cirrus clouds. The inconsistency of the CERES and the AIRS product in OLR needs to be understood for reliable earth radiation studies.
C1 [Sun, Wenbo] Sci Syst & Applicat Inc, Hampton, VA 23681 USA.
[Sun, Wenbo; Lin, Bing; Hu, Yongxiang; Lukashin, Constantine; Kato, Seiji] NASA Langley Res Ctr, Hampton, VA 23681 USA.
[Liu, Zhaoyan] Natl Inst Aerosp, Hampton, VA 23666 USA.
RP Sun, WB (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23681 USA.
EM wenbo.sun-1@nasa.gov
RI Liu, Zhaoyan/B-1783-2010; Hu, Yongxiang/K-4426-2012; Richards,
Amber/K-8203-2015
OI Liu, Zhaoyan/0000-0003-4996-5738;
FU NASA
FX This work was supported by NASA CERES, CLARREO, and GLORY missions. The
authors thank Bruce A. Wielicki, Norman G. Loeb, David F. Young, Michael
I. Mishchenko, and Hal B. Maring for their support on this work.
NR 13
TC 8
Z9 8
U1 1
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 1
PY 2011
VL 116
AR D17101
DI 10.1029/2011JD016153
PG 5
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 816TM
UT WOS:000294625000001
ER
PT J
AU Bonfield, DG
Jarvis, MJ
Hardcastle, MJ
Cooray, A
Hatziminaoglou, E
Ivison, RJ
Page, MJ
Stevens, JA
de Zotti, G
Auld, R
Baes, M
Buttiglione, S
Cava, A
Dariush, A
Dunlop, JS
Dunne, L
Dye, S
Eales, S
Fritz, J
Hopwood, R
Ibar, E
Maddox, SJ
Michalowski, MJ
Pascale, E
Pohlen, M
Rigby, EE
Rodighiero, G
Serjeant, S
Smith, DJB
Temi, P
van der Werf, P
AF Bonfield, D. G.
Jarvis, M. J.
Hardcastle, M. J.
Cooray, A.
Hatziminaoglou, E.
Ivison, R. J.
Page, M. J.
Stevens, J. A.
de Zotti, G.
Auld, R.
Baes, M.
Buttiglione, S.
Cava, A.
Dariush, A.
Dunlop, J. S.
Dunne, L.
Dye, S.
Eales, S.
Fritz, J.
Hopwood, R.
Ibar, E.
Maddox, S. J.
Michalowski, M. J.
Pascale, E.
Pohlen, M.
Rigby, E. E.
Rodighiero, G.
Serjeant, S.
Smith, D. J. B.
Temi, P.
van der Werf, P.
TI Herschel-ATLAS: the link between accretion luminosity and star formation
in quasar host galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; galaxies: high-redshift; quasars: general
ID ACTIVE GALACTIC NUCLEI; SCIENCE DEMONSTRATION PHASE; REDSHIFT OBSCURED
QUASARS; DIGITAL SKY SURVEY; RADIO-GALAXIES; BLACK-HOLES; SUBMILLIMETER
SURVEY; FORMATION HISTORY; COSMIC EVOLUTION; ULIRG EVOLUTION
AB We use the science demonstration field data of the Herschel Astrophysical Terahertz Large Area Survey to study how star formation, traced by the far-infrared Herschel data, is related to both the accretion luminosity and redshift of quasars selected from the Sloan Digital Sky Survey (SDSS) and the 2dF-SDSS luminous red galaxy (LRG) and Quasar Spectroscopic Catalogue survey. By developing a maximum-likelihood estimator to investigate the presence of correlations between the far-infrared and optical luminosities, we find evidence that the star formation in quasar hosts is correlated with both redshift and quasar accretion luminosity. Assuming a relationship of the form L-IR alpha L-QSO(theta)(1 + z)(zeta), we find theta = 0.22 +/- 0.08 and zeta = 1.6 +/- 0.4, although there is substantial additional uncertainty in zeta of the order of +/- 1, due to uncertainties in the host galaxy dust temperature. We find evidence for a large intrinsic dispersion in the redshift dependence, but no evidence for intrinsic dispersion in the correlation between L-QSO and L-IR, suggesting that the latter may be due to a direct physical connection between star formation and black hole accretion. This is consistent with the idea that both the quasar activity and star formation are dependent on the same reservoir of cold gas, so that they are both affected by the influx of cold gas during mergers or heating of gas via feedback processes.
C1 [Bonfield, D. G.; Jarvis, M. J.; Hardcastle, M. J.; Stevens, J. A.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Hatziminaoglou, E.] ESO, D-85748 Garching, Germany.
[Ivison, R. J.; Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.; Dunlop, J. S.; Michalowski, M. J.; van der Werf, P.] Univ Edinburgh, Royal Observ, Inst Astron, Scottish Univ Phys Alliance, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Page, M. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[de Zotti, G.; Buttiglione, S.; Rodighiero, G.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy.
[de Zotti, G.] SISSA, I-34136 Trieste, Italy.
[Auld, R.; Dariush, A.; Dye, S.; Eales, S.; Pascale, E.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Cava, A.] Univ Complutense Madrid, Dept Astrofis, Fac CC Fis, E-28040 Madrid, Spain.
[Dariush, A.] Inst Res Fundamental Sci IPM, Sch Astron, Tehran, Iran.
[Dunne, L.; Maddox, S. J.; Rigby, E. E.; Smith, D. J. B.] Univ Nottingham, Sch Phys & Astron, Ctr Astron & Particle Theory, Nottingham NG7 1HR, England.
[Hopwood, R.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[Temi, P.] NASA Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA.
[van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Bonfield, DG (reprint author), Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
EM d.bonfield@herts.ac.uk
RI Hardcastle, Martin/E-2264-2012; Baes, Maarten/I-6985-2013; Ivison,
R./G-4450-2011; Cava, Antonio/C-5274-2017;
OI Hardcastle, Martin/0000-0003-4223-1117; Baes,
Maarten/0000-0002-3930-2757; Ivison, R./0000-0001-5118-1313; Cava,
Antonio/0000-0002-4821-1275; Maddox, Stephen/0000-0001-5549-195X; Dye,
Simon/0000-0002-1318-8343; Smith, Daniel/0000-0001-9708-253X;
Rodighiero, Giulia/0000-0002-9415-2296
FU RCUK; Royal Society; Alfred P. Sloan Foundation; National Science
Foundation; US Department of Energy; National Aeronautics and Space
Administration; Japanese Monbukagakusho; Max Planck Society; Higher
Education Funding Council for England; American Museum of Natural
History; Astrophysical Institute Potsdam; University of Basel;
University of Cambridge; Case Western Reserve University; University of
Chicago; Drexel University; Fermilab; Institute for Advanced Study;
Japan Participation Group; Johns Hopkins University; Joint Institute for
Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and
Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST);
Los Alamos National Laboratory; Max-Planck-Institute for Astronomy
(MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State
University; Ohio State University; University of Pittsburgh; University
of Portsmouth; Princeton University; United States Naval Observatory;
University of Washington
FX MJJ acknowledges support from an RCUK fellowship. MJH thanks the Royal
Society for a Research Fellowship.; Funding for the SDSS and SDSS-II has
been provided by the Alfred P. Sloan Foundation, the Participating
Institutions, the National Science Foundation, the US Department of
Energy, the National Aeronautics and Space Administration, the Japanese
Monbukagakusho, the Max Planck Society and the Higher Education Funding
Council for England. The SDSS website is http://www.sdss.org/.; The SDSS
is managed by the Astrophysical Research Consortium for the
Participating Institutions. The Participating Institutions are the
American Museum of Natural History, Astrophysical Institute Potsdam,
University of Basel, University of Cambridge, Case Western Reserve
University, University of Chicago, Drexel University, Fermilab, the
Institute for Advanced Study, the Japan Participation Group, Johns
Hopkins University, the Joint Institute for Nuclear Astrophysics, the
Kavli Institute for Particle Astrophysics and Cosmology, the Korean
Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos
National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the
Max-Planck-Institute for Astrophysics (MPA), New Mexico State
University, Ohio State University, University of Pittsburgh, University
of Portsmouth, Princeton University, the United States Naval Observatory
and the University of Washington.
NR 71
TC 42
Z9 42
U1 0
U2 2
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 SEP
PY 2011
VL 416
IS 1
BP 13
EP 21
DI 10.1111/j.1365-2966.2011.18826.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808YD
UT WOS:000294017000002
ER
PT J
AU Esposito, P
Israel, GL
Turolla, R
Mattana, F
Tiengo, A
Possenti, A
Zane, S
Rea, N
Burgay, M
Gotz, D
Mereghetti, S
Stella, L
Wieringa, MH
Sarkissian, JM
Enoto, T
Romano, P
Sakamoto, T
Nakagawa, YE
Makishima, K
Nakazawa, K
Nishioka, H
Francois-Martin, C
AF Esposito, P.
Israel, G. L.
Turolla, R.
Mattana, F.
Tiengo, A.
Possenti, A.
Zane, S.
Rea, N.
Burgay, M.
Goetz, D.
Mereghetti, S.
Stella, L.
Wieringa, M. H.
Sarkissian, J. M.
Enoto, T.
Romano, P.
Sakamoto, T.
Nakagawa, Y. E.
Makishima, K.
Nakazawa, K.
Nishioka, H.
Francois-Martin, C.
TI Long-term spectral and timing properties of the soft gamma-ray repeater
SGR 1833-0832 and detection of extended X-ray emission around the radio
pulsar PSR B1830-08
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: neutron; pulsars: general; X-rays: individual: PSR B1830-08
(J1833-0827); X-rays: individual: SGR 1833-0832
ID MAGNETIZED NEUTRON-STARS; XMM-NEWTON OBSERVATIONS; PHOTON IMAGING
CAMERA; 1E 1547.0-5408; SUPERNOVA-REMNANTS; XTE J1810-197; WIND NEBULAE;
SPIN-DOWN; DISCOVERY; OUTBURST
AB SGR 1833-0832 was discovered on 2010 March 19, thanks to the Swift detection of a short hard X-ray burst and follow-up X-ray observations. Since then, it was repeatedly observed with Swift, Rossi X-ray Timing Explorer and XMM-Newton. Using these data, which span about 225 d, we studied the long-term spectral and timing characteristics of SGR 1833-0832. We found evidence for diffuse emission surrounding SGR 1833-0832, which is most likely a halo produced by the scattering of the point-source X-ray radiation by dust along the line of sight, and we show that the source X-ray spectrum is well described by an absorbed blackbody, with temperature kT similar to 1.2 keV and absorbing column N-H = (10.4 +/- 0.2) x 10(22) cm(-2), while different or more complex models are disfavoured. The source persistent X-ray emission remained fairly constant at similar to 3.7 x 10(-12) erg cm(-2) s(-1) for the first similar to 20 d after the onset of the bursting episode, then it faded by a factor of similar to 40 in the subsequent similar to 140 d, following a power-law trend with index alpha similar or equal to -0.5. We obtained a phase-coherent timing solution with the longest baseline (similar to 225 d) to date for this source which, besides period P = 7.565 4084(4) s and period derivative. P = 3.5(3) x 10(-12) s s(-1), includes higher order period derivatives. We also report on our search of the counterpart to the soft gamma-ray repeater (SGR) at radio frequencies using the Australia Telescope Compact Array and the Parkes Radio Telescope. No evidence for radio emission was found, down to flux densities of 0.9 mJy (at 1.5 GHz) and 0.09 mJy (at 1.4 GHz) for the continuum and pulsed emissions, respectively, consistently with other observations at different epochs. Finally, the analysis of the field of PSR B1830-08 (J1833-0827), which was serendipitously imaged by the XMM-Newton observations, led to the discovery of the X-ray pulsar wind nebula generated by this 85-ms radio pulsar. We discuss its possible association with the unidentified TeV source HESS J1834-087.
C1 [Esposito, P.; Possenti, A.; Burgay, M.] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, Italy.
[Israel, G. L.; Stella, L.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Turolla, R.] Univ Padua, Dipartimento Fis, I-35131 Padua, Italy.
[Turolla, R.; Zane, S.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Mattana, F.] Univ Paris Diderot, CNRS IN2P3, CEA DSM, Francois Arago Ctr,APC,Observ Paris, F-75205 Paris 13, France.
[Tiengo, A.; Mereghetti, S.] INAF Ist Astrofis Spaziale & Fis Cosm Milano, I-20133 Milan, Italy.
[Rea, N.] CSIC IEEC, Fac Ciencies, Inst Ciencies Espai, E-08193 Barcelona, Spain.
[Goetz, D.] Univ Paris Diderot, CNRS, CEA DSM, AIM,Irfu Serv Astrophys,UMR 7158, F-91191 Gif Sur Yvette, France.
[Wieringa, M. H.; Sarkissian, J. M.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Enoto, T.] SLAC Stanford Univ, KIPAC, Stanford, CA 94309 USA.
[Romano, P.] INAF Ist Astrofis Spaziale & Fis Cosm Palermo, I-90146 Palermo, Italy.
[Sakamoto, T.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nakagawa, Y. E.; Makishima, K.] RIKEN, Inst Phys & Chem Res, High Energy Astrophys Lab, Wako, Saitama 3510198, Japan.
[Makishima, K.; Nakazawa, K.; Nishioka, H.] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Francois-Martin, C.] Univ Paris 07, F-75252 Paris 5, France.
RP Esposito, P (reprint author), INAF Osservatorio Astron Cagliari, Str 54, I-09012 Capoterra, Italy.
EM paoloesp@oa-cagliari.inaf.it
RI Rea, Nanda/I-2853-2015;
OI Rea, Nanda/0000-0003-2177-6388; Israel, GianLuca/0000-0001-5480-6438;
Burgay, Marta/0000-0002-8265-4344; Tiengo, Andrea/0000-0002-6038-1090;
MEREGHETTI, SANDRO/0000-0003-3259-7801; Esposito,
Paolo/0000-0003-4849-5092
FU ESA Member States; NASA; Commonwealth of Australia; ASI (ASI/INAF)
[I/009/10/0, I/011/07/0, I/010/06/0, I/088/06/0, AAE TH-058]; Autonomous
Region of Sardinia [FSE 2007-2013]; CNES; Ramon y Cajal fellowship
FX We thank the referee, Vicky Kaspi, for valuable and constructive
comments. This research is based on observations obtained with
XMM-Newton, an ESA science mission with instruments and contributions
directly funded by ESA Member States and NASA. We thank Norbert Schartel
and the staff of the XMM-Newton Science Operation Center for promptly
scheduling and executing our observations. The RXTE and Swift data were
obtained through the HEASARC Online Service, provided by the NASA/GSFC.
We thank the Swift PI, Neil Gehrels, the Swift duty scientists and
science planners for making our Swift target of opportunity observations
possible. We thank Hans Krimm for re-analysing the Swift/BAT transient
monitor and survey data for the time period following the outburst. We
thank Philip Edwards of CSIRO for prompt allocations of observing time
at the Parkes Observatory and the ATCA. The Parkes Observatory and the
ATCA are part of the Australia Telescope, which is funded by the
Commonwealth of Australia for operation as a National Facility managed
by CSIRO. The Italian authors acknowledge the partial support from ASI
(ASI/INAF contracts I/009/10/0, I/011/07/0, I/010/06/0, I/088/06/0 and
AAE TH-058). PE acknowledges financial support from the Autonomous
Region of Sardinia through a research grant under the programme PO
Sardegna FSE 2007-2013, L. R. 7/2007 'Promoting scientific research and
innovation technology in Sardinia'. FM and DG acknowledge the CNES for
financial funding. NR is supported by a Ramon y Cajal fellowship.
NR 83
TC 20
Z9 20
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2011
VL 416
IS 1
BP 205
EP 215
DI 10.1111/j.1365-2966.2011.19022.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808YD
UT WOS:000294017000016
ER
PT J
AU Coppin, KEK
Geach, JE
Smail, I
Dunne, L
Edge, AC
Ivison, RJ
Maddox, S
Auld, R
Baes, M
Buttiglione, S
Cava, A
Clements, DL
Cooray, A
Dariush, A
De Zotti, G
Dye, S
Eales, S
Fritz, J
Hopwood, R
Ibar, E
Jarvis, M
Michalowski, MJ
Murphy, DNA
Negrello, M
Pascale, E
Pohlen, M
Rigby, E
Rodighiero, G
Scott, D
Serjeant, S
Smith, DJB
Temi, P
van der Werf, P
AF Coppin, K. E. K.
Geach, J. E.
Smail, Ian
Dunne, L.
Edge, A. C.
Ivison, R. J.
Maddox, S.
Auld, R.
Baes, M.
Buttiglione, S.
Cava, A.
Clements, D. L.
Cooray, A.
Dariush, A.
De Zotti, G.
Dye, S.
Eales, S.
Fritz, J.
Hopwood, R.
Ibar, E.
Jarvis, M.
Michalowski, M. J.
Murphy, D. N. A.
Negrello, M.
Pascale, E.
Pohlen, M.
Rigby, E.
Rodighiero, G.
Scott, D.
Serjeant, S.
Smith, D. J. B.
Temi, P.
van der Werf, P.
TI Herschel-Astrophysical Terahertz Large Area Survey: detection of a
far-infrared population around galaxy clusters
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: strong; galaxies: clusters: general; galaxies:
evolution; galaxies: starburst; submillimetre: galaxies
ID DIGITAL SKY SURVEY; OBSCURED STAR-FORMATION; STELLAR MASS FUNCTIONS;
LUMINOSITY FUNCTION; DISTANT CLUSTERS; BAND LUMINOSITY; ISOCAM SURVEY;
ABELL 1689; EVOLUTION; ATLAS
AB We report the detection of a significant excess in the surface density of far-infrared sources from the Herschel-Astrophysical Terahertz Large Area Survey within similar to 1Mpc of the centres of 66 optically selected clusters of galaxies in the Sloan Digital Sky Survey with < z > similar to 0.25. From the analysis of the multiwavelength properties of their counterparts we conclude that the far-infrared emission is associated with dust-obscured star formation and/or active galactic nuclei (AGN) within galaxies in the clusters themselves. The excess reaches a maximum at a radius of similar to 0.8Mpc, where we find 1.0 +/- 0.3 S-250 > 34 mJy sources on average per cluster above what would be expected for random field locations. If the far-infrared emission is dominated by star formation (as opposed to AGN) then this corresponds to an average star formation rate of similar to 7M(circle dot) yr(-1) per cluster in sources with L-IR > 5 x 10(10) L-circle dot. Although lensed sources make a negligible contribution to the excess signal, a fraction of the sources around the clusters could be gravitationally lensed, and we have identified a sample of potential cases of cluster-lensed Herschel sources that could be targeted in follow-up studies.
C1 [Coppin, K. E. K.; Geach, J. E.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Coppin, K. E. K.; Geach, J. E.; Smail, Ian; Edge, A. C.; Murphy, D. N. A.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England.
[Dunne, L.; Maddox, S.; Rigby, E.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Ivison, R. J.; Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.; Michalowski, M. J.; van der Werf, P.] Univ Edinburgh, Inst Astron, SUPA, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Auld, R.; Dariush, A.; Dye, S.; Eales, S.; Pascale, E.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Buttiglione, S.; De Zotti, G.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy.
[Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain.
[Clements, D. L.; Dariush, A.; Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Dept Phys, Astrophys Grp, London SW7 2AZ, England.
[Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Dariush, A.] Inst Res Fundamental Sci IPM, Sch Astron, Tehran, Iran.
[De Zotti, G.] SISSA, I-34136 Trieste, Italy.
[Jarvis, M.; Smith, D. J. B.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Jarvis, M.] Univ Western Cape, Dept Phys, ZA-7535 Cape Town, South Africa.
[Negrello, M.; Serjeant, S.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[Rodighiero, G.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Temi, P.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Coppin, KEK (reprint author), McGill Univ, Dept Phys, Ernest Rutherford Bldg,3600 Rue Univ, Montreal, PQ H3A 2T8, Canada.
EM coppink@physics.mcgill.ca
RI Baes, Maarten/I-6985-2013; Smail, Ian/M-5161-2013; Ivison,
R./G-4450-2011; Cava, Antonio/C-5274-2017;
OI Rodighiero, Giulia/0000-0002-9415-2296; Baes,
Maarten/0000-0002-3930-2757; /0000-0002-0729-2988; Smail,
Ian/0000-0003-3037-257X; Ivison, R./0000-0001-5118-1313; Cava,
Antonio/0000-0002-4821-1275; Scott, Douglas/0000-0002-6878-9840; Maddox,
Stephen/0000-0001-5549-195X; Edge, Alastair/0000-0002-3398-6916; Dye,
Simon/0000-0002-1318-8343; Smith, Daniel/0000-0001-9708-253X
FU endowment of the Lorne Trottier Chair in Astrophysics and Cosmology at
McGill; National Science and Engineering Research Council of Canada; UK
Science and Technology Facilities Council (STFC); Centre of Research in
Astrophysics of Quebec; ASI-INAF [I/009/10/0]
FX We thank the referee, Pierre-Alain Duc, for his suggestions which helped
to improve the paper, and also Tracy Webb for useful discussions. KEKC
and JEG acknowledge support from the endowment of the Lorne Trottier
Chair in Astrophysics and Cosmology at McGill, the National Science and
Engineering Research Council of Canada and the UK Science and Technology
Facilities Council (STFC). KEKC also acknowledges the Centre of Research
in Astrophysics of Quebec for a fellowship. ACE, IS and RJI acknowledge
support from STFC. GDZ acknowledges financial contribution from the
agreement ASI-INAF I/009/10/0. The Herschel-ATLAS is a project with
Herschel.
NR 55
TC 12
Z9 12
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 SEP
PY 2011
VL 416
IS 1
BP 680
EP 688
DI 10.1111/j.1365-2966.2011.19084.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808YD
UT WOS:000294017000062
ER
PT J
AU Parmentier, G
Kauffmann, J
Pillai, T
Menten, KM
AF Parmentier, Genevieve
Kauffmann, Jens
Pillai, Thushara
Menten, Karl M.
TI Volume density thresholds for overall star formation imply mass-size
thresholds for massive star formation
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: formation; ISM: clouds; galaxies: star clusters: general
ID MOLECULAR CLOUDS; DUST CONTINUUM; CLUSTER-MASS; O-STARS; ORIGIN; I.;
CANDIDATES; EMISSION; SEARCH; GAS
AB We aim at understanding the massive star formation (MSF) limit m(r) = 870M(circle dot)(r/pc)(1.33) in the mass-size space of molecular structures recently proposed by Kauffmann & Pillai. As a first step, we build on the property that power-law density profiles for molecular clumps combined with a volume density threshold for the overall star formation naturally leads to mass-radius relations for molecular clumps containing given masses of star-forming gas. Specifically, we show that the mass mclump and radius rclump of molecular clumps whose density profile slope is -p and which contain a mass mth of gas denser than a density threshold.th obeys the following: mclump = m p/ 3 rho(th) m(clump) = m(th)(p/3) (4 pi rho th/3-p)((3-p)/3)r(clump)(3 p). In a second step, we use the relation between the mass of embedded clusters and the mass of their most massive star to estimate the minimum mass of the star-forming gas needed to form a 10-M-circle dot star. Assuming a star formation efficiency (SFE) of SFE similar or equal to 0.30, this gives mth, crit similar or equal to 150M(circle dot). In a third step, we demonstrate that, for sensible choices of the clump density index (p similar or equal to 1.7) and of the cluster formation density threshold (n(th) similar or equal to 10(4) cm(-3)), the line of constant m(th, crit) similar or equal to 150M(circle dot) in the mass-radius space of molecular structures equates to the MSF limit for spatial scales larger than 0.3 pc. Hence, the observationally inferred MSF limit of Kauffmann & Pillai is consistent with a threshold in star-forming gas mass beyond which the star-forming gas reservoir is large enough to allow the formation of massive stars. For radii smaller than 0.3 pc, the MSF limit is shown to be consistent with the formation of a 10-M-circle dot star (m(th, crit) similar or equal to 30M(circle dot) with SFE similar or equal to 0.3) out of its individual pre-stellar core of density threshold n(th) similar or equal to 10(5) cm(-3). The inferred density thresholds for the formation of star clusters and individual stars within star clusters match those previously suggested in the literature.
C1 [Parmentier, Genevieve; Menten, Karl M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Parmentier, Genevieve] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Kauffmann, Jens] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Pillai, Thushara] CALTECH, Pasadena, CA 91125 USA.
RP Parmentier, G (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM gparm@mpifr-bonn.mpg.de
FU Max-Planck-Institut fur Radioastronomie (Bonn); NASA; National Air and
Space Administration; Combined Array for Research in Millimeter-wave
Astronomy (CARMA); National Science Foundation [AST 05-40399]
FX GP acknowledges support from the Max-Planck-Institut fur Radioastronomie
(Bonn) in the form of a Research Fellowship. JK thanks Di Li, his host
at JPL, for making this research possible. This project was supported by
an appointment of JK to the NASA Postdoctoral Program at the Jet
Propulsion Laboratory, administered by Oak Ridge Associated Universities
through a contract with NASA. JK's research was executed at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Air and Space Administration. TP acknowledges
support from the Combined Array for Research in Millimeter-wave
Astronomy (CARMA), which is supported by the National Science Foundation
through grant AST 05-40399. We thank the referee for the original
suggestion to combine the individual-and clustered-star formation models
into one additional figure.
NR 32
TC 9
Z9 9
U1 0
U2 0
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 SEP
PY 2011
VL 416
IS 1
BP 783
EP 789
DI 10.1111/j.1365-2966.2011.19096.x
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808YD
UT WOS:000294017000071
ER
PT J
AU Stephens, C
Pope, A
Scerbo, M
AF Stephens, Chad
Pope, Alan
Scerbo, Mark
TI Biocybernetic Closed-Loop System for Mitigating Hazardous States of
Awareness
SO APPLIED PSYCHOPHYSIOLOGY AND BIOFEEDBACK
LA English
DT Meeting Abstract
DE Adaptive automation; Biocybernetic; Closed-loop
C1 [Stephens, Chad] NASA, Hampton, VA 23681 USA.
EM chad.l.stephens@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1090-0586
J9 APPL PSYCHOPHYS BIOF
JI Appl. Psychophysiol. Biofeedback
PD SEP
PY 2011
VL 36
IS 3
BP 217
EP 218
PG 2
WC Psychology, Clinical
SC Psychology
GA 814MS
UT WOS:000294460100011
ER
PT J
AU Romanek, CS
Morse, JW
Grossman, EL
AF Romanek, Christopher S.
Morse, John W.
Grossman, Ethan L.
TI Aragonite Kinetics in Dilute Solutions
SO AQUATIC GEOCHEMISTRY
LA English
DT Article
DE Aragonite; Precipitation rate; Activation energy; Kinetics
ID CALCIUM-CARBONATE; SEA-WATER; DISSOLUTION KINETICS; GROWTH-KINETICS;
CRYSTAL-GROWTH; SEEDED GROWTH; PRECIPITATION; CRYSTALLIZATION; SEAWATER;
TEMPERATURE
AB Aragonite was synthesized inorganically using a seeded-growth technique to characterize precipitation kinetics for the heterogeneous growth of solid from dilute solutions (ionic strength: 0.05-0.07 mol l(-1)). The concentration of all aqueous constituents, including Ca (similar to 5-15 mmol l(-1)), Na (similar to 10-35 mmol l(-1)), Cl (similar to 30-35 mmol l(-1)), and carbon (as total alkalinity: similar to 10 to 17 meq l(-1)), was held constant by the addition of titrants that contained excess solute concentrations to balance the growth of solid phase during the precipitation reaction, and a CO(2)/N(2) gas mixture (0.009-0.178) was bubbled through each solution to facilitate mass exchange between gaseous and aqueous carbon species. Forty-three experiments were conducted at 10A degrees (similar to n = 13), 25A degrees (n = 21), and 40A degrees C (n = 9), over a range of average saturation states with respect to aragonite from 8.3 to 28.5, 2.9 to 19.6 and 2.0 to 12.2, and average precipitation rates from 10(2.8) to 10(3.8), 10(2.3) to 10(4.0), and 10(2.5) to 10(4.1) micromol m(-2) h(-1), respectively. Reaction orders averaged 1.7 +/- A 0.10 at 10A degrees, 1.7 +/- A 0.07 at 25A degrees and 1.5 +/- A 0.06 at 40A degrees, and they were independent of temperature while rate constants averaged 10(1.3) +/- A 0.12, 10(1.9) +/- A 0.06, and 10(2.6) +/- A 0.04 micromol m(-2) h(-1), respectively, increasing one-half order of magnitude for each 15A degrees C rise in temperature. From these data, an Arrhenius activation energy of 71.2 kJ mol(-1) is calculated for the heterogeneous precipitation of aragonite. This value is comparable to a sole independent measurement of 80.7 kJ mol(-1) reported for the solid-solution recrystallization of monohydrocalcite to aragonite (Munemoto and Fukushi in J Mineral Petrol Sci 103: 345-349, 2008).
C1 [Romanek, Christopher S.] Univ Kentucky, NASA, Astrobiol Inst, Lexington, KY 40506 USA.
[Romanek, Christopher S.] Univ Kentucky, Dept Earth & Environm Sci, Lexington, KY 40506 USA.
[Morse, John W.] Texas A&M Univ, Dept Oceanog, College Stn, TX 77843 USA.
[Grossman, Ethan L.] Texas A&M Univ, Dept Geol & Geophys, College Stn, TX 77843 USA.
RP Romanek, CS (reprint author), Univ Kentucky, NASA, Astrobiol Inst, Lexington, KY 40506 USA.
EM c.romanek@uky.edu
FU National Science Foundation [EAR-851187]; NASA Astrobiology Institute
FX This project could not have succeeded without John Morse's thoughtful
guidance and mastery of carbonate experimental systems. The writing is
posthumous, but the science is a product of his mentorship and
enthusiasm for carbonate geochemistry. This work was supported
financially by the National Science Foundation (EAR-851187) and the NASA
Astrobiology Institute.
NR 49
TC 9
Z9 10
U1 1
U2 20
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1380-6165
J9 AQUAT GEOCHEM
JI Aquat. Geochem.
PD SEP
PY 2011
VL 17
IS 4-5
SI SI
BP 339
EP 356
DI 10.1007/s10498-011-9127-2
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 814MY
UT WOS:000294460900004
ER
PT J
AU Mawet, D
Mennesson, B
Serabyn, E
Stapelfeldt, K
Absil, O
AF Mawet, D.
Mennesson, B.
Serabyn, E.
Stapelfeldt, K.
Absil, O.
TI A DIM CANDIDATE COMPANION TO epsilon CEPHEI
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE brown dwarfs; instrumentation: adaptive optics; instrumentation: high
angular resolution; stars: low-mass; techniques: high angular resolution
ID INFRARED INTERFEROMETRIC SURVEY; DEBRIS DISKS; HOT DUST; STARS;
CHARA/FLUOR; CATALOG; IRAS
AB Using a vector vortex coronagraph behind the 1.5 m well-corrected subaperture (WCS) at Palomar, we detected a second object very close to epsilon Cephei, a delta Scuti F0 IV star. The candidate companion, similar to 50 times fainter than epsilon Cephei, if physically associated, is a late-type K or early M star, and lies at an angular separation of 330 mas, or 1.1 lambda/D for the WCS, making it the smallest angle detection ever realized with a coronagraph in terms of lambda/D units. The projected separation of the putative companion is similar to 8.6 AU, most likely on a highly eccentric orbit. The recently detected near-infrared excess is thus likely not due to hot dust. Moreover, we also show that the previously reported IRAS 60 mu m excess was due to source confusion on the galactic plane.
C1 [Mawet, D.] European So Observ, Santiago, Chile.
[Mawet, D.; Mennesson, B.; Serabyn, E.; Stapelfeldt, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Absil, O.] Univ Liege, Inst Astrophys & Geophys Liege, B-4000 Sart Tilman Par Liege, Belgium.
RP Mawet, D (reprint author), European So Observ, Alonso de Cordova 3107, Santiago, Chile.
FU NASA
FX This work was carried out at the European Southern Observatory (ESO)
site of Vitacura (Santiago, Chile), and the Jet Propulsion Laboratory
(JPL), California Institute of Technology (Caltech), under contract with
the National Aeronautics and Space Administration (NASA). The data
presented in this Letter are based on observations obtained at the Hale
Telescope, Palomar Observatory, as part of a continuing collaboration
between Caltech, NASA/JPL, and Cornell University. This work is also
based (in part) on observations made with the Spitzer Space Telescope,
which is operated by the JPL, Caltech, under a contract with NASA. This
research has made use of the NASA/IPAC/NExScI Star and Exoplanet
Database, which is operated by the JPL, Caltech, under contract with
NASA, and NASA's Astrophysics Data System and of the SIMBAD database,
operated at CDS (Strasbourg, France).
NR 26
TC 22
Z9 22
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 1
PY 2011
VL 738
IS 1
AR L12
DI 10.1088/2041-8205/738/1/L12
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808FA
UT WOS:000293961400012
ER
PT J
AU Shi, J
Raut, U
Kim, JH
Loeffler, M
Baragiola, RA
AF Shi, J.
Raut, U.
Kim, J. -H.
Loeffler, M.
Baragiola, R. A.
TI ULTRAVIOLET PHOTON-INDUCED SYNTHESIS AND TRAPPING OF H2O2 AND O-3 IN
POROUS WATER ICE FILMS IN THE PRESENCE OF AMBIENT O-2: IMPLICATIONS FOR
EXTRATERRESTRIAL ICE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE atomic processes; methods: laboratory; planets and satellites:
atmospheres; planets and satellites: surfaces; radiation mechanisms:
general
ID OUTER SOLAR-SYSTEM; HYDROGEN-PEROXIDE; GALILEAN SATELLITES; ION
IRRADIATION; SATURNS MAGNETOSPHERE; GANYMEDE; SPECTRA; EUROPA; OXYGEN;
OZONE
AB The mass uptake of ambient oxygen in nanoporous ice is enhanced by irradiation with 193 nm photons, due to conversion of O-2 into H2O2 and O-3, with an efficiency that increases with decreasing temperature. These findings show a new way to form H2O2 and O-3 on icy surfaces in the outer solar system at depths much larger than are accessible by typical ionizing radiation, with possible astrobiological implications.
C1 [Shi, J.; Raut, U.; Kim, J. -H.; Baragiola, R. A.] Univ Virginia, Lab Atom & Surface Phys, Charlottesville, VA 22904 USA.
[Loeffler, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Baragiola, RA (reprint author), Univ Virginia, Lab Atom & Surface Phys, Charlottesville, VA 22904 USA.
EM raul@virginia.edu
RI Loeffler, Mark/C-9477-2012; shi, jianming/A-3278-2013
FU NASA Planetary Atmospheres; NSF Astronomy
FX This research was supported by NASA Planetary Atmospheres and NSF
Astronomy.
NR 45
TC 5
Z9 5
U1 1
U2 14
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 SEP 1
PY 2011
VL 738
IS 1
AR L3
DI 10.1088/2041-8205/738/1/L3
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808FA
UT WOS:000293961400003
ER
PT J
AU Lim, YK
Stefanova, LB
Chan, SC
Schubert, SD
O'Brien, JJ
AF Lim, Young-Kwon
Stefanova, Lydia B.
Chan, Steven C.
Schubert, Siegfried D.
O'Brien, James J.
TI High-resolution subtropical summer precipitation derived from dynamical
downscaling of the NCEP/DOE reanalysis: how much small-scale information
is added by a regional model?
SO CLIMATE DYNAMICS
LA English
DT Article
ID CLIMATE MODEL; UNITED-STATES; SPECTRAL MODEL; US PRECIPITATION; SYSTEM
RAMS; PART I; SIMULATIONS; PARAMETERIZATION; CIRCULATION; PREDICTION
AB This study assesses the regional-scale summer precipitation produced by the dynamical downscaling of analyzed large-scale fields. The main goal of this study is to investigate how much the regional model adds smaller scale precipitation information that the large-scale fields do not resolve. The modeling region for this study covers the southeastern United States (Florida, Georgia, Alabama, South Carolina, and North Carolina) where the summer climate is subtropical in nature, with a heavy influence of regional-scale convection. The coarse resolution (2.5A degrees latitude/longitude) large-scale atmospheric variables from the National Center for Environmental Prediction (NCEP)/DOE reanalysis (R2) are downscaled using the NCEP/Environmental Climate Prediction Center regional spectral model (RSM) to produce precipitation at 20 km resolution for 16 summer seasons (1990-2005). The RSM produces realistic details in the regional summer precipitation at 20 km resolution. Compared to R2, the RSM-produced monthly precipitation shows better agreement with observations. There is a reduced wet bias and a more realistic spatial pattern of the precipitation climatology compared with the interpolated R2 values. The root mean square errors of the monthly R2 precipitation are reduced over 93% (1,697) of all the grid points in the five states (1,821). The temporal correlation also improves over 92% (1,675) of all grid points such that the domain-averaged correlation increases from 0.38 (R2) to 0.55 (RSM). The RSM accurately reproduces the first two observed eigenmodes, compared with the R2 product for which the second mode is not properly reproduced. The spatial patterns for wet versus dry summer years are also successfully simulated in RSM. For shorter time scales, the RSM resolves heavy rainfall events and their frequency better than R2. Correlation and categorical classification (above/near/below average) for the monthly frequency of heavy precipitation days is also significantly improved by the RSM.
C1 [Lim, Young-Kwon; Stefanova, Lydia B.; Chan, Steven C.; O'Brien, James J.] Florida State Univ, Ctr Ocean Atmospher Predict Studies, Tallahassee, FL 32306 USA.
[Lim, Young-Kwon; Schubert, Siegfried D.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Lim, YK (reprint author), Florida State Univ, Ctr Ocean Atmospher Predict Studies, Tallahassee, FL 32306 USA.
EM lim@coaps.fsu.edu
RI stefanova, lydia/B-2759-2013
NR 53
TC 11
Z9 11
U1 0
U2 9
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD SEP
PY 2011
VL 37
IS 5-6
BP 1061
EP 1080
DI 10.1007/s00382-010-0891-2
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 814ZU
UT WOS:000294496700014
ER
PT J
AU Cook, BI
Cook, ER
Anchukaitis, KJ
Seager, R
Miller, RL
AF Cook, Benjamin I.
Cook, Edward R.
Anchukaitis, Kevin J.
Seager, Richard
Miller, Ron L.
TI Forced and unforced variability of twentieth century North American
droughts and pluvials
SO CLIMATE DYNAMICS
LA English
DT Article
DE Drought; Forcing; Predictability; North America; Dust Bowl
ID ATLANTIC MULTIDECADAL OSCILLATION; SEA-SURFACE TEMPERATURE; WESTERN
UNITED-STATES; DUST BOWL DROUGHT; US; CLIMATE; 1930S; LATE-19TH-CENTURY;
RECONSTRUCTIONS; MECHANISMS
AB Research on the forcing of drought and pluvial events over North America is dominated by general circulation model experiments that often have operational limitations (e.g., computational expense, ability to simulate relevant processes, etc). We use a statistically based modeling approach to investigate sea surface temperature (SST) forcing of the twentieth century pluvial (1905-1917) and drought (1932-1939, 1948-1957, 1998-2002) events. A principal component (PC) analysis of Palmer Drought Severity Index (PDSI) from the North American Drought Atlas separates the drought variability into five leading modes accounting for 62% of the underlying variance. Over the full period spanning these events (1900-2005), the first three PCs significantly correlate with SSTs in the equatorial Pacific (PC 1), North Pacific (PC 2), and North Atlantic (PC 3), with spatial patterns (as defined by the empirical orthogonal functions) consistent with our understanding of North American drought responses to SST forcing. We use a large ensemble statistical modeling approach to determine how successfully we can reproduce these drought/pluvial events using these three modes of variability. Using Pacific forcing only (PCs 1-2), we are able to reproduce the 1948-1957 drought and 1905-1917 pluvial above a 95% random noise threshold in over 90% of the ensemble members; the addition of Atlantic forcing (PCs 1-2-3) provides only marginal improvement. For the 1998-2002 drought, Pacific forcing reproduces the drought above noise in over 65% of the ensemble members, with the addition of Atlantic forcing increasing the number passing to over 80%. The severity of the drought, however, is underestimated in the ensemble median, suggesting this drought intensity can only be achieved through internal variability or other processes. Pacific only forcing does a poor job of reproducing the 1932-1939 drought pattern in the ensemble median, and less than one third of ensemble members exceed the noise threshold (28%). Inclusion of Atlantic forcing improves the ensemble median drought pattern and nearly doubles the number of ensemble members passing the noise threshold (52%). Even with the inclusion of Atlantic forcing, the intensity of the simulated 1932-1939 drought is muted, and the drought itself extends too far into the southwest and southern Great Plains. To an even greater extent than the 1998-2002 drought, these results suggest much of the variance in the 1932-1939 drought is dependent on processes other than SST forcing. This study highlights the importance of internal noise and non SST processes for hydroclimatic variability over North America, complementing existing research using general circulation models.
C1 [Cook, Benjamin I.; Miller, Ron L.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Cook, Edward R.; Anchukaitis, Kevin J.; Seager, Richard] Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
RP Cook, BI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM bc9z@ldeo.columbia.edu
RI Miller, Ron/E-1902-2012; Cook, Benjamin/H-2265-2012;
OI Anchukaitis, Kevin/0000-0002-8509-8080
FU National Science Foundation [ATM-06-20066]
FX This project received support from the Climate Dynamics Program of the
National Science Foundation under ATM-06-20066. The authors also wish to
thank anonymous reviewers who greatly improved the quality of this
manuscript. Lamont contribution number 7387.
NR 45
TC 17
Z9 17
U1 2
U2 21
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD SEP
PY 2011
VL 37
IS 5-6
BP 1097
EP 1110
DI 10.1007/s00382-010-0897-9
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 814ZU
UT WOS:000294496700016
ER
PT J
AU Campbell, BA
Putzig, NE
Carter, LM
Phillips, RJ
AF Campbell, Bruce A.
Putzig, Nathaniel E.
Carter, Lynn M.
Phillips, Roger J.
TI Autofocus Correction of Phase Distortion Effects on SHARAD Echoes
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Mars; radar signal processing; spaceborne radar
ID MAGNETIC-FIELD; MARS; IONOSPHERE; SHARPNESS
AB SHARAD is a frequency-modulated (15-25 MHz) radar sounder that probes the upper few kilometers of the Martian crust and polar layered deposits. At solar zenith angles less than about 100 degrees, the ionosphere of Mars can induce phase distortion in surface and subsurface radar echoes that substantially degrades the signal-to-noise ratio and vertical resolution of the range-compressed data. We present a range-compression autofocus approach that estimates the phase distortion of SHARAD data along ground-track segments of about 100 km, using a power-law image-sharpness metric and an empirically derived scaling between the phase correction and radar frequency. This method is rapid, yields a greatly improved subsurface image, and provides a means to track regional and temporal changes in the Martian ionosphere.
C1 [Campbell, Bruce A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
[Putzig, Nathaniel E.; Phillips, Roger J.] SW Res Inst, Boulder, CO 80302 USA.
[Carter, Lynn M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20706 USA.
RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
EM campbellb@si.edu; nathaniel@putzig.com; lynn.m.carter@nasa.gov;
roger@boulder.swri.edu
RI Carter, Lynn/D-2937-2012
NR 23
TC 9
Z9 10
U1 0
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1545-598X
EI 1558-0571
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD SEP
PY 2011
VL 8
IS 5
BP 939
EP 942
DI 10.1109/LGRS.2011.2143692
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 815RY
UT WOS:000294546900021
ER
PT J
AU Xie, Y
Xiong, XX
AF Xie, Yong
Xiong, Xiaoxiong
TI On-Orbit Spatial Characterization of MODIS With ASTER Aboard the Terra
Spacecraft
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER);
band-to-band registration (BBR); MODerate resolution Imaging
Spectroradiometer (MODIS); spatial characterization
ID REFLECTIVE SOLAR BANDS; CALIBRATION
AB This letter presents a novel approach for on-orbit characterization of MODerate resolution Imaging Spectroradiometer (MODIS) band-to-band registration (BBR) using Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) aboard the Terra spacecraft. The spatial resolution of ASTER spectral bands is much higher than that of MODIS, making it feasible to characterize MODIS on-orbit BBR using their simultaneous observations. The ground target selected for on-orbit MODIS BBR characterization in this letter is a water body, which is a uniform scene with high signal contrast relative to its neighbor areas. A key step of this approach is to accurately localize the measurements of each MODIS band in an ASTER measurement plane coordinate (AMPC). The ASTER measurements are first interpolated and aggregated to simulate the measurements of each MODIS band. The best measurement match between ASTER and each MODIS band is obtained when the measurement difference reaches its weighted minimum. The position of each MODIS band in the AMPC is then used to calculate the BBR. The results are compared with those derived from MODIS onboard Spectro-Radiometric Calibration Assembly. They are in good agreement, generally less than 0.1 MODIS pixel. This approach is useful for other sensors without onboard spatial characterization capability.
C1 [Xie, Yong] Sigma Space Corp, Lanham, MD 20706 USA.
[Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Xie, Y (reprint author), Sigma Space Corp, Lanham, MD 20706 USA.
EM yxie2u@gmail.com; Xiaoxiong.Xiong.1@gsfc.nasa.gov
FU National Aeronautics and Space Administration Goddard Space Flight
Center
FX The authors would like to thank the MODIS Characterization Support Team
of National Aeronautics and Space Administration Goddard Space Flight
Center for supporting this letter.
NR 19
TC 2
Z9 2
U1 0
U2 3
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 SEP
PY 2011
VL 8
IS 5
BP 993
EP 996
DI 10.1109/LGRS.2011.2147276
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 815RY
UT WOS:000294546900032
ER
PT J
AU Ma, J
Chung, TH
Burdick, J
AF Ma, Jeremy
Chung, Timothy H.
Burdick, Joel
TI A probabilistic framework for object search with 6-DOF pose estimation
SO INTERNATIONAL JOURNAL OF ROBOTICS RESEARCH
LA English
DT Article
DE Range sensing; recognition; sensing and perception computer vision;
visual tracking
ID VISUAL-ATTENTION
AB This article presents a systematic approach to the problem of autonomous 3D object search in indoor environments, using a two-wheeled non-holonomic robot equipped with an actuated stereo-camera head and processing done on a single laptop. A probabilistic grid-based map encodes the likelihood of object existence in each cell and is updated after each sensing action. The updating schema incorporates characteristic parameters modeled after the robot's sensing modalities and allows for sequential updating via Bayesian recursion methods. Two types of sensing modalities are used to update the map: a coarse search method (global search) based on a color histogram approach, and a more refined search method (local search) based on Scale-Invariant Feature Transform (SIFT) feature matching. If the local search correctly locates the desired object, its 6-DOF pose is estimated using stereo applied to each SIFT feature (i.e. 3D SIFT feature), which is then fed as measurements into an Extended Kalman Filter (EKF) for sustained tracking. If the local search fails to locate the desired object in a particular cell, the cell is updated in the probability map and the next peak probability cell is identified and planned to using a separate grid-based costmap populated via obstacle detection from stereo, with planning done using an A* planner. Experimental results obtained from the use of this method on a mobile robot are presented to illustrate and validate the approach, confirming that the search strategy can be carried out with modest computation on a single laptop.
C1 [Ma, Jeremy] Jet Prop Lab, Pasadena, CA 91109 USA.
[Chung, Timothy H.] Naval Postgrad Sch, Monterey, CA USA.
[Burdick, Joel] CALTECH, Pasadena, CA 91109 USA.
RP Ma, J (reprint author), Jet Prop Lab, 4800 Oak Grove Dr,M-S 198-235, Pasadena, CA 91109 USA.
EM Jeremy.C.Ma@jpl.nasa.gov
NR 23
TC 16
Z9 16
U1 0
U2 11
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0278-3649
EI 1741-3176
J9 INT J ROBOT RES
JI Int. J. Robot. Res.
PD SEP
PY 2011
VL 30
IS 10
SI SI
BP 1209
EP 1228
DI 10.1177/0278364911410090
PG 20
WC Robotics
SC Robotics
GA 814XT
UT WOS:000294491200002
ER
PT J
AU Stoop, J
Mishchenko, MI
Menguc, MP
Rothman, LS
AF Stoop, Jose
Mishchenko, Michael I.
Menguc, M. Pinar
Rothman, Laurence S.
TI SPECIAL ISSUE POLARIMETRIC DETECTION, CHARACTERIZATION, AND REMOTE
SENSING
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Editorial Material
C1 [Stoop, Jose] Elsevier, NL-1043 NX Amsterdam, Netherlands.
[Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Menguc, M. Pinar] Ozyegin Univ, Ctr Energy Environm & Econ, TR-34662 Istanbul, Turkey.
[Rothman, Laurence S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
RP Stoop, J (reprint author), Elsevier, Radarweg 29, NL-1043 NX Amsterdam, Netherlands.
EM J.Stoop@elsevier.com; mmishchenko@giss.nasa.gov;
pinar.menguc@ozyegin.edu.tr; lrothman@cfa.harvard.edu
RI Menguc, Pinar/O-3114-2013; Mishchenko, Michael/D-4426-2012
NR 1
TC 2
Z9 2
U1 0
U2 4
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 SEP
PY 2011
VL 112
IS 13
SI SI
BP 2041
EP 2041
DI 10.1016/j.jqsrt.2011.06.020
PG 1
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 815IC
UT WOS:000294518300001
ER
PT J
AU Mishchenko, MI
Videen, G
Rosenbush, VK
Yatskiv, YS
AF Mishchenko, Michael I.
Videen, Gorden
Rosenbush, Vera K.
Yatskiv, Yaroslav S.
TI Polarimetric detection, characterization, and remote sensing Preface
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Editorial Material
C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Videen, Gorden] USA, Res Lab, Adelphi, MD 20783 USA.
[Rosenbush, Vera K.; Yatskiv, Yaroslav S.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM mmishchenko@giss.nasa.gov
RI Mishchenko, Michael/D-4426-2012
NR 4
TC 1
Z9 1
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 SEP
PY 2011
VL 112
IS 13
SI SI
BP 2042
EP 2045
DI 10.1016/j.jqsrt.2011.04.004
PG 4
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 815IC
UT WOS:000294518300002
ER
PT J
AU Dlugach, JM
Mishchenko, MI
Liu, L
Mackowski, DW
AF Dlugach, Janna M.
Mishchenko, Michael I.
Liu, Li
Mackowski, Daniel W.
TI Numerically exact computer simulations of light scattering by densely
packed, random particulate media
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Review
DE Maxwell equations; Electromagnetic scattering; Opposition effects;
Coherent backscattering; Radiative transfer
ID COHERENT BACKSCATTERING; WEAK-LOCALIZATION; ELECTROMAGNETIC SCATTERING;
ENHANCED BACKSCATTERING; SPHERICAL-PARTICLES; MULTIPLE-SCATTERING;
MAXWELLS EQUATIONS; RADIATIVE-TRANSFER; POLARIZED-LIGHT; ABSORPTION
AB Direct computer simulations of electromagnetic scattering by discrete random media have become an active area of research. In this progress review, we summarize and analyze our main results obtained by means of numerically exact computer solutions of the macroscopic Maxwell equations. We consider finite scattering volumes with size parameters in the range [20,60], composed of varying numbers of randomly distributed particles with different refractive indices. The main objective of our analysis is to examine whether all backscattering effects predicted by the low-density theory of coherent backscattering (CB) also take place in the case of densely packed media. Based on our extensive numerical data we arrive at the following conclusions: (i) all backscattering effects predicted by the asymptotic theory of CB can also take place in the case of densely packed media; (ii) in the case of very large particle packing density, scattering characteristics of discrete random media can exhibit behavior not predicted by the low-density theories of CB and radiative transfer; (iii) increasing the absorptivity of the constituent particles can either enhance or suppress typical manifestations of CB depending on the particle packing density and the real part of the refractive index. Our numerical data strongly suggest that spectacular backscattering effects identified in laboratory experiments and observed for a class of high-albedo Solar System objects are caused by CB. Published by Elsevier Ltd.
C1 [Mishchenko, Michael I.; Liu, Li] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Dlugach, Janna M.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine.
[Mackowski, Daniel W.] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM mmishchenko@giss.nasa.gov
RI Mackowski, Daniel/K-1917-2013; Mishchenko, Michael/D-4426-2012
FU Ukrainian National Academy of Sciences; NASA
FX We acknowledge support from the Ukrainian National Academy of Sciences
under the Main Astronomical Observatory GRAPE/GPU/GRID computing cluster
project. This research was sponsored by the NASA Radiation Sciences
Program managed by Hal Maring and by the NASA Glory Mission project.
NR 70
TC 28
Z9 29
U1 2
U2 16
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 SEP
PY 2011
VL 112
IS 13
SI SI
BP 2068
EP 2078
DI 10.1016/j.jqsrt.2011.02.009
PG 11
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 815IC
UT WOS:000294518300005
ER
PT J
AU Mishchenko, MI
AF Mishchenko, Michael I.
TI Directional radiometry and radiative transfer: A new paradigm
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Review
DE Electromagnetic scattering; Directional radiometry; Radiative transfer;
Coherent backscattering; Optical particle characterization; Remote
sensing; Macroscopic Maxwell equations
ID DISCRETE RANDOM-MEDIA; COHERENT BACKSCATTERING; WEAK-LOCALIZATION;
POLARIZED-LIGHT; QUANTUM-THEORY; ELECTROMAGNETIC-WAVES; GALILEAN
SATELLITES; MAXWELL EQUATIONS; SCATTERING; PARTICLES
AB Measurements with directional radiometers and calculations based on the radiative transfer equation (RTE) have been at the very heart of weather and climate modeling and terrestrial remote sensing. The quantification of the energy budget of the Earth's climate system requires exquisite measurements and computations of the incoming and outgoing electromagnetic energy, while global characterization of climate system's components relies heavily on theoretical inversions of observational data obtained with various passive and active instruments. The same basic problems involving electromagnetic energy transport and its use for diagnostic and characterization purposes are encountered in numerous other areas of science, biomedicine, and engineering. Yet both the discipline of directional radiometry and the radiative transfer theory (RTT) have traditionally been based on phenomenological concepts many of which turn out to be profound misconceptions. Contrary to the widespread belief, a collimated radiometer does not, in general, measure the flow of electromagnetic energy along its optical axis, while the specific intensity does not quantify the amount of electromagnetic energy transported in a given direction.
The recently developed microphysical approach to radiative transfer and directional radiometry is explicitly based on the Maxwell equations and clarifies the physical nature of measurements with collimated radiometers and the actual content of the RTE. It reveals that the specific intensity has no fundamental physical meaning besides being a mathematical solution of the RTE, while the RTE itself is nothing more than an intermediate auxiliary equation. Only under special circumstances detailed in this review can the solution of the RTE be used to compute the time-averaged local Poynting vector as well as be measured by a collimated radiometer. These firmly established facts make the combination of the RTE and a collimated radiometer useful in a well-defined range of applications. However, outside the domain of validity of the FM the practical usefulness of measurements with collimated radiometers remains uncertain, while the theoretical modeling of these measurements and the solution of the energy-budget problem require a more sophisticated approach than solving the RTE. Published by Elsevier Ltd.
C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM mmishchenko@giss.nasa.gov
RI Mishchenko, Michael/D-4426-2012
FU NASA
FX I thank Brian Cairns, Joop Hovenier, Michael Kahnert, Nikolai Khlebtsov,
Pavel Litvinov, Dan Mackowski, Pinar Menguc, Victor Tishkovets, and
Larry Travis for numerous useful discussions and two anonymous reviewers
for helpful comments. This basic research was funded by the NASA
Radiation Sciences Program managed by Hal Maring and by the NASA Glory
Mission project.
NR 130
TC 14
Z9 14
U1 1
U2 14
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 SEP
PY 2011
VL 112
IS 13
SI SI
BP 2079
EP 2094
DI 10.1016/j.jqsrt.2011.04.006
PG 16
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 815IC
UT WOS:000294518300006
ER
PT J
AU Tishkovets, VP
Petrova, EV
Mishchenko, MI
AF Tishkovets, Victor P.
Petrova, Elena V.
Mishchenko, Michael I.
TI Scattering of electromagnetic waves by ensembles of particles and
discrete random media
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Review
DE Electromagnetic scattering; Multiple scattering; Coherent
backscattering; Radiative transfer; Discrete random media; Near-field
effects; Quasi-crystalline approximation
ID RADIATIVE-TRANSFER EQUATION; MATRIX REFERENCE DATABASE; SOLAR-SYSTEM
OBJECTS; COHERENT BACKSCATTERING; MULTIPLE-SCATTERING; T-MATRIX;
WEAK-LOCALIZATION; LIGHT-SCATTERING; SPHERICAL-PARTICLES;
POLARIZED-LIGHT
AB Current problems of the theory of multiple scattering of electromagnetic waves by discrete random media are reviewed, with an emphasis on densely packed media. All equations presented are based on the rigorous theory of electromagnetic scattering by an arbitrary system of non-spherical particles. The main relations are derived in the circular-polarization basis. By applying methods of statistical electromagnetics to a discrete random medium in the form of a plane-parallel layer, we transform these relations into equations describing the average (coherent) field and equations for the sums of ladder and cyclical diagrams in the framework of the quasi-crystalline approximation. The equation for the average field yields analytical expressions for the generalized Lorentz-Lorenz law and the generalized Ewald-Oseen extinction theorem, which are traditionally used for the calculation of the effective refractive index. By assuming that the particles are in the far-field zones of each other, we transform all equations asymptotically into the well-known equations for sparse media. Specifically, the equation for the sum of the ladder diagrams is reduced to the classical vector radiative transfer equation. We present a simple approximate solution of the equation describing the weak localization (WL) effect (i.e., the sum of cyclical diagrams) and validate it by using experimental and numerically exact theoretical data. Examples of the characteristics of WL as functions of the physical properties of a particulate medium are given. The applicability of the interference concept of WL to densely packed media is discussed using results of numerically exact computer solutions of the macroscopic Maxwell equations for large ensembles of spherical particles. These results show that theoretical predictions for spare media composed of non-absorbing or weakly absorbing particles are reasonably accurate if the particle packing density is less than similar to 30%. However, a further increase of the packing density and/or absorption may cause optical effects not predicted by the low-density theory and caused by near-field effects. The origin of the near-filed effects is discussed in detail. Published by Elsevier Ltd.
C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Tishkovets, Victor P.] NASU, Inst Radio Astron, UA-61002 Kharkov, Ukraine.
[Petrova, Elena V.] Space Res Inst RAS, Moscow 117997, Russia.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM crmim2@gmail.com
RI Mishchenko, Michael/D-4426-2012
FU NASA
FX We gratefully acknowledge extensive discussion with Anatoli Borovoi,
Zhanna Dlugach, Klaus Jockers, Nikolai Khlebtsov, Pavel Litvinov,
Anatoli Minakov, Gorden Videen, and many other colleagues. This research
was sponsored in part by the NASA Radiation Sciences Program managed by
Hal Maring.
NR 113
TC 33
Z9 33
U1 4
U2 30
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 SEP
PY 2011
VL 112
IS 13
SI SI
BP 2095
EP 2127
DI 10.1016/j.jqsrt.2011.04.010
PG 33
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 815IC
UT WOS:000294518300007
ER
PT J
AU Kalashnikova, OV
Garay, MJ
Davis, AB
Diner, DJ
Martonchik, JV
AF Kalashnikova, Olga V.
Garay, Michael J.
Davis, Anthony B.
Diner, David J.
Martonchik, John V.
TI Sensitivity of multi-angle photo-polarimetry to vertical layering and
mixing of absorbing aerosols: Quantifying measurement uncertainties
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Absorbing aerosols; Vertical layering; Photo-polarimetry
ID OPTICAL-DEPTH; OCEAN; SCATTERING; RETRIEVAL; POLARIZATION; VARIABILITY;
ABSORPTION; ATMOSPHERE; MIXTURES; MISSION
AB The impact of tropospheric aerosols on climate can vary greatly based upon relatively small variations in aerosol properties, such as composition, shape and size distributions, as well as vertical layering. Polarimetric measurements have been advocated in recent years as an additional tool to better understand and retrieve the aerosol properties needed for improved predictions of aerosol radiative forcing on climate. The goal of this study is to introduce a formal approach to assessing the sensitivity of both intensity and polarization signals to absorbing aerosol layering, explicitly accounting for instrument measurement uncertainties. If ignored, sensitivity to aerosol height can introduce biases in aerosol property retrievals at short (ultraviolet or blue) wavelengths; if properly exploited, it may enable the extraction of some basic information on aerosol profiles. Employing a vector successive-orders-of-scattering (SOS) radiative transfer code, we conducted modeling experiments to determine how the measured Stokes vector elements are affected at 446 nm (blue band) by the vertical distribution, mixing and layering of smoke and dust aerosols under the assumption of a simple Lambertian surface and predefined aerosol microphysical properties. We find that smoke and dust vertical layering, if ignored, can introduce biases in radiometric and polarimetric aerosol property retrievals for aerosol optical depth (AOD) above 0.3 (polarimetric) and ADD above 0.5 (radiometric), and should, therefore, be accounted for in retrievals at high aerosol loadings. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Kalashnikova, Olga V.; Garay, Michael J.; Davis, Anthony B.; Diner, David J.; Martonchik, John V.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Garay, Michael J.] Raytheon Co, Pasadena, CA USA.
RP Kalashnikova, OV (reprint author), CALTECH, Jet Prop Lab, MS 169-237,Oak Grove Dr, Pasadena, CA 91125 USA.
EM Olga.Kalashnikova@jpl.nasa.gov
FU NASA
FX We thank Prof. Irina Sokolik for providing dust refractive indices that
were used as part of this study, and Dr. Oleg Dubovik for providing dust
size distributions inferred from AERONET retrievals and the AERONET
numerical tool. We thank the MISR team for providing facilities and
useful discussions. This work was performed at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA.
NR 48
TC 10
Z9 10
U1 0
U2 6
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 SEP
PY 2011
VL 112
IS 13
SI SI
BP 2149
EP 2163
DI 10.1016/j.jqsrt.2011.05.010
PG 15
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 815IC
UT WOS:000294518300010
ER
PT J
AU Kolokolova, L
Liu, L
Buratti, B
Mishchenko, MI
AF Kolokolova, Ludmilla
Liu, Li
Buratti, Bonnie
Mishchenko, Michael I.
TI Modeling variations in near-infrared spectra caused by the coherent
backscattering effect
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Coherent backscattering; Cassini mission; Near-infrared spectra; Icy
satellites; Modeling; T-matrix method
ID DISCRETE RANDOM MEDIUM; RANDOM-MEDIA; BIDIRECTIONAL REFLECTANCE; MAPPING
SPECTROMETER; SPHERICAL-PARTICLES; PLANETARY REGOLITHS;
MULTIPLE-SCATTERING; ENHANCEMENT FACTORS; WEAK-LOCALIZATION; PHASE-ANGLE
AB We study a new optical effect, a spectral manifestation of coherent backscattering, which reveals itself as systematic variations in the depth of absorption bands with changing phase angle. We used Cassini VIMS near-infrared spectra of Saturn's icy satellite Rhea in order to identify and characterize the spectral change with phase angle, focusing on the change in the depth of water-ice absorption bands. To model realistic characteristics of the surfaces of icy satellites, which are most likely covered by micron-sized densely packed particles, we perform simulations using a theoretical approach based on direct computer solutions of the macroscopic Maxwell equations. Our results show that this approach can reproduce the observed phase-angle variations in the depth of the absorption bands. The modeled changes in the absorption bands are strongly affected by physical properties of the regolith, especially by the size and packing density of the ice particles. Thus, the phase-angle spectral variations demonstrate a promising remote-sensing capability for studying properties of the surfaces of icy bodies and other objects that exhibit a strong coherent backscattering effect. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Kolokolova, Ludmilla] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Liu, Li] Columbia Univ, New York, NY 10025 USA.
[Buratti, Bonnie] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Kolokolova, L (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM ludmilla@astro.umd.edu
RI Mishchenko, Michael/D-4426-2012
FU NATO ASI; NASA
FX L. Kolokolova highly appreciates the NATO ASI travel grant. The research
by L. Liu and M. Mishchenko was partially supported by the NASA
Radiation Sciences Program managed by Hal Maring.
NR 46
TC 7
Z9 7
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 SEP
PY 2011
VL 112
IS 13
SI SI
BP 2175
EP 2181
DI 10.1016/j.jqsrt.2011.03.010
PG 7
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 815IC
UT WOS:000294518300012
ER
PT J
AU Mackowski, DW
Mishchenko, MI
AF Mackowski, D. W.
Mishchenko, M. I.
TI A multiple sphere T-matrix Fortran code for use on parallel computer
clusters
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE T-matrix method; Multiple sphere scattering; Numerical methods
ID REFERENCE DATABASE; SCATTERING
AB A general-purpose Fortran-90 code for calculation of the electromagnetic scattering and absorption properties of multiple sphere clusters is described. The code can calculate the efficiency factors and scattering matrix elements of the cluster for either fixed or random orientation with respect to the incident beam and for plane wave or localized-approximation Gaussian incident fields. In addition, the code can calculate maps of the electric field both interior and exterior to the spheres. The code is written with message passing interface instructions to enable the use on distributed memory compute clusters, and for such platforms the code can make feasible the calculation of absorption, scattering, and general EM characteristics of systems containing several thousand spheres. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Mackowski, D. W.] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
[Mishchenko, M. I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Mackowski, DW (reprint author), Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
EM mackodw@auburn.edu
RI Mackowski, Daniel/K-1917-2013; Mishchenko, Michael/D-4426-2012
NR 21
TC 113
Z9 116
U1 1
U2 18
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 SEP
PY 2011
VL 112
IS 13
SI SI
BP 2182
EP 2192
DI 10.1016/j.jqsrt.2011.02.019
PG 11
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 815IC
UT WOS:000294518300013
ER
PT J
AU Kidd, C
Huffman, G
AF Kidd, Chris
Huffman, George
TI Global precipitation measurement
SO METEOROLOGICAL APPLICATIONS
LA English
DT Review
DE precipitation; satellite observations; infrared; microwave
ID RAINFALL MEASURING MISSION; MICROWAVE SOUNDING UNIT; SATELLITE INFRARED
TECHNIQUE; MARITIME CONVECTIVE CLOUDS; ARTIFICIAL NEURAL-NETWORKS;
COMBINED PASSIVE MICROWAVE; WEATHER PREDICTION MODEL; DENSITY GAUGE
DATASET; TROPICAL RAINFALL; PART I
AB The quantification of precipitation on a global scale is critical for applications ranging from climate monitoring to water resource management. Conventional observations through surface gauge networks provide the most direct measure of precipitation, although these are very much limited to land areas, with very few in situ measurements over the oceans. Weather radars, although providing a spatial measure of precipitation, are limited in extent and number. Satellite observations offer an unrivalled vantage point to observe precipitation on a global basis. Since precipitation is spatially and temporally highly variable, satellites are able to provide temporal and spatial samples commensurate with many precipitation characteristics. This paper provides an overall review of global precipitation estimation, providing an outline of conventional measurements, the basis of the satellite systems used in the observation of precipitation, and the generation, availability and validation of the derived precipitation products. Finally, future satellite precipitation missions are presented. Copyright (C) 2011 Royal Meteorological Society
C1 [Kidd, Chris] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Kidd, Chris] NASA, Goddard Space Flight Ctr, College Pk, MD 20740 USA.
[Huffman, George] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Huffman, George] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kidd, C (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
EM chris.kidd@nasa.gov
RI Huffman, George/F-4494-2014; Kidd, Christopher/H-9910-2014
OI Huffman, George/0000-0003-3858-8308;
NR 205
TC 53
Z9 55
U1 6
U2 41
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1350-4827
J9 METEOROL APPL
JI Meteorol. Appl.
PD SEP
PY 2011
VL 18
IS 3
SI SI
BP 334
EP 353
DI 10.1002/met.284
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 813WN
UT WOS:000294401000007
ER
PT J
AU Wei, SJ
Fielding, E
Leprince, S
Sladen, A
Avouac, JP
Helmberger, D
Hauksson, E
Chu, RS
Simons, M
Hudnut, K
Herring, T
Briggs, R
AF Wei, Shengji
Fielding, Eric
Leprince, Sebastien
Sladen, Anthony
Avouac, Jean-Philippe
Helmberger, Don
Hauksson, Egill
Chu, Risheng
Simons, Mark
Hudnut, Kenneth
Herring, Thomas
Briggs, Richard
TI Superficial simplicity of the 2010 El Mayor-Cucapah earthquake of Baja
California in Mexico
SO NATURE GEOSCIENCE
LA English
DT Article
ID LANDERS EARTHQUAKE; SATELLITE IMAGES; RUPTURE; SLIP; FAULT; DEFORMATION;
AFTERSHOCKS; INVERSION; SUMATRA
AB The geometry of faults is usually thought to be more complicated at the surface than at depth and to control the initiation, propagation and arrest of seismic ruptures(1-6). The fault system that runs from southern California into Mexico is a simple strike-slip boundary: the west side of California and Mexico moves northwards with respect to the east. However, the M-w 7.2 2010 El Mayor-Cucapah earthquake on this fault system produced a pattern of seismic waves that indicates a far more complex source than slip on a planar strike-slip fault(7). Here we use geodetic, remote-sensing and seismological data to reconstruct the fault geometry and history of slip during this earthquake. We find that the earthquake produced a straight 120-km-long fault trace that cut through the Cucapah mountain range and across the Colorado River delta. However, at depth, the fault is made up of two different segments connected by a small extensional fault. Both segments strike N130 degrees E, but dip in opposite directions. The earthquake was initiated on the connecting extensional fault and 15 s later ruptured the two main segments with dominantly strike-slip motion. We show that complexities in the fault geometry at depth explain well the complex pattern of radiated seismic waves. We conclude that the location and detailed characteristics of the earthquake could not have been anticipated on the basis of observations of surface geology alone.
C1 [Wei, Shengji; Leprince, Sebastien; Sladen, Anthony; Avouac, Jean-Philippe; Helmberger, Don; Hauksson, Egill; Chu, Risheng; Simons, Mark; Hudnut, Kenneth] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Fielding, Eric] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sladen, Anthony] Univ Nice Sophia Antipolis, CNRS, IRD, Observ Cote Azur, F-06103 Nice 2, France.
[Hudnut, Kenneth] US Geol Survey, Pasadena, CA 91106 USA.
[Herring, Thomas] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Briggs, Richard] US Geol Survey, Golden, CO 80401 USA.
RP Wei, SJ (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM shjwei@caltech.edu
RI Briggs, Richard/A-1348-2013; Hudnut, Kenneth/B-1945-2009; Simons,
Mark/N-4397-2015; Avouac, Jean-Philippe/B-5699-2015; Wei,
Shengji/M-2137-2015; Fielding, Eric/A-1288-2007; Sladen,
Anthony/A-2532-2017
OI Briggs, Richard/0000-0001-8108-0046; Hudnut,
Kenneth/0000-0002-3168-4797; Simons, Mark/0000-0003-1412-6395; Avouac,
Jean-Philippe/0000-0002-3060-8442; Wei, Shengji/0000-0002-0319-0714;
Fielding, Eric/0000-0002-6648-8067; Sladen, Anthony/0000-0003-4126-0020
FU NSF [EAR-0529922]; USGS [07HQAG0008]; Gordon and Betty Moore Foundation;
NASA; SCEC
FX This work was financially supported by NSF, USGS, the Gordon and Betty
Moore Foundation, NASA and SCEC. Regional seismic data were provided by
SCSN and RESNOM. The Incorporated Research Institutions for Seismology
(IRIS) Data Management System (DMS) was used to access the Global
Seismographic Network data. The GPS analyses were obtained from the
Earthscope PBO data products system and UNAVCO. Optical data were
provided by USGS. Envisat data are copyright 2009, 2010 ESA and were
obtained from the WInSAR archive and the Group on Earth Observation
Geohazards Supersite virtual archive. ALOS data are copyright METI, JAXA
and were obtained from the Alaska Satellite Facility Level 1 Data Pool.
Part of this research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology under contract with the National
Aeronautics and Space Administration. We thank CICESE colleagues J.
Gonzalez and J. Fletcher for their support and interest, and we thank J.
Hollingsworth for his suggestions to improve the figures. This is
Tectonics Observatory contribution #172. SCEC is funded by NSF
Cooperative Agreement EAR-0529922 and USGS Cooperative Agreement
07HQAG0008.
NR 26
TC 87
Z9 88
U1 2
U2 26
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
EI 1752-0908
J9 NAT GEOSCI
JI Nat. Geosci.
PD SEP
PY 2011
VL 4
IS 9
BP 615
EP 618
DI 10.1038/ngeo1213
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 814KY
UT WOS:000294452400010
ER
PT J
AU Yong, A
Hough, SE
Cox, BR
Rathje, EM
Bachhuber, J
Dulberg, R
Hulslander, D
Christiansen, L
Abrams, MJ
AF Yong, Alan
Hough, Susan E.
Cox, Brady R.
Rathje, Ellen M.
Bachhuber, Jeff
Dulberg, Ranon
Hulslander, David
Christiansen, Lisa
Abrams, Michael J.
TI Seismic-zonation of Port-au-Prince Using Pixel- and Object-based Imaging
Analysis Methods on ASTER GDEM
SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING
LA English
DT Article
ID SATELLITE DATA; DEM; PAKISTAN
AB We report about a preliminary study to evaluate the use of semi-automated imaging analysis of remotely-sensed DEM and field geophysical measurements to develop a seismic-zonation map of Port-au-Prince, Haiti. For in situ data, V(s)30 values are derived from the MASW technique deployed in and around the city. For satellite imagery, we use an ASTER GDEM of Hispaniola. We apply both pixel- and object-based imaging methods on the ASTER GDEM to explore local topography (absolute elevation values) and classify terrain types such as mountains, alluvial fans and basins/near-shore regions. We assign NEHRP seismic site class ranges based on available V(s)30 values. A comparison of results from imagery-based methods to results from traditional geologic-based approaches reveals good overall correspondence. We conclude that image analysis of RS data provides reliable first-order site characterization results in the absence of local data and can be useful to refine detailed site maps with sparse local data.
C1 [Yong, Alan; Hough, Susan E.] US Geol Survey, Earthquake Sci Ctr, Pasadena, CA 91106 USA.
[Cox, Brady R.] Univ Arkansas, Dept Civil Engn, Fayetteville, AR 72701 USA.
[Rathje, Ellen M.] Univ Texas Austin, Dept Civil Architecture & Environm Engn, Austin, TX 78712 USA.
[Bachhuber, Jeff; Dulberg, Ranon] Fugro William Lettis & Associates, Walnut Creek, CA 94596 USA.
[Hulslander, David] ITT VIS, Boulder, CO 80305 USA.
[Christiansen, Lisa] CALTECH, Pasadena, CA 91125 USA.
[Abrams, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Yong, A (reprint author), US Geol Survey, Earthquake Sci Ctr, 525 S Wilson Ave, Pasadena, CA 91106 USA.
EM yong@usgs.gov
FU US Agency for International Development - Office of Foreign Disaster
Assistance (USAid-OFDA)
FX We thank the US Agency for International Development - Office of Foreign
Disaster Assistance (USAid-OFDA) for their partial support. Work done by
Michael J. Abrams was performed at the Jet Propulsion
Laboratory/California Institute of Technology under a contract to the
National Aeronautics and Space Administration. ASTER GDEM is a product
of the Japan Ministry of Economy, Trade and Industry and the United
States National Aeronautics and Space Administration. We are grateful
for the beneficial remarks from USGS reviewers Robert S. Dollar and
Sinan Akciz, in addition to insightful comments by three anonymous
journal referees.
NR 42
TC 2
Z9 2
U1 1
U2 6
PU AMER SOC PHOTOGRAMMETRY
PI BETHESDA
PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA
SN 0099-1112
J9 PHOTOGRAMM ENG REM S
JI Photogramm. Eng. Remote Sens.
PD SEP
PY 2011
VL 77
IS 9
SI SI
BP 909
EP 921
PG 13
WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing;
Imaging Science & Photographic Technology
SC Physical Geography; Geology; Remote Sensing; Imaging Science &
Photographic Technology
GA 812VQ
UT WOS:000294321400008
ER
PT J
AU McWilliams, ST
Lang, RN
Baker, JG
Thorpe, JI
AF McWilliams, Sean T.
Lang, Ryan N.
Baker, John G.
Thorpe, James Ira
TI Sky localization of complete inspiral-merger-ringdown signals for
nonspinning massive black hole binaries
SO PHYSICAL REVIEW D
LA English
DT Article
ID WAVE STANDARD SIRENS; GRAVITATIONAL-WAVES; GALACTIC-CENTER; STELLAR
ORBITS; LISA
AB We investigate the capability of LISA to measure the sky position of equal-mass, nonspinning black hole binaries, combining for the first time the entire inspiral-merger-ringdown signal, the effect of the LISA orbits, and the complete three-channel LISA response. We consider an ensemble of systems near the peak of LISA's sensitivity band, with total rest mass of 2 X 10(6) M(circle dot), a redshift of z = 1, and randomly chosen orientations and sky positions. We find median sky localization errors of approximately similar to 3 arcminutes. This is comparable to the field of view of powerful electromagnetic telescopes, such as the James Webb Space Telescope, that could be used to search for electromagnetic signals associated with merging massive black holes. We investigate the way in which parameter errors decrease with measurement time, focusing specifically on the additional information provided during the merger-ringdown segment of the signal. We find that this information improves all parameter estimates directly, rather than through diminishing correlations with any subset of well-determined parameters. Although we have employed the baseline LISA design for this study, many of our conclusions regarding the information provided by mergers will be applicable to alternative mission designs as well.
C1 [McWilliams, Sean T.; Lang, Ryan N.; Baker, John G.; Thorpe, James Ira] NASA, Gravitat Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McWilliams, Sean T.] Columbia Univ, ISCAP, New York, NY 10027 USA.
[McWilliams, Sean T.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
RP McWilliams, ST (reprint author), NASA, Gravitat Astrophys Lab, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM sean@astro.columbia.edu
RI Thorpe, James/D-3150-2012
FU NASA [08-ATFP08-0126]; Oak Ridge Associated Universities
FX We thank Tuck Stebbins for helpful discussions and Bernard Kelly for his
thorough review of the manuscript. We acknowledge the support of NASA
Grant No. 08-ATFP08-0126. R. N. L. was supported by Oak Ridge Associated
Universities. The simulations were carried out using resources from the
NASA Center for Computational Sciences (Goddard Space Flight Center).
NR 47
TC 6
Z9 6
U1 0
U2 1
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 SEP 1
PY 2011
VL 84
IS 6
AR 064003
DI 10.1103/PhysRevD.84.064003
PG 9
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 813YE
UT WOS:000294405500011
ER
PT J
AU Gao, YH
Xue, YK
Peng, W
Kang, HS
Waliser, D
AF Gao Yanhong
Xue, Yongkang
Peng Wen
Kang, Hyun-Suk
Waliser, Duane
TI Assessment of dynamic downscaling of the extreme rainfall over East Asia
using a regional climate model
SO ADVANCES IN ATMOSPHERIC SCIENCES
LA English
DT Article
DE DDM; MM5; cumulus convection scheme; land parameterization;
re-initialization; lateral boundary location
ID CONVECTIVE PARAMETERIZATION SCHEMES; SUMMER MONSOON PRECIPITATION;
LAND-SURFACE PROCESSES; PART I; BOUNDARY-LAYER; TIBETAN PLATEAU;
MESOSCALE-MODEL; SOIL HYDROLOGY; RIVER VALLEY; WEST-AFRICA
AB This study investigates the capability of the dynamic downscaling method (DDM) in an East Asian climate study for June 1998 using the fifth-generation Pennsylvania State University-National Center for Atmospheric Research non-hydrostatic Mesoscale Model (MM5). Sensitivity experiments show that MM5 results at upper atmospheric levels cannot match reanalyses data, but the results show consistent improvement in simulating moisture transport at low levels. The downscaling ability for precipitation is regionally dependent. During the monsoon season over the Yangtze River basin and the pre-monsoon season over North China, the DDM cannot match observed precipitation. Over Northwest China and the Tibetan Plateau (TP), where there is high topography, the DDM shows better performance than reanalyses. Simulated monsoon evolution processes over East Asia, however, are much closer to observational data than reanalyses. The convection scheme has a substantial impact on extreme rainfall over the Yangtze River basin and the pre-monsoon over North China, but only a marginal contribution for Northwest China and the TP. Land surface parameterizations affect the locations and pattern of rainfall bands. The 10-day re-initialization in this study shows some improvement in simulated precipitation over some sub-regions but with no obvious improvement in circulation. The setting of the location of lateral boundaries (LLB) westward improves performance of the DDM. Including the entire TP in the western model domain improves the DDM performance in simulating precipitation in most sub-regions. In addition, a seasonal simulation demonstrates that the DDM can also obtain consistent results, as in the June case, even when another two months consist of no strong climate/weather events.
C1 [Gao Yanhong; Peng Wen] Chinese Acad Sci, Cold & Arid Reg Environm & Engn Res Inst, Lab Climate Environm & Disasters Western China, Lanzhou 730000, Peoples R China.
[Xue, Yongkang] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90024 USA.
[Xue, Yongkang] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90024 USA.
[Waliser, Duane] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Gao, YH (reprint author), Chinese Acad Sci, Cold & Arid Reg Environm & Engn Res Inst, Lab Climate Environm & Disasters Western China, Lanzhou 730000, Peoples R China.
EM gaoyh@lzb.ac.cn
RI AAS, AAS/C-2949-2014;
OI gao, yan hong/0000-0002-0403-2929
FU Chinese Academy of Sciences [KZCX2-YW-328]; National Key Basic Research
Program [2005CB422003]; National Science Foundation Center of China
(NSFC) [40871001]; US JPL [1278492]; NOAA [NA07OAR4310226,
NA08OAR4310591]
FX The GAME reanalysis project was conducted by the Meteorological Research
Institute, Japan Meteorological Agency, and Earth Observation Research
Center/National Space Development Agency of Japan. The station rainfall
data were provided by the China Meteorological Data Sharing Service
Center. The authors are grateful to the APHRODITE project for providing
the newly released daily precipitation datasets with high-resolution
grids. We also thank Mr. Ratko Vasic of NCEP for his help with MM5/SSiB
coupling. This research is jointly supported by the funding of the Key
Program of the Chinese Academy of Sciences (Grant No. KZCX2-YW-328), the
National Key Basic Research Program (2005CB422003), National Science
Foundation Center of China (NSFC) (40871001), the US JPL Grant No.
1278492, NOAA Grant Nos. NA07OAR4310226 and NA08OAR4310591.
NR 79
TC 11
Z9 14
U1 1
U2 22
PU SCIENCE PRESS
PI BEIJING
PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA
SN 0256-1530
EI 1861-9533
J9 ADV ATMOS SCI
JI Adv. Atmos. Sci.
PD SEP
PY 2011
VL 28
IS 5
BP 1077
EP 1098
DI 10.1007/s00376-010-0039-7
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 809PI
UT WOS:000294068800010
ER
PT J
AU Crucian, B
Stowe, R
Quiriarte, H
Pierson, D
Sams, C
AF Crucian, Brian
Stowe, Raymond
Quiriarte, Heather
Pierson, Duane
Sams, Clarence
TI Monocyte Phenotype and Cytokine Production Profiles Are Dysregulated by
Short-Duration Spaceflight
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Article
DE gravity; immune system; innate immunity
ID IMMUNE-SYSTEM DYSREGULATION; HLA-DR EXPRESSION; SPACE-FLIGHT;
SIGNAL-TRANSDUCTION; MISSION DURATION; T-LYMPHOCYTES; ASTRONAUTS;
MICROGRAVITY; REACTIVATION; EXPLORATION
AB Introduction: Immune system dysregulation has been demonstrated to occur during and immediately following spaceflight. As the initial bias and magnitude for an immune response is heavily influenced by monocyte/macrophage secreted cytokines, this study investigated monocyte phenotype and cytokine production patterns following short-duration spaceflight. Methods: Secreted cytokine profiles were examined by cytometric bead array analysis of culture supernatants following whole blood culture activation with LPS or PMA+ionomycin. Nine short-duration Space Shuttle crewmembers participated in this study. Results: Peripheral monocyte percentages were unaltered postflight. Constitutive monocyte expression of both CD62L and HLA-DR was reduced following spaceflight in a mission-specific fashion. Loss of either molecule indicates a functional disability of monocytes, either by inhibition of adhesion and tissue migration (CD62L) or by impaired antigen presentation (HLA-DR). Following LPS stimulation of monocytes, postflight expression of IL-6, TNF alpha, and IL-10 were significantly reduced (by 43%, 44%, and 41%, respectively) and expression of IL-1b was elevated (65%). IL-8 production was either elevated or reduced in a mission-specific fashion. Following PMA+ionomycin stimulation of all leukocyte populations, only expression of IL-6 was significantly reduced postflight. Discussion: These data indicate that changes in monocyte constitutive phenotype and inflammatory cytokine production occur following short-duration spaceflight, which may impact overall crewmember immunocompetence. Also, monocyte/macrophage function may be highly sensitive to mission specific parameters.
C1 [Crucian, Brian; Stowe, Raymond; Quiriarte, Heather; Pierson, Duane; Sams, Clarence] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Crucian, B (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM brian.crucian-1@nasa.gov
FU NASA [NAS9-01006, NNJ06HB73A]; JSC Clinical Laboratory
FX This work was funded by NASA grants NAS9-01006 and NNJ06HB73A to R.P.S.
The authors wish to thank the crews of Shuttle missions STS-124,
STS-125, and STS-126 for participating in this study. The authors also
wish to acknowledge the support provided by the JSC Clinical Laboratory,
JSC Mission Integration Team, and KSC Baseline Data Collection Facility
during this study. The authors are also grateful for technical support
provided by Mimi Shao at the Kennedy Space Center, Baseline Data
Collection Facility. Assistance with statistical analysis was provided
by Dr. Al Feiveson, NASA-JSC.
NR 36
TC 21
Z9 27
U1 0
U2 10
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD SEP
PY 2011
VL 82
IS 9
BP 857
EP 862
DI 10.3357/ASEM.3047.2011
PG 6
WC Public, Environmental & Occupational Health; Medicine, General &
Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
Medicine; Sport Sciences
GA 812EH
UT WOS:000294273400001
PM 21888268
ER
PT J
AU Minard, CG
de Carvalho, MF
Iyengar, MS
AF Minard, Charles G.
de Carvalho, Mary Freire
Iyengar, M. Sriram
TI Optimizing Medical Resources for Spaceflight Using the Integrated
Medical Model
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Article
DE Monte Carlo; simulation; multi-objective; spaceflight; medical kit
ID SPACE-STATION
AB Introduction: Efficient allocation of medical resources for spaceflight is important for crew health. The Integrated Medical Model (IMM) was developed to estimate medical event occurrences, mitigation, and resource requirements. An optimization module was created for IMM that uses a systematic process of elimination and preservation to maximize crew health outcomes subject to resource constraints. Methods: A maximum medical kit is identified and resources are eliminated according to their relative impact on outcomes of interest. Additional steps allow opportunities for resources to be added back into the medical kit if possible. The effectiveness of the module is demonstrated under six alternative mission profiles by optimizing the medical kit to maximize the expected Crew Health Index (CHI), and comparisons are made with minimum and maximum kits. Results: The optimum and maximum kits had similar expected CHI, but CHI was more variable for the optimum kit. The maximum kit resulted in the best outcomes, but required at least 13.7 times the mass of the optimum kit and 26.6 times the volume. The largest difference in mean CHI between the optimum and maximum kits occurred for four crewmembers on a 180-d mission (91.1% vs. 95.4%). Conclusions: The optimization module may be used as an objective tool to assist with the efficient allocation of medical resources for spaceflight. The module provides a flexible algorithm that may be used in conjunction with the IMM model to assist in medical kit requirements and design.
C1 [Minard, Charles G.; de Carvalho, Mary Freire; Iyengar, M. Sriram] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Minard, CG (reprint author), 1290 Hercules Blvd, Houston, TX 77058 USA.
EM charles.g.minard@nasa.gov
FU NASA Bioastronautics [NAS9-02078]
FX This work was funded, in part, by the NASA Bioastronautics contract
NAS9-02078. The authors would like to thank Eric Kerstman, M.D., Douglas
Butler, Jerry Myers, Ph.D., Marlei Walton, Ph.D., Lynn Saile, Vilma
Lopez, Grandin Bickham, Kristina Barsten, David Baumann, Mary Fitts, and
Kathy Johnson-Throop, Ph.D., for their contributions to the Integrated
Medical Model effort.
NR 14
TC 5
Z9 5
U1 0
U2 3
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD SEP
PY 2011
VL 82
IS 9
BP 890
EP 894
DI 10.3357/ASEM.3028.2011
PG 5
WC Public, Environmental & Occupational Health; Medicine, General &
Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
Medicine; Sport Sciences
GA 812EH
UT WOS:000294273400006
PM 21888273
ER
PT J
AU Shen, BW
Tao, WK
Green, B
AF Shen, Bo-Wen
Tao, Wei-Kuo
Green, Bryan
TI Coupling Advanced Modeling and Visualization to Improve High-Impact
Tropical Weather Prediction
SO COMPUTING IN SCIENCE & ENGINEERING
LA English
DT Article
ID GENERAL-CIRCULATION MODEL
C1 [Shen, Bo-Wen] Univ Maryland, College Pk, MD 20742 USA.
[Tao, Wei-Kuo] NASA, Goddard Space Flight Ctr, Washington, DC USA.
RP Shen, BW (reprint author), Univ Maryland, College Pk, MD 20742 USA.
EM bowen.shen@gmail.com; wei-kuo.tao-1@nasa.gov; bryan@grid-net.com
FU NASA Earth Science Technology Office; Advanced Information Systems
Technology Program; US National Science Foundation Science and
Technology Center; NASA; Energy and Water Cycle Study; NASA Advanced
Supercomputing facility at Ames Research Center; NASA Center for
Computational Science at Goddard Space Flight Center
FX We thank the reviewers for their valuable suggestions, which have
substantially improved this article. We're also grateful to the
following organizations for their support: the NASA Earth Science
Technology Office; the Advanced Information Systems Technology Program;
the US National Science Foundation Science and Technology Center; the
NASA Modeling, Analysis Prediction Program; the Energy and Water Cycle
Study; the NASA High-End Computing Program; the NASA Advanced
Supercomputing facility at Ames Research Center; and the NASA Center for
Computational Science at Goddard Space Flight Center. Finally, we thank
Steve Lang for proofreading this manuscript.
NR 15
TC 4
Z9 5
U1 0
U2 0
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 1521-9615
J9 COMPUT SCI ENG
JI Comput. Sci. Eng.
PD SEP-OCT
PY 2011
VL 13
IS 5
BP 56
EP 67
DI 10.1109/MCSE.2010.141
PG 12
WC Computer Science, Interdisciplinary Applications
SC Computer Science
GA 809ZW
UT WOS:000294096200007
ER
PT J
AU Bolton, ML
Siminiceanu, RI
Bass, EJ
AF Bolton, Matthew L.
Siminiceanu, Radu I.
Bass, Ellen J.
TI A Systematic Approach to Model Checking Human-Automation Interaction
Using Task Analytic Models
SO IEEE TRANSACTIONS ON SYSTEMS MAN AND CYBERNETICS PART A-SYSTEMS AND
HUMANS
LA English
DT Article
DE Formal methods; human-automation interaction; model checking; task
analysis
ID OPERATOR FUNCTION; FORMAL METHODS; METHODOLOGY; DESIGN
AB Formal methods are typically used in the analysis of complex system components that can be described as "automated" (digital circuits, devices, protocols, and software). Humanautomation interaction has been linked to system failure, where problems stem from human operators interacting with an automated system via its controls and information displays. As part of the process of designing and analyzing human-automation interaction, human factors engineers use task analytic models to capture the descriptive and normative human operator behavior. In order to support the integration of task analyses into the formal verification of larger system models, we have developed the enhanced operator function model (EOFM) as an Extensible Markup Language-based, platform-and analysis-independent language for describing task analytic models. We present the formal syntax and semantics of the EOFM and an automated process for translating an instantiated EOFM into the model checking language Symbolic Analysis Laboratory. We present an evaluation of the scalability of the translation algorithm. We then present an automobile cruise control example to illustrate how an instantiated EOFM can be integrated into a larger system model that includes environmental features and the human operator's mission. The system model is verified using model checking in order to analyze a potentially hazardous situation related to the human-automation interaction.
C1 [Bolton, Matthew L.] San Jose State Univ, Res Fdn, Natl Aeronaut & Space Adm, Ames Res Ctr, Mountain View, CA 94043 USA.
[Siminiceanu, Radu I.] NIA, Hampton, VA 23666 USA.
[Bass, Ellen J.] Univ Virginia, Dept Syst & Informat Engn, Charlottesville, VA 22904 USA.
RP Bolton, ML (reprint author), San Jose State Univ, Res Fdn, Natl Aeronaut & Space Adm, Ames Res Ctr, Mountain View, CA 94043 USA.
EM mlb4b@virginia.edu; radu@nianet.org; ejb4n@virginia.edu
RI Bolton, Matthew/G-5199-2012; Bolton, Matthew/A-6390-2016
FU National Library of Medicine [T15LM009462]; National Aeronautics and
Space Administration (NASA) Cooperative Agreement [NCC1002043]; NASA
[NNA10DE79C]
FX Manuscript received January 11, 2010; revised August 17, 2010; accepted
November 26, 2010. Date of publication March 22, 2011; date of current
version August 23, 2011. This work was supported in part by the National
Library of Medicine under Grant T15LM009462, by the National Aeronautics
and Space Administration (NASA) Cooperative Agreement NCC1002043, and by
the NASA Contract NNA10DE79C. This paper was recommended by Associate
Editor M. Dorneich.
NR 60
TC 27
Z9 27
U1 0
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1083-4427
EI 1558-2426
J9 IEEE T SYST MAN CY A
JI IEEE Trans. Syst. Man Cybern. Paart A-Syst. Hum.
PD SEP
PY 2011
VL 41
IS 5
SI SI
BP 961
EP 976
DI 10.1109/TSMCA.2011.2109709
PG 16
WC Computer Science, Cybernetics; Computer Science, Theory & Methods
SC Computer Science
GA 810OJ
UT WOS:000294134300013
ER
PT J
AU Giardino, MJ
AF Giardino, Marco J.
TI A history of NASA remote sensing contributions to archaeology
SO JOURNAL OF ARCHAEOLOGICAL SCIENCE
LA English
DT Article
DE NASA; Stennis space center; Archaeology Remote sensing; History;
Hyperspectral
AB During its long history of developing and deploying remote sensing instruments, NASA has provided scientific data that have benefitted a variety of scientific applications among them archaeology. Multispectral and hyperspectral instruments mounted on orbiting and sub-orbital platforms have provided new and important information for the discovery, delineation and analysis of archaeological sites worldwide. Since the early 1970s, several of the ten NASA centers have collaborated with archaeologists to refine and validate the use of active and passive remote sensing for archaeological use. The Stennis Space Center (SSC), located in Mississippi USA has been the NASA leader in archaeological research. Together with colleagues from Goddard Space Flight Center (GSFC), Marshall Space Flight Center (MSFC), and the Jet Propulsion Laboratory (JPL), SSC scientists have provided the archaeological community with useful images and sophisticated processing that have pushed the technological frontiers of archaeological research and applications. Successful projects include identifying prehistoric roads in Chaco canyon, identifying sites from the Lewis and Clark Corps of Discovery exploration, and assessing prehistoric settlement patterns in southeast Louisiana. The Scientific Data Purchase (SDP) stimulated commercial companies to collect archaeological data. At present, NASA formally solicits "space archaeology" proposals through its Earth Science Directorate and continues to assist archaeologists and cultural resource managers in doing their work more efficiently and effectively. This paper focuses on passive remote sensing and does not consider the significant contributions made by NASA active sensors. Hyperspectral data offers new opportunities for future archaeological discoveries. (C) 2010 Published by Elsevier Ltd.
C1 NASA, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA.
RP Giardino, MJ (reprint author), NASA, Stennis Space Ctr, Bldg 3204,Room 200A, Stennis Space Ctr, MS 39529 USA.
EM marco.j.giardino@nasa.gov
NR 49
TC 17
Z9 18
U1 3
U2 33
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0305-4403
J9 J ARCHAEOL SCI
JI J. Archaeol. Sci.
PD SEP
PY 2011
VL 38
IS 9
BP 2003
EP 2009
DI 10.1016/j.jas.2010.09.017
PG 7
WC Anthropology; Archaeology; Geosciences, Multidisciplinary
SC Anthropology; Archaeology; Geology
GA 803AD
UT WOS:000293551200002
ER
PT J
AU Hemmati, H
AF Hemmati, Hamid
TI Interplanetary laser communications and precision ranging
SO LASER & PHOTONICS REVIEWS
LA English
DT Article
DE Free space optical communications; laser communications; lasercom; laser
beam pointing
ID SPACE OPTICAL COMMUNICATION; LINK; PERFORMANCE; SATELLITE; TESTS; CODES
AB Future interplanetary missions, including robotic probes and human travel, will require significantly enhanced communications bandwidth that will be difficult to realize with current radio/microwave frequency links. Besides satisfying this requirement, optical (laser) communications has the potential for substantially lowering mass, power, and volume burden on the host spacecraft; is free from spectrum allocation issues; and can potentially support tracking functions resulting in improved spacecraft navigation. Primary challenges of optical communications include precision laser beam pointing over the huge planetary range, inefficiency of laser transmitters, quantum noise limited detection, especially in presence of additive background during periods of near Sun pointing, atmospheric degradation due to attenuation and turbulence and weather outages. This paper will briefly review the status of technologies that have been devised to meet these challenges and system-level developments for bi-directional telecommunications and ranging to distant probes.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Hemmati, H (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM hamid.hemmati@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration. Many thanks to members and
associates of JPL's Optical Communications Group whose work is reported
here, particularly W. Farr, A. Biswas, J. Kovalik, G. Ortiz, K. Wilson,
S. Piazzolla, W. T. Roberts, M. Wright, K. Birnbaum, Y. Chen, J.
Charles, M. Regher, N. Page, B. Moision, J. Hamkins, K. Quirk, J. Gin,
A. Sahasrabudhi, D. Nguyen, J. Lesh, S. Townes, F. Pollara, P.
Estabrook, D. Antsos, and F. Davarian.
NR 96
TC 2
Z9 2
U1 2
U2 16
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA POSTFACH 101161, 69451 WEINHEIM, GERMANY
SN 1863-8880
EI 1863-8899
J9 LASER PHOTONICS REV
JI Laser Photon. Rev.
PD SEP
PY 2011
VL 5
IS 5
BP 697
EP 710
DI 10.1002/lpor.201000040
PG 14
WC Optics; Physics, Applied; Physics, Condensed Matter
SC Optics; Physics
GA 811OQ
UT WOS:000294221800006
ER
PT J
AU Bullo, F
Frazzoli, E
Pavone, M
Savla, K
Smith, SL
AF Bullo, Francesco
Frazzoli, Emilio
Pavone, Marco
Savla, Ketan
Smith, Stephen L.
TI Dynamic Vehicle Routing for Robotic Systems
SO PROCEEDINGS OF THE IEEE
LA English
DT Article
DE Adaptive algorithm; cooperative systems; intelligent robots; mobile
agents; multirobot systems; partitioning algorithms; queueing analysis;
unmanned aerial vehicles
ID TRAVELING-SALESMAN PROBLEM; TARGET ASSIGNMENT; DELIVERY PROBLEM;
EUCLIDEAN PLANE; TASK ASSIGNMENT; NETWORKS; OPTIMIZATION; INFORMATION;
ALGORITHMS; COMPLEXITY
AB Recent years have witnessed great advancements in the science and technology of autonomy, robotics, and networking. This paper surveys recent concepts and algorithms for dynamic vehicle routing (DVR), that is, for the automatic planning of optimal multivehicle routes to perform tasks that are generated over time by an exogenous process. We consider a rich variety of scenarios relevant for robotic applications. We begin by reviewing the basic DVR problem: demands for service arrive at random locations at random times and a vehicle travels to provide on-site service while minimizing the expected wait time of the demands. Next, we treat different multivehicle scenarios based on different models for demands (e. g., demands with different priority levels and impatient demands), vehicles (e. g., motion constraints, communication, and sensing capabilities), and tasks. The performance criterion used in these scenarios is either the expected wait time of the demands or the fraction of demands serviced successfully. In each specific DVR scenario, we adopt a rigorous technical approach that relies upon methods from queueing theory, combinatorial optimization, and stochastic geometry. First, we establish fundamental limits on the achievable performance, including limits on stability and quality of service. Second, we design algorithms, and provide provable guarantees on their performance with respect to the fundamental limits.
C1 [Bullo, Francesco] Univ Calif Santa Barbara, Ctr Control Dynam Syst & Computat, Santa Barbara, CA 93106 USA.
[Bullo, Francesco] Univ Calif Santa Barbara, Dept Mech Engn, Santa Barbara, CA 93106 USA.
[Frazzoli, Emilio] MIT, Dept Aeronaut & Astronaut, Lab Informat & Decis Syst, Cambridge, MA 02139 USA.
[Pavone, Marco] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Smith, Stephen L.] Univ Waterloo, Dept Elect & Comp Engn, Waterloo, ON N2L 3G1, Canada.
RP Bullo, F (reprint author), Univ Calif Santa Barbara, Ctr Control Dynam Syst & Computat, Santa Barbara, CA 93106 USA.
EM bullo@engineering.ucsb.edu; frazzoli@mit.edu; marco.pavone@jpl.nasa.gov;
ksavla@mit.edu; stephen.smith@uwaterloo.ca
RI Bullo, Francesco/B-8146-2013
FU AFOSR [FA 8650-07-2-3744]; ARO MURI [W911NF-05-1-0219]; NSF
[ECCS-0705451, CMMI-0705453]; ARO [W911NF-11-1-0092]
FX Manuscript received May 31, 2010; revised February 22, 2011; accepted
May 7, 2011. Date of publication July 14, 2011; date of current version
August 19, 2011. This work was supported in part by AFOSR award FA
8650-07-2-3744, ARO MURI award W911NF-05-1-0219, NSF awards ECCS-0705451
and CMMI-0705453, and ARO award W911NF-11-1-0092.
NR 61
TC 67
Z9 67
U1 5
U2 34
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9219
EI 1558-2256
J9 P IEEE
JI Proc. IEEE
PD SEP
PY 2011
VL 99
IS 9
SI SI
BP 1482
EP 1504
DI 10.1109/JPROC.2011.2158181
PG 23
WC Engineering, Electrical & Electronic
SC Engineering
GA 810LH
UT WOS:000294126300004
ER
PT J
AU Binienda, WK
Goldberg, RK
AF Binienda, Wieslaw K.
Goldberg, Robert K.
TI Dynamic Testing and Characterization of Woven/Braided Polymer
Composites: A Review
SO APPLIED MECHANICS REVIEWS
LA English
DT Review
AB Woven and braided polymer composite structures are used in many primary aerospace applications because of their superior behavior under dynamic loading conditions and light weight. Characterization of all anisotropic properties under various strain rate and temperature conditions becomes essential for analysis, design, and numerical simulations. This paper aims to present a review of critical testing methods of polymer and composite materials. In the second part, a review of numerical and analytical models for the dynamic analysis of woven and braided composites is presented. This review article cites 138 references. [DOI: 10.1115/1.4007873]
C1 [Binienda, Wieslaw K.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA.
[Goldberg, Robert K.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Binienda, WK (reprint author), Univ Akron, Dept Civil Engn, Akron, OH 44325 USA.
EM wbinienda@uakron.edu; robert.k.goldberg@nasa.gov
NR 138
TC 0
Z9 0
U1 4
U2 26
PU ASME
PI NEW YORK
PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0003-6900
J9 APPL MECH REV
JI Appl. Mech. Rev.
PD SEP
PY 2011
VL 64
IS 5
AR 050803
DI 10.1115/1.4007873
PG 16
WC Mechanics
SC Mechanics
GA V27ST
UT WOS:000208633600003
ER
PT J
AU Bala, G
Caldeira, K
Nemani, R
Cao, L
Ban-Weiss, G
Shin, HJ
AF Bala, G.
Caldeira, Ken
Nemani, Rama
Cao, Long
Ban-Weiss, George
Shin, Ho-Jeong
TI Albedo enhancement of marine clouds to counteract global warming:
impacts on the hydrological cycle
SO CLIMATE DYNAMICS
LA English
DT Article
DE Climate change; Global warming; Geoengineering; Solar radiation
management; Marine cloud-albedo enhancement; Hydrological cycle
ID EARTHS RADIATION BALANCE; CLIMATE-CHANGE; GEOENGINEERING SCHEMES; ENERGY
BUDGET; SIMULATIONS; MODEL; CO2
AB Recent studies have shown that changes in solar radiation affect the hydrological cycle more strongly than equivalent CO2 changes for the same change in global mean surface temperature. Thus, solar radiation management "geoengineering" proposals to completely offset global mean temperature increases by reducing the amount of absorbed sunlight might be expected to slow the global water cycle and reduce runoff over land. However, proposed countering of global warming by increasing the albedo of marine clouds would reduce surface solar radiation only over the oceans. Here, for an idealized scenario, we analyze the response of temperature and the hydrological cycle to increased reflection by clouds over the ocean using an atmospheric general circulation model coupled to a mixed layer ocean model. When cloud droplets are reduced in size over all oceans uniformly to offset the temperature increase from a doubling of atmospheric CO2, the global-mean precipitation and evaporation decreases by about 1.3% but runoff over land increases by 7.5% primarily due to increases over tropical land. In the model, more reflective marine clouds cool the atmospheric column over ocean. The result is a sinking motion over oceans and upward motion over land. We attribute the increased runoff over land to this increased upward motion over land when marine clouds are made more reflective. Our results suggest that, in contrast to other proposals to increase planetary albedo, offsetting mean global warming by reducing marine cloud droplet size does not necessarily lead to a drying, on average, of the continents. However, we note that the changes in precipitation, evaporation and P-E are dominated by small but significant areas, and given the highly idealized nature of this study, a more thorough and broader assessment would be required for proposals of altering marine cloud properties on a large scale.
C1 [Bala, G.] Indian Inst Sci, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India.
[Bala, G.] Indian Inst Sci, Divecha Ctr Climate Change, Bangalore 560012, Karnataka, India.
[Caldeira, Ken; Cao, Long; Ban-Weiss, George; Shin, Ho-Jeong] Carnegie Inst, Dept Global Ecol, Stanford, CA 94305 USA.
[Nemani, Rama] NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Bala, G (reprint author), Indian Inst Sci, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India.
EM bala.gov@gmail.com
RI Caldeira, Ken/E-7914-2011;
OI Ban-Weiss, George/0000-0001-8211-2628
NR 53
TC 31
Z9 31
U1 4
U2 42
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD SEP
PY 2011
VL 37
IS 5-6
BP 915
EP 931
DI 10.1007/s00382-010-0868-1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 814ZU
UT WOS:000294496700005
ER
PT J
AU Siegel, PH
AF Siegel, Peter H.
TI The 23rd International Symposium on Space Terahertz Technology ISSTT
2012 April 2-4, 2012 in Tokyo, JAPAN hosted by NAOJ-NINS and ISAS-JAXA
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Editorial Material
C1 [Siegel, Peter H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Siegel, Peter H.] CALTECH, Pasadena, CA 91109 USA.
RP Siegel, PH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM phs@caltech.edu
NR 0
TC 8
Z9 8
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD SEP
PY 2011
VL 1
IS 1
SI SI
BP 1
EP 4
DI 10.1109/TTHZ.2011.2162013
PG 4
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA V28TJ
UT WOS:000208702800001
ER
PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Terahertz Pioneers A Series of Interviews With Significant Contributors
to Terahertz Science and Technology
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Editorial Material
C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91125 USA.
[Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA.
[Siegel, Peter H.] NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91125 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD SEP
PY 2011
VL 1
IS 1
SI SI
BP 5
EP 5
DI 10.1109/TTHZ.2011.2153490
PG 1
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA V28TJ
UT WOS:000208702800002
ER
PT J
AU Samoska, LA
AF Samoska, Lorene A.
TI An Overview of Solid-State Integrated Circuit Amplifiers in the
Submillimeter-Wave and THz Regime
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Cryogenic electronics; HBTs; HEMTs; low-noise amplifiers; MMICs;
submillimeter-wave; THz
AB We present an overview of solid-state integrated circuit amplifiers approaching terahertz frequencies based on the latest device technologies which have emerged in the past several years. Highlights include the best reported data from heterojunction bipolar transistor (HBT) circuits, high electron mobility transistor (HEMT) circuits, and metamorphic HEMT (mHEMT) amplifier circuits. We discuss packaging techniques for the various technologies in waveguide modules and describe the best reported noise figures measured in these technologies. A consequence of THz transistors, namely ultra-low-noise at cryogenic temperatures, will be explored and results presented. We also present a short review of power amplifier technologies for the THz regime. Finally, we discuss emerging materials for THz amplifiers into the next decade.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Samoska, LA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Lorene.Samoska@jpl.nasa.gov
FU National Aeronautics and Space Administration; W. M. Keck Institute
FX This work was carried out in part at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. This research was also supported
in part by the W. M. Keck Institute for Space Studies.
NR 93
TC 104
Z9 108
U1 4
U2 26
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD SEP
PY 2011
VL 1
IS 1
SI SI
BP 9
EP 24
DI 10.1109/TTHZ.2011.2159558
PG 16
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA V28TJ
UT WOS:000208702800004
ER
PT J
AU Chattopadhyay, G
AF Chattopadhyay, Goutam
TI Technology, Capabilities, and Performance of Low Power Terahertz Sources
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Frequency multipliers; heterostructure barrier varactor (HBV); photo
mixer; quantum cascade laser (QCL); Schottky diodes; terahertz
ID HETEROSTRUCTURE-BARRIER-VARACTOR; QUANTUM-CASCADE LASER; DIODE
FREQUENCY-MULTIPLIERS; TEMPERATURE-GROWN GAAS; MILLIMETER-WAVE;
SUBMILLIMETER WAVELENGTHS; LOCAL OSCILLATOR; SCHOTTKY VARACTOR; 1 THZ;
HETERODYNE RECEIVER
AB New and emerging terahertz technology applications make this a very exciting time for the scientists, engineers, and technologists in the field. New sensors and detectors have been the primary driving force behind the unprecedented progress in terahertz technology, but in the last decade extraordinary developments in terahertz sources have also occurred. Driven primarily by space based missions for Earth, planetary, and astrophysical science, frequency multiplied sources have dominated the field in recent years, at least in the 2-3 THz frequency range. More recently, over the past few years terahertz quantum cascade lasers (QCLs) have made tremendous strides, finding increasing applications in terahertz systems. Vacuum electronic devices and photonic sources are not far behind either. In this article, the various technologies for terahertz sources are reviewed, and future trends are discussed.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Chattopadhyay, G (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM goutam@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA)
FX This work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, Pasadena, CA, under a contract with National
Aeronautics and Space Administration (NASA).
NR 226
TC 63
Z9 69
U1 5
U2 32
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD SEP
PY 2011
VL 1
IS 1
SI SI
BP 33
EP 53
DI 10.1109/TTHZ.2011.2159561
PG 21
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA V28TJ
UT WOS:000208702800006
ER
PT J
AU Groppi, CE
Kawamura, JH
AF Groppi, Christopher E.
Kawamura, Jonathan H.
TI Coherent Detector Arrays for Terahertz Astrophysics Applications
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Radio astronomy; sensor systems and applications; submillimeter wave
technology
ID FOCAL-PLANE ARRAY; HETERODYNE ARRAY; GHZ; TELESCOPE; RECEIVER; ASTRONOMY
AB This paper reviews the key technologies, challenges, and solutions related to the construction of coherent detector arrays in the terahertz waveband for astrophysics applications. We review fundamental performance limits and design constraints for arrays of coherent detectors, review several coherent array systems fielded to date, discuss the design and construction of next-generation systems, and review future prospects for advancements in coherent array technology.
C1 [Groppi, Christopher E.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Kawamura, Jonathan H.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
RP Groppi, CE (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
EM cgroppi@asu.edu; jonathan.h.kawa-mura@jpl.nasa.gov
RI Groppi, Christopher/L-5284-2013
OI Groppi, Christopher/0000-0002-2021-1628
NR 38
TC 15
Z9 15
U1 0
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD SEP
PY 2011
VL 1
IS 1
SI SI
BP 85
EP 96
DI 10.1109/TTHZ.2011.2159555
PG 12
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA V28TJ
UT WOS:000208702800009
ER
PT J
AU Karasik, BS
Sergeev, AV
Prober, DE
AF Karasik, Boris S.
Sergeev, Andrei V.
Prober, Daniel E.
TI Nanobolometers for THz Photon Detection
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Bolometers; infrared detectors; submillimeter wave devices;
superconducting photodetectors
ID HOT-ELECTRON BOLOMETER; TRANSITION-EDGE SENSORS; THIN SUPERCONDUCTING
FILMS; PHONON INTERACTION; ELECTROMAGNETIC-RADIATION; ELECTROTHERMAL
FEEDBACK; DISORDERED CONDUCTORS; RESISTIVE STATE; LOW-NOISE;
MICROBOLOMETER
AB This paper reviews the state of rapidly emerging terahertz hot-electron nanobolometers (nano-HEB), which are currently among of the most sensitive radiation power detectors at submillimeter wavelengths. With the achieved noise equivalent power close to 10(-19) W/Hz(1/2) and potentially capable of approaching NEP similar to 10(-20) W/Hz(1/2), nano-HEBs are very important for future space astrophysics platforms with ultralow submillimeter radiation background. The ability of these sensors to detect single low-energy photons with high dynamic range opens interesting possibilities for quantum calorimetry in the mid-infrared and even in the far-infrared parts of the electromagnetic spectrum. We discuss the competition in the field of ultrasensitive detectors, the physics and technology of nano-HEBs, recent experimental results, and perspectives for future development.
C1 [Karasik, Boris S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sergeev, Andrei V.] SUNY Buffalo, Dept Elect Engn, Buffalo, NY 14260 USA.
[Prober, Daniel E.] Yale Univ, Dept Appl Phys, New Haven, CT 06520 USA.
[Prober, Daniel E.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
RP Karasik, BS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM boris.s.karasik@jpl.nasa.gov; asergeev@eng.buffalo.edu;
daniel.prober@yale.edu
FU National Aeronautical and Space Administration
FX This work was carried out in part at the Jet Propulsion Laboratory,
California Institute of Technology, Pasadena, CA, under a contract with
the National Aeronautical and Space Administration.
NR 127
TC 33
Z9 34
U1 2
U2 19
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD SEP
PY 2011
VL 1
IS 1
SI SI
BP 97
EP 111
DI 10.1109/TTHZ.2011.2159560
PG 15
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA V28TJ
UT WOS:000208702800010
ER
PT J
AU Cooper, KB
Dengler, RJ
Llombart, N
Thomas, B
Chattopadhyay, G
Siegel, PH
AF Cooper, Ken B.
Dengler, Robert J.
Llombart, Nuria
Thomas, Bertrand
Chattopadhyay, Goutam
Siegel, Peter H.
TI THz Imaging Radar for Standoff Personnel Screening
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Terahertz imaging; ultra-wideband radar
AB A summary of the NASA Jet Propulsion Laboratory's 675 GHz imaging radar is presented, with an emphasis on several key design aspects that enable fast, reliable through-clothes imaging of person-borne concealed objects. Using the frequency-modulated continuous-wave (FMCW) radar technique with a nearly 30 GHz bandwidth, sub-centimeter range resolution is achieved. To optimize the radar's range resolution, a reliable software calibration procedure compensates for signal distortion from radar waveform nonlinearities. Low-noise, high dynamic range detection comes from the radar's heterodyne RF architecture, low-noise chirp source, and high-performance 675 GHz transceiver. The radar's optical design permits low-distortion fast beam scanning for single-pixel imaging, and a real-time radar image frame rate of 1 Hz is now possible. Still faster speeds are on the horizon as multi-beam THz transceivers are developed.
C1 [Cooper, Ken B.; Dengler, Robert J.; Llombart, Nuria; Thomas, Bertrand; Chattopadhyay, Goutam; Siegel, Peter H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Cooper, KB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ken.b.cooper@jpl.nasa.gov
FU U.S. Naval Explosive Ordnance Disposal Technology Division; Department
of Defense Physical Security Equipment Action Group
FX This work was carried out at the NASA Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the U.S. Naval
Explosive Ordnance Disposal Technology Division, supported by the
Department of Defense Physical Security Equipment Action Group and the
Technical Support Working Group.
NR 31
TC 196
Z9 207
U1 12
U2 55
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD SEP
PY 2011
VL 1
IS 1
SI SI
BP 169
EP 182
DI 10.1109/TTHZ.2011.2159556
PG 14
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA V28TJ
UT WOS:000208702800016
ER
PT J
AU Alexander, DM
Bauer, FE
Brandt, WN
Daddi, E
Hickox, RC
Lehmer, BD
Luo, B
Xue, YQ
Young, M
Comastri, A
Del Moro, A
Fabian, AC
Gilli, R
Goulding, AD
Mainieri, V
Mullaney, JR
Paolillo, M
Rafferty, DA
Schneider, DP
Shemmer, O
Vignali, C
AF Alexander, D. M.
Bauer, F. E.
Brandt, W. N.
Daddi, E.
Hickox, R. C.
Lehmer, B. D.
Luo, B.
Xue, Y. Q.
Young, M.
Comastri, A.
Del Moro, A.
Fabian, A. C.
Gilli, R.
Goulding, A. D.
Mainieri, V.
Mullaney, J. R.
Paolillo, M.
Rafferty, D. A.
Schneider, D. P.
Shemmer, O.
Vignali, C.
TI X-RAY SPECTRAL CONSTRAINTS FOR z approximate to 2 MASSIVE GALAXIES: THE
IDENTIFICATION OF REFLECTION-DOMINATED ACTIVE GALACTIC NUCLEI
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: high-redshift; infrared: galaxies;
ultraviolet: galaxies; X-rays: galaxies
ID DEEP FIELD-SOUTH; SUPERMASSIVE BLACK-HOLES; COMPTON-THICK QUASARS;
HEAVILY OBSCURED AGN; DIGITAL SKY SURVEY; ULTRALUMINOUS INFRARED
GALAXIES; STAR-FORMATION; HIGH-REDSHIFT; LUMINOSITY FUNCTION;
SEYFERT-GALAXIES
AB We use the 4 Ms Chandra Deep Field-South (CDF-S) survey to place direct constraints on the ubiquity of z approximate to 2 heavily obscured active galactic nuclei (AGNs) in K < 22 BzK-selected galaxies. Forty-seven (approximate to 21%) of the 222 BzK-selected galaxies in the central region of the CDF-S are detected at X-ray energies, 11 (approximate to 5%) of which have hard X-ray spectral slopes (Gamma less than or similar to 1), indicating the presence of heavily obscured AGN activity (N-H greater than or similar to 3 x 10(23) cm(-2)). The other 36 X-ray detected BzK galaxies appear to be relatively unobscured AGNs and starburst galaxies; we use X-ray variability analyses over a rest-frame baseline of approximate to 3 years to further confirm the presence of AGN activity in many of these systems. The majority (7 out of 11) of the heavily obscured AGNs have excess infrared emission over that expected from star formation (termed "infrared-excess galaxies"). However, we find that X-ray detected heavily obscured AGNs only comprise approximate to 25% of the infrared-excess galaxy population, which is otherwise composed of relatively unobscured AGNs and starburst galaxies. We find that the typical X-ray spectrum of the heavily obscured AGNs is better characterized by a pure reflection model than an absorbed power-law model, suggesting extreme Compton-thick absorption (N-H greater than or similar to 10(24) cm(-2)) in some systems. We verify this result by producing a composite rest-frame 2-20 keV spectrum, which has a similar shape as a reflection-dominated X-ray spectrum and reveals an emission feature at rest-frame energy approximate to 6.4 keV, likely to be due to Fe K. These heavily obscured AGNs are likely to be the distant analogs of the reflection-dominated AGNs recently identified at z approximate to 0 with >10 keV observatories. On the basis of these analyses, we estimate the space density for typical (intrinsic X-ray luminosities of L2-10 (keV) greater than or similar to 10(43) erg s (1)) heavily obscured and Compton-thick AGNs at z approximate to 2. Our space-density constraints are conservative lower limits but they are already consistent with the range of predictions from X-ray background models.
C1 [Alexander, D. M.; Hickox, R. C.; Del Moro, A.; Goulding, A. D.; Mullaney, J. R.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Bauer, F. E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Brandt, W. N.; Luo, B.; Xue, Y. Q.; Young, M.; Rafferty, D. A.; Schneider, D. P.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Brandt, W. N.; Luo, B.; Xue, Y. Q.; Young, M.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Daddi, E.; Mullaney, J. R.] Univ Paris Diderot, Lab AIM, CEA, DSM,CNRS,Irfu SAp, F-91191 Gif Sur Yvette, France.
[Hickox, R. C.; Goulding, A. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lehmer, B. D.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Lehmer, B. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Comastri, A.; Gilli, R.] INAF, Osservatorio Astron Bologna, I-04127 Bologna, Italy.
[Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Mainieri, V.] European So Observ, D-85748 Garching, Germany.
[Paolillo, M.] Univ Naples Federico II, Dipartimento Sci Fis, I-80126 Naples, Italy.
[Shemmer, O.] Univ N Texas, Dept Phys, Denton, TX 76203 USA.
[Vignali, C.] Univ Bologna, Dept Astron, I-40127 Bologna, Italy.
RP Alexander, DM (reprint author), Univ Durham, Dept Phys, Durham DH1 3LE, England.
RI Daddi, Emanuele/D-1649-2012; Paolillo, Maurizio/J-1733-2012; Vignali,
Cristian/J-4974-2012; Brandt, William/N-2844-2015; Comastri,
Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015;
OI Daddi, Emanuele/0000-0002-3331-9590; Paolillo,
Maurizio/0000-0003-4210-7693; Vignali, Cristian/0000-0002-8853-9611;
Brandt, William/0000-0002-0167-2453; Comastri,
Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177;
Alexander, David/0000-0002-5896-6313
FU Royal Society; Philip Leverhulme Prize; Science and Technology
Facilities Council; Chilean CONICYT [FONDECYT 1101024]; FONDAP [CATA
15010003]; Chandra X-ray Center [SP8-9001X, G09-0134B, SP1-12007A,
SP1-12007B]; NASA [NNX10AC99G]; ERC-StG [UPGAL 240039]; French ANR
[ANR-08-JCJC-008]; Italian Space Agency (ASI) [I/009/10/0, I/088/06/0]
FX We acknowledge financial support from the Royal Society (D.M.A.,
A.C.F.), a Philip Leverhulme Prize (D. M. A., J.R.M.), the Science and
Technology Facilities Council (D.M.A., R.C.H., A.D.G., A.D.M.), the
Chilean CONICYT grants of FONDECYT 1101024 (F. E. B.) and FONDAP CATA
15010003 (F. E. B.), the Chandra X-ray Center grants SP8-9001X (R. C.
H.), G09-0134B (F. E. B.), SP1-12007A (W.N.B., B. D. L., Y.Q.X.), and
SP1-12007B (F. E. B.), the NASA ADP grant NNX10AC99G (W.N.B., B. D. L.,
Y.Q.X., M.Y.), the ERC-StG grant UPGAL 240039 (E. D.), the French ANR
under contract ANR-08-JCJC-008 (E. D.), and the Italian Space Agency
(ASI) under the ASI-INAF contracts I/009/10/0 and I/088/06/0 (A.C.,
R.G., C.V.). We thank the referee for a prompt and considered report and
thank Y. Ueda for providing the Suzaku data and best-fitting model for
Swift J0601.9-8636 used in Figure 5.
NR 118
TC 39
Z9 39
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2011
VL 738
IS 1
AR 44
DI 10.1088/0004-637X/738/1/44
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500044
ER
PT J
AU Andersson, K
Benson, BA
Ade, PAR
Aird, KA
Armstrong, B
Bautz, M
Bleem, LE
Brodwin, M
Carlstrom, JE
Chang, CL
Crawford, TM
Crites, AT
de Haan, T
Desai, S
Dobbs, MA
Dudley, JP
Foley, RJ
Forman, WR
Garmire, G
George, EM
Gladders, MD
Halverson, NW
High, FW
Holder, GP
Holzapfel, WL
Hrubes, JD
Jones, C
Joy, M
Keisler, R
Knox, L
Lee, AT
Leitch, EM
Lueker, M
Marrone, DP
McMahon, JJ
Mehl, J
Meyer, SS
Mohr, JJ
Montroy, TE
Murray, SS
Padin, S
Plagge, T
Pryke, C
Reichardt, CL
Rest, A
Ruel, J
Ruhl, JE
Schaffer, KK
Shaw, L
Shirokoff, E
Song, J
Spieler, HG
Stalder, B
Staniszewski, Z
Stark, AA
Stubbs, CW
Vanderlinde, K
Vieira, JD
Vikhlinin, A
Williamson, R
Yang, Y
Zahn, O
Zenteno, A
AF Andersson, K.
Benson, B. A.
Ade, P. A. R.
Aird, K. A.
Armstrong, B.
Bautz, M.
Bleem, L. E.
Brodwin, M.
Carlstrom, J. E.
Chang, C. L.
Crawford, T. M.
Crites, A. T.
de Haan, T.
Desai, S.
Dobbs, M. A.
Dudley, J. P.
Foley, R. J.
Forman, W. R.
Garmire, G.
George, E. M.
Gladders, M. D.
Halverson, N. W.
High, F. W.
Holder, G. P.
Holzapfel, W. L.
Hrubes, J. D.
Jones, C.
Joy, M.
Keisler, R.
Knox, L.
Lee, A. T.
Leitch, E. M.
Lueker, M.
Marrone, D. P.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Mohr, J. J.
Montroy, T. E.
Murray, S. S.
Padin, S.
Plagge, T.
Pryke, C.
Reichardt, C. L.
Rest, A.
Ruel, J.
Ruhl, J. E.
Schaffer, K. K.
Shaw, L.
Shirokoff, E.
Song, J.
Spieler, H. G.
Stalder, B.
Staniszewski, Z.
Stark, A. A.
Stubbs, C. W.
Vanderlinde, K.
Vieira, J. D.
Vikhlinin, A.
Williamson, R.
Yang, Y.
Zahn, O.
Zenteno, A.
TI X-RAY PROPERTIES OF THE FIRST SUNYAEV-ZEL'DOVICH EFFECT SELECTED GALAXY
CLUSTER SAMPLE FROM THE SOUTH POLE TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: intracluster medium; X-rays: galaxies: clusters
ID SCALING RELATIONS; COSMOLOGICAL SIMULATIONS; RELATIVISTIC CORRECTIONS;
LENSING MEASUREMENTS; INTRACLUSTER MEDIUM; POWER SPECTRUM; VIRIAL
RADIUS; MASS; GAS; CONSTRAINTS
AB We present results of X-ray observations of a sample of 15 clusters selected via their imprint on the cosmic microwave background from the thermal Sunyaev-Zel'dovich (SZ) effect. These clusters are a subset of the first SZ-selected cluster catalog, obtained from observations of 178 deg(2) of sky surveyed by the South Pole Telescope (SPT). Using X-ray observations with Chandra and XMM-Newton, we estimate the temperature, T-X, and mass, M-g, of the intracluster medium within r(500) for each cluster. From these, we calculate Y-X = MgTX and estimate the total cluster mass using an M-500-Y-X scaling relation measured from previous X-ray studies. The integrated Comptonization, Y-SZ, is derived from the SZ measurements, using additional information from the X-ray-measured gas density profiles and a universal temperature profile. We calculate scaling relations between the X-ray and SZ observables and find results generally consistent with other measurements and the expectations from simple self-similar behavior. Specifically, we fit a Y-SZ-Y-X relation and find a normalization of 0.82 +/- 0.07, marginally consistent with the predicted ratio of Y-SZ/Y-X = 0.91 +/- 0.01 that would be expected from the density and temperature models used in this work. Using the Y-X-derived mass estimates, we fit a Y-SZ-M-500 relation and find a slope consistent with the self-similar expectation of Y-SZ proportional to M-5/3 with a normalization consistent with predictions from other X-ray studies. We find that the SZ mass estimates, derived from cosmological simulations of the SPT survey, are lower by a factor of 0.78 +/- 0.06 relative to the X-ray mass estimates. This offset is at a level of 1.3 sigma when considering the similar to 15% systematic uncertainty for the simulation-based SZ masses. Overall, the X-ray measurements confirm that the scaling relations of the SZ-selected clusters are consistent with the properties of other X-ray-selected samples of massive clusters, even allowing for the broad redshift range (0.29 < z < 1.08) of the sample.
C1 [Andersson, K.; Bautz, M.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Andersson, K.; Mohr, J. J.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Keisler, R.; Leitch, E. M.; Marrone, D. P.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Padin, S.; Pryke, C.; Schaffer, K. K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; McMahon, J. J.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Ade, P. A. R.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales.
[Aird, K. A.; Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Hrubes, J. D.; Leitch, E. M.; Marrone, D. P.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Armstrong, B.; Desai, S.; Song, J.; Yang, Y.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Brodwin, M.; Foley, R. J.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[de Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Shaw, L.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Garmire, G.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Plagge, T.; Reichardt, C. L.; Shirokoff, E.; Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[High, F. W.; Rest, A.; Ruel, J.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Joy, M.] NASA, Marshall Space Flight Ctr, Dept Space Sci, VP62, Huntsville, AL 35812 USA.
[Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Lee, A. T.; Spieler, H. G.] Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Montroy, T. E.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA.
[Montroy, T. E.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, CERCA, Cleveland, OH 44106 USA.
[Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
[Vikhlinin, A.] Space Res Inst IKI, Moscow, Russia.
RP Andersson, K (reprint author), MIT, MIT Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM kanderss@space.mit.edu
RI Stubbs, Christopher/C-2829-2012; Williamson, Ross/H-1734-2015;
Holzapfel, William/I-4836-2015;
OI Stubbs, Christopher/0000-0003-0347-1724; Williamson,
Ross/0000-0002-6945-2975; Marrone, Daniel/0000-0002-2367-1080; Aird,
Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169;
Stark, Antony/0000-0002-2718-9996
FU National Science Foundation [ANT-0638937]; NSF Physics Frontier Center
[PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; NASA
through Chandra X-ray Observatory Center [GO0-11143]; NASA [NAS8-03060,
NNX09AQ04G, 2834-MIT-SAO-4018]; Chandra Award [AR0-11015A]; DFG "The
Dark Universe" [TRR33]; Excellence Cluster Universe; National Sciences
and Engineering Research Council of Canada; Quebec Fonds de recherche
sur la nature et les technologies; Canadian Institute for Advanced
Research; Brinson Foundation; KICP; Clay Fellowship; Hubble Fellowship
[HF-51259.01-A]; Alfred P. Sloan Research Fellowship; Keck Foundation
FX The South Pole Telescope is supported by the National Science Foundation
through grant ANT-0638937. Partial support is also provided by the NSF
Physics Frontier Center grant PHY-0114422 to the Kavli Institute of
Cosmological Physics at the University of Chicago, the Kavli Foundation,
and the Gordon and Betty Moore Foundation.; Support for X-ray analysis
was provided by NASA through Chandra Award Number GO0-11143 issued by
the Chandra X-ray Observatory Center, which is operated by the
Smithsonian Astrophysical Observatory for and on behalf of NASA under
contract NAS8-03060. Additional support is provided by,NASA through
XMM-Newton Award NNX09AQ04G and Chandra Award AR0-11015A. K. Andersson
is supported in part by NASA through SAO Award Number 2834-MIT-SAO-4018
issued by the Chandra X-ray Observatory Center.; The Munich group is
supported by the DFG through TRR33 "The Dark Universe" and the
Excellence Cluster Universe. The McGill group acknowledges funding from
the National Sciences and Engineering Research Council of Canada, the
Quebec Fonds de recherche sur la nature et les technologies and the
Canadian Institute for Advanced Research. The following individuals
acknowledge additional support: B. Stalder from the Brinson Foundation,
B. Benson from a KICP Fellowship, R. Foley from a Clay Fellowship, D.
Marrone from Hubble Fellowship grant HF-51259.01-A, N. W. Halverson
acknowledges support from an Alfred P. Sloan Research Fellowship. M.
Brodwin from the Keck Foundation, and A. T. Lee from the Miller
Institute for Basic Research in Science, University of California
Berkeley.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2011
VL 738
IS 1
AR 48
DI 10.1088/0004-637X/738/1/48
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500048
ER
PT J
AU Dwek, E
Staguhn, JG
Arendt, RG
Capak, PL
Kovacs, A
Benford, DJ
Fixsen, D
Karim, A
Leclercq, S
Maher, SF
Moseley, SH
Schinnerer, E
Sharp, EH
AF Dwek, Eli
Staguhn, Johannes G.
Arendt, Richard G.
Capak, Peter L.
Kovacs, Attila
Benford, Dominic J.
Fixsen, Dale
Karim, Alexander
Leclercq, Samuel
Maher, Stephen F.
Moseley, Samuel H.
Schinnerer, Eva
Sharp, Elmer H.
TI STAR AND DUST FORMATION ACTIVITIES IN AzTEC-3, A STARBURST GALAXY AT
z=5.3
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; galaxies: individual:
AzTEC-3; galaxies: starburst; infrared: galaxies
ID EARLY UNIVERSE; SUBMILLIMETER GALAXIES; SOLAR NEIGHBORHOOD; EVOLUTION;
POPULATION; QUASARS; MODELS; ORIGIN; NUCLEOSYNTHESIS; SUPERNOVAE
AB Analyses of high-redshift ultraluminous infrared (IR) galaxies traditionally use the observed optical to submillimeter spectral energy distribution (SED) and estimates of the dynamical mass as observational constraints to derive the star formation rate (SFR), the stellar mass, and age of these objects. An important observational constraint neglected in the analysis is the mass of dust giving rise to the IR emission. In this paper we add this constraint to the analysis of AzTEC-3. Adopting an upper limit to the mass of stars and a bolometric luminosity for this object, we construct different stellar and chemical evolutionary scenarios, constrained to produce the inferred dust mass and observed luminosity before the associated stellar mass exceeds the observational limit. We use the PEGASE population synthesis code and a chemical evolution model to follow the evolution of the galaxy's SED and its stellar and dust masses as a function of galactic age for seven different stellar initial mass functions (IMFs). We find that the model with a Top Heavy IMF provided the most plausible scenario consistent with the observational constraints. In this scenario the dust formed over a period of similar to 200 Myr, with an SFR of similar to 500 M-circle dot yr(-1). These values for the age and SFR in AzTEC-3 are significantly higher and lower, respectively, from those derived without the dust mass constraint. However, this scenario is not unique, and others cannot be completely ruled out because of the prevailing uncertainties in the age of the galaxy, its bolometric luminosity, and its stellar and dust masses. A robust result of our models is that all scenarios require most of the radiating dust mass to have been accreted in molecular clouds. Our new procedure highlights the importance of a multiwavelength approach, and of the use of dust evolution models in constraining the age and the star formation activity and history in galaxies.
C1 [Dwek, Eli; Staguhn, Johannes G.; Arendt, Richard G.; Benford, Dominic J.; Fixsen, Dale; Maher, Stephen F.; Moseley, Samuel H.; Sharp, Elmer H.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Staguhn, Johannes G.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA.
[Arendt, Richard G.; Fixsen, Dale] Univ Maryland, CRESST, College Pk, MD 20742 USA.
[Capak, Peter L.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Kovacs, Attila] Univ Minnesota, Minneapolis, MN 55414 USA.
[Karim, Alexander; Schinnerer, Eva] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Leclercq, Samuel] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France.
[Maher, Stephen F.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Sharp, Elmer H.] Global Sci & Technol Inc, Greenbelt, MD 20770 USA.
RP Dwek, E (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
RI Dwek, Eli/C-3995-2012; Benford, Dominic/D-4760-2012; Kovacs,
Attila/C-1171-2010;
OI Benford, Dominic/0000-0002-9884-4206; Kovacs,
Attila/0000-0001-8991-9088; Arendt, Richard/0000-0001-8403-8548;
Schinnerer, Eva/0000-0002-3933-7677
FU NSF [AST-0705185, AST-1020981]
FX E.D. acknowledges helpful discussions with Dominik Riechers. GISMO
millimeter observations used in the analysis were supported through NSF
grants AST-0705185 and AST-1020981.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2011
VL 738
IS 1
AR 36
DI 10.1088/0004-637X/738/1/36
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500036
ER
PT J
AU Line, MR
Vasisht, G
Chen, P
Angerhausen, D
Yung, YL
AF Line, Michael R.
Vasisht, Gautam
Chen, Pin
Angerhausen, D.
Yung, Yuk L.
TI THERMOCHEMICAL AND PHOTOCHEMICAL KINETICS IN COOLER HYDROGEN-DOMINATED
EXTRASOLAR PLANETS: A METHANE-POOR GJ436b?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; methods: numerical; planets and satellites: atmospheres;
planets and satellites: composition; planets and satellites: individual
(GJ436b)
ID TRANSITING HOT NEPTUNE; EXOPLANET GJ 1214B; MASS DWARF STARS; HD
189733B; ATMOSPHERIC CIRCULATION; TRANSMISSION SPECTRUM;
CHEMICAL-EQUILIBRIUM; SPACE-TELESCOPE; CARBON-MONOXIDE; GIANT PLANETS
AB We introduce a thermochemical kinetics and photochemical model. We use high-temperature bidirectional reaction rates for important H, C, O, and N reactions (most importantly for CH4 to CO interconversion), allowing us to attain thermochemical equilibrium, deep in an atmosphere, purely kinetically. This allows the chemical modeling of an entire atmosphere, from deep-atmosphere thermochemical equilibrium to the photochemically dominated regime. We use our model to explore the atmospheric chemistry of cooler (T-eff < 10(3) K) extrasolar giant planets. In particular, we choose to model the nearby hot-Neptune GJ436b, the only planet in this temperature regime for which spectroscopic measurements and estimates of chemical abundances now exist. Recent Spitzer measurements with retrieval have shown that methane is driven strongly out of equilibrium and is deeply depleted on the day side of GJ436b, whereas quenched carbon monoxide is abundant. This is surprising because GJ436b is cooler than many of the heavily irradiated hot Jovians and thermally favorable for CH4, and thus requires an efficient mechanism for destroying it. We include realistic estimates of ultraviolet flux from the parent dM star GJ436, to bound the direct photolysis and photosensitized depletion of CH4. While our models indicate fairly rich disequilibrium conditions are likely in cooler exoplanets over a range of planetary metallicities, we are unable to generate the conditions for substantial CH4 destruction. One possibility is an anomalous source of abundant H atoms between 0.01 and 1 bars (which attack CH4), but we cannot as yet identify an efficient means to produce these hot atoms.
C1 [Line, Michael R.; Yung, Yuk L.] CALTECH, Pasadena, CA 91106 USA.
[Vasisht, Gautam; Chen, Pin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Angerhausen, D.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany.
RP Line, MR (reprint author), CALTECH, Pasadena, CA 91106 USA.
EM mrl@gps.caltech.edu; gv@s383.jpl.nasa.gov
RI Chen, Pin/B-1112-2008
OI Chen, Pin/0000-0003-1195-9666
FU JPL; National Aeronautics and Space Administration
FX We thank Julie Moses, Channon Visscher, Karen Willacy, and M. C. Liang
for useful chemistry discussions and tips. We also thank Xi Zhang,
Heather Knutson, Mimi Gerstell, Mark Allen, the Yuk Yung Group, and the
anonymous referee for reading the paper and providing valuable feedback.
M. Line is supported by the JPL Graduate Fellowship funded by the JPL
Research and Technology Development Program. P. Chen and G. Vasisht are
supported by the JPL Research & Technology Development Program, and
contributions herein were supported by the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2011
VL 738
IS 1
AR 32
DI 10.1088/0004-637X/738/1/32
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500032
ER
PT J
AU Melendez, M
Kraemer, SB
Weaver, KA
Mushotzky, RF
AF Melendez, M.
Kraemer, S. B.
Weaver, K. A.
Mushotzky, R. F.
TI UNCOVERING THE SPECTRAL ENERGY DISTRIBUTION IN ACTIVE GALAXIES USING
HIGH-IONIZATION MID-INFRARED EMISSION LINES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: nuclei; galaxies: Seyfert; infrared:
galaxies; X-rays: galaxies
ID GALACTIC NUCLEI; SEYFERT-GALAXIES; X-RAY; MU-M; INFRARED-SPECTROSCOPY;
SPITZER-IRS; NGC 4151; QUASARS; REGION; AGN
AB The shape of the spectral energy distribution (SED) of active galaxies in the extreme-ultraviolet (EUV)-soft X-ray band (13.6 eV-1 keV) is uncertain because obscuration by dust and gas can hamper our view of the continuum. To investigate the shape of the SED in this energy band, we have generated a set of photoionization models which reproduce the small dispersion found in correlations between high-ionization mid-infrared emission lines in a sample of hard X-ray-selected active galactic nuclei (AGNs). Our calculations show that a broken power-law continuum model is sufficient to reproduce the [Ne v](14.32) mu m/[Ne III], [Ne v](24.32) mu m/[O IV](25.89) mu m, and [O IV](25.89) mu m/[Ne III] ratios and does not require the addition of a "big bump" EUV model component. We constrain the EUV-soft X-ray slope, alpha(i), to be between 1.5 and 2.0 and derive a best fit of alpha(i) similar to 1.9 for Seyfert 1 galaxies, consistent with previous studies of intermediate-redshift quasars. If we assume a blue bump model, most sources in our sample have derived temperatures between T-BB = 10(5.18) K and 10(5.7) K, suggesting that the peak of this component spans a large range of energies extending from similar to 600 angstrom to 1900 angstrom. In this case, the best-fitting peak energy that matches the mid-infrared line ratios of Seyfert 1 galaxies occurs between similar to 700 and 1000 angstrom. Despite the fact that our results do not rule out the presence of an EUV bump, we conclude that our power-law model produces enough photons with energies >4 Ry to generate the observed amount of mid-infrared emission in our sample of Burst Alert Telescope AGNs.
C1 [Melendez, M.; Weaver, K. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kraemer, S. B.] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
[Mushotzky, R. F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Melendez, M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Melendez, M (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
FU NASA
FX We thank our anonymous referee for suggestions that improved the paper.
This research was supported by an appointment to the NASA Postdoctoral
Program at the Goddard Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA. This research has
made use of NASA's Astrophysics Data System.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2011
VL 738
IS 1
AR 6
DI 10.1088/0004-637X/738/1/6
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500006
ER
PT J
AU O'Dea, DT
Ade, PAR
Amiri, M
Benton, SJ
Bock, JJ
Bond, JR
Bonetti, JA
Bryan, S
Burger, B
Chiang, HC
Clark, CN
Contaldi, CR
Crill, BP
Davis, G
Dore, O
Farhang, M
Filippini, JP
Fissel, LM
Fraisse, AA
Gandilo, NN
Golwala, S
Gudmundsson, JE
Hasselfield, M
Hilton, G
Holmes, W
Hristov, VV
Irwin, K
Jones, WC
Kuo, CL
MacTavish, CJ
Mason, PV
Montroy, TE
Morford, TA
Netterfield, CB
Rahlin, AS
Reintsema, C
Ruhl, JE
Runyan, MC
Schenker, MA
Shariff, JA
Soler, JD
Trangsrud, A
Tucker, C
Tucker, RS
Turner, AD
Wiebe, D
AF O'Dea, D. T.
Ade, P. A. R.
Amiri, M.
Benton, S. J.
Bock, J. J.
Bond, J. R.
Bonetti, J. A.
Bryan, S.
Burger, B.
Chiang, H. C.
Clark, C. N.
Contaldi, C. R.
Crill, B. P.
Davis, G.
Dore, O.
Farhang, M.
Filippini, J. P.
Fissel, L. M.
Fraisse, A. A.
Gandilo, N. N.
Golwala, S.
Gudmundsson, J. E.
Hasselfield, M.
Hilton, G.
Holmes, W.
Hristov, V. V.
Irwin, K.
Jones, W. C.
Kuo, C. L.
MacTavish, C. J.
Mason, P. V.
Montroy, T. E.
Morford, T. A.
Netterfield, C. B.
Rahlin, A. S.
Reintsema, C.
Ruhl, J. E.
Runyan, M. C.
Schenker, M. A.
Shariff, J. A.
Soler, J. D.
Trangsrud, A.
Tucker, C.
Tucker, R. S.
Turner, A. D.
Wiebe, D.
TI SPIDER OPTIMIZATION. II. OPTICAL, MAGNETIC, AND FOREGROUND EFFECTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; gravitational
waves; methods: analytical; methods: data analysis; polarization
ID PROBE WMAP OBSERVATIONS; MICROWAVE BACKGROUND POLARIMETRY; POLARIZATION
POWER SPECTRA; GALACTIC DUST EMISSION; 2003 FLIGHT; OBSERVATIONAL
CONSTRAINTS; STARLIGHT POLARIZATION; FIELD; BOOMERANG; TEMPERATURE
AB SPIDER is a balloon-borne instrument designed to map the polarization of the cosmic microwave background (CMB) with degree-scale resolution over a large fraction of the sky. SPIDER'S main goal is to measure the amplitude of primordial gravitational waves through their imprint on the polarization of the CMB if the tensor-to-scalar ratio, r, is greater than 0.03. To achieve this goal, instrumental systematic errors must be controlled with unprecedented accuracy. Here, we build on previous work to use simulations of SPIDERobservations to examine the impact of several systematic effects that have been characterized through testing and modeling of various instrument components. In particular, we investigate the impact of the non-ideal spectral response of the half-wave plates, coupling between focal-plane components and Earth's magnetic field, and beam mismatches and asymmetries. We also present a model of diffuse polarized foreground emission based on a three-dimensional model of the Galactic magnetic field and dust, and study the interaction of this foreground emission with our observation strategy and instrumental effects. We find that the expected level of foreground and systematic contamination is sufficiently low for Spider to achieve its science goals.
C1 [O'Dea, D. T.; Clark, C. N.; Contaldi, C. R.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London, England.
[Ade, P. A. R.; Tucker, C.] Cardiff Univ, Sch Phys & Astron, Cardiff, S Glam, Wales.
[Amiri, M.; Burger, B.; Davis, G.; Hasselfield, M.; Wiebe, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
[Benton, S. J.; Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Bock, J. J.; Crill, B. P.; Dore, O.; Filippini, J. P.; Golwala, S.; Hristov, V. V.; Mason, P. V.; Morford, T. A.; Runyan, M. C.; Schenker, M. A.; Trangsrud, A.; Tucker, R. S.] CALTECH, Dept Phys, Pasadena, CA 91125 USA.
[Bock, J. J.; Bonetti, J. A.; Crill, B. P.; Dore, O.; Holmes, W.; Turner, A. D.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Bond, J. R.; Farhang, M.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 1A1, Canada.
[Bryan, S.; Montroy, T. E.; Ruhl, J. E.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA.
[Chiang, H. C.; Fraisse, A. A.; Gudmundsson, J. E.; Jones, W. C.; Rahlin, A. S.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Farhang, M.; Fissel, L. M.; Gandilo, N. N.; Netterfield, C. B.; Shariff, J. A.; Soler, J. D.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada.
[Hilton, G.; Irwin, K.; Reintsema, C.] Natl Inst Stand & Technol, Boulder, CO USA.
[Kuo, C. L.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[MacTavish, C. J.] Univ Cambridge, Kavli Inst Cosmol, Cambridge, England.
RP O'Dea, DT (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London, England.
FU STFC [PP/E002129]; NASA [NNX07AL64G]; Alfred P. Sloan Foundation
FX D.T.O. acknowledges support from STFC under the standard grant scheme
(PP/E002129). The Spider project is supported by NASA award NNX07AL64G.
W.C.J. acknowledges the support of the Alfred P. Sloan Foundation. Some
of the results in this paper have been derived using the HEALPIX package
(Gorski et al. 2005) as well as the FFTW package (Frigo & Johnson 2005).
NR 60
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2011
VL 738
IS 1
AR 63
DI 10.1088/0004-637X/738/1/63
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500063
ER
PT J
AU Rogers, LA
Bodenheimer, P
Lissauer, JJ
Seager, S
AF Rogers, Leslie A.
Bodenheimer, Peter
Lissauer, Jack J.
Seager, Sara
TI FORMATION AND STRUCTURE OF LOW-DENSITY EXO-NEPTUNES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: formation; planets and satellites: interiors
ID EXTRASOLAR GIANT PLANETS; HOT JUPITERS; PROTOPLANETARY ATMOSPHERES;
INTERNAL STRUCTURE; OCEAN-PLANETS; SUPER-EARTHS; GJ 1214B; LOW-MASS;
ACCRETION; EXOPLANETS
AB Kepler has found hundreds of Neptune-size (2-6 R-circle plus) planet candidates within 0.5 AU of their stars. The nature of the vast majority of these planets is not known because their masses have not been measured. Using theoretical models of planet formation, evolution, and structure, we explore the range of minimum plausible masses for low-density exo-Neptunes. We focus on highly irradiated planets with T-eq >= 500 K. We consider two separate formation pathways for low-mass planets with voluminous atmospheres of light gases: core-nucleated accretion and outgassing ;of hydrogen from dissociated ices. We show that Neptune-size planets at T-eq = 500 K with masses as small as a few times that of Earth can plausibly be formed by core-nucleated accretion coupled with subsequent inward migration. We also derive a limiting low-density mass-radius relation for rocky planets with outgassed hydrogen envelopes but no surface water. Rocky planets with outgassed hydrogen envelopes typically have computed radii well below 3 R-circle plus. For both planets with H/He envelopes from core-nucleated accretion and planets with outgassed hydrogen envelopes, we employ planet interior models to map the range of planet mass-envelope mass-equilibrium temperature parameter space that is consistent with Neptune-size planet radii. Atmospheric mass loss mediates which corners of this parameter space are populated by actual planets and ultimately governs the minimum plausible mass at a specified transit radius. We find that Kepler's 2-6 R-circle plus planet candidates at T-eq = 500-1000 K could potentially have masses less than or similar to 4 M-circle plus. Although our quantitative results depend on several assumptions, our qualitative finding that warm Neptune-size planets can have masses substantially smaller than those given by interpolating the masses and radii of planets within our Solar System is robust.
C1 [Rogers, Leslie A.; Seager, Sara] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Bodenheimer, Peter] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Lissauer, Jack J.] NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Seager, Sara] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
RP Rogers, LA (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA.
FU NASA; NSF [AST0908807]
FX P.B. and J.L. acknowledge support from the NASA origins program. P.B.
acknowledges support from NSF grant AST0908807. The authors thank Olenka
Hubickyj for making Figures 1-3. We also thank Linda Elkins-Tanton for
helpful discussions about planet outgassing and silicate mantles,
Benjamin Weiss for his insights into EH chondrite compositions, and
Geoff Marcy and an anonymous referee for comments on the manuscript.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2011
VL 738
IS 1
AR 59
DI 10.1088/0004-637X/738/1/59
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500059
ER
PT J
AU Shariff, K
Cuzzi, JN
AF Shariff, Karim
Cuzzi, Jeffrey N.
TI GRAVITATIONAL INSTABILITY OF SOLIDS ASSISTED BY GAS DRAG: SLOWING BY
TURBULENT MASS DIFFUSIVITY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; protoplanetary disks
ID SOLAR NEBULA; PLANETESIMAL FORMATION; PROTOPLANETARY DISKS; TERRESTRIAL
PLANETS; DUST LAYER; COAGULATION; PARTICLES; ACCRETION; EVOLUTION;
GRAINS
AB The Goldreich & Ward (axisymmetric) gravitational instability of a razor thin particle layer occurs when the Toomre parameter Q(T) = c(p)Omega(0)/pi G Sigma(p) < 1 (c(p) being the particle dispersion velocity). Ward extended this analysis by adding the effect of gas drag upon particles and found that even when Q(T) > 1, sufficiently long waves were always unstable. Youdin carried out a detailed analysis and showed that the instability allows chondrule-sized (similar to 1 mm) particles to undergo radial clumping with reasonable growth times even in the presence of a moderate amount of turbulent stirring. The analysis of Youdin includes the role of turbulence in setting the thickness of the dust layer and in creating a turbulent particle pressure in the momentum equation. However, he ignores the effect of turbulent mass diffusivity on the disturbance wave. Here, we show that including this effect reduces the growth rate significantly, by an amount that depends on the level of turbulence, and reduces the maximum intensity of turbulence the instability can withstand by 1-3 orders of magnitude. The instability is viable only when turbulence is extremely weak and the solid to gas surface density of the particle layer is considerably enhanced over minimum-mass-nebula values. A simple mechanistic explanation of the instability shows how the azimuthal component of drag promotes instability while the radial component hinders it. A gravito-diffusive overstability is also possible but never realized in the nebula models.
C1 [Shariff, Karim; Cuzzi, Jeffrey N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Shariff, K (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
OI Shariff, Karim/0000-0002-7256-2497
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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 SEP 1
PY 2011
VL 738
IS 1
AR 73
DI 10.1088/0004-637X/738/1/73
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500073
ER
PT J
AU Shim, HJ
Chary, RR
Dickinson, M
Lin, LW
Spinrad, H
Stern, D
Yan, CH
AF Shim, Hyunjin
Chary, Ranga-Ram
Dickinson, Mark
Lin, Lihwai
Spinrad, Hyron
Stern, Daniel
Yan, Chi-Hung
TI z similar to 4 H alpha EMITTERS IN THE GREAT OBSERVATORIES ORIGINS DEEP
SURVEY: TRACING THE DOMINANT MODE FOR GROWTH OF GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: evolution; galaxies: high-redshift;
galaxies: starburst
ID STAR-FORMING GALAXIES; LYMAN BREAK GALAXIES; HIGH-REDSHIFT GALAXIES;
GOODS-SOUTH FIELD; FORMATION RATE DENSITY; UV-CONTINUUM SLOPE; VLT/FORS2
SPECTROSCOPY; MS 1512-CB58; INTERSTELLAR EXTINCTION; SPECTRAL
DISTRIBUTIONS
AB We present evidence for strong H alpha emission in galaxies with spectroscopic redshifts in the range of 3.8 < z < 5.0 over the Great Observatories Origins Deep Survey fields. Among 74 galaxies detected in the Spitzer IRAC 3.6 and 4.5 mu m bands, more than 70% of the galaxies show clear excess at 3.6 mu m compared to the expected flux density from stellar continuum only. We provide evidence that this 3.6 mu m excess is due to H alpha emission redshifted into the 3.6 mu m band, and classify these 3.6 mu m excess galaxies to be H alpha emitter (HAE) candidates. The selection of HAE candidates using an excess in broadband filters is sensitive to objects whose rest-frame H alpha equivalent width (EW) is larger than 350 angstrom. The H alpha inferred star formation rates (SFRs) of the HAEs range between 20 and 500 M-circle dot yr (1) and are a factor of similar to 6 larger than SFRs inferred from the UV continuum. The ratio between the H alpha luminosity and UV luminosity of HAEs is also on average larger than that of local starbursts. Possible reasons for such strong H alpha emission in these galaxies include different dust extinction properties, young stellar population ages, extended star formation histories, low metallicity, and a top-heavy stellar initial mass function. Although the correlation between UV slope beta and L-H alpha/L-UV raises the possibility that HAEs prefer a dust extinction curve which is steeper in the UV, the most dominant factor that results in strong H alpha emission appears to be star formation history. The H alpha EWs of HAEs are large despite their relatively old stellar population ages constrained by spectral energy distribution fitting, suggesting that at least 60% of HAEs produce stars at a constant rate. Under the assumption that the gas supply is sustained, HAEs are able to produce greater than or similar to 50% of the stellar mass density that is encompassed in massive (M-* > 10(11) M-circle dot) galaxies at z similar to 3. This "strong H alpha phase" of star formation plays a dominant role in galaxy growth at z similar to 4, and they are likely progenitors of massive red galaxies at lower redshifts.
C1 [Shim, Hyunjin; Chary, Ranga-Ram] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Chary, Ranga-Ram] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Lin, Lihwai; Yan, Chi-Hung] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Spinrad, Hyron] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Shim, HJ (reprint author), CALTECH, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA.
NR 74
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2011
VL 738
IS 1
AR 69
DI 10.1088/0004-637X/738/1/69
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500069
ER
PT J
AU Stewart, KR
Kaufmann, T
Bullock, JS
Barton, EJ
Maller, AH
Diemand, J
Wadsley, J
AF Stewart, Kyle R.
Kaufmann, Tobias
Bullock, James S.
Barton, Elizabeth J.
Maller, Ariyeh H.
Diemand, Juerg
Wadsley, James
TI ORBITING CIRCUMGALACTIC GAS AS A SIGNATURE OF COSMOLOGICAL ACCRETION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: halos; methods:
numerical; quasars: absorption lines
ID DARK-MATTER HALOES; ABSORPTION-SELECTED GALAXIES; LAMBDA-CDM
SIMULATIONS; ANGULAR-MOMENTUM; GALACTIC HALOS; MGII ABSORBERS; DISK
GALAXIES; COLD FLOWS; INTERMEDIATE REDSHIFT; ULTRAVIOLET-SPECTRA
AB We use cosmological smoothed particle hydrodynamic simulations to study the kinematic signatures of cool gas accretion onto a pair of well-resolved galaxy halos. We find that cold-flow streams and gas-rich mergers produce a circumgalactic component of cool gas that generally orbits with high angular momentum about the galaxy halo before falling in to build the disk. This signature of cosmological accretion should be observable using background-object absorption-line studies as features that are offset from the galaxy's systemic velocity by similar to 100 km s(-1). In most cases, the accreted gas co-rotates with the central disk in the form of a warped, extended cold flow disk, such that the observed velocity offset will be in the same direction as galaxy rotation, appearing in sight lines that avoid the galactic poles. This prediction provides a means to observationally distinguish accreted gas from outflow gas: the accreted gas will show large one-sided velocity offsets in absorption-line studies while radial/bi-conical outflows will not (except possibly in special polar projections). Such a signature of rotation has already been seen in studies of intermediate-redshift galaxy-absorber pairs, and we suggest that these observations may be among the first to provide indirect observational evidence for cold accretion onto galactic halos. This cold-mode halo gas typically has similar to 3-5 times more specific angular momentum than the dark matter. The associated cold-mode disk configurations are likely related to extended H I/extended UV disks that are seen around galaxies in the local universe. The fraction of galaxies with extended cold flow disks and associated offset absorption-line gas should decrease around bright galaxies at low redshift as cold-mode accretion dies out.
C1 [Stewart, Kyle R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kaufmann, Tobias] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Bullock, James S.; Barton, Elizabeth J.] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA.
[Bullock, James S.; Barton, Elizabeth J.] Univ Calif Irvine, Ctr Galaxy Evolut, Dept Phys & Astron, Irvine, CA 92697 USA.
[Maller, Ariyeh H.] New York City Coll Technol, Dept Phys, Brooklyn, NY 11201 USA.
[Diemand, Juerg] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland.
[Wadsley, James] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada.
RP Stewart, KR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RI Diemand, Juerg/G-9448-2011; Bullock, James/K-1928-2015
OI Bullock, James/0000-0003-4298-5082
FU National Aeronautics and Space Administration [NNX09AG01G]; NASA at the
Jet Propulsion Laboratory; Swiss National Science Foundation (SNF)
FX We thank Leonidas Moustakas and David Weinberg for useful discussions.
We thank the anonymous referee, whose insightful comments helped improve
the quality of this paper. The simulations used in this paper were run
on the Cosmos cluster at JPL and the Greenplanet cluster at UC Irvine.
This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. J.S.B. and K. R. S. were partially
supported by NASA grant NNX09AG01G. K.R.S. is supported by an
appointment to the NASA Postdoctoral Program at the Jet Propulsion
Laboratory, administered by Oak Ridge Associated Universities through a
contract with NASA. T. K. and J.D. have been supported by the Swiss
National Science Foundation (SNF).
NR 97
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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 SEP 1
PY 2011
VL 738
IS 1
AR 39
DI 10.1088/0004-637X/738/1/39
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500039
ER
PT J
AU Viall, NM
Klimchuk, JA
AF Viall, Nicholeen M.
Klimchuk, James A.
TI PATTERNS OF NANOFLARE STORM HEATING EXHIBITED BY AN ACTIVE REGION
OBSERVED WITH SOLAR DYNAMICS OBSERVATORY/ATMOSPHERIC IMAGING ASSEMBLY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: atmosphere; Sun: corona; Sun: UV radiation
ID TRANSITION-REGION; CORONAL LOOPS; HOT PLASMA; TRACE; EXPLORER; HINODE
AB It is largely agreed that many coronal loops-those observed at a temperature of about 1 MK-are bundles of unresolved strands that are heated by storms of impulsive nanoflares. The nature of coronal heating in hotter loops and in the very important but largely ignored diffuse component of active regions is much less clear. Are these regions also heated impulsively, or is the heating quasi-steady? The spectacular new data from the Atmospheric Imaging Assembly (AIA) telescopes on the Solar Dynamics Observatory offer an excellent opportunity to address this question. We analyze the light curves of coronal loops and the diffuse corona in six different AIA channels and compare them with the predicted light curves from theoretical models. Light curves in the different AIA channels reach their peak intensities with predictable orderings as a function the nanoflare storm properties. We show that while some sets of light curves exhibit clear evidence of cooling after nanoflare storms, other cases are less straightforward to interpret. Complications arise because of line-of-sight integration through many different structures, the broadband nature of the AIA channels, and because physical properties can change substantially depending on the magnitude of the energy release. Nevertheless, the light curves exhibit predictable and understandable patterns consistent with impulsive nanoflare heating.
C1 [Viall, Nicholeen M.; Klimchuk, James A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Viall, NM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RI Klimchuk, James/D-1041-2012; Viall, Nicholeen/D-1687-2012
OI Klimchuk, James/0000-0003-2255-0305;
FU NASA
FX The research of N.M.V. was supported by an appointment to the NASA
Postdoctoral Program at the Goddard Space Flight Center, administered by
Oak Ridge Associated Universities through a contract with NASA. The
research of J.A.K. was supported by the NASA Supporting Research and
Technology program. The data are courtesy of NASA/SDO and the AIA
science team.
NR 29
TC 53
Z9 53
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2011
VL 738
IS 1
AR 24
DI 10.1088/0004-637X/738/1/24
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500024
ER
PT J
AU Fishman, J
Silverman, ML
Crawford, JH
Creilson, JK
AF Fishman, Jack
Silverman, Morgan L.
Crawford, James H.
Creilson, John K.
TI A study of regional-scale variability of in situ and model-generated
tropospheric trace gases: Insights into observational requirements for a
satellite in geostationary orbit
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Tropospheric chemistry; Regional modeling; Trace gas variability;
Tropospheric trace gas satellite measurements
ID AIR-QUALITY; INSTRUMENT; POLLUTION; FORECAST; HOUSTON; MOPITT; SYSTEM;
SPACE
AB We examine the results from a regional-scale chemical-transport model with 4-km resolution to determine the spatial variability of trace gases on this scale. Model-derived variability statistics are generated using 1st-order structure functions and then compared with in situ trace gas measurements from a series of aircraft campaigns. The variability of the observations and the model-derived concentrations are found to be in reasonable agreement for O-3 and CO, but the model underestimates the observed variability of NO2. Variability statistics are then calculated for model-derived tropospheric column integrals. These integrals are calculated for 0-10 km (representative of the entire tropospheric column), 0-2 km (representative of the planetary boundary layer, PBL) and 2-10 km (representative of the free troposphere, FT). For each of the species examined, the variability of the tropospheric column is generally controlled by the variability in the lowest 2 km. The degree of control for each trace gas, however, is different. Whereas NO2 is completely dominated by PBL processes, CO variability in the FT contributes appreciably to the variability of the entire tropospheric column, suggesting that two independent pieces of information for CO would be most helpful for describing the variability of the entire tropospheric column. Likewise, the variability of an independent free tropospheric measurement of 03 would provide additional insight into the observed variability of the entire column, but the amount of additional information provided by a separate FT measurement is not as beneficial to what was found for CO. We provide additional analyses to quantify relationships that can be used to better understand the model-derived structure functions and their dependence on grid size and time of day. Lastly we present a practical example of how this information may be used for guidance in the development of science requirements for future satellite instruments since measurements from these instruments must be able to resolve smaller scale gradients to be used successfully for air quality applications. Published by Elsevier Ltd.
C1 [Fishman, Jack; Silverman, Morgan L.; Crawford, James H.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Silverman, Morgan L.; Creilson, John K.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
RP Fishman, J (reprint author), NASA, Langley Res Ctr, 21 Langley Blvd,Mail Stop 401A, Hampton, VA 23681 USA.
EM jack.fishman@nasa.gov
RI Crawford, James/L-6632-2013
OI Crawford, James/0000-0002-6982-0934
NR 24
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 1352-2310
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD SEP
PY 2011
VL 45
IS 27
BP 4682
EP 4694
DI 10.1016/j.atmosenv.2011.05.008
PG 13
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 807VM
UT WOS:000293931100016
ER
PT J
AU Tsai, TC
Jeng, YJ
Chu, DA
Chen, JP
Chang, SC
AF Tsai, Tzu-Chin
Jeng, Yung-Jyh
Chu, D. Allen
Chen, Jen-Ping
Chang, Shuenn-Chin
TI Analysis of the relationship between MODIS aerosol optical depth and
particulate matter from 2006 to 2008
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE MODIS; Aerosol optical depth; Boundary layer height; Haze layer height;
Particulate matter; Taiwan
ID AIR-POLLUTION; MICROPULSE LIDAR; HONG-KONG; VALIDATION; QUALITY; TAIWAN;
RETRIEVAL; PARTICLES; ALGORITHM; TRANSPORT
AB This study used sunphotometer, lidar, and surface particulate matter measurements to assess MODIS AOD products for air quality monitoring in Taiwan. The MODIS AOD retrievals revealed a satisfactory validation against AERONET measurements with correlation coefficient similar to 0.91 during Terra and similar to 0.83 during Aqua overpasses in the period of 2006-2008. The correlations in cold season (September-February) similar to 0.85-0.96 appear to be slightly higher than those in warm season (March-August) similar to 0.78-0.87. The relationships derived between PM2.5 and AOD from both MODIS and AEROENT show a strong seasonality as a result of aerosol vertical distribution. The high correlations (similar to 0.88-0.93) obtained in autumn between PM2.5 and AOD normalized by boundary layer height (or equivalent haze layer height) are attributed to stable and well-mixed boundary layers as opposed to the summer lows (similar to 0.12-0.67) resulted from strong convection associated with unstable weather systems. With the long-range transport of Asian dust and pollution in winter and spring under prevalent northeasterly and biomass burning from Southeast Asia in spring under prevalent southwesterly flows, better correlation is derived from the normalization by haze layer height than boundary layer height owing to abundance of aerosols aloft above boundary layer. The former is shown with correlation coefficients in the range of similar to 0.76-0.87 and similar to 0.77-0.80 and the latter similar to 0.56-0.79 and similar to 0.39-0.54 for winter and spring, respectively. The results of MODIS that uphold the relationships derived from AERONET in autumn, winter, and spring suggest MODIS AOD products have the level of quality as sunphotometer measurements for monitoring local PM2.5 in Taiwan. (C) 2009 Elsevier Ltd. All rights reserved.
C1 [Chu, D. Allen] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Goddard Earth Sci & Technol Ctr, Greenbelt, MD 20771 USA.
[Chang, Shuenn-Chin] Environm Protect Adm, Taipei 10042, Taiwan.
[Tsai, Tzu-Chin; Jeng, Yung-Jyh; Chen, Jen-Ping] Natl Taiwan Univ, Dept Atmospher Sci, Taipei 10764, Taiwan.
RP Chu, DA (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Goddard Earth Sci & Technol Ctr, Code 613-2, Greenbelt, MD 20771 USA.
EM tzuchin@webmail2.as.ntu.edu.tw; yjjeng@webmail2.as.ntu.edu.tw;
allen.chu@nasa.gov; jpchen@as.ntu.edu.tw; scchang@epa.gov.tw
RI Chen, Jen-Ping/F-2947-2010; Wang, Linden/M-6617-2014; Xiongfei,
Zhao/G-7690-2015
OI Chen, Jen-Ping/0000-0003-4188-6189;
FU Taiwan EPA [EPA-96-L105-03-002]
FX We would like to thank NASA Data Distribution and Archive Center for
processing and providing MODIS AOD products. In addition, we thank Dr.
Neng-Huei (George) Lin of NCU for his effort in establishing and
maintaining TWEPA-NCU sites and Taiwan EPA for providing data and
supporting this study by Grant EPA-96-L105-03-002.
NR 37
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U1 1
U2 26
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD SEP
PY 2011
VL 45
IS 27
BP 4777
EP 4788
DI 10.1016/j.atmosenv.2009.10.006
PG 12
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 807VM
UT WOS:000293931100026
ER
PT J
AU Wang, SH
Tsay, SC
Lin, NH
Hsu, NC
Bell, SW
Li, C
Ji, Q
Jeong, MJ
Hansell, RA
Welton, EJ
Holben, BN
Sheu, GR
Chu, YC
Chang, SC
Liu, JJ
Chiang, WL
AF Wang, Sheng-Hsiang
Tsay, Si-Chee
Lin, Neng-Huei
Hsu, N. Christina
Bell, Shaun W.
Li, Can
Ji, Qiang
Jeong, Myeong-Jae
Hansell, Richard A.
Welton, Ellsworth J.
Holben, Brent N.
Sheu, Guey-Rong
Chu, Yu-Chi
Chang, Shuenn-Chin
Liu, Jyh-Jian
Chiang, Wei-Li
TI First detailed observations of long-range transported dust over the
northern South China Sea
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Asian dust; South China Sea; Aerosol optical thickness (AOT); 7SEAS;
Lidar; Dongsha
ID ACE-ASIA; AEROSOL; POLLUTION
AB Trans-Pacific Asian dust transport has been well documented, but little is known about dust invasion to the South China Sea (SCS). This study presents the first detailed characterization of dust aerosols transported to the northern SCS. On 21 March 2010, a strong Asian dust storm affected large areas from the Gobi deserts to the West Pacific, including Taiwan and Hong Kong, and was also observed by a comprehensive set of instruments at Dongsha Island, a small island (about 2 km(2), 20 degrees 42'52 '' N, 116 degrees 43'51 '' E) in the northern SCS. Aerosol measurements including particle mass concentrations, size distribution, optical properties, hygroscopicity, and vertical profiles help depict the evolution of this dust event. Our results indicate that the dust particles were mixed with anthropogenic and marine aerosols, and transported within 250 m above ground level. The long-range transport of Asian dust to the northern SCS could significantly impact the ecosystems in the region. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Wang, Sheng-Hsiang; Lin, Neng-Huei; Sheu, Guey-Rong] Natl Cent Univ, Dept Atmospher Sci, Chungli 32054, Taiwan.
[Wang, Sheng-Hsiang; Tsay, Si-Chee; Hsu, N. Christina; Bell, Shaun W.; Li, Can; Ji, Qiang; Jeong, Myeong-Jae; Hansell, Richard A.; Welton, Ellsworth J.; Holben, Brent N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wang, Sheng-Hsiang; Li, Can; Ji, Qiang; Hansell, Richard A.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Bell, Shaun W.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Jeong, Myeong-Jae] Gangneung Wonju Natl Univ, Dept Atmospher & Environm Sci, Kangnung, Gangwon Do, South Korea.
[Chu, Yu-Chi; Chang, Shuenn-Chin; Liu, Jyh-Jian; Chiang, Wei-Li] Taiwan Environm Protect Adm, Taipei, Taiwan.
RP Lin, NH (reprint author), Natl Cent Univ, Dept Atmospher Sci, Chungli 32054, Taiwan.
EM nhlin@cc.ncu.edu.tw
RI Li, Can/F-6867-2011; Jeong, Myeong/B-8803-2008; Welton,
Ellsworth/A-8362-2012; Ma, Wentao/A-8800-2010; Hsu, N.
Christina/H-3420-2013; Tsay, Si-Chee/J-1147-2014; Hansell,
Richard/J-2065-2014; Wang, Sheng-Hsiang/F-4532-2010
OI Wang, Sheng-Hsiang/0000-0001-9675-3135
FU NASA; Taiwan EPA [EPA-99-FA11-03-A097]; National Science Council of
Taiwan [NSC98-2811-M-008-073]
FX This work was supported by the NASA Radiation Sciences Program managed
by Dr. Hal Maring, and the Taiwan EPA under contracts No.
EPA-99-FA11-03-A097, and also by the National Science Council of Taiwan
under grants No. NSC98-2811-M-008-073.
NR 15
TC 48
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U1 1
U2 26
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD SEP
PY 2011
VL 45
IS 27
BP 4804
EP 4808
DI 10.1016/j.atmosenv.2011.04.077
PG 5
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 807VM
UT WOS:000293931100028
ER
PT J
AU Yildiz, Y
Annaswamy, AM
Yanakiev, D
Kolmanovsky, I
AF Yildiz, Yildiray
Annaswamy, Anuradha M.
Yanakiev, Diana
Kolmanovsky, Ilya
TI Spark-Ignition-Engine Idle Speed Control: An Adaptive Control Approach
SO IEEE TRANSACTIONS ON CONTROL SYSTEMS TECHNOLOGY
LA English
DT Article
DE Adaptive control; delay effects; internal combustion (IC) engines; road
vehicles
ID DELAY SYSTEMS; CONTROL SCHEMES; ASSIGNMENT
AB The paper presents an application of a recently developed adaptive posicast controller (APC) for time-delay systems to the idle speed control (ISC) problem in spark ignition (SI) internal combustion (IC) engines. The objective is to regulate the engine speed to a prescribed set-point in the presence of accessory load torque disturbances such as those due to air conditioning and power steering. The adaptive controller, integrated with the existing proportional spark controller, is used to drive the electronic throttle actuator. We present both simulation and experimental results demonstrating the performance improvement by employing the adaptive controller. We also present the modifications and improvements to the controller structure which were developed during the course of experimentation to solve specific problems. In addition, the potential for the reduction in calibration time and effort which can be achieved with our approach is discussed.
C1 [Yildiz, Yildiray] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Annaswamy, Anuradha M.] MIT, Dept Mech Engn, Cambridge, MA 02139 USA.
[Yanakiev, Diana] Ford Motor Co, Res & Innovat Ctr, Dearborn, MI 48121 USA.
[Kolmanovsky, Ilya] Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA.
RP Yildiz, Y (reprint author), NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
EM yildiray.yildiz@nasa.gov; aanna@mit.edu; dyanakie@ford.com;
ilya@umich.edu
FU Ford-MIT Alliance Initiative
FX Manuscript received May 19, 2009; revised May 02, 2010; accepted August
05, 2010. Manuscript received in final form September 13, 2010. Date of
publication November 09, 2010; date of current version August 17, 2011.
Recommended by Associate Editor Luigi Villani. This work was supported
through the Ford-MIT Alliance Initiative.
NR 37
TC 15
Z9 15
U1 1
U2 17
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1063-6536
J9 IEEE T CONTR SYST T
JI IEEE Trans. Control Syst. Technol.
PD SEP
PY 2011
VL 19
IS 5
BP 990
EP 1002
DI 10.1109/TCST.2010.2078818
PG 13
WC Automation & Control Systems; Engineering, Electrical & Electronic
SC Automation & Control Systems; Engineering
GA 808MQ
UT WOS:000293982200004
ER
PT J
AU Singh, RP
Daniels, VR
Crady, CJ
Derendorf, H
Putcha, L
AF Singh, Rajendra P.
Daniels, Vernie R.
Crady, Camille J.
Derendorf, Hartmut
Putcha, Lakshmi
TI Pharmacokinetics of intranasal scopolamine gel formulation during
antiorthostatic bedrest - a microgravity analog
SO JOURNAL OF CLINICAL PHARMACOLOGY
LA English
DT Meeting Abstract
C1 [Singh, Rajendra P.; Derendorf, Hartmut] Univ Florida, Gainesville, FL USA.
[Daniels, Vernie R.; Crady, Camille J.; Putcha, Lakshmi] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RI Derendorf, Hartmut/B-4628-2012
OI Derendorf, Hartmut/0000-0003-4016-1370
NR 0
TC 0
Z9 0
U1 0
U2 0
PU SAGE PUBLICATIONS INC
PI THOUSAND OAKS
PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA
SN 0091-2700
J9 J CLIN PHARMACOL
JI J. Clin. Pharmacol.
PD SEP
PY 2011
VL 51
IS 9
BP 1337
EP 1338
PG 2
WC Pharmacology & Pharmacy
SC Pharmacology & Pharmacy
GA 806EM
UT WOS:000293789100046
ER
PT J
AU Rosenzweig, C
AF Rosenzweig, Cynthia
TI All Climate Is Local Mayors are often better equipped than presidents to
cut greenhouse gases
SO SCIENTIFIC AMERICAN
LA English
DT Article
C1 [Rosenzweig, Cynthia] NASA, Goddard Inst Space Studies, New York, NY 10027 USA.
[Rosenzweig, Cynthia] Columbia Univ, Earth Inst, New York, NY 10027 USA.
RP Rosenzweig, C (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10027 USA.
NR 0
TC 4
Z9 4
U1 0
U2 2
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 0036-8733
J9 SCI AM
JI Sci.Am.
PD SEP
PY 2011
VL 305
IS 3
BP 70
EP 73
DI 10.1038/scientificamerican0911-70
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 808UK
UT WOS:000294004900031
PM 21870447
ER
PT J
AU Soibel, A
Frez, C
Ksendzov, A
Keo, S
Forouhar, S
Tsvid, G
Kipshidze, G
Shterengas, L
Belenky, G
AF Soibel, Alex
Frez, Cliff
Ksendzov, Alexander
Keo, Sam
Forouhar, Siamak
Tsvid, Gene
Kipshidze, Gela
Shterengas, Leon
Belenky, Gregory
TI The 3.0-3.2 mu m wavelength range narrow ridge waveguide Sb-based
semiconductor diode lasers operating up to 333 K
SO SEMICONDUCTOR SCIENCE AND TECHNOLOGY
LA English
DT Article
ID INTERBAND CASCADE LASERS
AB We have demonstrated Fabry-Perot single spatial mode antimonide-based type-I quantum-well ridge waveguide semiconductor diode lasers operating at 3.0-3.2 mu m wavelength in continuous mode up to 333 K. Internal optical loss in narrow ridge devices was significantly reduced by using thick Si(3)N(4) dielectric films for planarization. The fabricated lasers operate in CW mode at room temperature with output powers exceeding 5 mW and have power consumption of less than 0.2 W at the output power of 1 mW, which is the power level needed in many gas sensing applications.
C1 [Soibel, Alex; Frez, Cliff; Ksendzov, Alexander; Keo, Sam; Forouhar, Siamak] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tsvid, Gene; Kipshidze, Gela; Shterengas, Leon; Belenky, Gregory] SUNY Stony Brook, Stony Brook, NY 11794 USA.
RP Soibel, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Alexander.Soibel@jpl.nasa.gov
RI Soibel, Alexander/A-1313-2007
FU US Air Force Office of Scientific Research [FA95500810458,
FA95500810083]; National Science Foundation [DMR0710154]; Advanced
Environmental Monitoring and Control Program office of the National
Aeronautics and Space Administration; JPL Director's Research and
Development Fund (DRDF)
FX The research described in this paper was performed at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration (NASA) and at State
University of New York at Sony Brook (supported by US Air Force Office
of Scientific Research contract FA95500810458 and award FA95500810083,
and National Science Foundation under grant DMR0710154). This work was
supported by the Advanced Environmental Monitoring and Control Program
office of the National Aeronautics and Space Administration, by JPL
Director's Research and Development Fund (DRDF).
NR 13
TC 6
Z9 6
U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0268-1242
J9 SEMICOND SCI TECH
JI Semicond. Sci. Technol.
PD SEP
PY 2011
VL 26
IS 9
AR 095024
DI 10.1088/0268-1242/26/9/095024
PG 4
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Condensed Matter
SC Engineering; Materials Science; Physics
GA 807NC
UT WOS:000293904400026
ER
PT J
AU Doarn, CR
Merrell, RC
AF Doarn, Charles R.
Merrell, Ronald C.
TI Spacebridge to Armenia: A Look Back at Its Impact on Telemedicine in
Disaster Response
SO TELEMEDICINE AND E-HEALTH
LA English
DT Article
DE telemedicine; international health; disaster response
ID SPACE PROGRAM; TELECOMMUNICATIONS; EVOLUTION; MEDICINE
AB On December 7, 1988, an earthquake destroyed a significant portion of the Spitak Region of Soviet Armenia. The destruction resulted in significant death toll, building and infrastructure destroyed, and the displacement of hundreds of thousands of people. The entire local medical infrastructure was significantly damaged. Before the disaster, the space medical leadership of the United States and the Union of Soviet Socialist Republics were collaborating on joint activities in medicine and biology. The leaders of this collaborative effort devised an approach to support a disaster recovery utilizing telecommunications assets. This effort was focused on healthcare in a postdisaster event and became known as the Spacebridge to Armenia. This spacebridge was put in place 5 months after the calamity and operated for several months in the spring-summer of 1989. The spacebridge was extended to Ufa, Russia, in response to a second disaster. The influence of the Spacebridge to Armenia in the 20 years since has been significant. This article summarizes how telemedicine has evolved from the response to the earthquake in 1988. It presents lessons learned and illustrates the many influences that have been made.
C1 [Doarn, Charles R.] Univ Cincinnati, Dept Publ Hlth Sci, Cincinnati, OH 45267 USA.
[Doarn, Charles R.] NASA, Off Chief Hlth & Med Officer, Washington, DC 20546 USA.
[Merrell, Ronald C.] Virginia Commonwealth Univ, Dept Surg, Richmond, VA USA.
RP Doarn, CR (reprint author), Univ Cincinnati, Dept Publ Hlth Sci, 260 Stetson,Suite 4200,POB 670840,ML 0840, Cincinnati, OH 45267 USA.
EM charles.doarn@uc.edu
NR 18
TC 5
Z9 5
U1 0
U2 2
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1530-5627
J9 TELEMED E-HEALTH
JI Telemed. e-Health
PD SEP
PY 2011
VL 17
IS 7
BP 546
EP 552
DI 10.1089/tmj.2010.0212
PG 7
WC Health Care Sciences & Services
SC Health Care Sciences & Services
GA 809LS
UT WOS:000294058200006
PM 21718090
ER
PT J
AU Osterman, S
Green, J
Froning, C
Beland, S
Burgh, E
France, K
Penton, S
Delker, T
Ebbets, D
Sahnow, D
Bacinski, J
Kimble, R
Andrews, J
Wilkinson, E
McPhate, J
Siegmund, O
Ake, T
Aloisi, A
Biagetti, C
Diaz, R
Dixon, W
Friedman, S
Ghavamian, P
Goudfrooij, P
Hartig, G
Keyes, C
Lennon, D
Massa, D
Niemi, S
Oliveira, C
Osten, R
Proffitt, C
Smith, T
Soderblom, D
AF Osterman, S.
Green, J.
Froning, C.
Beland, S.
Burgh, E.
France, K.
Penton, S.
Delker, T.
Ebbets, D.
Sahnow, D.
Bacinski, J.
Kimble, R.
Andrews, J.
Wilkinson, E.
McPhate, J.
Siegmund, O.
Ake, T.
Aloisi, A.
Biagetti, C.
Diaz, R.
Dixon, W.
Friedman, S.
Ghavamian, P.
Goudfrooij, P.
Hartig, G.
Keyes, C.
Lennon, D.
Massa, D.
Niemi, S.
Oliveira, C.
Osten, R.
Proffitt, C.
Smith, T.
Soderblom, D.
TI The Cosmic Origins Spectrograph: on-orbit instrument performance
SO ASTROPHYSICS AND SPACE SCIENCE
LA English
DT Article
DE Hubble Space Telescope; Cosmic Origins Spectrograph; Ultraviolet
AB The Cosmic Origins Spectrograph (COS) was installed in the Hubble Space Telescope in May, 2009 as part of Servicing Mission 4 to provide high sensitivity, medium and low resolution spectroscopy at far- and near-ultraviolet wavelengths (FUV, NUV). COS is the most sensitive FUV/NUV spectrograph flown to date, spanning the wavelength range from 900 to 3200 with peak effective area approaching 3000 cm(2). This paper describes instrument design, the results of the Servicing Mission Orbital Verification (SMOV), and the ongoing performance monitoring program.
C1 [Osterman, S.; Green, J.; Froning, C.; Beland, S.; Burgh, E.; France, K.; Penton, S.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Delker, T.; Ebbets, D.] Ball Aerosp Technol Corp, Boulder, CO 80301 USA.
[Sahnow, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Bacinski, J.; Kimble, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Andrews, J.; Wilkinson, E.] SW Res Inst, Boulder, CO 80302 USA.
[McPhate, J.; Siegmund, O.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Ake, T.; Aloisi, A.; Biagetti, C.; Diaz, R.; Dixon, W.; Friedman, S.; Ghavamian, P.; Goudfrooij, P.; Hartig, G.; Keyes, C.; Lennon, D.; Massa, D.; Niemi, S.; Oliveira, C.; Osten, R.; Proffitt, C.; Smith, T.; Soderblom, D.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Osterman, S (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, Campus Box 391, Boulder, CO 80309 USA.
EM steve.osterman@colorado.edu
RI Kimble, Randy/D-5317-2012;
OI Lennon, Daniel/0000-0003-3063-4867
NR 27
TC 71
Z9 72
U1 0
U2 7
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0004-640X
J9 ASTROPHYS SPACE SCI
JI Astrophys. Space Sci.
PD SEP
PY 2011
VL 335
IS 1
BP 257
EP 265
DI 10.1007/s10509-011-0699-5
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 804CP
UT WOS:000293631900037
ER
PT J
AU Forney, KA
Kobayashi, DR
Johnston, DW
Marchetti, JA
Marsik, MG
AF Forney, Karin A.
Kobayashi, Donald R.
Johnston, David W.
Marchetti, Jamie A.
Marsik, Michael G.
TI What's the catch? Patterns of cetacean bycatch and depredation in
Hawaii-based pelagic longline fisheries
SO MARINE ECOLOGY-AN EVOLUTIONARY PERSPECTIVE
LA English
DT Article
DE Bycatch; cetacean; depredation; false killer whale; generalized additive
models; pelagic longline
ID MARINE MAMMALS; IMPACTS; US
AB U.S. Pacific pelagic longline fisheries operating in the central North Pacific have been subject to a series of regulations to reduce bycatch of protected species, including seabirds and sea turtles. Cetaceans are also occasionally caught, and the bycatch of false killer whales, Pseudorca crassidens, in the Hawaii-based deep-set longline fishery currently exceeds allowable levels under the Marine Mammal Protection Act (MMPA). In this study, we examined longline observer data collected between 1994 and 2009, with emphasis on 2003-2009, to identify patterns of cetacean bycatch and depredation in relation to area, time, vessel, habitat variables, fishing gear, and set characteristics. The objectives of these analyses were to identify relationships amongst fishery interaction rates and variables that could provide opportunities to reduce depredation by cetaceans, reduce the likelihood of incidentally catching a cetacean when present, or reduce the severity of injuries to cetaceans if caught. The results of this study were provided to the False Killer Whale Take Reduction Team, convened under the MMPA, as they developed a plan to reduce serious injury and mortality of false killer whales in these fisheries. No correlates were identified that could markedly reduce depredation rates, but a slight (16%) reduction in repeat depredation within a fishing trip was evident when vessels moved at least 100 km following a depredation event. The most practical option for reducing bycatch of false killer whales was determined to be the use of small (14/0-16/0) circle hooks, which could result in an estimated 6% reduction in bycatch and a greater likelihood of releasing animals with non-serious injuries. Additional research is needed to address unresolved questions relating to processes involved in depredation events and hookings or entanglements of false killer whales.
C1 [Forney, Karin A.] NOAA, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Santa Cruz, CA USA.
[Kobayashi, Donald R.] NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI USA.
[Johnston, David W.] Duke Univ, Marine Lab, Div Marine Sci & Conservat, Nicholas Sch Environm, Beaufort, NC 28516 USA.
[Marchetti, Jamie A.; Marsik, Michael G.] NOAA, Pacific Isl Reg Off, Natl Marine Fisheries Serv, Honolulu, HI USA.
RP Forney, KA (reprint author), NOAA, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, 110 Shaffer Rd, Santa Cruz, CA USA.
EM karin.forney@noaa.gov
FU NMFS Pacific Islands Region, Pacific Islands Fisheries Science Center;
Southwest Fisheries Science Center
FX We wish to thank the many observers and staff members of the observer
program who spent long hours collecting, entering, and verifying the
observer data that formed the basis of this analysis, and the fishing
industry for their cooperation with observers at sea. The members of the
False Killer Whale Take Reduction Team provided valuable input and
feedback on several of the analyses presented. Funding for this research
was provided by the NMFS Pacific Islands Region, Pacific Islands
Fisheries Science Center, and the Southwest Fisheries Science Center.
This manuscript was improved by the helpful reviews of S. Benson, J.
Carretta, W. Perrin, N. Young and two anonymous reviewers. Special
thanks to Lisa Levin for inviting the lead author (K.A.F.) to contribute
to this special issue honoring Paul Dayton. Paul has been an incredible
friend and mentor, sharing his unique ecological insights, boundless
enthusiasm, and dedication to marine conservation with so many students
of diverse disciplines. I am grateful to count myself among them - thank
you, Paul!
NR 28
TC 14
Z9 16
U1 2
U2 28
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0173-9565
EI 1439-0485
J9 MAR ECOL-EVOL PERSP
JI Mar. Ecol.-Evol. Persp.
PD SEP
PY 2011
VL 32
IS 3
BP 380
EP 391
DI 10.1111/j.1439-0485.2011.00454.x
PG 12
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 803DD
UT WOS:000293560400012
ER
PT J
AU Mielke, SP
Kiang, NY
Blankenship, RE
Gunner, MR
Mauzerall, D
AF Mielke, S. P.
Kiang, N. Y.
Blankenship, R. E.
Gunner, M. R.
Mauzerall, D.
TI Efficiency of photosynthesis in a Chl d-utilizing cyanobacterium is
comparable to or higher than that in Chl a-utilizing oxygenic species
SO BIOCHIMICA ET BIOPHYSICA ACTA-BIOENERGETICS
LA English
DT Article
DE Acaryochloris marina; Oxygenic photosynthesis; Energy-storage
efficiency; Photoacoustics
ID D-DOMINATED CYANOBACTERIUM; PHOTOSYSTEM-II; CHLOROPHYLL-D;
ACARYOCHLORIS-MARINA; ELECTRON-TRANSFER; CHARGE RECOMBINATION;
ENERGY-STORAGE; SPECIAL PAIR; KINETICS; TIME
AB The cyanobacterium Acaryochloris marina uses chlorophyll d to carry out oxygenic photosynthesis in environments depleted in visible and enhanced in lower-energy, far-red light. However, the extent to which low photon energies limit the efficiency of oxygenic photochemistry in A. marina is not known. Here, we report the first direct measurements of the energy-storage efficiency of the photosynthetic light reactions in A. marina whole cells, and find it is comparable to or higher than that in typical, chlorophyll a-utilizing oxygenic species. This finding indicates that oxygenic photosynthesis is not fundamentally limited at the photon energies employed by A. marina, and therefore is potentially viable in even longer-wavelength light environments. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Mielke, S. P.; Kiang, N. Y.] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10027 USA.
[Mielke, S. P.; Mauzerall, D.] Rockefeller Univ, Lab Photobiol, New York, NY 10021 USA.
[Blankenship, R. E.] Washington Univ, Dept Biol, St Louis, MO 63130 USA.
[Blankenship, R. E.] Washington Univ, Dept Chem, St Louis, MO 63130 USA.
[Gunner, M. R.] CUNY City Coll, Dept Phys, New York, NY USA.
RP Mielke, SP (reprint author), Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10027 USA.
EM smielke@giss.nasa.gov
FU NASA [NNX08AP62G]; Photosynthetic Antenna Research Center (PARC); DOE,
Office of Science, Office of Basic Energy Sciences [DE-SC 0001035]; DOE
[DE-SC 0001423]; NIH [5G12 RR03060]
FX We are grateful to Irena Zielinski-Large for technical support; Mr.
Xianglu Li and Dr. Min Chen for critical advice on culturing
Acaryochloris marina; Prof. Shmuel Malkin and Dr. Minghui Dong for
helpful discussions; the NASA Astrobiology Institute, Dr. Carl Pilcher,
and Prof. Victoria Meadows for support by a NASA Postdoctoral Program
fellowship and Director's Discretionary Fund grant. This research is
partially supported by the Photosynthetic Antenna Research Center
(PARC), an Energy Frontier Research Center funded by the DOE, Office of
Science, Office of Basic Energy Sciences under Award Number DE-SC
0001035. REB also thanks the Exobiology program of NASA for support
under grant number NNX08AP62G. MRG acknowledges DOE Grant DE-SC 0001423
and infrastructure support from the NIH Grant 5G12 RR03060.
NR 35
TC 18
Z9 20
U1 1
U2 18
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0005-2728
J9 BBA-BIOENERGETICS
JI Biochim. Biophys. Acta-Bioenerg.
PD SEP
PY 2011
VL 1807
IS 9
BP 1231
EP 1236
DI 10.1016/j.bbabio.2011.06.007
PG 6
WC Biochemistry & Molecular Biology; Biophysics
SC Biochemistry & Molecular Biology; Biophysics
GA 802ZU
UT WOS:000293550300024
PM 21708123
ER
PT J
AU Carton, JA
Hakkinen, S
AF Carton, James A.
Hakkinen, Sirpa
TI Introduction to: Atlantic Meridional Overturning Circulation (AMOC)
SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY
LA English
DT Editorial Material
C1 [Carton, James A.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Hakkinen, Sirpa] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Carton, JA (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
EM carton@atmos.umd.edu
RI Hakkinen, Sirpa/E-1461-2012; carton, james/C-4807-2009
OI carton, james/0000-0003-0598-5198
NR 21
TC 4
Z9 4
U1 0
U2 13
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0645
J9 DEEP-SEA RES PT II
JI Deep-Sea Res. Part II-Top. Stud. Oceanogr.
PD SEP
PY 2011
VL 58
IS 17-18
BP 1741
EP 1743
DI 10.1016/j.dsr2.2010.10.055
PG 3
WC Oceanography
SC Oceanography
GA 801ZY
UT WOS:000293480300001
ER
PT J
AU McGovern, A
Wagstaff, KL
AF McGovern, Amy
Wagstaff, Kiri L.
TI Machine learning in space: extending our reach
SO MACHINE LEARNING
LA English
DT Article
DE Space missions; Machine learning applications; Autonomy
ID MARS
AB We introduce the challenge of using machine learning effectively in space applications and motivate the domain for future researchers. Machine learning can be used to enable greater autonomy to improve the duration, reliability, cost-effectiveness, and science return of space missions. In addition to the challenges provided by the nature of space itself, the requirements of a space mission severely limit the use of many current machine learning approaches, and we encourage researchers to explore new ways to address these challenges.
C1 [Wagstaff, Kiri L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[McGovern, Amy] Univ Oklahoma, Sch Comp Sci, Norman, OK 73019 USA.
RP Wagstaff, KL (reprint author), CALTECH, Jet Prop Lab, Mail Stop 306-463,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM amcgovern@ou.edu; kiri.wagstaff@jpl.nasa.gov
OI Wagstaff, Kiri/0000-0003-4401-5506
FU University of Oklahoma; National Aeronautics and Space Administration
FX The writing of this paper was supported by the University of Oklahoma
and 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 14
TC 0
Z9 0
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0885-6125
J9 MACH LEARN
JI Mach. Learn.
PD SEP
PY 2011
VL 84
IS 3
BP 335
EP 340
DI 10.1007/s10994-011-5249-4
PG 6
WC Computer Science, Artificial Intelligence
SC Computer Science
GA 799OY
UT WOS:000293297200003
ER
PT J
AU Burl, MC
Wetzler, PG
AF Burl, Michael C.
Wetzler, Philipp G.
TI Onboard object recognition for planetary exploration
SO MACHINE LEARNING
LA English
DT Article
DE Support vector machines; Convolution; Run-time efficiency;
Overlap-and-add; Crater detection
ID SUPPORT VECTOR MACHINES; FACE DETECTION; ALGORITHMS
AB Machine learning techniques have shown considerable promise for automating common visual inspection tasks such as the detection of human faces in cluttered scenes. Here, we examine whether similar techniques can be used (or adapted) for the problem of automatically locating geologic landforms in planetary images gathered by spacecraft. Beyond enabling more efficient and comprehensive ground analysis of down-linked data, we are aiming toward perceptive spacecraft that use onboard processing to autonomously analyze their collected imagery and take appropriate actions. In our current study, we have employed various supervised learning algorithms, including neural networks, ensemble methods, support vector machines (SVM), and continuously-scalable template models (CSTM) to derive detectors for craters from ground-truthed images. The resulting detectors are evaluated on a challenging set of Viking Orbiter images of Mars containing roughly one thousand craters. The SVM approach with normalized image patches provides detection and localization performance closest to that of human labelers and is shown to be substantially superior to boundary-based approaches such as the Hough transform. However, the run-time cost in applying the SVM solution in the standard way (spatial scanning in which the SVM is applied to each patch of the image on a window-by-window basis) is too high due both to the number of support vectors required and the number of test vectors generated by sliding a window across the data. We have developed an implementation using FFTs and the overlap-and-add technique, which can be used to efficiently apply SVMs to sensor data in resource-constrained environments such as on a spacecraft. The technique allows exact computation of the SVM decision function over an image using minimal RAM (typically less than 5% of the size of the image) and only O(n(s) (log(2) d + 11)) real multiplications per pixel for spatial scanning. Our approach is complementary to reduced set methods providing (in theory) a multiplicative gain in performance.
C1 [Burl, Michael C.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Wetzler, Philipp G.] Univ Colorado, Boulder, CO 80309 USA.
RP Burl, MC (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Michael.C.Burl@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This work was performed in part at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration.
NR 48
TC 3
Z9 4
U1 0
U2 13
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0885-6125
J9 MACH LEARN
JI Mach. Learn.
PD SEP
PY 2011
VL 84
IS 3
BP 341
EP 367
DI 10.1007/s10994-011-5239-6
PG 27
WC Computer Science, Artificial Intelligence
SC Computer Science
GA 799OY
UT WOS:000293297200004
ER
PT J
AU Ryan, S
Christiansen, EL
AF Ryan, S.
Christiansen, E. L.
TI A ballistic limit analysis programme for shielding against
micrometeoroids and orbital debris
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Ballistic limit; Space debris; Hypervelocity impact; Risk assessment
ID NONSPHERICAL PROJECTILES; HYPERVELOCITY IMPACTS; MANNED SPACECRAFT;
EQUATIONS
AB A software programme has been developed that enables the user to quickly and simply perform ballistic limit calculations for common spacecraft structures that are subjected to hypervelocity impact of micrometeoroid and orbital debris (MMOD) projectiles. This analysis programme consists of two core modules: design and performance. The design module enables a user to calculate preliminary dimensions of a shield configuration (e.g. thicknesses/areal densities, spacing, etc.) for a "design" particle (diameter, density, impact velocity, and incidence). The performance module enables a more detailed shielding analysis, providing the particle size that is "stopped" by a user-defined shielding configuration over the range of relevant in-orbit impact conditions. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Christiansen, E. L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX USA.
EM shannon.ryan@dsto.defence.gov.au; eric.l.christiansen@nasa.gov
NR 27
TC 7
Z9 8
U1 2
U2 7
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD SEP-OCT
PY 2011
VL 69
IS 5-6
BP 245
EP 257
DI 10.1016/j.actaastro.2011.04.012
PG 13
WC Engineering, Aerospace
SC Engineering
GA 791MP
UT WOS:000292669600003
ER
PT J
AU Sherwood, B
AF Sherwood, Brent
TI Comparing future options for human space flight
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Human space flight; Exploration; Mars; Moon; Space solar power; Tourism;
Passenger travel; Colonization; Myth; Strategy
AB The paper analyzes the "value proposition" for government-funded human space flight, a vexing question that persistently dogs efforts to justify its $10(10)/year expense in the US. The original Mercury/Gemini/Apollo value proposition is not valid today. Neither was it the value proposition actually promoted by von Braun, which the post-Apollo 80% of human space flight history has persistently attempted to fulfill. Divergent potential objectives for human space flight are captured in four strategic options Explore Mars; accelerate Space Passenger Travel; enable Space Power for Earth; and Settle the Moon-which are then analyzed for their purpose, societal myth, legacy benefits, core needs, and result as measured by the number and type of humans they would fly in space. This simple framework is proposed as a way to support productive dialog with public and other stakeholders, to determine a sustainable value proposition for human space flight. (C) 2011 Elsevier Ltd. All rights reserved.
C1 NASA, Jet Prop Lab, Off 150, Pasadena, CA 91109 USA.
RP Sherwood, B (reprint author), NASA, Jet Prop Lab, Off 150, 4800 Oak Drove Dr,M-S 301-335, Pasadena, CA 91109 USA.
EM brent.sherwood@jpl.nasa.gov
NR 24
TC 5
Z9 5
U1 1
U2 12
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD SEP-OCT
PY 2011
VL 69
IS 5-6
BP 346
EP 353
DI 10.1016/j.actaastro.2011.04.006
PG 8
WC Engineering, Aerospace
SC Engineering
GA 791MP
UT WOS:000292669600012
ER
PT J
AU Williams, B
Klein, G
Reid, I
AF Williams, Brian
Klein, Georg
Reid, Ian
TI Automatic Relocalization and Loop Closing for Real-Time Monocular SLAM
SO IEEE TRANSACTIONS ON PATTERN ANALYSIS AND MACHINE INTELLIGENCE
LA English
DT Article
DE Tracking; 3D/stereo scene analysis; autonomous vehicles
ID RANDOMIZED TREES; RECOGNITION
AB Monocular SLAM has the potential to turn inexpensive cameras into powerful pose sensors for applications such as robotics and augmented reality. We present a relocalization module for such systems which solves some of the problems encountered by previous monocular SLAM systems-tracking failure, map merging, and loop closure detection. This module extends recent advances in keypoint recognition to determine the camera pose relative to the landmarks within a single frame time of 33 ms. We first show how this module can be used to improve the robustness of these systems. Blur, sudden motion, and occlusion can all cause tracking to fail, leading to a corrupted map. Using the relocalization module, the system can automatically detect and recover from tracking failure while preserving map integrity. Extensive tests show that the system can then reliably generate maps for long sequences even in the presence of frequent tracking failure. We then show that the relocalization module can be used to recognize overlap in maps, i.e., when the camera has returned to a previously mapped area. Having established an overlap, we determine the relative pose of the maps using trajectory alignment so that independent maps can be merged and loop closure events can be recognized. The system combining all of these abilities is able to map larger environments and for significantly longer periods than previous systems.
C1 [Williams, Brian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Klein, Georg] Microsoft Corp, Seattle, WA 98112 USA.
[Reid, Ian] Univ Oxford, Dept Engn Sci, Oxford OX1 3PJ, England.
RP Williams, B (reprint author), CALTECH, Jet Prop Lab, M-S 198-233J,Oak Grove Dr, Pasadena, CA 91109 USA.
EM Brian.P.Williams@jpl.nasa.gov; gk@robots.ox.ac.uk; ian@robots.ox.ac.uk
FU EPSRC [GR/T24685, GR/S97774, EP/D037077]
FX This work was supported by the EPSRC through grants GR/T24685,
GR/S97774, and EP/D037077 and a studentship to BW. The authors are
grateful for discussions with Andrew Davison, Juan Tardo's, Jose Neira,
David Murray, and Tom Drummond, and to the Ashmolean and Natural History
Museums for granting filming permission.
NR 22
TC 19
Z9 21
U1 3
U2 14
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 0162-8828
J9 IEEE T PATTERN ANAL
JI IEEE Trans. Pattern Anal. Mach. Intell.
PD SEP
PY 2011
VL 33
IS 9
BP 1699
EP 1712
DI 10.1109/TPAMI.2011.41
PG 14
WC Computer Science, Artificial Intelligence; Engineering, Electrical &
Electronic
SC Computer Science; Engineering
GA 792JN
UT WOS:000292740000001
PM 21358004
ER
PT J
AU Palm, SP
Yang, YK
Spinhirne, JD
Marshak, A
AF Palm, Stephen P.
Yang, Yuekui
Spinhirne, James D.
Marshak, Alexander
TI Satellite remote sensing of blowing snow properties over Antarctica
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID MESOSCALE-PREDICTION-SYSTEM; ATMOSPHERIC ICE CRYSTALS; GLAS ALTIMETRY;
SEA-ICE; PART I; REDISTRIBUTION; BUDGET; AIR; SUBLIMATION; PLATEAU
AB A new technique for the detection of blowing snow events using satellite lidar data is applied to Cloud-Aerosol LIdar with Orthogonal Polarization (CALIOP) observations to obtain the spatial and temporal frequency, layer height, and optical depth of blowing snow events over Antarctica for 2007 through 2009. In addition, spatially and temporally collocated multichannel Moderate resolution Imaging Spectroradiometer (MODIS) data are utilized for the detection of two blowing snow events in sunlight. Blowing snow frequency as high as 70% is found to occur in some regions of Antarctica during winter. The spatial distribution of blowing snow closely follows the katabatic wind pattern with the exception of an area in East Antarctica that encompasses the megadune region, where the most persistent and largest area of blowing snow occurs. Layer thickness ranges from the minimum detectable (30 m) to about 1000 m with an average depth of 120 m for all blowing snow events. The layer optical depth estimated from the lidar data ranged from 0.05 to 1.0 with an average of 0.20. A very large, organized blowing snow "storm" is tracked over 3 days and is estimated to transport a mass of 6.3 x 10(3) kg m(-1) d(-1) which is comparable to surface-based measurements of mass transport during blowing snow events. Results from the application of the retrieval technique to ICESat data are also presented with a demonstration of the large multiple scattering-induced elevation error that blowing snow layers can cause.
C1 [Marshak, Alexander] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA.
[Spinhirne, James D.] Univ Arizona, Dept Elect & Comp Engn, Tucson, AZ 85721 USA.
[Yang, Yuekui] Univ Space Res Assoc, Columbia, MD 21044 USA.
RP Palm, SP (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
EM stephen.p.palm@nasa.gov
RI Marshak, Alexander/D-5671-2012; Yang, Yuekui/B-4326-2015
FU NASA Headquarters
FX The authors are sincerely grateful to Thomas Wagner, the Cryosphere
Program Manager at NASA Headquarters, for providing the funding and
encouragement to perform this blowing snow study. We also thank the NASA
Langley Research Center's Atmospheric Science Data Center for supplying
the CALIPSO data used in this research and Julien Nicolas of the Byrd
Polar Research Center at Ohio State University for supplying the AMPS 10
m wind speeds.
NR 44
TC 16
Z9 19
U1 2
U2 28
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 AUG 30
PY 2011
VL 116
AR D16123
DI 10.1029/2011JD015828
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 816TV
UT WOS:000294625900001
ER
PT J
AU Villanueva, GL
Mumma, MJ
Magee-Sauer, K
AF Villanueva, G. L.
Mumma, M. J.
Magee-Sauer, K.
TI Ethane in planetary and cometary atmospheres: Transmittance and
fluorescence models of the nu(7) band at 3.3 mu m
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID HALF-WIDTH COEFFICIENTS; INFRARED SOLAR SPECTRUM; INTERNAL PARTITION
SUMS; C/1999 H1 LEE; LINE PARAMETERS; SPECTROSCOPIC MEASUREMENTS; HITRAN
DATABASE; CROSS-SECTIONS; ISOTOPIC CO2; C2H6
AB Ethane and other hydrocarbon gases have strong rovibrational transitions in the 3.3 mu m spectral region owing to C-H, CH2, and CH3 vibrational modes, making this spectral region prime for searching possible biomarker gases in extraterrestrial atmospheres (e. g., Mars, exoplanets) and organic molecules in comets. However, removing ethane spectral signatures from high-resolution terrestrial transmittance spectra has been imperfect because existing quantum mechanical models have been unable to reproduce the observed spectra with sufficient accuracy. To redress this problem, we constructed a line-by-line model for the nu(7) band of ethane (C2H6) and applied it to compute telluric transmittances and cometary fluorescence efficiencies. Our model considers accurate spectral parameters, vibration-rotation interactions, and a functional characterization of the torsional hot band. We integrated the new band model into an advanced radiative transfer code for synthesizing the terrestrial atmosphere (LBLRTM), achieving excellent agreement with transmittance data recorded against Mars using three different instruments located in the Northern and Southern hemispheres. The retrieved ethane abundances demonstrate the strong hemispheric asymmetry noted in prior surveys of volatile hydrocarbons. We also retrieved sensitive limits for the abundance of ethane on Mars. The most critical validation of the model was obtained by comparing simulations of C2H6 fluorescent emission with spectra of three hydrocarbon-rich comets: C/2004 Q2 (Machholz), 8P/Tuttle, and C/2007W1 (Boattini). The new model accurately describes the complex emission morphology of the nu(7) band at low rotational temperatures and greatly increases the confidence of the retrieved production rates (and rotational temperatures) with respect to previously available fluorescence models.
C1 [Villanueva, G. L.; Mumma, M. J.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Magee-Sauer, K.] Rowan Univ, Dept Phys & Astron, Glassboro, NJ 08028 USA.
[Villanueva, G. L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Villanueva, GL (reprint author), NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Mailstop 690-3, Greenbelt, MD 20771 USA.
EM villanueva@nasa.gov
RI Magee-Sauer, Karen/K-6061-2015; mumma, michael/I-2764-2013
OI Magee-Sauer, Karen/0000-0002-4979-9875;
FU NASA [08-PAST08-0034, 08-PATM08-0031, RTOP 344-32-07, RTOP 344-53-51];
National Science Foundation
FX G. L. V. acknowledges support from NASA's Planetary Astronomy Program
(08-PAST08-0034) and Planetary Atmospheres Program (08-PATM08-0031).
M.J.M. was supported by NASA's Planetary Astronomy Program (RTOP
344-32-07) and Astrobiology Program (RTOP 344-53-51). K. M. S. was
supported by the Planetary Astronomy RUI program of the National Science
Foundation. We thank Hans-Ulrich Kaufl for assisting with the Mars
(CRIRES) observations in 2009, and Robert Novak and Avram M. Mandell for
assisting with the acquisition of Mars (CSHELL) data in 2006. We thank
the staff at the VLT Observatory (operated by ESO), W. M. Keck
Observatory (operated as a scientific partnership among Caltech, UCLA,
and NASA), and NASA's InfraRed Telescope Facility (operated for NASA by
the University of Hawaii) for their exceptional support throughout our
long Mars and cometary observing programs. The authors want to recognize
and acknowledge the significant cultural role and reverence that the
summit of Mauna Kea has always had within the indigenous Hawaiian
community. We are most fortunate to have the opportunity to conduct
observations from this mountain.
NR 58
TC 17
Z9 17
U1 1
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD AUG 30
PY 2011
VL 116
AR E08012
DI 10.1029/2010JE003794
PG 23
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 816TY
UT WOS:000294626200001
ER
PT J
AU Allen, M
Witasse, O
AF Allen, Mark
Witasse, Olivier
TI Remote sensing for atmospheric evidence of Martian habitability and
habitancy
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Allen, Mark] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Witasse, Olivier] European Space Agcy, Res & Sci Support Dept, NL-2200 AG Noordwijk, ZH, Netherlands.
EM Mark.Allen@jpl.nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 2
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 28-CASW
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378300857
ER
PT J
AU Aubrey, AD
Grunthaner, FJ
Greer, F
O'Neil, GD
Lee, MC
AF Aubrey, Andrew D.
Grunthaner, Frank J.
Greer, Frank
O'Neil, Glen D.
Lee, Michael C.
TI Lab-on-a-chip aqueous chemical sensing technologies for planetary
science
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Aubrey, Andrew D.; Grunthaner, Frank J.; Greer, Frank; Lee, Michael C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[O'Neil, Glen D.] Tufts Univ, Dept Chem, Medford, MA 02155 USA.
EM Andrew.D.Aubrey@jpl.nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 6
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 50-CASW
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378300882
ER
PT J
AU Bada, JL
Aubrey, A
Grunthaner, F
AF Bada, Jeffrey L.
Aubrey, Andrew
Grunthaner, Frank
TI Searching for organic compounds on Mars: Intensive in situ
investigations are required prerequisites to a sample return mission
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Bada, Jeffrey L.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Aubrey, Andrew; Grunthaner, Frank] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM jbada@ucsd.edu
NR 0
TC 0
Z9 0
U1 2
U2 5
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 34-CASW
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378300864
ER
PT J
AU Cable, ML
Beauchamp, PM
Stockton, AM
Mora, MF
Fisher, AM
Greer, HF
Willis, PA
AF Cable, Morgan L.
Beauchamp, Patricia M.
Stockton, Amanda M.
Mora, Maria F.
Fisher, Anita M.
Greer, Harold F.
Willis, Peter A.
TI Micro-total-analysis technologies for in situ organic analysis of Titan
environmental aerosols
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Cable, Morgan L.; Stockton, Amanda M.; Mora, Maria F.; Fisher, Anita M.; Greer, Harold F.; Willis, Peter A.] CALTECH, Div Instruments & Sci Data Syst, NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Beauchamp, Patricia M.] CALTECH, Strateg Missions & Adv Concepts Off, NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
EM Morgan.L.Cable@jpl.nasa.gov
RI Stockton, Amanda/C-1173-2012; Willis, Peter/I-6621-2012
NR 0
TC 0
Z9 0
U1 0
U2 3
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 217-ANYL
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378300576
ER
PT J
AU Cooper, MR
AF Cooper, Maya R.
TI Challenges of developing a food system for a Mars mission
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Cooper, Maya R.] NASA JSC, Space Food Syst Lab, Houston, TX 77058 USA.
EM maya.cooper@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 2
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 16-AGFD
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378300120
ER
PT J
AU Des Marais, DJ
AF Des Marais, David J.
TI Formation and preservation of evidence for habitable environments on
Mars
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Des Marais, David J.] NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM David.J.DesMarais@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 3
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 47-CASW
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378300878
ER
PT J
AU Glavin, DP
Conrad, P
Dworkin, JP
Eigenbrode, J
Mahaffy, PR
AF Glavin, Daniel P.
Conrad, Pan
Dworkin, Jason P.
Eigenbrode, Jennifer
Mahaffy, Paul R.
TI Search for chemical biomarkers on Mars using the sample analysis at Mars
Instrument Suite on the Mars Science Laboratory
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Glavin, Daniel P.; Conrad, Pan; Dworkin, Jason P.; Eigenbrode, Jennifer; Mahaffy, Paul R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM daniel.p.glavin@nasa.gov
RI Eigenbrode, Jennifer/D-4651-2012; Conrad, Pamela/F-1506-2012; Glavin,
Daniel/D-6194-2012; Dworkin, Jason/C-9417-2012
OI Conrad, Pamela/0000-0001-8805-7981; Glavin, Daniel/0000-0001-7779-7765;
Dworkin, Jason/0000-0002-3961-8997
NR 0
TC 0
Z9 0
U1 0
U2 4
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 35-CASW
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378300865
ER
PT J
AU Gordon, K
Penner, R
Bogert, P
Yost, WT
Siochi, E
AF Gordon, K.
Penner, R.
Bogert, P.
Yost, W. T.
Siochi, E.
TI Puncture self-healing polymers for aerospace applications
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Gordon, K.; Penner, R.; Bogert, P.; Yost, W. T.; Siochi, E.] NASA Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
EM k.l.gordon@larc.nasa.gov
NR 0
TC 0
Z9 0
U1 1
U2 8
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 110-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378306693
ER
PT J
AU Grunthaner, FJ
Coleman, M
Aubrey, AD
Mielke, R
Amashukeli, X
Bryson, C
AF Grunthaner, Frank J.
Coleman, Max
Aubrey, Andrew D.
Mielke, Randall
Amashukeli, Xenia
Bryson, Charles
TI Enabling technologies for in situ chemical astrobiology in planetary
exploration
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Grunthaner, Frank J.; Coleman, Max; Aubrey, Andrew D.; Mielke, Randall; Amashukeli, Xenia] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bryson, Charles] Apparati Inc, Mountain View, CA 94041 USA.
EM Frank.J.Grunthaner@JPL.NASA.gov
NR 0
TC 0
Z9 0
U1 0
U2 2
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 52-CASW
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378300884
ER
PT J
AU Hecht, MH
AF Hecht, Michael H.
TI Aqueous soil chemistry on a not-so-dry planet: Retrospective on the
Phoenix Wet Chemistry Laboratory
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Hecht, Michael H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM michael.h.hecht@jpl.nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 2
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 48-CASW
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378300879
ER
PT J
AU Jimenez, JL
Cubison, MJ
Ortega, AM
Hayes, PL
Farmer, DK
Day, DA
Lechner, MJ
Brune, WH
Apel, E
Diskin, GS
Fisher, JA
Fuelberg, HA
Hecobian, A
Knapp, DJ
Mikoviny, T
Riemer, D
Sachse, GW
Sessions, W
Weber, RJ
Weinheimer, AJ
Wisthaler, A
AF Jimenez, Jose L.
Cubison, Michael J.
Ortega, Amber M.
Hayes, Patrick L.
Farmer, Delphine K.
Day, Douglas A.
Lechner, Michael J.
Brune, William H.
Apel, Eric
Diskin, Glenn S.
Fisher, Jenny A.
Fuelberg, Henry A.
Hecobian, Arsineh
Knapp, David J.
Mikoviny, Tomas
Riemer, Daniel
Sachse, Glen W.
Sessions, Walter
Weber, Rodney J.
Weinheimer, Andrew J.
Wisthaler, Armin
TI Effects of aging on organic aerosol from open biomass burning smoke in
aircraft & lab studies
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Jimenez, Jose L.; Cubison, Michael J.; Ortega, Amber M.; Hayes, Patrick L.; Farmer, Delphine K.; Day, Douglas A.; Lechner, Michael J.] Univ Colorado, Dept Chem & Biochem, CIRES, Boulder, CO 80309 USA.
[Jimenez, Jose L.; Cubison, Michael J.; Ortega, Amber M.; Hayes, Patrick L.; Farmer, Delphine K.; Day, Douglas A.; Lechner, Michael J.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[Brune, William H.] Penn State Univ, University Pk, PA 16802 USA.
[Diskin, Glenn S.] NASA Langley Res Ctr, Washington, DC USA.
[Fisher, Jenny A.] Harvard Univ, Cambridge, MA 02138 USA.
[Fuelberg, Henry A.; Sessions, Walter] Florida State Univ, Tallahassee, FL 32306 USA.
[Hecobian, Arsineh; Weber, Rodney J.] Georgia Inst Technol, Atlanta, GA 30332 USA.
[Mikoviny, Tomas; Wisthaler, Armin] Univ Innsbruck, A-6020 Innsbruck, Austria.
[Riemer, Daniel] Univ Miami, Coral Gables, FL 33124 USA.
[Sachse, Glen W.] NIA, Bethesda, MD 20892 USA.
EM jose.jimenez@colorado.edu
RI Jimenez, Jose/A-5294-2008
OI Jimenez, Jose/0000-0001-6203-1847
NR 0
TC 0
Z9 0
U1 0
U2 11
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 106-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378305764
ER
PT J
AU Kennedy, MS
Economy, DR
Miller, SG
AF Kennedy, Marian S.
Economy, David R.
Miller, Sandi G.
TI Nanocomposite filler influence on thermal oxidative stability and
mechanical properties of polymers used in space applications
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Kennedy, Marian S.; Economy, David R.] Clemson Univ, Sch Mat Sci & Engn, Clemson, SC 29634 USA.
[Miller, Sandi G.] NASA, Struct & Mat Div, John H Glenn Res Ctr, Cleveland, OH 44135 USA.
EM mskenne@clemson.edu
RI Economy, David Ross/F-4877-2015
OI Economy, David Ross/0000-0003-1378-9488
NR 0
TC 0
Z9 0
U1 1
U2 5
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 180-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378306764
ER
PT J
AU Lorenzi, TM
Wohl, CJ
Penner, RK
Smith, JG
Siochi, EJ
AF Lorenzi, Tyler M.
Wohl, Christopher J.
Penner, Ronald K.
Smith, Joseph G.
Siochi, Emilie J.
TI Insect residue contamination on wing leading edge surfaces: A materials
investigation for mitigation
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Lorenzi, Tyler M.] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Wohl, Christopher J.; Smith, Joseph G.; Siochi, Emilie J.] NASA, Adv Mat & Proc Branch, Langley Res Ctr, Hampton, VA 23681 USA.
[Penner, Ronald K.] ATK Aerosp Syst Inc, Hampton, VA 23681 USA.
EM christopher.j.wohl@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 4
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 28-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378306866
ER
PT J
AU Mathies, RA
Stockton, AM
Jensen, EC
Benhabib, M
Chiesl, TN
AF Mathies, Richard A.
Stockton, Amanda M.
Jensen, Erik C.
Benhabib, Merwan
Chiesl, Thomas N.
TI Automated analysis of carbonaceous biomarkers with the Mars Organic
Analyzer microchip capillary electrophoresis system: Amines, amino
acids, aldehydes, ketones, carboxylic acids, and polycyclic aromatic
hydrocarbons
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Mathies, Richard A.; Stockton, Amanda M.; Chiesl, Thomas N.] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA.
[Stockton, Amanda M.] CALTECH, Jet Prop Lab, Div Instruments & Sci Data Syst, Pasadena, CA 91109 USA.
[Jensen, Erik C.] Univ Calif Berkeley, Biophys Grad Grp, Berkeley, CA 94720 USA.
[Chiesl, Thomas N.] Abbott Mol, Ibis Biosci, Carlsbad, CA 92008 USA.
[Benhabib, Merwan] Ondavia Inc, Haywood, CA 94545 USA.
EM amanda.m.stockton@jpl.nasa.gov
RI Stockton, Amanda/C-1173-2012
NR 0
TC 0
Z9 0
U1 1
U2 9
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 49-CASW
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378300880
ER
PT J
AU Meador, MAB
Guo, HQ
Nguyen, B
Vivod, SL
AF Meador, Mary Ann B.
Guo, Haiquan
Nguyen, Baochau
Vivod, Stephanie L.
TI Tailoring properties of aerogels for aerospace applications
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Meador, Mary Ann B.; Guo, Haiquan; Nguyen, Baochau; Vivod, Stephanie L.] NASA, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM maryann.meador@nasa.gov
NR 0
TC 0
Z9 0
U1 2
U2 9
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 336-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378307031
ER
PT J
AU Meador, MA
AF Meador, Michael A.
TI Nanotechnology at NASA: Future directions and funding opportunities in
nanostructured polymeric materials
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Meador, Michael A.] NASA, Polymers Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Michael.A.Meador@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 5
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 261-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378306847
ER
PT J
AU Novak, RE
Mumma, MJ
Villanueva, GL
AF Novak, Robert E.
Mumma, Michael J.
Villanueva, Geronimo L.
TI Physical properties and seasonal behavior of H2O, HDO, CO2 and trace
gases on Mars: Quantitative mapping from Earth-based observatories
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Novak, Robert E.] Iona Coll, Dept Phys, New Rochelle, NY 10801 USA.
[Mumma, Michael J.; Villanueva, Geronimo L.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM rnovak@iona.edu
RI mumma, michael/I-2764-2013
NR 0
TC 0
Z9 0
U1 0
U2 2
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 31-CASW
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378300861
ER
PT J
AU O'Neil, GD
Aubrey, AD
Greer, F
DeFlores, LP
Hecht, MH
AF O'Neil, Glen D.
Aubrey, Andrew D.
Greer, Frank
DeFlores, Lauren P.
Hecht, Michael H.
TI NERNST: An electrofluidic platform for planetary surface analysis
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [O'Neil, Glen D.; Hecht, Michael H.] Tufts Univ, Dept Chem, Medford, MA 02155 USA.
[Aubrey, Andrew D.; Greer, Frank; DeFlores, Lauren P.] CALTECH, Jet Prop Lab, Pasadena, CA 90019 USA.
EM Glen.O_Neil@tufts.edu
NR 0
TC 0
Z9 0
U1 0
U2 2
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 51-CASW
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378300883
ER
PT J
AU Smith, RL
Fast, KE
Kostiuk, T
Lefevre, F
Hewagama, T
Livengood, TA
AF Smith, Ramsey L.
Fast, Kelly E.
Kostiuk, Theodor
Lefevre, Franck
Hewagama, Tilak
Livengood, Timothy A.
TI Extended view of ozone and chemistry in the atmosphere of Mars
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Smith, Ramsey L.; Fast, Kelly E.; Kostiuk, Theodor; Hewagama, Tilak; Livengood, Timothy A.] NASA, Planetary Syst Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lefevre, Franck] CNRS, LATMOS, Paris, France.
[Hewagama, Tilak] Univ Maryland, College Pk, MD 20742 USA.
[Livengood, Timothy A.] Natl Ctr Earth & Space Sci Educ, Capital Hts, MD 20791 USA.
EM Ramsey.L.Smith@nasa.gov
RI Hewagama, T/C-8488-2012; Livengood, Timothy/C-8512-2012; Smith,
Ramsey/D-4710-2012; Kostiuk, Theodor/A-3077-2014
NR 0
TC 0
Z9 0
U1 0
U2 5
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 32-CASW
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378300862
ER
PT J
AU Stockton, AM
Mora, MF
Greer, F
Cable, ML
Fisher, AM
Jiao, H
AF Stockton, Amanda M.
Mora, Maria F.
Greer, Frank
Cable, Morgan L.
Fisher, Anita M.
Jiao, Hong
TI Automation of fluidic sample handling and analysis for extraterrestrial
chemical exploration
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Stockton, Amanda M.; Mora, Maria F.; Greer, Frank; Cable, Morgan L.; Fisher, Anita M.] CALTECH, Jet Prop Lab, Div Instruments & Sci Data Syst, Pasadena, CA 91109 USA.
[Jiao, Hong] Los Gatos Res Inc, Mountain View, CA 94041 USA.
EM amanda.m.stockton@jpl.nasa.gov
RI Stockton, Amanda/C-1173-2012
NR 0
TC 0
Z9 0
U1 0
U2 3
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 53-CASW
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378300885
ER
PT J
AU Tazaz, AM
Bebout, BM
Chanton, JP
Kelley, CA
Poole, J
AF Tazaz, Amanda M.
Bebout, Brad M.
Chanton, Jeffrey P.
Kelley, Cheryl A.
Poole, Jennifer
TI Isotopic expansion of traditional biogenic methane boundaries obtained
from data collected from Mars analog hypersaline ponds
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Tazaz, Amanda M.; Chanton, Jeffrey P.] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA.
[Kelley, Cheryl A.; Poole, Jennifer] Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA.
[Bebout, Brad M.] NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM amt02e@fsu.edu
NR 0
TC 0
Z9 0
U1 0
U2 3
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 33-CASW
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378300863
ER
PT J
AU Tsigaridis, K
Koch, D
Menon, S
AF Tsigaridis, Kostas
Koch, Dorothy
Menon, Surabi
TI Importance and uncertainties of sea spray sources and chemical
composition on climate
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Tsigaridis, Kostas; Koch, Dorothy] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
[Tsigaridis, Kostas; Koch, Dorothy] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Menon, Surabi] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
EM ktsigaridis@giss.nasa.gov
RI Tsigaridis, Kostas/K-8292-2012
OI Tsigaridis, Kostas/0000-0001-5328-819X
NR 0
TC 0
Z9 0
U1 0
U2 3
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 263-ENVR
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378302546
ER
PT J
AU Vivod, SL
Meador, MAB
Cakmak, M
Guo, HQ
AF Vivod, Stephanie L.
Meador, Mary Ann B.
Cakmak, Miko
Guo, Haiquan
TI Carbon nanofiber/polyimide aerogel thin films
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Vivod, Stephanie L.; Meador, Mary Ann B.] NASA, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Cakmak, Miko] Univ Akron, Akron, OH 44325 USA.
[Guo, Haiquan] Ohio Aerosp Inst, Cleveland, OH USA.
EM Stephanie.L.Vivod@nasa.gov
NR 0
TC 0
Z9 0
U1 2
U2 21
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 338-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378307033
ER
PT J
AU Webster, CR
Mahaffy, PR
AF Webster, Christopher R.
Mahaffy, Paul R.
TI Measuring stable isotope ratios in the Martian atmosphere sampled by
balloon, aircraft and surface rover
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Webster, Christopher R.] CALTECH, Jet Prop Lab, Planetary Sci Instruments Off, Pasadena, CA 91109 USA.
[Mahaffy, Paul R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Chris.R.Webster@jpl.nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 4
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 40-CASW
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378300871
ER
PT J
AU Wennberg, PO
Hipkin, V
Toon, G
Drummond, J
AF Wennberg, Paul O.
Hipkin, Victoria
Toon, Geoffrey
Drummond, James
TI Probing the chemical composition of the Martian atmosphere with solar
occultation Fourier transform infrared spectrometry
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Wennberg, Paul O.] CALTECH, Pasadena, CA 91104 USA.
[Hipkin, Victoria] Canadian Space Agcy, Montreal, PQ, Canada.
[Toon, Geoffrey] NASA Jet Prop Lab, Pasadena, CA USA.
[Drummond, James] Dalhousie Univ, Halifax, NS, Canada.
EM wennberg@caltech.edu
RI Drummond, James/O-7467-2014
NR 0
TC 0
Z9 0
U1 0
U2 3
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 29-CASW
PG 2
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378300858
ER
PT J
AU Wohl, CJ
Applin, SI
Cooper, LL
Connell, JW
AF Wohl, Christopher J.
Applin, Samantha I.
Cooper, Leanna L.
Connell, John W.
TI Copolyimide surface modifying agents for particle adhesion mitigation
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Wohl, Christopher J.; Connell, John W.] NASA, Adv Mat & Proc Branch, Langley Res Ctr, Hampton, VA 23681 USA.
EM christopher.j.wohl@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 2
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 31-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378307003
ER
PT J
AU Xu, JC
Hunter, GW
Biaggi-Labiosa, AM
Evans, LJ
Chang, CW
Berger, GM
AF Xu, Jennifer C.
Hunter, Gary W.
Biaggi-Labiosa, Azlin M.
Evans, Laura J.
Chang, Carl W.
Berger, Gordon M.
TI Nitric oxide microsensors for engine emission, environmental, and human
breath monitoring applications
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Xu, Jennifer C.; Hunter, Gary W.; Biaggi-Labiosa, Azlin M.; Evans, Laura J.] NASA, Sensor & Elect Branch, Glenn Res Ctr, Clevaland, OH 44135 USA.
[Chang, Carl W.] ASRC Aerosp Corp, Cleveland, OH 44135 USA.
[Berger, Gordon M.] Natl Ctr Space Explorat, Cleveland, OH 44135 USA.
EM Jennifer.C.Xu@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 4
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 8-ANYL
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378300631
ER
PT J
AU Yi, TH
Uvarov, C
Klavins, P
Bux, S
Fleurial, JP
Makhmudov, F
Abdusalyamova, M
Kauzlarich, S
AF Yi, Tanghong
Uvarov, Catherine
Klavins, Peter
Bux, Sabah
Fleurial, Jean-Pierre
Makhmudov, Farukh
Abdusalyamova, Maxsuda
Kauzlarich, Susan
TI Magnetism and transport properties of Te doped Yb14MnSb11
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Yi, Tanghong; Uvarov, Catherine; Kauzlarich, Susan] Univ Calif Davis, Dept Chem, Davis, CA 95616 USA.
[Klavins, Peter] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Bux, Sabah; Fleurial, Jean-Pierre] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Makhmudov, Farukh; Abdusalyamova, Maxsuda] Tajik Acad Sci, Inst Chem, Dushanbe, Tajikistan.
EM tyi@ucdavis.edu
NR 0
TC 0
Z9 0
U1 1
U2 3
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 159-INOR
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378303725
ER
PT J
AU Castellanos, P
Marufu, LT
Doddridge, BG
Taubman, BF
Schwab, JJ
Hains, JC
Ehrman, SH
Dickerson, RR
AF Castellanos, Patricia
Marufu, Lackson T.
Doddridge, Bruce G.
Taubman, Brett F.
Schwab, James J.
Hains, Jennifer C.
Ehrman, Sheryl H.
Dickerson, Russell R.
TI Ozone, oxides of nitrogen, and carbon monoxide during pollution events
over the eastern United States: An evaluation of emissions and vertical
mixing
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CMAQ MODELING SYSTEM; AIR-QUALITY; TRACE GAS; TRANSPORT; FOREST; CO;
ATLANTIC; DIOXIDE; SURFACE; SOILS
AB Chemical transport models such as the Community Multiscale Air Quality (CMAQ) model provide useful guidance on air pollution control strategies. We evaluate the performance of a 12 km resolution CMAQ simulation with surface and aircraft observations of CO, O-3, and NOx during the summer of 2002. When all data are considered, on average, modeled and observed CO total column contents (surface to 3,000 m) agreed to within 14% in the morning and 22% in the afternoon. Reducing the deposition velocity for CO improves model-measurement agreement but did not eliminate the model bias. The majority of observed vertical profiles have a maximum near the surface. Although many observed spirals had a secondary maximum at the top of the boundary layer, indicating subgrid-scale shallow convection. The model was not able to replicate these vertical structures. Water vapor profiles likewise showed greater vertical variability in the observations than in the model. General conclusions from these model-measurement comparisons: total CO emissions estimates are either adequate or underestimated, but there is no evidence of gross error; NOx emissions from mobile sources may be overestimated while the lifetime of NOx may be underestimated in CMAQ 4.5.1 with CBIV, and vertical mixing in the model boundary layer may be too fast, but venting out of the boundary layer into the lower free troposphere may be too slow.
C1 [Castellanos, Patricia; Ehrman, Sheryl H.] Univ Maryland, Dept Chem & Biomol Engn, College Pk, MD 20742 USA.
[Marufu, Lackson T.; Dickerson, Russell R.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Doddridge, Bruce G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Hains, Jennifer C.] Maryland Dept Environm, Baltimore, MD 21230 USA.
[Schwab, James J.] SUNY Albany, Atmospher Sci Res Ctr, Albany, NY 12203 USA.
[Taubman, Brett F.] Appalachian State Univ, Dept Chem, Boone, NC 28608 USA.
RP Castellanos, P (reprint author), Univ Maryland, Dept Chem & Biomol Engn, College Pk, MD 20742 USA.
EM russ@atmos.umd.edu
RI Dickerson, Russell/F-2857-2010
OI Dickerson, Russell/0000-0003-0206-3083
FU Maryland Department of the Environment
FX The authors would like to acknowledge Da-Lin Zhang for his help
regarding simulation and interpretation of meteorological fields. This
work is funded by the Maryland Department of the Environment.
NR 60
TC 18
Z9 19
U1 5
U2 26
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 AUG 27
PY 2011
VL 116
AR D16307
DI 10.1029/2010JD014540
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 813LS
UT WOS:000294368700001
ER
PT J
AU Lane, MD
Glotch, TD
Dyar, MD
Pieters, CM
Klima, R
Hiroi, T
Bishop, JL
Sunshine, J
AF Lane, Melissa D.
Glotch, Timothy D.
Dyar, M. Darby
Pieters, Carle M.
Klima, Rachel
Hiroi, Takahiro
Bishop, Janice L.
Sunshine, Jessica
TI Midinfrared spectroscopy of synthetic olivines: Thermal emission,
specular and diffuse reflectance, and attenuated total reflectance
studies of forsterite to fayalite
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MU-M; OPTICAL-CONSTANTS; SINGLE-CRYSTAL; PARTICULATE SURFACES; INFRARED
REFLECTANCE; VIBRATIONAL-SPECTRA; PARTICLE-SIZE; ABSORPTION-SPECTRA;
MINERALS; MARS
AB Synthetic olivine samples ranging in composition from forsterite to fayalite are analyzed in the midinfrared using thermal emission, specular and diffuse reflectance, and attenuated total reflectance spectroscopies to study the spectral effects of Mg-Fe solid solution. For each method, fundamental bands gradually change in position and strength from Mg2SiO4 at larger wave numbers to Fe2SiO4 at smaller wave numbers. Each spectrum is diagnostic of chemistry within the continuum, as previously noted. In this study, 10 identified fundamental bands are traceable across the solid solution series for each technique. In pelletized sample spectra, the 10 bands shift approximately linearly in position by as little as 11 to as much as 64 cm(-1). In powdered sample spectra, the bands shift by as little as 12 to as much as 74 cm(-1) (disregarding one outlier point). Moreover, for every spectral technique, an even larger linear shift is identified of a specific emissivity maximum/reflectivity minimum (the flection position). From forsterite to fayalite, this flection position shifts by at least 88 cm(-1), which is, on average, 48% more than the largest fundamental band shift within the same data set for the pelletized spectra and 44% more for the powdered spectra. Also the R-2 and 2 sigma values of the best fit line for the flection position shift (versus Fo#) generally were as good as or routinely better than those of the fundamental bands. Thus, the flection position should be considered as a means of determining Mg-Fe olivine composition when using thermal emission, specular reflectance, diffuse reflectance, or attenuated total reflectance spectroscopic data.
C1 [Lane, Melissa D.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Glotch, Timothy D.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA.
[Dyar, M. Darby] Mt Holyoke Coll, Dept Astron & Geol, S Hadley, MA 01075 USA.
[Pieters, Carle M.; Hiroi, Takahiro] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Klima, Rachel] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA.
[Bishop, Janice L.] SETI Inst, Mountain View, CA 94043 USA.
[Bishop, Janice L.] NASA Ames Res Ctr, Mountain View, CA USA.
[Sunshine, Jessica] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Lane, MD (reprint author), Planetary Sci Inst, 1700 E Ft Lowell Rd,Ste 106, Tucson, AZ 85719 USA.
EM lane@psi.edu
RI Klima, Rachel/H-9383-2012
OI Klima, Rachel/0000-0002-9151-6429
FU NASA
FX Thanks are extended to Donald Lindsley at SUNY Stony Brook for
synthesizing the olivine samples and to Phil Christensen at Arizona
State University for the use of his thermal emission spectrometer
facility. This work is supported by NASA's Mars Fundamental Research and
Mars Odyssey Programs and is PSI contribution 507. Detailed reviews by
Vicky Hamilton and an anonymous reviewer are greatly appreciated and
resulted in an improved manuscript.
NR 88
TC 11
Z9 11
U1 1
U2 20
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 AUG 27
PY 2011
VL 116
AR E08010
DI 10.1029/2010JE003588
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 813KT
UT WOS:000294366200001
ER
PT J
AU Nigam, S
Guan, B
Ruiz-Barradas, A
AF Nigam, Sumant
Guan, Bin
Ruiz-Barradas, Alfredo
TI Key role of the Atlantic Multidecadal Oscillation in 20th century
drought and wet periods over the Great Plains
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; UNITED-STATES; REANALYSIS PROJECT;
NORTH-AMERICAN; VARIABILITY; US; PACIFIC; CLIMATE; SIMULATIONS; RAINFALL
AB The Great Plains of North America are susceptible to multi-year droughts, such as the 1930s 'Dust Bowl'. The droughts have been linked to SST variability in the Pacific and Atlantic basins. This observationally rooted analysis shows the SST influence in multi-year droughts and wet episodes over the Great Plains to be significantly more extensive than previously indicated. The remarkable statistical reconstruction of the major hydroclimate episodes attests to the extent of the SST influence in nature, and facilitated evaluation of the basin contributions. We find the Atlantic SSTs to be especially influential in forcing multi-year droughts; often, more than the Pacific ones. The Atlantic Multidecadal Oscillation (AMO), in particular, contributed the most in two of the four reconstructed episodes (Dust Bowl Spring, 1980s fall wetness), accounting for almost half the precipitation signal in each case. The AMO influence on continental precipitation was provided circulation context from analysis of NOAA's 20th Century Atmospheric Reanalysis. A hypothesis for how the AMO atmospheric circulation anomalies are generated from AMO SSTs is proposed to advance discussion of the influence pathways of the mid-to-high latitude SST anomalies. Our analysis suggests that the La Nina-US Drought paradigm, operative on interannual time scales, has been conferred excessive relevance on decadal time scales in the recent literature. Citation: Nigam, S., B. Guan, and A. Ruiz-Barradas (2011), Key role of the Atlantic Multidecadal Oscillation in 20th century drought and wet periods over the Great Plains, Geophys. Res. Lett., 38, L16713, doi: 10.1029/2011GL048650.
C1 [Nigam, Sumant; Ruiz-Barradas, Alfredo] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Guan, Bin] CALTECH, Jet Prop Lab, Climate Phys Grp, Pasadena, CA 91109 USA.
RP Nigam, S (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, 3419 Comp & Space Sci Bldg, College Pk, MD 20742 USA.
EM nigam@atmos.umd.edu
RI Guan, Bin/F-6735-2010; Nigam, Sumant/A-8338-2009; Ruiz-Barradas,
Alfredo/F-4499-2010
OI Ruiz-Barradas, Alfredo/0000-0003-3633-3950
FU University of Maryland Graduate School; [NSF-ATM-0649666];
[DOE-DEFG0208ER64548]; [DOE-DESC0001660]; [NOAA-NA10OAR4310158]
FX The authors acknowledge support of NSF-ATM-0649666, DOE-DEFG0208ER64548
and DOE-DESC0001660, and NOAA-NA10OAR4310158 grants. They thank Yongjing
Zhao for updating the SST principal component analysis in the Pacific
and Atlantic basins. Bin Guan's Maryland efforts were supported, in
part, by the Ann G. Wylie Dissertation Fellowship from the University of
Maryland Graduate School.
NR 32
TC 50
Z9 51
U1 3
U2 25
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 26
PY 2011
VL 38
AR L16713
DI 10.1029/2011GL048650
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 813LO
UT WOS:000294368300007
ER
PT J
AU Putman, WM
Suarez, M
AF Putman, William M.
Suarez, Max
TI Cloud-system resolving simulations with the NASA Goddard Earth Observing
System global atmospheric model (GEOS-5)
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID GENERAL-CIRCULATION MODELS; VOLUME DYNAMICAL CORE; MULTISCALE
INTERACTIONS; ARAKAWA-SCHUBERT; LIFE-CYCLE; PART I; PARAMETERIZATION;
SCALE
AB The NASA Global Modeling and Assimilation Office (GMAO) has developed a global non-hydrostatic cloud-system resolving capability within the NASA Goddard Earth Observing System global atmospheric model version 5 (GEOS-5). Using a non-hydrostatic finite-volume dynamical core coupled with advances in the moist physics and convective parameterization the model has been used to perform cloud-system resolving experiments at resolutions as fine as 3.5- to 14-km globally. An overview of preliminary results highlights the development of mid-latitude cyclones, the overall representation of global tropical convection, intense convective activity within the eye wall and outer rain bands of the 2009 Atlantic hurricane Bill validated by satellite observations, and the seasonal predictability of global tropical cyclone activity with realistic intensities. These preliminary results provide motivation for the use of GEOS-5 to simulate multi-scale convective systems within a global model at cloud resolving resolutions. Citation: Putman, W. M., and M. Suarez (2011), Cloud-system resolving simulations with the NASA Goddard Earth Observing System global atmospheric model (GEOS-5), Geophys. Res. Lett., 38, L16809, doi: 10.1029/2011GL048438.
C1 [Putman, William M.; Suarez, Max] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Putman, WM (reprint author), NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA.
EM William.M.Putman@nasa.gov
NR 22
TC 20
Z9 20
U1 1
U2 7
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 AUG 26
PY 2011
VL 38
AR L16809
DI 10.1029/2011GL048438
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 813LO
UT WOS:000294368300003
ER
PT J
AU Rinaldi, M
Decesari, S
Carbone, C
Finessi, E
Fuzzi, S
Ceburnis, D
O'Dowd, CD
Sciare, J
Burrows, JP
Vrekoussis, M
Ervens, B
Tsigaridis, K
Facchini, MC
AF Rinaldi, Matteo
Decesari, Stefano
Carbone, Claudio
Finessi, Emanuela
Fuzzi, Sandro
Ceburnis, Darius
O'Dowd, Colin D.
Sciare, Jean
Burrows, John P.
Vrekoussis, Mihalis
Ervens, Barbara
Tsigaridis, Kostas
Facchini, Maria Cristina
TI Evidence of a natural marine source of oxalic acid and a possible link
to glyoxal
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SECONDARY ORGANIC AEROSOL; SOLUBLE DICARBOXYLIC-ACIDS; AIR-SEA EXCHANGE;
PACIFIC-OCEAN; AQUEOUS PHOTOOXIDATION; ATMOSPHERIC AEROSOLS; SIZE
DISTRIBUTIONS; CARBONYL-COMPOUNDS; CARBOXYLIC-ACIDS; BOUNDARY-LAYER
AB This paper presents results supporting the existence of a natural source of oxalic acid over the oceans. Oxalate was detected in "clean-sector" marine aerosol samples at Mace Head (Ireland) (53 degrees 20'N, 9 degrees 54'W) during 2006, and at Amsterdam Island (37 degrees 48'S, 77 degrees 34'E) from 2003 to 2007, in concentrations ranging from 2.7 to 39 ng m(-3) and from 0.31 to 17 ng m(-3), respectively. The oxalate concentration showed a clear seasonal trend at both sites, with maxima in spring-summer and minima in fall-winter, being consistent with other marine biogenic aerosol components (e.g., methanesulfonic acid, non-sea-salt sulfate, and aliphatic amines). The observed oxalate was distributed along the whole aerosol size spectrum, with both a submicrometer and a supermicrometer mode, unlike the dominant submicrometer mode encountered in many polluted environments. Given its mass size distribution, the results suggest that over remote oceanic regions oxalate is produced through a combination of different formation processes. It is proposed that the cloud-mediated oxidation of gaseous glyoxal, recently detected over remote oceanic regions, may be an important source of submicrometer oxalate in the marine boundary layer. Supporting this hypothesis, satellite-retrieved glyoxal column concentrations over the two sampling sites exhibited the same seasonal concentration trend of oxalate. Furthermore, chemical box model simulations showed that the observed submicrometer oxalate concentrations were consistent with the in-cloud oxidation of typical marine air glyoxal mixing ratios, as retrieved by satellite measurements, at both sites.
C1 [Rinaldi, Matteo; Decesari, Stefano; Carbone, Claudio; Finessi, Emanuela; Fuzzi, Sandro; Facchini, Maria Cristina] CNR, Inst Atmospher Sci & Climate, I-40126 Bologna, Italy.
[Ceburnis, Darius; O'Dowd, Colin D.] Natl Univ Ireland Galway, Sch Expt Phys, Galway, Ireland.
[Ceburnis, Darius; O'Dowd, Colin D.] Natl Univ Ireland Galway, Environm Change Inst, Galway, Ireland.
[Sciare, Jean] CNRS CEA IPSL, Lab Sci Climat & Environm, Gif Sur Yvette, France.
[Burrows, John P.; Vrekoussis, Mihalis] Univ Bremen, Inst Environm Phys & Remote Sensing, D-28334 Bremen, Germany.
[Ervens, Barbara] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Ervens, Barbara] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO USA.
[Tsigaridis, Kostas] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Tsigaridis, Kostas] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Rinaldi, M (reprint author), CNR, Inst Atmospher Sci & Climate, I-40126 Bologna, Italy.
RI Fuzzi, Sandro/F-2675-2010; Carbone, Claudio/K-1859-2012; Tsigaridis,
Kostas/K-8292-2012; Ervens, Barbara/D-5495-2013; Facchini, Maria
Cristina/B-3369-2014; Vrekoussis, Mihalis/G-9424-2012; Manager, CSD
Publications/B-2789-2015; Burrows, John/B-6199-2014; O'Dowd ,
Colin/K-8904-2012; rinaldi, matteo/K-6083-2012; CHEMATMO Group,
Isac/P-7180-2014; Decesari, Stefano/B-9588-2015; FACCHINI, MARIA
CRISTINA/O-1230-2015;
OI Fuzzi, Sandro/0000-0002-5275-2381; Carbone, Claudio/0000-0001-5185-2535;
Tsigaridis, Kostas/0000-0001-5328-819X; Ervens,
Barbara/0000-0002-6223-1635; Facchini, Maria
Cristina/0000-0003-4833-9305; Vrekoussis, Mihalis/0000-0001-8292-8352;
Burrows, John/0000-0002-6821-5580; O'Dowd , Colin/0000-0002-3068-2212;
rinaldi, matteo/0000-0001-6543-4000; Decesari,
Stefano/0000-0001-6486-3786; FACCHINI, MARIA
CRISTINA/0000-0003-4833-9305; Ceburnis, Darius/0000-0003-0231-5324
FU EU; Irish EPA; French Polar Institute (IPEV; U.S. Department of Energy
[DE-FG02-08ER64539]; A. von Humboldt Foundation; European Union
FX The experimental work performed at Mace Head was supported by the EU
Project MAP (Marine Aerosol Production) and the Irish EPA project
EASI-AQCIS (Exchange at the Air-Sea Interface: Air Quality and Climate
Impacts). ACCENT (Atmospheric Composition Change the European Network of
Excellence) is also gratefully acknowledged. Results obtained at
Amsterdam Island were supported by the French Polar Institute (IPEV)
within the AEROTRACE project. Barbara Ervens acknowledges funding from
the U.S. Department of Energy (BER), ASP program, grant
DE-FG02-08ER64539. Mihalis Vrekoussis acknowledges the A. von Humboldt
Foundation and the European Union (Marie Curie, EIF and RG) for the
consecutive research fellowships.
NR 69
TC 31
Z9 32
U1 2
U2 47
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 26
PY 2011
VL 116
AR D16204
DI 10.1029/2011JD015659
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 813LR
UT WOS:000294368600003
ER
PT J
AU Yamaguchi, A
Barrat, JA
Ito, M
Bohn, M
AF Yamaguchi, Akira
Barrat, Jean-Alix
Ito, Motoo
Bohn, Marcel
TI Posteucritic magmatism on Vesta: Evidence from the petrology and thermal
history of diogenites
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID HED PARENT BODY; ORTHO-PYROXENE; EUCRITIC METEORITES; ELEMENT CHEMISTRY;
ASTEROID VESTA; CRUST; GEOCHEMISTRY; HOWARDITE; INSIGHTS; MELTS
AB We report on the petrology and the thermal histories of 13 diogenites in order to constrain the formation processes of the Vestan crust. We classify diogenites into unequilibrated and equilibrated diogenites in a scheme similar to that for basaltic eucrites. Pyroxenes in unequilibrated diogenites are chemically zoned, indicating that they crystallized rapidly from melts and escaped from global crustal metamorphism. The presence of unequilibrated diogenites casts doubt on the fact that all the diogenites formed at depth in the parent body, as commonly thought. Some diogenites probably crystallized in shallow intrusions or were extruded on the surface. These facts strengthen the geochemical evidence that diogenites and eucrites are not directly cogenetic and suggest that at least some diogenites have intruded the early formed eucritic crust. Thus, diogenites are certainly not the products of the crystallization of the magma ocean that triggered the differentiation of Vesta but are more likely cumulates associated with a later stage of magmatism. Furthermore, the intrusion of diogenites could have significantly thickened the early formed crust, making it difficult to excavate deep-seated olivine mantle by moderate impact events.
C1 [Yamaguchi, Akira] Natl Inst Polar Res, Tokyo 1908518, Japan.
[Yamaguchi, Akira] Grad Univ Adv Studies, Sch Multidisciplinary Sci, Dept Polar Sci, Tokyo, Japan.
[Barrat, Jean-Alix] Univ Europeenne Bretagne, Brest, France.
[Barrat, Jean-Alix; Bohn, Marcel] Univ Brest, CNRS, IUEM, UMR 6538, F-29280 Plouzane, France.
[Ito, Motoo] NASA, Robert M Walker Lab Space Sci, Johnson Space Ctr, Houston, TX USA.
[Ito, Motoo] Lunar & Planetary Inst, Houston, TX 77058 USA.
RP Yamaguchi, A (reprint author), Natl Inst Polar Res, Tokyo 1908518, Japan.
EM yamaguch@nipr.ac.jp
RI Jean-Alix, BARRAT/F-8035-2012; Barrat, Jean-Alix/C-8416-2017
OI Barrat, Jean-Alix/0000-0003-3158-3109
FU Ministry of Education, Science, and Technology, Japan [19540511]; NIPR
[KP-6]
FX This research was partly supported by a Grant-in-Aid for Scientific
Research from the Ministry of Education, Science, and Technology, Japan,
19540511 (A.Y.) and NIPR, Research Project Funds, KP-6 and was initiated
while one of the authors (A.Y.) visited UBO in Brest. We thank the
Associate Editor, D.W Mittlefehldt, and an anonymous reviewer for
constructive reviews, and R. Hewins for discussion and improvement of
the English.
NR 46
TC 17
Z9 17
U1 0
U2 17
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 AUG 26
PY 2011
VL 116
AR E08009
DI 10.1029/2010JE003753
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 813KR
UT WOS:000294366000001
ER
PT J
AU Oughton, S
Matthaeus, WH
Smith, CW
Breech, B
Isenberg, PA
AF Oughton, S.
Matthaeus, W. H.
Smith, C. W.
Breech, B.
Isenberg, P. A.
TI Transport of solar wind fluctuations: A two-component model
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID INTERSTELLAR PICKUP PROTONS; MEAN MAGNETIC-FIELD; COSMIC-RAY TRANSPORT;
MAGNETOHYDRODYNAMIC TURBULENCE; ALFVENIC TURBULENCE; MHD TURBULENCE;
HYDROMAGNETIC TURBULENCE; OUTER HELIOSPHERE; RADIAL EVOLUTION; CROSS
HELICITY
AB We present a new model for the transport of solar wind fluctuations which treats them as two interacting incompressible components: quasi-two-dimensional turbulence and a wave-like piece. Quantities solved for include the energy, cross helicity, and characteristic transverse length scale of each component, plus the proton temperature. The development of the model is outlined and numerical solutions are compared with spacecraft observations. Compared to previous single-component models, this new model incorporates a more physically realistic treatment of fluctuations induced by pickup ions and yields improved agreement with observed values of the correlation length, while maintaining good observational accord with the energy, cross helicity, and temperature.
C1 [Oughton, S.] Univ Waikato, Dept Math, Hamilton 3240, New Zealand.
[Matthaeus, W. H.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Matthaeus, W. H.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Smith, C. W.; Isenberg, P. A.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Breech, B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Oughton, S (reprint author), Univ Waikato, Dept Math, Private Bag 3105, Hamilton 3240, New Zealand.
EM whm@udel.edu
RI Oughton, Sean/A-3380-2012
OI Oughton, Sean/0000-0002-2814-7288
FU University of Waikato; NASA [NNX08AI47G, NNX07AH75G, NNX09AVA49G]; NSF
[SHINE ATM-0752135, ATM-0635863]; DoE [DEFG0207ER46372]
FX This research was supported by the University of Waikato Strategic
Research Investment Fund, by NASA through the Heliospheric Theory
(NNX08AI47G) and SR&T (NNX07AH75G, NNX09AVA49G) programs, by the NSF
(SHINE ATM-0752135, ATM-0635863), and by the DoE (DEFG0207ER46372).
B.A.B.'s research was supported in part by an appointment to the NASA
Postdoctoral Program at Goddard Space Flight Center, administered by Oak
Ridge Associated Universities through a contract with NASA. Our thanks
to John Richardson and the MIT Space Plasma Group for making the Voyager
temperature data available online at
http://web.mit.edu/space/www/voyager/voyager.html.
NR 82
TC 31
Z9 31
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 AUG 26
PY 2011
VL 116
AR A08105
DI 10.1029/2010JA016365
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 813KV
UT WOS:000294366400001
ER
PT J
AU Nakamura, T
Noguchi, T
Tanaka, M
Zolensky, ME
Kimura, M
Tsuchiyama, A
Nakato, A
Ogami, T
Ishida, H
Uesugi, M
Yada, T
Shirai, K
Fujimura, A
Okazaki, R
Sandford, SA
Ishibashi, Y
Abe, M
Okada, T
Ueno, M
Mukai, T
Yoshikawa, M
Kawaguchi, J
AF Nakamura, Tomoki
Noguchi, Takaaki
Tanaka, Masahiko
Zolensky, Michael E.
Kimura, Makoto
Tsuchiyama, Akira
Nakato, Aiko
Ogami, Toshihiro
Ishida, Hatsumi
Uesugi, Masayuki
Yada, Toru
Shirai, Kei
Fujimura, Akio
Okazaki, Ryuji
Sandford, Scott A.
Ishibashi, Yukihiro
Abe, Masanao
Okada, Tatsuaki
Ueno, Munetaka
Mukai, Toshifumi
Yoshikawa, Makoto
Kawaguchi, Junichiro
TI Itokawa Dust Particles: A Direct Link Between S-Type Asteroids and
Ordinary Chondrites
SO SCIENCE
LA English
DT Article
ID HAYABUSA SPACECRAFT; OLIVINE; GEOTHERMOMETRY; METAMORPHISM; THERMOMETRY;
PYROXENE; HISTORY
AB The Hayabusa spacecraft successfully recovered dust particles from the surface of near-Earth asteroid 25143 Itokawa. Synchrotron-radiation x-ray diffraction and transmission and scanning electron microscope analyses indicate that the mineralogy and mineral chemistry of the Itokawa dust particles are identical to those of thermally metamorphosed LL chondrites, consistent with spectroscopic observations made from Earth and by the Hayabusa spacecraft. Our results directly demonstrate that ordinary chondrites, the most abundant meteorites found on Earth, come from S-type asteroids. Mineral chemistry indicates that the majority of regolith surface particles suffered long-term thermal annealing and subsequent impact shock, suggesting that Itokawa is an asteroid made of reassembled pieces of the interior portions of a once larger asteroid.
C1 [Nakamura, Tomoki; Nakato, Aiko; Ogami, Toshihiro; Ishida, Hatsumi] Tohoku Univ, Dept Earth & Planetary Mat Sci, Fac Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan.
[Noguchi, Takaaki; Kimura, Makoto] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Tanaka, Masahiko] Natl Inst Mat Sci, Synchrotron Xray Stn SPring 8, Sayo, Hyogo 6795198, Japan.
[Zolensky, Michael E.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA.
[Tsuchiyama, Akira] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Uesugi, Masayuki; Yada, Toru; Shirai, Kei; Fujimura, Akio; Ishibashi, Yukihiro; Abe, Masanao; Okada, Tatsuaki; Ueno, Munetaka; Mukai, Toshifumi; Yoshikawa, Makoto; Kawaguchi, Junichiro] JAXA ISAS, Sagamihara, Kanagawa 2298510, Japan.
[Okazaki, Ryuji] Kyushu Univ, Dept Earth & Planetary Sci, Fac Sci, Fukuoka 8128581, Japan.
[Sandford, Scott A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Nakamura, T (reprint author), Tohoku Univ, Dept Earth & Planetary Mat Sci, Fac Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan.
EM tomoki@m.tohoku.ac.jp
RI U-ID, Kyushu/C-5291-2016
FU NASA [769583.07.03]
FX We thank the Hayabusa project team for sample return; KEK for
synchrotron experiments; H. Nakano, Y. Yamazaki, K. Shimada, Y. Kakazu,
T. Hashimoto, M. Konno, Y. Katsuya, and Y. Matsushita, for technical
support; and J. Grossman, T. Ikeda, T. Hokada, K. Ozawa, Y. Nakamuta,
and S. Wakita for helpful discussions. Supported by NASA grant
769583.07.03 (M.E.Z. and S.A.S.).
NR 27
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PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD AUG 26
PY 2011
VL 333
IS 6046
BP 1113
EP 1116
DI 10.1126/science.1207758
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 811VM
UT WOS:000294244300038
PM 21868667
ER
PT J
AU Yurimoto, H
Abe, K
Abe, M
Ebihara, M
Fujimura, A
Hashiguchi, M
Hashizume, K
Ireland, TR
Itoh, S
Katayama, J
Kato, C
Kawaguchi, J
Kawasaki, N
Kitajima, F
Kobayashi, S
Meike, T
Mukai, T
Nagao, K
Nakamura, T
Naraoka, H
Noguchi, T
Okazaki, R
Park, C
Sakamoto, N
Seto, Y
Takei, M
Tsuchiyama, A
Uesugi, M
Wakaki, S
Yada, T
Yamamoto, K
Yoshikawa, M
Zolensky, ME
AF Yurimoto, Hisayoshi
Abe, Ken-ichi
Abe, Masanao
Ebihara, Mitsuru
Fujimura, Akio
Hashiguchi, Minako
Hashizume, Ko
Ireland, Trevor R.
Itoh, Shoichi
Katayama, Juri
Kato, Chizu
Kawaguchi, Junichiro
Kawasaki, Noriyuki
Kitajima, Fumio
Kobayashi, Sachio
Meike, Tatsuji
Mukai, Toshifumi
Nagao, Keisuke
Nakamura, Tomoki
Naraoka, Hiroshi
Noguchi, Takaaki
Okazaki, Ryuji
Park, Changkun
Sakamoto, Naoya
Seto, Yusuke
Takei, Masashi
Tsuchiyama, Akira
Uesugi, Masayuki
Wakaki, Shigeyuki
Yada, Toru
Yamamoto, Kosuke
Yoshikawa, Makoto
Zolensky, Michael E.
TI Oxygen Isotopic Compositions of Asteroidal Materials Returned from
Itokawa by the Hayabusa Mission
SO SCIENCE
LA English
DT Article
ID SOLAR-SYSTEM; NEBULA; ORIGIN
AB Meteorite studies suggest that each solar system object has a unique oxygen isotopic composition. Chondrites, the most primitive of meteorites, have been believed to be derived from asteroids, but oxygen isotopic compositions of asteroids themselves have not been established. We measured, using secondary ion mass spectrometry, oxygen isotopic compositions of rock particles from asteroid 25143 Itokawa returned by the Hayabusa spacecraft. Compositions of the particles are depleted in O-16 relative to terrestrial materials and indicate that Itokawa, an S-type asteroid, is one of the sources of the LL or L group of equilibrated ordinary chondrites. This is a direct oxygen-isotope link between chondrites and their parent asteroid.
C1 [Yurimoto, Hisayoshi; Abe, Ken-ichi; Hashiguchi, Minako; Itoh, Shoichi; Katayama, Juri; Kato, Chizu; Kawasaki, Noriyuki; Kobayashi, Sachio; Meike, Tatsuji; Park, Changkun; Sakamoto, Naoya; Takei, Masashi; Wakaki, Shigeyuki; Yamamoto, Kosuke] Hokkaido Univ, Sapporo, Hokkaido 0600810, Japan.
[Abe, Masanao; Fujimura, Akio; Kawaguchi, Junichiro; Mukai, Toshifumi; Uesugi, Masayuki; Yada, Toru; Yoshikawa, Makoto] Japan Aerosp Explorat Agency, Inst Space & Astronaut Sci, Chuo Ku, Kanagawa 2525210, Japan.
[Ebihara, Mitsuru] Tokyo Metropolitan Univ, Grad Sch Sci & Engn, Tokyo 1920397, Japan.
[Hashizume, Ko; Tsuchiyama, Akira] Osaka Univ, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Ireland, Trevor R.] Australian Natl Univ, Res Sch Earth Sci, Coll Phys & Math Sci, Canberra, ACT 0200, Australia.
[Kitajima, Fumio; Naraoka, Hiroshi; Okazaki, Ryuji] Kyushu Univ, Dept Earth & Planetary Sci, Higashi Ku, Fukuoka 8128581, Japan.
[Nagao, Keisuke] Univ Tokyo, Geochem Res Ctr, Tokyo 1130033, Japan.
[Nakamura, Tomoki] Tohoku Univ, Dept Earth & Planetary Mat Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan.
[Noguchi, Takaaki] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Seto, Yusuke] Kobe Univ, Dept Earth & Planetary Sci, Kobe, Hyogo 6578501, Japan.
[Zolensky, Michael E.] NASA, Lyndon B Johnson Space Ctr, KT, Houston, TX 77058 USA.
RP Yurimoto, H (reprint author), Hokkaido Univ, Sapporo, Hokkaido 0600810, Japan.
EM yuri@ep.sci.hokudai.ac.jp
RI Ireland, Trevor/A-4993-2008; Seto, Yusuke/D-5751-2015; U-ID,
Kyushu/C-5291-2016
OI Ireland, Trevor/0000-0001-7617-3889; Seto, Yusuke/0000-0002-5423-2136;
FU Monka-sho grant; NASA
FX We thank the Hayabusa sample curation team and the Hayabusa project team
for close cooperation. This study was supported by the Monka-sho grant
(H.Y.) and by the NASA Muses-CN/Hayabusa Program (M.E.Z.).
NR 17
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PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD AUG 26
PY 2011
VL 333
IS 6046
BP 1116
EP 1119
DI 10.1126/science.1207776
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 811VM
UT WOS:000294244300039
PM 21868668
ER
PT J
AU Ebihara, M
Sekimoto, S
Shirai, N
Hamajima, Y
Yamamoto, M
Kumagai, K
Oura, Y
Ireland, TR
Kitajima, F
Nagao, K
Nakamura, T
Naraoka, H
Noguchi, T
Okazaki, R
Tsuchiyama, A
Uesugi, M
Yurimoto, H
Zolensky, ME
Abe, M
Fujimura, A
Mukai, T
Yada, Y
AF Ebihara, M.
Sekimoto, S.
Shirai, N.
Hamajima, Y.
Yamamoto, M.
Kumagai, K.
Oura, Y.
Ireland, T. R.
Kitajima, F.
Nagao, K.
Nakamura, T.
Naraoka, H.
Noguchi, T.
Okazaki, R.
Tsuchiyama, A.
Uesugi, M.
Yurimoto, H.
Zolensky, M. E.
Abe, M.
Fujimura, A.
Mukai, T.
Yada, Y.
TI Neutron Activation Analysis of a Particle Returned from Asteroid Itokawa
SO SCIENCE
LA English
DT Article
ID HAYABUSA SPACECRAFT; ORDINARY CHONDRITES; COMPONENTS; CHONDRULES;
MINERALS; HISTORY; ORIGIN; METAL
AB A single grain (similar to 3 micrograms) returned by the Hayabusa spacecraft was analyzed by neutron activation analysis. This grain is mainly composed of olivine with minor amounts of plagioclase, troilite, and metal. Our results establish that the Itokawa sample has similar chemical characteristics (iron/scandium and nickel/cobalt ratios) to chondrites, confirming that this grain is extraterrestrial in origin and has primitive chemical compositions. Estimated iridium/nickel and iridium/cobalt ratios for metal in the Itokawa samples are about five times lower than CI carbonaceous chondrite values. A similar depletion of iridium was observed in chondrule metals of ordinary chondrites. These metals must have condensed from the nebular where refractory siderophile elements already condensed and were segregated.
C1 [Ebihara, M.; Shirai, N.; Kumagai, K.; Oura, Y.] Tokyo Metropolitan Univ, Dept Chem, Tokyo 1920397, Japan.
[Sekimoto, S.] Kyoto Univ, Inst Res Reactor, Osaka 59004, Japan.
[Hamajima, Y.; Yamamoto, M.] Kanazawa Univ, Low Level Radioact Lab, Tatsunokuchi, Japan.
[Ireland, T. R.] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT, Australia.
[Kitajima, F.; Naraoka, H.; Okazaki, R.] Kyushu Univ, Dept Earth & Planetary Sci, Fukuoka 812, Japan.
[Nagao, K.] Univ Tokyo, Geochem Res Ctr, Tokyo, Japan.
[Nakamura, T.] Tohoku Univ, Dept Earth & Planetary Mat Sci, Sendai, Miyagi 980, Japan.
[Noguchi, T.] Ibaraki Univ, Coll Sci, Mito, Ibaraki, Japan.
[Tsuchiyama, A.] Osaka Univ, Dept Earth & Space Sci, Toyonaka, Osaka 560, Japan.
[Uesugi, M.; Abe, M.; Fujimura, A.; Mukai, T.; Yada, Y.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Kanagawa, Japan.
[Yurimoto, H.] Hokkaido Univ, Sapporo, Hokkaido, Japan.
[Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Ebihara, M (reprint author), Tokyo Metropolitan Univ, Dept Chem, Tokyo 1920397, Japan.
EM ebihara-mitsuru@tmu.ac.jp
RI Ireland, Trevor/A-4993-2008; HAMAJIMA, Yasunori/L-3802-2015
OI Ireland, Trevor/0000-0001-7617-3889; HAMAJIMA,
Yasunori/0000-0002-8485-4606
FU Ministry of Education, Culture, Science and Technology of Japan; NASA
FX This work was supported in part by a grant-in-aid defrayed by the
Ministry of Education, Culture, Science and Technology of Japan. M.E.Z.
was supported by NASA.
NR 17
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PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD AUG 26
PY 2011
VL 333
IS 6046
BP 1119
EP 1121
DI 10.1126/science.1207865
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 811VM
UT WOS:000294244300040
PM 21868669
ER
PT J
AU Noguchi, T
Nakamura, T
Kimura, M
Zolensky, ME
Tanaka, M
Hashimoto, T
Konno, M
Nakato, A
Ogami, T
Fujimura, A
Abe, M
Yada, T
Mukai, T
Ueno, M
Okada, T
Shirai, K
Ishibashi, Y
Okazaki, R
AF Noguchi, T.
Nakamura, T.
Kimura, M.
Zolensky, M. E.
Tanaka, M.
Hashimoto, T.
Konno, M.
Nakato, A.
Ogami, T.
Fujimura, A.
Abe, M.
Yada, T.
Mukai, T.
Ueno, M.
Okada, T.
Shirai, K.
Ishibashi, Y.
Okazaki, R.
TI Incipient Space Weathering Observed on the Surface of Itokawa Dust
Particles
SO SCIENCE
LA English
DT Article
ID NEAR-EARTH ASTEROIDS; S-TYPE ASTEROIDS; HAYABUSA SPACECRAFT; ORDINARY
CHONDRITES; LUNAR REGOLITH; IRRADIATION; SIMULATION; SAMPLES; ORIGIN
AB The reflectance spectra of the most abundant meteorites, ordinary chondrites, are different from those of the abundant S-type (mnemonic for siliceous) asteroids. This discrepancy has been thought to be due to space weathering, which is an alteration of the surfaces of airless bodies exposed to the space environment. Here we report evidence of space weathering on particles returned from the S-type asteroid 25143 Itokawa by the Hayabusa spacecraft. Surface modification was found in 5 out of 10 particles, which varies depending on mineral species. Sulfur-bearing Fe-rich nanoparticles exist in a thin (5 to 15 nanometers) surface layer on olivine, low-Ca pyroxene, and plagioclase, which is suggestive of vapor deposition. Sulfur-free Fe-rich nanoparticles exist deeper inside (<60 nanometers) ferromagnesian silicates. Their texture suggests formation by metamictization and in situ reduction of Fe2+.
C1 [Noguchi, T.; Kimura, M.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Nakamura, T.; Nakato, A.; Ogami, T.] Tohoku Univ, Dept Earth Sci, Grad Sch Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan.
[Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA.
[Tanaka, M.] Natl Inst Mat Sci, Synchrotron Xray Stn SPring 8, Sayo, Hyogo 6795148, Japan.
[Hashimoto, T.; Konno, M.] Hitachi High Technol, Hitachinaka, Ibaraki 3128504, Japan.
[Fujimura, A.; Abe, M.; Yada, T.; Mukai, T.; Ueno, M.; Okada, T.; Shirai, K.; Ishibashi, Y.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Kanagawa 2525210, Japan.
[Okazaki, R.] Kyushu Univ, Dept Earth & Planetary Sci, Fukuoka 8128581, Japan.
RP Noguchi, T (reprint author), Ibaraki Univ, Coll Sci, 2-1-1 Bunkyo, Mito, Ibaraki 3108512, Japan.
EM tngc@mx.ibaraki.ac.jp
RI U-ID, Kyushu/C-5291-2016
FU NASA
FX Special thanks to the Hayabusa project team for sample return. We are
grateful to Y. Suzuki, S. Tsujimoto, R. Sagae, R. Hinoki, and M.
Kawamoto for supporting N2 purge sample preparation at the Institute of
Space and Astronautical Sciences of the Japan Aerospace Exploration
Agency and Ibaraki University, and for STEM observation at Hitachi
High-Technologies. Thanks to H. Hidaka, we could compare the rims of the
Itokawa particles and those of space-weathered lunar soil. M. Zolensky
was supported by NASA's Muses-C/Hayabusa Program.
NR 32
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PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD AUG 26
PY 2011
VL 333
IS 6046
BP 1121
EP 1125
DI 10.1126/science.1207794
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 811VM
UT WOS:000294244300041
PM 21868670
ER
PT J
AU Tsuchiyama, A
Uesugi, M
Matsushima, T
Michikami, T
Kadono, T
Nakamura, T
Uesugi, K
Nakano, T
Sandford, SA
Noguchi, R
Matsumoto, T
Matsuno, J
Nagano, T
Imai, Y
Takeuchi, A
Suzuki, Y
Ogami, T
Katagiri, J
Ebihara, M
Ireland, TR
Kitajima, F
Nagao, K
Naraoka, H
Noguchi, T
Okazaki, R
Yurimoto, H
Zolensky, ME
Mukai, T
Abe, M
Yada, T
Fujimura, A
Yoshikawa, M
Kawaguchi, J
AF Tsuchiyama, Akira
Uesugi, Masayuki
Matsushima, Takashi
Michikami, Tatsuhiro
Kadono, Toshihiko
Nakamura, Tomoki
Uesugi, Kentaro
Nakano, Tsukasa
Sandford, Scott A.
Noguchi, Ryo
Matsumoto, Toru
Matsuno, Junya
Nagano, Takashi
Imai, Yuta
Takeuchi, Akihisa
Suzuki, Yoshio
Ogami, Toshihiro
Katagiri, Jun
Ebihara, Mitsuru
Ireland, Trevor R.
Kitajima, Fumio
Nagao, Keisuke
Naraoka, Hiroshi
Noguchi, Takaaki
Okazaki, Ryuji
Yurimoto, Hisayoshi
Zolensky, Michael E.
Mukai, Toshifumi
Abe, Masanao
Yada, Toru
Fujimura, Akio
Yoshikawa, Makoto
Kawaguchi, Junichiro
TI Three-Dimensional Structure of Hayabusa Samples: Origin and Evolution of
Itokawa Regolith
SO SCIENCE
LA English
DT Article
ID ASTEROID ITOKAWA; IMPACT EXPERIMENTS; SPACECRAFT
AB Regolith particles on the asteroid Itokawa were recovered by the Hayabusa mission. Their three-dimensional (3D) structure and other properties, revealed by x-ray microtomography, provide information on regolith formation. Modal abundances of minerals, bulk density (3.4 grams per cubic centimeter), and the 3D textures indicate that the particles represent a mixture of equilibrated and less-equilibrated LL chondrite materials. Evidence for melting was not seen on any of the particles. Some particles have rounded edges. Overall, the particles' size and shape are different from those seen in particles from the lunar regolith. These features suggest that meteoroid impacts on the asteroid surface primarily form much of the regolith particle, and that seismic-induced grain motion in the smooth terrain abrades them over time.
C1 [Tsuchiyama, Akira; Noguchi, Ryo; Matsumoto, Toru; Matsuno, Junya; Nagano, Takashi; Imai, Yuta] Osaka Univ, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Uesugi, Masayuki; Mukai, Toshifumi; Abe, Masanao; Yada, Toru; Fujimura, Akio; Yoshikawa, Makoto; Kawaguchi, Junichiro] Japan Aerosp Explorat Agcy, Sagamihara, Kanagawa 2525210, Japan.
[Matsushima, Takashi; Katagiri, Jun] Univ Tsukuba, Dept Engn Mech & Energy, Grad Sch Syst & Informat Engn, Tsukuba, Ibaraki 3058573, Japan.
[Michikami, Tatsuhiro] Fukushima Natl Coll Technol, Fukushima 9708034, Japan.
[Kadono, Toshihiko] Osaka Univ, Inst Laser Engn, Suita, Osaka 5650871, Japan.
[Nakamura, Tomoki; Ogami, Toshihiro] Tohoku Univ, Dept Earth & Planetary Mat Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan.
[Uesugi, Kentaro; Takeuchi, Akihisa; Suzuki, Yoshio] Japan Synchrotron Radiat Res Inst JASRI SPring 8, Sayo, Hyogo 6795198, Japan.
[Nakano, Tsukasa] Natl Inst Adv Ind Sci & Technol, Geol Survey Japan, Tsukuba, Ibaraki 3058568, Japan.
[Sandford, Scott A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ebihara, Mitsuru] Tokyo Metropolitan Univ, Grad Sch Sci & Engn, Hachioji, Tokyo 1920397, Japan.
[Ireland, Trevor R.] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia.
[Kitajima, Fumio; Naraoka, Hiroshi; Okazaki, Ryuji] Kyushu Univ, Dept Earth & Planetary Sci, Higashi Ku, Fukuoka 8128581, Japan.
[Nagao, Keisuke] Univ Tokyo, Geochem Res Ctr, Bunkyo Ku, Tokyo 1130033, Japan.
[Noguchi, Takaaki] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3100056, Japan.
[Yurimoto, Hisayoshi] Hokkaido Univ, Kita Ku, Sapporo, Hokkaido 0600808, Japan.
[Zolensky, Michael E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Tsuchiyama, A (reprint author), Osaka Univ, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
EM akira@ess.sci.osaka-u.ac.jp
RI Ireland, Trevor/A-4993-2008; U-ID, Kyushu/C-5291-2016
OI Ireland, Trevor/0000-0001-7617-3889;
FU Japan Ministry of Education, Culture, Sports, Science, and Technology
[19104012]; NASA
FX We thank the Hayabusa sample curation team and the Hayabusa project
team. A. Tsuchiyama was supported by a grant-in-aid of the Japan
Ministry of Education, Culture, Sports, Science, and Technology
(19104012). M.E.Z. and S.A.S. were supported by NASA's Muses-C/Hayabusa
Program. The tomography experiment was performed under the approval of
the SPring-8 Proposal Review Committee (2010B1531).
NR 23
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PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD AUG 26
PY 2011
VL 333
IS 6046
BP 1125
EP 1128
DI 10.1126/science.1207807
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 811VM
UT WOS:000294244300042
PM 21868671
ER
PT J
AU Nagao, K
Okazaki, R
Nakamura, T
Miura, YN
Osawa, T
Bajo, K
Matsuda, S
Ebihara, M
Ireland, TR
Kitajima, F
Naraoka, H
Noguchi, T
Tsuchiyama, A
Yurimoto, H
Zolensky, ME
Uesugi, M
Shirai, K
Abe, M
Yada, T
Ishibashi, Y
Fujimura, A
Mukai, T
Ueno, M
Okada, T
Yoshikawa, M
Kawaguchi, J
AF Nagao, Keisuke
Okazaki, Ryuji
Nakamura, Tomoki
Miura, Yayoi N.
Osawa, Takahito
Bajo, Ken-ichi
Matsuda, Shintaro
Ebihara, Mitsuru
Ireland, Trevor R.
Kitajima, Fumio
Naraoka, Hiroshi
Noguchi, Takaaki
Tsuchiyama, Akira
Yurimoto, Hisayoshi
Zolensky, Michael E.
Uesugi, Masayuki
Shirai, Kei
Abe, Masanao
Yada, Toru
Ishibashi, Yukihiro
Fujimura, Akio
Mukai, Toshifumi
Ueno, Munetaka
Okada, Tatsuaki
Yoshikawa, Makoto
Kawaguchi, Junichiro
TI Irradiation History of Itokawa Regolith Material Deduced from Noble
Gases in the Hayabusa Samples
SO SCIENCE
LA English
DT Article
ID SOLAR ENERGETIC PARTICLES; ASTEROID ITOKAWA; HELIUM; NEON; SPACECRAFT;
ISOTOPES; SYSTEM; ARGON; WIND
AB Noble gas isotopes were measured in three rocky grains from asteroid Itokawa to elucidate a history of irradiation from cosmic rays and solar wind on its surface. Large amounts of solar helium (He), neon (Ne), and argon (Ar) trapped in various depths in the grains were observed, which can be explained by multiple implantations of solar wind particles into the grains, combined with preferential He loss caused by frictional wear of space-weathered rims on the grains. Short residence time of less than 8 million years was implied for the grains by an estimate on cosmic-ray-produced (21)Ne. Our results suggest that Itokawa is continuously losing its surface materials into space at a rate of tens of centimeters per million years. The lifetime of Itokawa should be much shorter than the age of our solar system.
C1 [Nagao, Keisuke; Bajo, Ken-ichi; Matsuda, Shintaro] Univ Tokyo, Geochem Res Ctr, Bunkyo Ku, Tokyo 1130033, Japan.
[Okazaki, Ryuji; Kitajima, Fumio; Naraoka, Hiroshi] Kyushu Univ, Dept Earth & Planetary Sci, Higashi Ku, Fukuoka 812, Japan.
[Nakamura, Tomoki] Tohoku Univ, Dept Earth & Planetary Mat Sci, Aoba Ku, Sendai, Miyagi 980, Japan.
[Miura, Yayoi N.] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, Tokyo 1130033, Japan.
[Osawa, Takahito] Japan Atom Energy Agcy, Tokai, Ibaraki, Japan.
[Ebihara, Mitsuru] Tokyo Metropolitan Univ, Grad Sch Sci & Engn, Hachioji, Tokyo, Japan.
[Ireland, Trevor R.] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT, Australia.
[Noguchi, Takaaki] Ibaraki Univ, Coll Sci, Mito, Ibaraki, Japan.
[Tsuchiyama, Akira] Osaka Univ, Dept Earth & Space Sci, Toyonaka, Osaka 560, Japan.
[Yurimoto, Hisayoshi] Hokkaido Univ, Kita Ku, Sapporo, Hokkaido, Japan.
[Zolensky, Michael E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Uesugi, Masayuki; Shirai, Kei; Abe, Masanao; Yada, Toru; Ishibashi, Yukihiro; Fujimura, Akio; Mukai, Toshifumi; Ueno, Munetaka; Okada, Tatsuaki; Yoshikawa, Makoto; Kawaguchi, Junichiro] Japan Aerosp Explorat Agcy JAXA, ISAS, Sagamihara, Kanagawa, Japan.
RP Nagao, K (reprint author), Univ Tokyo, Geochem Res Ctr, Bunkyo Ku, Tokyo 1130033, Japan.
EM nagao@eqchem.s.u-tokyo.ac.jp
RI Ireland, Trevor/A-4993-2008
OI Ireland, Trevor/0000-0001-7617-3889
NR 26
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U1 3
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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 AUG 26
PY 2011
VL 333
IS 6046
BP 1128
EP 1131
DI 10.1126/science.1207785
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 811VM
UT WOS:000294244300043
PM 21868672
ER
PT J
AU Rocha, C
Munoz, C
Dowek, G
AF Rocha, Camilo
Munoz, Cesar
Dowek, Gilles
TI A formal library of set relations and its application to synchronous
languages
SO THEORETICAL COMPUTER SCIENCE
LA English
DT Article
DE Set relations; Synchronous languages; Small-step semantics; Rewriting
logic semantics; Plan execution
ID REWRITING LOGIC; COMPLEX-SYSTEMS; SEMANTICS; MODEL
AB Set relations are particularly suitable for specifying the small-step operational semantics of synchronous languages. In this paper, a formal library of set relations for the definition, verification of properties, and execution of binary set relations is presented. The formal library consists of a set of theories written in the Prototype Verification System (PVS) that contains definitions and proofs of properties, such as determinism and compositionality, for synchronous relations. The paper also proposes a serialization procedure that enables the simulation of synchronous set relations via set rewriting systems. The library and the serialization procedure are illustrated with the rewriting logic semantics of the Plan Execution Interchange Language (PLEXIL), a rich synchronous plan execution language developed by NASA to support autonomous spacecraft operations. Published by Elsevier B.V.
C1 [Rocha, Camilo] Univ Illinois, Dept Comp Sci, Urbana, IL 61801 USA.
[Munoz, Cesar] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Dowek, Gilles] Ecole Polytech, INRIA, LIX, F-91128 Palaiseau, France.
RP Rocha, C (reprint author), Univ Illinois, Dept Comp Sci, 1304 W Springfield Ave, Urbana, IL 61801 USA.
EM hrochan2@cs.illinois.edu; cesar.a.munoz@nasa.gov;
gilles.dowek@polytechnique.fr
FU National Aeronautics and Space Administration at Langley Research Center
[NCC-1-02043]; NSF [CNS 08-34709]
FX This document is a collaborative effort: authors are listed in reversed
alphabetical order. This work was supported in part by the National
Aeronautics and Space Administration at Langley Research Center under
the Research Cooperative Agreement No. NCC-1-02043 awarded to the
National Institute of Aerospace while the first and third authors were
visiting the institute and the second author was resident there. The
first author was partially supported by NSF Grant CNS 08-34709.
NR 31
TC 3
Z9 3
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0304-3975
J9 THEOR COMPUT SCI
JI Theor. Comput. Sci.
PD AUG 26
PY 2011
VL 412
IS 37
BP 4853
EP 4866
DI 10.1016/j.tcs.2011.01.027
PG 14
WC Computer Science, Theory & Methods
SC Computer Science
GA 810RV
UT WOS:000294145700002
ER
PT J
AU Pavelsky, TM
Kapnick, S
Hall, A
AF Pavelsky, Tamlin M.
Kapnick, Sarah
Hall, Alex
TI Accumulation and melt dynamics of snowpack from a multiresolution
regional climate model in the central Sierra Nevada, California
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID WESTERN UNITED-STATES; WATER-RESOURCES; CHANGE SCENARIOS; NORTH-AMERICA;
CONVECTIVE PARAMETERIZATION; SPATIAL VARIABILITY; POTENTIAL IMPACTS;
SPRING SNOWPACK; SNOWMELT RUNOFF; HYDROLOGY
AB The depth and timing of snowpack in the Sierra Nevada Mountains are of fundamental importance to California water resource availability, and recent studies indicate a shift toward earlier snowmelt consistent with projected impacts of anthropogenic climate change. In order for future studies to assess snowpack variability on seasonal to centennial time scales, physically based models of snowpack evolution at high spatial resolution must be improved. Here we evaluate modeled snowpack accuracy for the central Sierra Nevada in the Weather Research and Forecasting regional climate model coupled to the Noah land surface model. A simulation with nested domains at 27, 9, and 3 km grid spacings is presented for November 2001 to July 2002. Model outputs are compared with daily snowpack observations at 41 locations, air temperature at 31 locations, and precipitation at 10 locations. Comparison of snowpack at different resolutions suggests that 27 km simulations substantially underestimate snowpack, while 9 and 3 km simulations are closer to observations. Regional snowpack accumulation is accurately simulated at these high resolutions, but model snowmelt occurs an average of 22-25 days early. Some error can be traced to differences in elevation and observation scale between point-based measurements and model grid cells, but these factors cannot explain the persistent bias toward early snowmelt. A high correlation between snowmelt and error in modeled surface air temperature is found, with melt coinciding systematically with excessively cold air temperatures. One possible source of bias is an imbalance in turbulent heat fluxes, erroneously warming the snowpack while cooling the surface atmosphere.
C1 [Pavelsky, Tamlin M.] Univ N Carolina, Dept Geol Sci, Chapel Hill, NC 27599 USA.
[Kapnick, Sarah; Hall, Alex] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA.
[Kapnick, Sarah] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Pavelsky, TM (reprint author), Univ N Carolina, Dept Geol Sci, Chapel Hill, NC 27599 USA.
EM pavelsky@unc.edu
RI Kapnick, Sarah/C-5209-2014; Hall, Alex/D-8175-2014
OI Kapnick, Sarah/0000-0003-0979-3070;
FU National Science Foundation [AGS-0735056]; Pittsburgh Supercomputing
Center; National Energy Research Scientific Computing Center [m995];
Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231];
NASA [07-Earth07F-0232]; Switzer Environmental Fellowship
FX Funding for this research was provided by the National Science
Foundation grant AGS-0735056 in part by the NSF through TeraGrid
resources provided by the Pittsburgh Supercomputing Center. This
research also used resources of the National Energy Research Scientific
Computing Center under contract m995, which is supported by the Office
of Science of the U.S. Department of Energy under contract
DE-AC02-05CH11231. Sarah Kapnick is also supported by a NASA Earth and
Space Science Graduate Fellowship (07-Earth07F-0232) and a 2010 Switzer
Environmental Fellowship. Finally, we thank Michael Durand and two
anonymous reviewers for their useful comments.
NR 60
TC 9
Z9 10
U1 1
U2 15
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 AUG 25
PY 2011
VL 116
AR D16115
DI 10.1029/2010JD015479
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 813LP
UT WOS:000294368400002
ER
PT J
AU Kug, JS
Ham, YG
Lee, EJ
Kang, IS
AF Kug, Jong-Seong
Ham, Yoo-Geun
Lee, Eun-Jeong
Kang, In-Sik
TI Empirical singular vector method for ensemble El Nino-Southern
Oscillation prediction with a coupled general circulation model
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID BRED VECTORS; INTERCOMPARISON PROJECT; PREDICTABILITY; SYSTEM; ENSO;
CLIMATE; PERTURBATIONS; SIMULATION; ERRORS; NCEP
AB Optimal initial perturbation is an important issue related to the improvement of the current seasonal climate prediction. In this study, we have applied the empirical singular vector method to ensemble El Nino-Southern Oscillation (ENSO) prediction with the Seoul National University coupled general circulation model. It is found that from the empirical linear operator, the leading singular mode, which represents the fast growing error mode in the tropical Pacific, shows El Nino-like perturbation in the present coupled model. When the singular vector is used as an initial perturbation, the forecast skill of ENSO is significantly improved. Further, it is demonstrated that the predictions with the singular vector have a more reliable ensemble spread, suggesting a potential merit for a probabilistic forecast.
C1 [Ham, Yoo-Geun] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kug, Jong-Seong] Korea Ocean Res & Dev Inst, Ansan 425600, South Korea.
[Lee, Eun-Jeong; Kang, In-Sik] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul 151742, South Korea.
[Ham, Yoo-Geun] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Studies & Invest, Columbia, MD USA.
RP Kug, JS (reprint author), Korea Ocean Res & Dev Inst, 1270 Sang Rok Gu, Ansan 425600, South Korea.
EM yoo-geun.ham@nasa.gov
RI KUG, JONG-SEONG/A-8053-2013; 안, 민섭/D-9972-2015
FU Korea Meteorological Administration [CATER_2006-4206]; second stage of
the Brain Korea 21 Project; Korea Institute of Science and Technology
Information [KSC-2009-S03-0002]
FX ISK is supported by the Korea Meteorological Administration Research and
Development Program under grant CATER_2006-4206 and the second stage of
the Brain Korea 21 Project. The model integration was carried out based
on the support by grant KSC-2009-S03-0002 from Korea Institute of
Science and Technology Information.
NR 29
TC 3
Z9 3
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-OCEANS
JI J. Geophys. Res.-Oceans
PD AUG 25
PY 2011
VL 116
AR C08029
DI 10.1029/2010JC006851
PG 9
WC Oceanography
SC Oceanography
GA 813KC
UT WOS:000294364400003
ER
PT J
AU Rao, MN
Nyquist, LE
Bogard, DD
Garrison, DH
Sutton, SR
Michel, R
Reedy, RC
Leya, I
AF Rao, M. N.
Nyquist, L. E.
Bogard, D. D.
Garrison, D. H.
Sutton, S. R.
Michel, R.
Reedy, R. C.
Leya, I.
TI Isotopic evidence for a Martian regolith component in shergottite
meteorites
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID NOBLE-GASES; SNC METEORITES; KRYPTON ISOTOPES; MARS; ORIGIN; NEUTRONS;
XENON; FLUX; TERRESTRIAL; EETA-79001
AB The (80)Kr excesses determined in the gas-rich impact-melt (GRIM) glasses in EET79001 and Shergotty correlate poorly with the (129)Xe(M) (Martian atmosphere) suggesting that the majority of the neutron-capture (80)Kr(n) was not shock-implanted along with (129)Xe(M) into these glasses during impact. This inference is consistent with the variations in delta (80)Kr(n) excesses observed in these samples. The results reported here indicate that the (80)Kr(n) excesses in these glasses were produced in the same way as the (149)Sm isotopic deficits, i.e., by thermal neutron (n) capture on Br and Sm occurring in the glass-precursor regolith materials on Mars. The thermal neutron fluences calculated from (80)Kr(n) excesses (similar to 0.3-1.0 x 10(15) n/cm(2)) and from (149)Sm deficits (1.0 +/- 0.4 x 10(15) n/cm(2)) agree with each other confirming that (80)Kr(n) was mostly produced in situ. In the Martian regolith, thermal (n) and fast (N) neutrons occur together. Also, in the GRIM glasses, the (83)Kr/(86)Kr ratios correlate positively with (84)Kr/(86)Kr indicating that the cosmogenic Kr contains a fast neutron-produced component in addition to Kr produced by galactic cosmic and solar cosmic irradiation. Using (83)Kr(N) and (84)Kr(N) excesses produced by fast neutron reactions on Rb and Sr targets in some of these glasses, we determine fast neutron fluences of similar to 3-47 x 10(15) N/cm(2). The integrated fluences of thermal and fast neutrons in GRIM glasses suggest that the glass-precursor materials were irradiated at different depths in the top few meters of the water-ice-bearing regolith near the shergottite source regions on Mars.
C1 [Rao, M. N.; Garrison, D. H.] NASA, Lyndon B Johnson Space Ctr, Jacobs ESCG, Houston, TX 77058 USA.
[Nyquist, L. E.; Bogard, D. D.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA.
[Leya, I.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland.
[Michel, R.] Leibniz Univ Hannover, Ctr Radiat Protect & Radioecol, D-30167 Hannover, Germany.
[Reedy, R. C.] Planetary Sci Inst, Los Alamos, NM 87545 USA.
[Sutton, S. R.] Univ Chicago, Dept Geol Sci, Chicago, IL 60637 USA.
RP Rao, MN (reprint author), NASA, Lyndon B Johnson Space Ctr, Jacobs ESCG, Houston, TX 77058 USA.
EM nageswara.rao@nasa.gov
OI Reedy, Robert/0000-0002-2189-1303
FU NASA
FX We thank C.-Y. Shih and Charles Meyer for help during this work. We are
grateful to Ulrich Ott and an anonymous reviewer for their valuable
comments and suggestions which contributed to a substantial improvement
of the paper. Also, we thank the Editor for his help during the review.
This work is supported by a NASA Mars Fundamental Research Program
Contract to L.E. Nyquist.
NR 49
TC 3
Z9 3
U1 0
U2 13
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 AUG 25
PY 2011
VL 116
AR E08006
DI 10.1029/2010JE003764
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 813KN
UT WOS:000294365600001
ER
PT J
AU Burrows, DN
Kennea, JA
Ghisellini, G
Mangano, V
Zhang, B
Page, KL
Eracleous, M
Romano, P
Sakamoto, T
Falcone, AD
Osborne, JP
Campana, S
Beardmore, AP
Breeveld, AA
Chester, MM
Corbet, R
Covino, S
Cummings, JR
D'Avanzo, P
D'Elia, V
Esposito, P
Evans, PA
Fugazza, D
Gelbord, JM
Hiroi, K
Holland, ST
Huang, KY
Im, M
Israel, G
Jeon, Y
Jeon, YB
Jun, HD
Kawai, N
Kim, JH
Krimm, HA
Marshall, FE
Meszaros, P
Negoro, H
Omodei, N
Park, WK
Perkins, JS
Sugizaki, M
Sung, HI
Tagliaferri, G
Troja, E
Ueda, Y
Urata, Y
Usui, R
Antonelli, LA
Barthelmy, SD
Cusumano, G
Giommi, P
Melandri, A
Perri, M
Racusin, JL
Sbarufatti, B
Siegel, MH
Gehrels, N
AF Burrows, D. N.
Kennea, J. A.
Ghisellini, G.
Mangano, V.
Zhang, B.
Page, K. L.
Eracleous, M.
Romano, P.
Sakamoto, T.
Falcone, A. D.
Osborne, J. P.
Campana, S.
Beardmore, A. P.
Breeveld, A. A.
Chester, M. M.
Corbet, R.
Covino, S.
Cummings, J. R.
D'Avanzo, P.
D'Elia, V.
Esposito, P.
Evans, P. A.
Fugazza, D.
Gelbord, J. M.
Hiroi, K.
Holland, S. T.
Huang, K. Y.
Im, M.
Israel, G.
Jeon, Y.
Jeon, Y. -B.
Jun, H. D.
Kawai, N.
Kim, J. H.
Krimm, H. A.
Marshall, F. E.
Meszaros, P.
Negoro, H.
Omodei, N.
Park, W. -K.
Perkins, J. S.
Sugizaki, M.
Sung, H. -I.
Tagliaferri, G.
Troja, E.
Ueda, Y.
Urata, Y.
Usui, R.
Antonelli, L. A.
Barthelmy, S. D.
Cusumano, G.
Giommi, P.
Melandri, A.
Perri, M.
Racusin, J. L.
Sbarufatti, B.
Siegel, M. H.
Gehrels, N.
TI Relativistic jet activity from the tidal disruption of a star by a
massive black hole
SO NATURE
LA English
DT Article
ID X-RAY OUTBURSTS; SWIFT; EVENTS; FLARES; TELESCOPE; NUCLEUS; MISSION;
GALAXY; GRBS
AB Supermassive black holes have powerful gravitational fields with strong gradients that can destroy stars that get too close(1,2), producing a bright flare in ultraviolet and X-ray spectral regions from stellar debris that forms an accretion disk around the black hole(3-7). The aftermath of this process may have been seen several times over the past two decades in the form of sparsely sampled, slowly fading emission from distant galaxies(8-14), but the onset of the stellar disruption event has not hitherto been observed. Here we report observations of a bright X-ray flare from the extragalactic transient Swift J164449.3+573451. This source increased in brightness in the X-ray band by a factor of at least 10,000 since 1990 and by a factor of at least 100 since early 2010. We conclude that we have captured the onset of relativistic jet activity from a supermassive black hole. A companion paper(15) comes to similar conclusions on the basis of radio observations. This event is probably due to the tidal disruption of a star falling into a supermassive black hole, but the detailed behaviour differs from current theoretical models of such events.
C1 [Burrows, D. N.; Kennea, J. A.; Eracleous, M.; Falcone, A. D.; Chester, M. M.; Fugazza, D.; Meszaros, P.; Siegel, M. H.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Ghisellini, G.; Campana, S.; Covino, S.; D'Avanzo, P.; Tagliaferri, G.; Melandri, A.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
[Mangano, V.; Romano, P.; Cusumano, G.; Sbarufatti, B.] INAF Ist Astrofis Spaziale & Fis Cosm, I-90146 Palermo, Italy.
[Zhang, B.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA.
[Page, K. L.; Osborne, J. P.; Beardmore, A. P.; Evans, P. A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Sakamoto, T.; Corbet, R.; Cummings, J. R.; Hiroi, K.; Krimm, H. A.; Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA.
[Sakamoto, T.; Corbet, R.; Cummings, J. R.; Hiroi, K.; Krimm, H. A.; Marshall, F. E.; Perkins, J. S.; Troja, E.; Barthelmy, S. D.; Racusin, J. L.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sakamoto, T.; Corbet, R.; Cummings, J. R.; Perkins, J. S.] Univ Maryland, Baltimore, MD 21250 USA.
[Breeveld, A. A.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[D'Elia, V.; Antonelli, L. A.; Giommi, P.; Perri, M.] ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Esposito, P.] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, Italy.
[Gelbord, J. M.; Ueda, Y.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Hiroi, K.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Holland, S. T.] Acad Sinica, Inst Astron & Astrophys, Tokyo 106, Japan.
[Huang, K. Y.; Jeon, Y.; Jun, H. D.; Kim, J. H.; Park, W. -K.] Seoul Natl Univ, Dept Phys & Astron, FPRD, Ctr Explorat Origin Universe, Seoul, South Korea.
[Im, M.; Antonelli, L. A.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Israel, G.; Sung, H. -I.] Korea Astron & Space Sci Inst KASI, Taejon 305348, South Korea.
[Jeon, Y. -B.; Usui, R.] Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan.
[Jeon, Y. -B.] RIKEN, MAXI Team, Wako, Saitama 3510198, Japan.
[Negoro, H.] Nihon Univ, Dept Phys, Chiyoda Ku, Tokyo 1018308, Japan.
[Omodei, N.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Omodei, N.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Urata, Y.] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan.
RP Burrows, DN (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
EM burrows@astro.psu.edu
RI Racusin, Judith/D-2935-2012; Barthelmy, Scott/D-2943-2012; Gehrels,
Neil/D-2971-2012; Im, Myungshin/B-3436-2013; Kim, Ji Hoon/A-8989-2009;
OI Omodei, Nicola/0000-0002-5448-7577; Perri, Matteo/0000-0003-3613-4409;
Esposito, Paolo/0000-0003-4849-5092; Sbarufatti,
Boris/0000-0001-6620-8347; Covino, Stefano/0000-0001-9078-5507;
Tagliaferri, Gianpiero/0000-0003-0121-0723; Antonelli, Lucio
Angelo/0000-0002-5037-9034; Im, Myungshin/0000-0002-8537-6714; D'Elia,
Valerio/0000-0002-7320-5862; Cusumano, Giancarlo/0000-0002-8151-1990;
Israel, GianLuca/0000-0001-5480-6438; Ghisellini,
Gabriele/0000-0002-0037-1974; Kim, Ji Hoon/0000-0002-1418-3309; Campana,
Sergio/0000-0001-6278-1576; giommi, paolo/0000-0002-2265-5003
FU NASA (US); NSF (US); DOE (US); UK Space Agency; ASI (Italy); INAF
(Italy); INFN (Italy); Autonomous Region of Sardinia; MEXT (Japan); KEK
(Japan); JAXA (Japan); CRI/NRF/MEST (Korea); NSC (Taiwan); Academia
Sinica (Taiwan); CEA/Irfu (France); IN2P3/CNRS (France); CNES (France);
K. A. Wallenberg Foundation (Sweden); Swedish Research Council (Sweden);
National Space Board (Sweden)
FX We acknowledge support from the following funding agencies: NASA, NSF
and DOE (US); the UK Space Agency; ASI, INAF and INFN (Italy); the
Autonomous Region of Sardinia; MEXT, KEK and JAXA (Japan); CRI/NRF/MEST
(Korea); NSC and Academia Sinica (Taiwan); CEA/Irfu, IN2P3/CNRS and CNES
(France); and the K. A. Wallenberg Foundation, the Swedish Research
Council and the National Space Board (Sweden). We thank the Swift, Fermi
and MAXI operation teams; and we thank A. Read for help with the most
recent XMM slew data. We acknowledge the contribution of pre-publication
upper limits by the VERITAS Collaboration. Finally, we acknowledge the
use of public data from the Swift and Fermi data archives
(http://heasarc.nasa.gov/docs/swift/archive/ and
http://fermi.gsfc.nasa.gov/ssc/, respectively), as well as data supplied
by the UK Swift Science Data Centre at the University of Leicester. E.T.
is a NASA Postdoctoral Fellow.
NR 29
TC 197
Z9 198
U1 0
U2 15
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD AUG 25
PY 2011
VL 476
IS 7361
BP 421
EP 424
DI 10.1038/nature10374
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 811KT
UT WOS:000294209400029
PM 21866154
ER
PT J
AU Callahan, MP
Smith, KE
Cleaves, HJ
Ruzicka, J
Stern, JC
Glavin, DP
House, CH
Dworkin, JP
AF Callahan, Michael P.
Smith, Karen E.
Cleaves, H. James, II
Ruzicka, Josef
Stern, Jennifer C.
Glavin, Daniel P.
House, Christopher H.
Dworkin, Jason P.
TI Carbonaceous meteorites contain a wide range of extraterrestrial
nucleobases
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
ID MURCHISON METEORITE; AMINO-ACIDS; MASS-SPECTROMETRY; ISOTOPIC ANALYSES;
CHONDRITES; PURINES; ORIGIN; PYRIMIDINES; MECHANISMS; ENRICHMENT
AB All terrestrial organisms depend on nucleic acids (RNA and DNA), which use pyrimidine and purine nucleobases to encode genetic information. Carbon-rich meteorites may have been important sources of organic compounds required for the emergence of life on the early Earth; however, the origin and formation of nucleobases in meteorites has been debated for over 50 y. So far, the few nucleobases reported in meteorites are biologically common and lacked the structural diversity typical of other indigenous meteoritic organics. Here, we investigated the abundance and distribution of nucleobases and nucleobase analogs in formic acid extracts of 12 different meteorites by liquid chromatography-mass spectrometry. The Murchison and Lonewolf Nunataks 94102 meteorites contained a diverse suite of nucleobases, which included three unusual and terrestrially rare nucleobase analogs: purine, 2,6-diaminopurine, and 6,8-diaminopurine. In a parallel experiment, we found an identical suite of nucleobases and nucleobase analogs generated in reactions of ammonium cyanide. Additionally, these nucleobase analogs were not detected above our parts-per-billion detection limits in any of the procedural blanks, control samples, a terrestrial soil sample, and an Antarctic ice sample. Our results demonstrate that the purines detected in meteorites are consistent with products of ammonium cyanide chemistry, which provides a plausible mechanism for their synthesis in the asteroid parent bodies, and strongly supports an extraterrestrial origin. The discovery of new nucleobase analogs in meteorites also expands the prebiotic molecular inventory available for constructing the first genetic molecules.
C1 [Callahan, Michael P.; Stern, Jennifer C.; Glavin, Daniel P.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Callahan, Michael P.; Stern, Jennifer C.; Glavin, Daniel P.; Dworkin, Jason P.] Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Smith, Karen E.; House, Christopher H.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
[Smith, Karen E.; House, Christopher H.] Penn State Univ, Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA.
[Cleaves, H. James, II] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA.
[Ruzicka, Josef] Thermo Fisher Sci, Sci Instruments Div, Somerset, NJ 08873 USA.
RP Callahan, MP (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM michael.p.callahan@nasa.gov
RI Callahan, Michael/D-3630-2012; Stern, Jennifer/E-3135-2012; Glavin,
Daniel/D-6194-2012; Dworkin, Jason/C-9417-2012;
OI Stern, Jennifer/0000-0002-0162-8807; Glavin, Daniel/0000-0001-7779-7765;
Dworkin, Jason/0000-0002-3961-8997; Cleaves,
Henderson/0000-0003-4101-0654
FU NASA; Goddard Center for Astrobiology; NASA Astrobiology Institute
FX The authors thank K. Righter (NASA Johnson Space Center, Houston, TX)
for providing the Antarctic meteorites and discussions, L. Welzenbach
and T. McCoy (Smithsonian National Museum of Natural History,
Washington, DC) for providing the Murchison meteorite sample, P.
Ehrenfreund (Affiliation, City, State) for providing the sample of
Orgueil, P. Jenniskens and M. Shaddad (Affiliation, City, State) for
providing the Almahata Sitta meteorite sample, R. Keays (University of
Melbourne, Melbourne, Australia) for providing the Murchison soil
sample, and the 2006 ANSMET team (Affiliation, City, State) for
providing the Antarctic ice sample. M.P.C. and H.J.C. acknowledge
support from the NASA Postdoctoral Program, administered by Oak Ridge
Associated Universities through a contract with NASA. K.E.S.
acknowledges support from the Goddard Center for Astrobiology. M.P.C.,
J.C.S., D.P.G., and J.P.D. acknowledge funding support from the NASA
Astrobiology Institute and the Goddard Center for Astrobiology and the
NASA Astrobiology: Exobiology and Evolutionary Biology Program. We thank
A. Burton, J. Cook, A. Lazcano, A. Mandell, M. Martin, and two anonymous
reviewers for valuable input regarding the writing of this manuscript.
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PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD AUG 23
PY 2011
VL 108
IS 34
BP 13995
EP 13998
DI 10.1073/pnas.1106493108
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 810XO
UT WOS:000294163500032
PM 21836052
ER
PT J
AU Cooper, G
Reed, C
Nguyen, D
Carter, M
Wang, Y
AF Cooper, George
Reed, Chris
Dang Nguyen
Carter, Malika
Wang, Yi
TI Detection and formation scenario of citric acid, pyruvic acid, and other
possible metabolism precursors in carbonaceous meteorites
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE pyruvate; citrate; Murchison meteorite; Alan Hills; interstellar
nitriles
ID IDENTIFICATION; CHONDRITES; CONVERSION; SULFUR
AB Carbonaceous meteorites deliver a variety of organic compounds to Earth that may have played a role in the origin and/or evolution of biochemical pathways. Some apparently ancient and critical metabolic processes require several compounds, some of which are relatively labile such as keto acids. Therefore, a prebiotic setting for any such individual process would have required either a continuous distant source for the entire suite of intact precursor molecules and/ or an energetic and compact local synthesis, particularly of the more fragile members. To date, compounds such as pyruvic acid, oxaloacetic acid, citric acid, isocitric acid, and aketoglutaric acid (all members of the citric acid cycle) have not been identified in extraterrestrial sources or, as a group, as part of a " one pot" suite of compounds synthesized under plausibly prebiotic conditions. We have identified these compounds and others in carbonaceous meteorites and/ or as low temperature (laboratory) reaction products of pyruvic acid. In meteorites, we observe many as part of three newly reported classes of compounds: keto acids (pyruvic acid and homologs), hydroxy tricarboxylic acids (citric acid and homologs), and tricarboxylic acids. Laboratory syntheses using 13C-labeled reactants demonstrate that one compound alone, pyruvic acid, can produce several (nonenzymatic) members of the citric acid cycle including oxaloacetic acid. The isotopic composition of some of the meteoritic keto acids points to interstellar or presolar origins, indicating that such compounds might also exist in other planetary systems.
C1 [Cooper, George; Reed, Chris; Dang Nguyen; Carter, Malika] NASA, Ames Res Ctr, Exobiol Branch, Div Space Sci, Moffett Field, CA 94035 USA.
[Wang, Yi] Dev Planning Res & Anal ZymaX Forens Isotope, Escondido, CA 92029 USA.
RP Cooper, G (reprint author), NASA, Ames Res Ctr, Exobiol Branch, Div Space Sci, Moffett Field, CA 94035 USA.
EM george.cooper@nasa.gov
FU NASA-Johnson Space Center [ALH 83102]; NASA
FX We thank Art Weber for helpful discussions; David Des Marais and Sandra
Pizzarello for comments on the manuscript; Beverly M. McLeod and Donna
H. Kleiner for library resources; Novelle Kimmich for assistance with
figures; Aliah Dugas, Amy Byrd, and Patricia Chang for assistance with
keto acid synthesis; Carlton Moore, Laurie Leshin, and the ASU Center
for Meteorite Studies for samples of Murchison; NASA-Johnson Space
Center Antarctic Meteorite Program for ALH 83102. This work was
supported by NASA's Astrobiology and Exobiology Program.
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PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD AUG 23
PY 2011
VL 108
IS 34
BP 14015
EP 14020
DI 10.1073/pnas.1105715108
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 810XO
UT WOS:000294163500036
PM 21825143
ER
PT J
AU Li, YF
Cucinotta, FA
AF Li, Yongfeng
Cucinotta, Francis A.
TI Modeling non-homologous end joining
SO JOURNAL OF THEORETICAL BIOLOGY
LA English
DT Article
DE DNA repair pathway; Two-phase model; Sequential model
ID DEPENDENT PROTEIN-KINASE; BREAK REPAIR PATHWAY; DOUBLE-STRAND BREAKS;
DNA-PK; CELL-CYCLE; KU; COMPLEX; ANTIGEN; CHOICE; XRCC4
AB Non-homologous end joining (NHEJ) is an important DNA repair pathway for DNA double-strand breaks. Several proteins, including Ku, DNA-PKcs, Artemis, XRCC4/Ligase IV and XLF, are involved in the NHEJ for the DNA damage detection, DNA free end processing and ligation. The classical model of NHEJ is a sequential model in which DNA-PKcs is first recruited by the Ku bound DNA prior to any other repair proteins. Recent experimental study (McElhinny et al., 2000; Costantini et al., 2007; Mari et al., 2006; Yano and Chen, 2008) suggested that the recruitment ordering is not crucial. In this work, by proposing a mathematical model in terms of biochemical reaction network and performing stability and related analysis, we demonstrate theoretically that if DSB repair pathway independent of DNA-PKcs exists, then the classical sequential model and new two-phase model are essentially indistinguishable in the sense that DSB can be repaired thoroughly in both models when the repair proteins are sufficient. Published by Elsevier Ltd.
C1 [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Li, Yongfeng] USRA, Div Space Life Sci, Houston, TX 77058 USA.
RP Cucinotta, FA (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
EM li@dsls.usra.edu; francis.a.cucinotta@nasa.gov
FU NASA; Department of Energy
FX This work was supported by the NASA Space Radiation Program and the
Department of Energy's Low Dose Program.
NR 32
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U1 0
U2 6
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0022-5193
J9 J THEOR BIOL
JI J. Theor. Biol.
PD AUG 21
PY 2011
VL 283
IS 1
BP 122
EP 135
DI 10.1016/j.jtbi.2011.05.015
PG 14
WC Biology; Mathematical & Computational Biology
SC Life Sciences & Biomedicine - Other Topics; Mathematical & Computational
Biology
GA 868ME
UT WOS:000298526600014
PM 21635903
ER
PT J
AU Dion, MP
Son, S
Hunter, SD
de Nolfo, GA
AF Dion, M. P.
Son, S.
Hunter, S. D.
de Nolfo, G. A.
TI Negative ion drift velocity and longitudinal diffusion in mixtures of
carbon disulfide and methane
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article
DE TPC; Fast neutron; Neutron imaging; Negative ion; Diffusion
ID GAS-MIXTURES; PROPORTIONAL-COUNTERS; ELECTRON; DETECTORS; OPERATION;
ENERGY; TPC
AB Negative ion drift velocity and longitudinal diffusion have been measured for gas mixtures of carbon disulfide (CS(2)) and methane (CH(4)). Measurements were made as a function of total pressure. CS(2) partial pressure and electric field. Constant mobility and thermal-limit longitudinal diffusion are observed for all gas mixtures tested. Gas gain for some of the mixtures is also included. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Dion, M. P.; Son, S.] CRESST, Greenbelt, MD 20771 USA.
[Dion, M. P.; Son, S.; Hunter, S. D.; de Nolfo, G. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Dion, M. P.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Son, S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
RP Dion, MP (reprint author), CRESST, Code 661, Greenbelt, MD 20771 USA.
EM michael.p.dion@nasa.gov
RI Hunter, Stanley/D-2942-2012; de Nolfo, Georgia/E-1500-2012;
OI Dion, Michael/0000-0002-3030-0050
NR 30
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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 AUG 21
PY 2011
VL 648
IS 1
BP 186
EP 191
DI 10.1016/j.nima.2011.06.006
PG 6
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 801GB
UT WOS:000293425400023
ER
PT J
AU Katz, A
Sankaran, V
AF Katz, Aaron
Sankaran, Venkateswaran
TI Mesh quality effects on the accuracy of CFD solutions on unstructured
meshes
SO JOURNAL OF COMPUTATIONAL PHYSICS
LA English
DT Article
DE Unstructured grids; Mesh quality; Manufactured solutions; Error
convergence; High-order methods
ID VERIFICATION; DYNAMICS; SCHEMES; GRIDS; CODE
AB The order of accuracy and error magnitude of node- and cell-centered schemes are examined on representative unstructured meshes and flowfield solutions for computation fluid dynamics. Specifically, we investigate the properties of inviscid and viscous flu), cretizations for isotropic and highly stretched meshes using the Method of Manufacture Solutions. Grid quality effects are studied by randomly perturbing the base meshes ant aloguing the error convergence as a function of grid size. For isotropic grids, node-ceni approaches produce less error than cell-centered approaches. Moreover, a corrected r centered scheme is shown to maintain third order accuracy for the inviscid terms on trary triangular meshes. In contrast, for stretched meshes, cell-centered scheme favored, with cell-centered prismatic approaches in particular showing the lowest of error. In three dimensions, simple flux integrations on non-planar control volume lead to first-order solution errors, while second-order accuracy is recovered by trian: tion of the non-planar faces. (C) 2011 Elsevier Inc. All rights reserve.
C1 [Katz, Aaron; Sankaran, Venkateswaran] USA, Aeroffightdynam Directorate AMRDEC, Moffett Field, CA 94035 USA.
RP Katz, A (reprint author), NASA, Ames Res Ctr, M-S 215-1, Moffett Field, CA 94035 USA.
EM akatz@merlin.arc.nasa.gov
RI Katz, Aaron/I-8244-2015
OI Katz, Aaron/0000-0003-2739-9384
FU Department of Defense High Performance Computing Modernization Office
(HPCMO); US Department of Defense HPC Modernization Program Office
FX Development was performed at the HPC Institute for Advanced Rotorcraft
Modeling and Simulation (HIARMS) located at the US Army
Aeroflightdynamics Directorate at Moffett Field, CA, which is supported
by the Department of Defense High Performance Computing Modernization
Office (HPCMO). Material presented in this paper is a product of the
CREATE-AV Element of the Computational Research and Engineering for
Acquisition Tools and Environments (CREATE) Program sponsored by the US
Department of Defense HPC Modernization Program Office.
NR 27
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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 0021-9991
J9 J COMPUT PHYS
JI J. Comput. Phys.
PD AUG 20
PY 2011
VL 230
IS 20
BP 7670
EP 7686
DI 10.1016/j.jcp.2011.06.023
PG 17
WC Computer Science, Interdisciplinary Applications; Physics, Mathematical
SC Computer Science; Physics
GA 815HY
UT WOS:000294517900007
ER
PT J
AU Bal, G
Davis, AB
Langmore, I
AF Bal, Guillaume
Davis, Anthony B.
Langmore, Ian
TI A hybrid (Monte Carlo/deterministic) approach for multi-dimensional
radiation transport
SO JOURNAL OF COMPUTATIONAL PHYSICS
LA English
DT Article
DE Linear transport; Monte Carlo; Hybrid methods; Importance sampling;
Variance reduction; 3D rendering; Remote sensing
ID IMPORTANCE FUNCTION TRANSFORM; AUTOMATIC VARIANCE REDUCTION; CARLO
SIMULATIONS
AB A novel hybrid Monte Carlo transport scheme is demonstrated in a scene with solar illumination, scattering and absorbing 2D atmosphere, a textured reflecting mountain, and a small detector located in the sky (mounted on a satellite or a airplane). It uses a deterministic approximation of an adjoint transport solution to reduce variance, computed quickly by ignoring atmospheric interactions. This allows significant variance and computational cost reductions when the atmospheric scattering and absorption coefficient are small. When combined with an atmospheric photon-redirection scheme, significant variance reduction (equivalently acceleration) is achieved in the presence of atmospheric interactions. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Bal, Guillaume; Langmore, Ian] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA.
[Davis, Anthony B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Davis, Anthony B.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
RP Langmore, I (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, 200 SW Mudd Bldg,500 W 120th St, New York, NY 10027 USA.
EM gb2030@columbia.edu; Anthony.B.Davis@jpl.nasa.gov; ianlangmore@gmail.com
FU DOE/NNSA [DE-FG52-08NA28779]; NSF [DMS-0804696, PHY05-51164,
DMS-060DMS-0602235]; National Aeronautics and Space Administration
FX This work was supported in part by DOE/NNSA Grant No. DE-FG52-08NA28779
and NSF Grants Nos. DMS-0804696 and PHY05-51164, as well as NSF Research
Training Grant No. DMS-060DMS-0602235. This research was partially
carried out partly at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. AD wishes to thank the Kavli Institute for
Theoretical Physics at UC Santa Barbara for hospitality and stimulation
while finishing this manuscript. Finally, we are grateful to
NR 32
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PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0021-9991
J9 J COMPUT PHYS
JI J. Comput. Phys.
PD AUG 20
PY 2011
VL 230
IS 20
BP 7723
EP 7735
DI 10.1016/j.jcp.2011.06.029
PG 13
WC Computer Science, Interdisciplinary Applications; Physics, Mathematical
SC Computer Science; Physics
GA 815HY
UT WOS:000294517900010
ER
EF