FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Hosokawa, T
Yoshida, N
Omukai, K
Yorke, HW
AF Hosokawa, Takashi
Yoshida, Naoki
Omukai, Kazuyuki
Yorke, Harold W.
TI PROTOSTELLAR FEEDBACK AND FINAL MASS OF THE SECOND-GENERATION PRIMORDIAL
STARS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; cosmology: theory; early universe; H II
regions; stars: evolution; stars: formation
ID FOSSIL HII-REGIONS; 1ST STARS; EARLY UNIVERSE; ACCRETION RATES; DISK
ACCRETION; GAS CLOUDS; EVOLUTION; BINARIES; IMPACT; HD
AB The first stars in the universe ionized the ambient primordial gas through various feedback processes. "Second-generation" primordial stars potentially form from this disturbed gas after its recombination. In this Letter, we study the late formation stage of such second-generation stars, where a large amount of gas accretes onto the protostar and the final stellar mass is determined when the accretion terminates. We directly compute the complex interplay between the accretion flow and stellar ultraviolet (UV) radiation, performing radiation-hydrodynamic simulations coupled with stellar evolution calculations. Because of more efficient H-2 and HD cooling in the prestellar stage, the accretion rates onto the star are 10 times lower than in the case of the formation of the first stars. The lower accretion rates and envelope density result in the occurrence of an expanding bipolar H II region at a lower protostellar mass M-* similar or equal to 10 M-circle dot, which blows out the circumstellar material, thereby quenching the mass supply from the envelope to the accretion disk. At the same time the disk loses mass due to photoevaporation by the growing star. In our fiducial case the stellar UV feedback terminates mass accretion onto the star at M-* similar or equal to 17 M-circle dot. Although the derived masses of the second-generation primordial stars are systematically lower than those of the first generation, the difference is within a factor of only a few. Our results suggest a new scenario, whereby the majority of the primordial stars are born as massive stars with tens of solar masses, regardless of their generations.
C1 [Hosokawa, Takashi; Yoshida, Naoki] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan.
[Hosokawa, Takashi; Yorke, Harold W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Yoshida, Naoki] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan.
[Omukai, Kazuyuki] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan.
RP Hosokawa, T (reprint author), Univ Tokyo, Dept Phys, Tokyo 1130033, Japan.
EM takashi.hosokawa@phys.s.u-tokyo.ac.jp
FU Fellowship of the Japan Society for the Promotion of Science for
Research Abroad; Ministry of Education, Science and Culture of Japan
[2168407, 21244021]; National Aeronautics and Space Administration
(NASA)
FX The authors thank Neal Turner and Rolf Kuiper for fruitful discussions
and comments. T.H. appreciates the support by the Fellowship of the
Japan Society for the Promotion of Science for Research Abroad. K.O. is
supported by the Grants-in-Aid by the Ministry of Education, Science and
Culture of Japan (2168407 and 21244021). Portions of this work were
conducted at the Jet Propulsion Laboratory, California Institute of
Technology, operating under a contract with the National Aeronautics and
Space Administration (NASA).
NR 42
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD DEC 1
PY 2012
VL 760
IS 2
AR L37
DI 10.1088/2041-8205/760/2/L37
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 037KM
UT WOS:000311103000018
ER
PT J
AU Mayama, S
Hashimoto, J
Muto, T
Tsukagoshi, T
Kusakabe, N
Kuzuhara, M
Takahashi, Y
Kudo, T
Dong, R
Fukagawa, M
Takami, M
Momose, M
Wisniewski, JP
Follette, K
Abe, L
Akiyama, E
Brandner, W
Brandt, T
Carson, J
Egner, S
Feldt, M
Goto, M
Grady, CA
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, S
Henning, T
Hodapp, KW
Ishii, M
Iye, M
Janson, M
Kandori, R
Kwon, J
Knapp, GR
Matsuo, T
McElwain, MW
Miyama, S
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, TS
Serabyn, E
Suto, H
Suzuki, R
Takato, N
Terada, H
Thalmann, C
Tomono, D
Turner, EL
Watanabe, M
Yamada, T
Takami, H
Usuda, T
Tamura, M
AF Mayama, S.
Hashimoto, J.
Muto, T.
Tsukagoshi, T.
Kusakabe, N.
Kuzuhara, M.
Takahashi, Y.
Kudo, T.
Dong, R.
Fukagawa, M.
Takami, M.
Momose, M.
Wisniewski, J. P.
Follette, K.
Abe, L.
Akiyama, E.
Brandner, W.
Brandt, T.
Carson, J.
Egner, S.
Feldt, M.
Goto, M.
Grady, C. A.
Guyon, O.
Hayano, Y.
Hayashi, M.
Hayashi, S.
Henning, T.
Hodapp, K. W.
Ishii, M.
Iye, M.
Janson, M.
Kandori, R.
Kwon, J.
Knapp, G. R.
Matsuo, T.
McElwain, M. W.
Miyama, S.
Morino, J. -I.
Moro-Martin, A.
Nishimura, T.
Pyo, T. -S.
Serabyn, E.
Suto, H.
Suzuki, R.
Takato, N.
Terada, H.
Thalmann, C.
Tomono, D.
Turner, E. L.
Watanabe, M.
Yamada, T.
Takami, H.
Usuda, T.
Tamura, M.
TI SUBARU IMAGING OF ASYMMETRIC FEATURES IN A TRANSITIONAL DISK IN UPPER
SCORPIUS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planetary systems; protoplanetary disks; stars: pre-main sequence;
techniques: polarimetric
ID T-TAURI STARS; PROTOPLANETARY DISK; OB ASSOCIATION; PRETRANSITIONAL
DISKS; INFRARED VARIABILITY; CIRCUMSTELLAR DISK; PLANET FORMATION;
MOLECULAR CLOUD; FORMING REGIONS; SCATTERED-LIGHT
AB We report high-resolution (0.07 arcsec) near-infrared polarized intensity images of the circumstellar disk around the star 2MASS J16042165-2130284 obtained with HiCIAO mounted on the Subaru 8.2 m telescope. We present our H-band data, which clearly exhibit a resolved, face-on disk with a large inner hole for the first time at infrared wavelengths. We detect the centrosymmetric polarization pattern in the circumstellar material as has been observed in other disks. Elliptical fitting gives the semimajor axis, semiminor axis, and position angle (P.A.) of the disk as 63 AU, 62 AU, and -14 degrees, respectively. The disk is asymmetric, with one dip located at P.A.s of similar to 85 degrees. Our observed disk size agrees well with a previous study of dust and CO emission at submillimeter wavelength with Submillimeter Array. Hence, the near-infrared light is interpreted as scattered light reflected from the inner edge of the disk. Our observations also detect an elongated arc (50 AU) extending over the disk inner hole. It emanates at the inner edge of the western side of the disk, extending inward first, then curving to the northeast. We discuss the possibility that the inner hole, the dip, and the arc that we have observed may be related to the existence of unseen bodies within the disk.
C1 [Mayama, S.] Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Hayama, Kanagawa 2400193, Japan.
[Mayama, S.; Hayano, Y.; Hayashi, M.; Hayashi, S.; Iye, M.; Kwon, J.; Takato, N.; Takami, H.; Usuda, T.; Tamura, M.] Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan.
[Hashimoto, J.; Kusakabe, N.; Kuzuhara, M.; Takahashi, Y.; Akiyama, E.; Hayashi, M.; Iye, M.; Kandori, R.; Morino, J. -I.; Suto, H.; Suzuki, R.; Tamura, M.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Muto, T.] Kogakuin Univ, Div Liberal Arts, Shinjuku Ku, Tokyo 1638677, Japan.
[Tsukagoshi, T.; Momose, M.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Kuzuhara, M.] Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan.
[Takahashi, Y.] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Kudo, T.; Egner, S.; Guyon, O.; Hayano, Y.; Hayashi, S.; Ishii, M.; Nishimura, T.; Pyo, T. -S.; Takato, N.; Terada, H.; Tomono, D.; Takami, H.; Usuda, T.] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Dong, R.; Brandt, T.; Janson, M.; Knapp, G. R.; Moro-Martin, A.; Turner, E. L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Fukagawa, M.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Wisniewski, J. P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Follette, K.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Follette, K.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Abe, L.] Univ Nice Sophia Antipolis, UMR6525, Lab Hippolyte Fizeau, F-06108 Nice 02, France.
[Brandner, W.; Feldt, M.; Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Carson, J.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Goto, M.] Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Grady, C. A.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Grady, C. A.] Eureka Sci, Oakland, CA 96002 USA.
[Grady, C. A.; McElwain, M. W.] NASA, Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Hodapp, K. W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Matsuo, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Miyama, S.] Hiroshima Univ, Off President, Hiroshima 7398511, Japan.
[Moro-Martin, A.] CSIC, INTA, CAB, Dept Astrofis, E-28850 Madrid, Spain.
[Serabyn, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Thalmann, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Turner, E. L.] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2278568, Japan.
[Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido 0600810, Japan.
[Yamada, T.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
RP Mayama, S (reprint author), Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Hayama, Kanagawa 2400193, Japan.
EM mayama_satoshi@soken.ac.jp
RI Turner, Edwin/A-4295-2011; MIYAMA, Shoken/A-3598-2015
FU MEXT [22000005]; KAKENHI [23103004, 24103504, 24840037]; US NSF grant
[1009314, 1009203]; Center for the Promotion of Integrated Sciences
(CPIS) of The Graduate University for Advanced Studies (SOKENDAI)
FX We thank the telescope staff and operators at the Subaru Telescope for
their assistance. We also thank our referee for the constructive
comments that have helped to improve this manuscript. Part of this
research was carried out at the JPL, under a contract with NASA. This
work is partially supported by a Grant-in-Aid for Science Research in a
Priority Area from MEXT 22000005 (M.T.), KAKENHI 23103004 (M.M. and
M.F.), 24103504 (T.T.), 24840037 (T.M.), US NSF grant 1009314 (J.P.W.),
and 1009203 (J.C.). This work was supported in part by the Center for
the Promotion of Integrated Sciences (CPIS) of The Graduate University
for Advanced Studies (SOKENDAI).
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD DEC 1
PY 2012
VL 760
IS 2
AR L26
DI 10.1088/2041-8205/760/2/L26
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 037KM
UT WOS:000311103000007
ER
PT J
AU Chatfield, RB
Esswein, RF
AF Chatfield, Robert B.
Esswein, Robert F.
TI Estimation of surface O-3 from lower-troposphere partial-column
information: Vertical correlations and covariances in ozonesonde
profiles
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Remote retrieval; Smog ozone; Surface ozone; Statistical structure of
atmosphere; Ozonesonde; Boundary layer structure; Pollution layering
ID SATELLITE MEASUREMENTS; POLLUTION
AB Analysis of the spatial correlation of ozone mixing ratio in the vertical provides information useful for several purposes: (a) it aids description of the degree of regionality of the ozone transport-transformation processes, (b) the information provided in the form of a priori covariance matrices for remote retrieval algorithms can simplify and sharpen accuracy of the resulting estimates, and most importantly, (c) it allows a first evaluation of the improvement that remote retrievals can give over boundary-layer climatology. Vertical profiles of mean, variance, and vertical autocovariance, and vertical autocorrelation of ozone mixing ratios were estimated and given parameterizations. The WOUDC ozonesonde network database was used. During the years 2004-2006, these were considerably augmented by sondes taken by NASA, NOAA, and Canadian agencies during recent summertime intensive periods in North America. There are large differences across the North American continent in the patterns and magnitudes of correlation, especially in the lowest 2-3 km of the troposphere. This is especially significant for the near-surface layers (100's of meters deep) which determine actual surface O-3 smog exposure and phytotoxicity, since satellite retrievals typically characterize at best a thick layer extending 3 km or more from the surface. The relative variation of O-3 decreases in the vertical, particularly for the somewhat polluted launch stations, and this affects inference of surface O-3 significantly. We outline a simple synthesis of mixed-layer and ozone-chemistry behavior to aid discussion of this and similar phenomena. Regional differences suggest broad if qualitative explanations in terms of larger-scale (interstate-transport) and local-scale phenomena (lake and sea breezes, degree/frequency of subsidence), inviting future study. The character of near-surface-to-full-layer covariance suggests that remote retrieval can describe surface ozone surprisingly well using 0-3 km partial-column ozone... for many situations. This indicates that there is substantial utility for new remote-retrieval methods that exploit ozone absorption in multiple wavelength regions, e.g., UV + Vis, UV + IR, or UV + Vis + IR. In summary, we find considerable value in interpreting retrievable O-3 columns to estimate O-3 quantities that are closely relevant to air pollution mitigation. Published by Elsevier Ltd.
C1 [Chatfield, Robert B.; Esswein, Robert F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Esswein, Robert F.] Bay Area Environm Res, Sonoma, CA 95476 USA.
RP Chatfield, RB (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Robert.B.Chatfield@nasa.gov
FU Environment Canada; NOAA; NASA; Earth Science Division of the NASA
Science Mission Directorate
FX We particularly appreciate the contributions of the many ozonesonde
operators and the industry of the organizers (especially D.W. Tarasick,
S.J. Oltmans, and A.M. Thompson) of the sonde networks, funded by
Environment Canada and allied organizations, NOAA, and NASA. Funding for
this effort was provided by the Earth Science Division of the NASA
Science Mission Directorate. Thanks to Laura Iraci and Michael Newchurch
who reviewed an earlier draft.
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD DEC
PY 2012
VL 61
BP 103
EP 113
DI 10.1016/j.atmosenv.2012.06.033
PG 11
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 038QA
UT WOS:000311188000012
ER
PT J
AU Beyersdorf, AJ
Thornhill, KL
Winstead, EL
Ziemba, LD
Blake, DR
Timko, MT
Anderson, BE
AF Beyersdorf, Andreas J.
Thornhill, K. Lee
Winstead, Edward L.
Ziemba, Luke D.
Blake, Donald R.
Timko, Michael T.
Anderson, Bruce E.
TI Power-dependent speciation of volatile organic compounds in aircraft
exhaust
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Aircraft emissions; Turbine engine; Hydrocarbon emission indices;
Oxygenated hydrocarbons
ID HYDROCARBON EMISSION INDEXES; IN-FLIGHT MEASUREMENT; COMMERCIAL
AIRCRAFT; CHEMICAL-COMPOSITION; TURBINE-ENGINES; AIRPORT; AIR;
REACTIVITY; CO
AB As part of the third NASA Aircraft Particle Emissions Experiment (APEX-3, November 2005), whole air samples were collected to determine the emission rates of volatile organic compounds (VOCs) from aircraft equipped with three different gas-turbine engines (an Allison Engine 3007-A1E, a Pratt-Whitney 4158, and a Rolls-Royce RB211-535E4B). Samples were collected 1 m behind the engine exhaust plane of the engines while they were operated at powers ranging from idle up to 30% of maximum rated thrust.
Exhaust emission indices (mass emitted per kilogram of fuel used) for CO and non-methane hydrocarbons (NMHCs) were calculated based on enhancements over background relative to CO2. Emissions of all NMHCs were greatest at low power with values decreasing by an order of magnitude with increasing power. Previous studies have shown that scaling idle hydrocarbon emissions to formaldehyde or ethene (which are typically emitted at a ratio of 1-to-1 at idle) reduces variability amongst engine types. NMHC emissions were found to scale at low power, with alkenes contributing over 50% of measured NMHCs. However, as the power increases hydrocarbon emissions no longer scale to ethene, as the aromatics become the dominant species emitted. This may be due in part to a shift in combustion processes from thermal cracking (producing predominantly alkenes) to production of new molecules (producing proportionally more aromatics) as power increases. The formation of these aromatics is an intermediate step in the production of soot, which also increases with increasing power. The increase in aromatics relative to alkenes additionally results in a decrease in the hydroxyl radical reactivity and ozone formation potential of aircraft exhaust.
Samples collected 30 m downwind of the engine were also analyzed for NMHCs and carbonyl compounds (acetone, 2-butanone and C-1-C-9 aldehydes). Formaldehyde was the predominant carbonyl emitted; however, the ratio of ethene-to-formaldehyde varied between the aircraft, possibly due to the sampling of transient emissions such as engine start-up and power changes. A large portion of the measured emissions (27-42% by mass) in the plume samples was made up of hazardous air pollutants (HAPs) with oxygenated compounds being most significant. Published by Elsevier Ltd.
C1 [Beyersdorf, Andreas J.; Thornhill, K. Lee; Winstead, Edward L.; Ziemba, Luke D.; Anderson, Bruce E.] NASA Langley Res Ctr, Hampton, VA 23662 USA.
[Thornhill, K. Lee; Winstead, Edward L.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Blake, Donald R.] Univ Calif Irvine, Irvine, CA 92697 USA.
[Timko, Michael T.] Aerodyne Res Inc, Billerica, MA 01821 USA.
RP Beyersdorf, AJ (reprint author), NASA Langley Res Ctr, Hampton, VA 23662 USA.
EM andreas.j.beyersdorf@nasa.gov
RI Beyersdorf, Andreas/N-1247-2013
FU NASA Aeronautics Research Mission Directorate
FX This research was supported by the NASA Aeronautics Research Mission
Directorate. Assistance during the field campaign was provided by
Charles Hudgins (NASA Langley) and was facilitated by Southwest
Airlines, Continental Airlines, Fed Ex and NASA Glenn Research Center.
Analytical assistance was provided by Changlie Wey at NASA Glenn
(CO2 data) and Gloria Liu, Brent Love and Simone Meinardi at
UC Irvine. John Kinsey at the EPA provided the APEX report and helpful
suggestions during manuscript preparation. Assistance with manuscript
preparation was also provided by Scott Herndon at Aerodyne Research,
Inc. and Angela Baker at the Max Planck Institute for Chemistry.
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PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD DEC
PY 2012
VL 61
BP 275
EP 282
DI 10.1016/j.atmosenv.2012.07.027
PG 8
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 038QA
UT WOS:000311188000029
ER
PT J
AU Jackson, WA
Davila, AF
Estrada, N
Lyons, WB
Coates, JD
Priscu, JC
AF Jackson, W. Andrew
Davila, Alfonso F.
Estrada, Nubia
Lyons, W. Berry
Coates, John D.
Priscu, John C.
TI Perchlorate and chlorate biogeochemistry in ice-covered lakes of the
McMurdo Dry Valleys, Antarctica
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID TAYLOR VALLEY; NATURAL PERCHLORATE; OXIDIZING BACTERIA; NITROUS-OXIDE;
FRYXELL BASIN; SALINE LAKES; EVOLUTION; BONNEY; GEOCHEMISTRY; REDUCTION
AB We measured chlorate (ClO3-) and perchlorate (ClO4-) concentrations in ice covered lakes of the McMurdo Dry Valleys (MDVs) of Antarctica, to evaluate their role in the ecology and geochemical evolution of the lakes. ClO3- and ClO4- are present throughout the MDV Lakes, streams, and other surface water bodies. ClO3- and ClO4- originate in the atmosphere and are transported to the lakes by surface inflow of glacier melt that has been differentially impacted by interaction with soils and aeolian matter. Concentrations of ClO3- and ClO4- in the lakes and between lakes vary based on both total evaporative concentration, as well as biological activity within each lake. All of the lakes except the East lobe of Lake Bonney support biological reduction of ClO3- and ClO4- either in the anoxic bottom waters or sediment. The younger less saline lakes (Miers and Hoare), have surface ClO3- and ClO4- concentrations, and ratios of ClO3-/Cl- and ClO4-/Cl-, similar to source streams, while Lake Fryxell has concentrations similar to input streams but much lower ClO3-/Cl- and ClO4-/Cl- ratios, reflecting the influence of a large Cl- source in bottom sediments. ClO3- and ClO4- in Lake Bonney are the highest of all the lakes reflecting the lake's greater age and higher concentration of Cl-. ClO4- appears to be stable in the East Lobe and its concentration is highly correlated with Cl- concentration suggesting that some ClO4- at depth is a remnant of the initial seawater that formed Lake Bonney. ClO3- and ClO4- concentrations provide a simple and sensitive means to evaluate microbial activity in these lakes due to their relatively low concentrations and lack of biological sources, unlike NO3-, NO2-, and SO42-. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Jackson, W. Andrew; Estrada, Nubia] Texas Tech Univ, Dept Civil & Environm Engn, Lubbock, TX 79409 USA.
[Davila, Alfonso F.] NASA, Ames Res Ctr, Moffett Field, CA 95136 USA.
[Davila, Alfonso F.] SETI Inst, Mountain View, CA 94043 USA.
[Lyons, W. Berry] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA.
[Coates, John D.] Univ Calif Berkeley, Dept Plant & Microbial Biol, Berkeley, CA 94720 USA.
[Priscu, John C.] Montana State Univ, Dept Land Resources & Environm Sci, Bozeman, MT 59717 USA.
RP Jackson, WA (reprint author), Texas Tech Univ, Dept Civil & Environm Engn, Lubbock, TX 79409 USA.
EM andrew.jackson@ttu.edu
RI Jackson, William/B-8999-2009; Davila, Alfonso/A-2198-2013
OI Davila, Alfonso/0000-0002-0977-9909
FU Strategic Environmental Research and Development Program (SERDP)
[ER-1435]; NSF OPP [0432595, 0631494]; Energy Biosciences Institute, UC
Berkeley, CA; NASA Exobiology program [NNX12AD61G]
FX This work was supported by the Strategic Environmental Research and
Development Program (SERDP Project ER-1435) and by NSF OPP grants
0432595 and 0631494. We are grateful to the McMurdo Long Term Ecological
Research Program for providing water samples from the MDV and would
especially like to acknowledge Kathy Welch and Amy Chiuchiolo for their
time and efforts. Work in the lab of J.D.C was supported by the Energy
Biosciences Institute, UC Berkeley, CA. A. F. D is supported by the NASA
Exobiology program (Grant Number NNX12AD61G).
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD DEC 1
PY 2012
VL 98
BP 19
EP 30
DI 10.1016/j.gca.2012.09.014
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 038ZB
UT WOS:000311211500002
ER
PT J
AU Cheng, SW
Garlan, D
AF Cheng, Shang-Wen
Garlan, David
TI Stitch: A language for architecture-based self-adaptation
SO JOURNAL OF SYSTEMS AND SOFTWARE
LA English
DT Article
DE Rainbow; Self-adaptation; Strategy; Tactic; Uncertainty; Utility
ID SYSTEMS
AB Requirements for high availability in computing systems today demand that systems be self-adaptive to maintain expected qualities-of-service in the presence of system faults, variable environmental conditions, and changing user requirements. Autonomic computing tackles the challenge of automating tasks that humans would otherwise have to perform to achieve this goal. However, existing approaches to autonomic computing lack the ability to capture routine human repair tasks in a way that takes into account the business context humans use in selecting an appropriate form of adaptation, while dealing with timing delays and uncertainties in outcome of repair actions. In this article, we present Stitch, a language for representing repair strategies within the context of an architecture-based self-adaptation framework. Stitch supports the explicit representation of repair decision trees together with the ability to express business objectives, allowing a self-adaptive system to select a strategy that has optimal utility in a given context, even in the presence of potential timing delays and outcome uncertainty. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Cheng, Shang-Wen; Garlan, David] Carnegie Mellon Univ, Sch Comp Sci, Pittsburgh, PA 15213 USA.
RP Cheng, SW (reprint author), NASA, Jet Prop Lab, Washington, DC 20546 USA.
EM chengs@cmu.edu; garlan@cs.cmu.edu
FU DARPA [N66001-99-2-8918, F30602-00-2-0616]; US Army Research Office
(ARO) [DAAD19-01-1-0485, DAAD19-02-1-0389]; NASA High Dependability
Computing Program [NCC-2-1298]; Foundation for Science and Technology
[CMU-PT/ELE/0030/2009]; FEDER via the "Programa Operacional Factores de
Competitividade" of QREN; COMPETE [FCOMP-01-0124-FEDER-012983]; IBM
Eclipse Innovation Grant
FX This research was sponsored by DARPA under grants N66001-99-2-8918 and
F30602-00-2-0616, the US Army Research Office (ARO) under grants
DAAD19-01-1-0485 and DAAD19-02-1-0389 ("Perpetually Available and Secure
Information Systems") to Carnegie Mellon University's CyLab, the NASA
High Dependability Computing Program under cooperative agreement
NCC-2-1298, a 2004 IBM Eclipse Innovation Grant, the Foundation for
Science and Technology via project CMU-PT/ELE/0030/2009, and by FEDER
via the "Programa Operacional Factores de Competitividade" of QREN with
COMPETE reference: FCOMP-01-0124-FEDER-012983. The views and conclusions
contained in this document are those of the author and should not be
interpreted as representing the official policies, either expressed or
implied, of DARPA, the ARO, the U.S. Government, NASA, IBM, or any other
entity.
NR 62
TC 29
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U1 1
U2 4
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0164-1212
EI 1873-1228
J9 J SYST SOFTWARE
JI J. Syst. Softw.
PD DEC
PY 2012
VL 85
IS 12
SI SI
BP 2860
EP 2875
DI 10.1016/j.jss.2012.02.060
PG 16
WC Computer Science, Software Engineering; Computer Science, Theory &
Methods
SC Computer Science
GA 031VB
UT WOS:000310669500014
ER
PT J
AU Bates, SD
Bailes, M
Barsdell, BR
Bhat, NDR
Burgay, M
Burke-Spolaor, S
Champion, DJ
Coster, P
D'Amico, N
Jameson, A
Johnston, S
Keith, MJ
Kramer, M
Levin, L
Lyne, A
Milia, S
Ng, C
Nietner, C
Possenti, A
Stappers, B
Thornton, D
van Straten, W
AF Bates, S. D.
Bailes, M.
Barsdell, B. R.
Bhat, N. D. R.
Burgay, M.
Burke-Spolaor, S.
Champion, D. J.
Coster, P.
D'Amico, N.
Jameson, A.
Johnston, S.
Keith, M. J.
Kramer, M.
Levin, L.
Lyne, A.
Milia, S.
Ng, C.
Nietner, C.
Possenti, A.
Stappers, B.
Thornton, D.
van Straten, W.
TI The High Time Resolution Universe Pulsar Survey - VI. An artificial
neural network and timing of 75 pulsars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: data analysis; stars: neutron; pulsars: general
ID MILLISECOND PULSARS; RADIO TELESCOPE; NEUTRON-STARS; DISCOVERY;
SEARCHES; CANDIDATES; CATALOG; LOFAR; ARRAY
AB We present 75 pulsars discovered in the mid-latitude portion of the High Time Resolution Universe survey, 54 of which have full timing solutions. All the pulsars have spin periods greater than 100 ms, and none of those with timing solutions is in binaries. Two display particularly interesting behaviour; PSR J1054-5944 is found to be an intermittent pulsar, and PSR J1809-0119 has glitched twice since its discovery.
In the second half of the paper we discuss the development and application of an artificial neural network in the data-processing pipeline for the survey. We discuss the tests that were used to generate scores and find that our neural network was able to reject over 99 per cent of the candidates produced in the data processing, and able to blindly detect 85 per cent of pulsars. We suggest that improvements to the accuracy should be possible if further care is taken when training an artificial neural network; for example, ensuring that a representative sample of the pulsar population is used during the training process, or the use of different artificial neural networks for the detection of different types of pulsars.
C1 [Bates, S. D.; Nietner, C.; Stappers, B.; Thornton, D.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Bates, S. D.; Kramer, M.; Lyne, A.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA.
[Bailes, M.; Barsdell, B. R.; Bhat, N. D. R.; Coster, P.; Jameson, A.; Levin, L.; van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Burgay, M.; D'Amico, N.; Milia, S.; Possenti, A.] INAF Osservatorio Astron Cagliari, I-09012 Caopterra, Italy.
[Burke-Spolaor, S.] NASA Jet Prop Lab, Pasadena, CA 91106 USA.
[Champion, D. J.; Kramer, M.; Ng, C.] MPI Radioastron, D-53121 Bonn, Germany.
[Johnston, S.; Keith, M. J.; Levin, L.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Milia, S.] Univ Cagliari, Dipartimento Fis, I-09042 Monserrato, CA, Italy.
RP Bates, SD (reprint author), Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
EM sam.d.bates@gmail.com
RI Bhat, Ramesh/B-7396-2013;
OI Champion, David/0000-0003-1361-7723; Burgay, Marta/0000-0002-8265-4344;
van Straten, Willem/0000-0003-2519-7375
FU Commonwealth of Australia
FX The authors thank Cristobal Espinoza for his helpful comments and
expertise on pulsar glitches. The Parkes Observatory is part of the
Australia Telescope which is funded by the Commonwealth of Australia for
operation as a National Facility managed by CSIRO. We thank the
anonymous referee for their helpful comment.
NR 48
TC 11
Z9 12
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 DEC
PY 2012
VL 427
IS 2
BP 1052
EP 1065
DI 10.1111/j.1365-2966.2012.22042.x
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 041PK
UT WOS:000311413500016
ER
PT J
AU Carvalho, P
Rocha, G
Hobson, MP
Lasenby, A
AF Carvalho, Pedro
Rocha, Graca
Hobson, M. P.
Lasenby, A.
TI PowellSnakes II: a fast Bayesian approach to discrete object detection
in multi-frequency astronomical data sets
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: data analysis; cosmology: observations
ID EXTRAGALACTIC RADIO-SOURCES; SUNYAEV-ZELDOVICH CLUSTERS; MICROWAVE
BACKGROUND MAPS; POINT SOURCES; PLANCK; CATALOG; FILTERS; PREDICTIONS;
EXTRACTION; EFFICIENT
AB PowellSnakes (PwS) is a Bayesian algorithm for detecting compact objects embedded in a diffuse background, and was selected and successfully employed by the Planck consortium in the production of its first public deliverable: the Early Release Compact Source Catalogue (ERCSC). We present the critical foundations and main directions of further development of PwS, which extend it in terms of formal correctness and the optimal use of all the available information in a consistent unified framework, where no distinction is made between point sources (unresolved objects), Sunyaev-Zel'dovich (SZ) clusters, single-or multi-channel detection. An emphasis is placed on the necessity of a multi-frequency, multi-model detection algorithm in order to achieve optimality.
C1 [Carvalho, Pedro; Hobson, M. P.; Lasenby, A.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England.
[Rocha, Graca] CALTECH, Pasadena, CA 91125 USA.
[Rocha, Graca] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lasenby, A.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England.
RP Carvalho, P (reprint author), Univ Cambridge, Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England.
EM carvalho@mrao.cam.ac.uk; graca@caltech.edu; mph@mrao.cam.ac.uk;
a.n.lasenby@mrao.cam.ac.uk
FU Fundacao para a Ciencia e Tecnologia (FCT) [SFRH/BD/42366/2007]; NASA
Science Mission Directorate via the US Planck Project
FX PC thanks all his colleagues at the Astrophysics Group of Cavendish
laboratory and the KICC, and his fellow members of the Planck consortium
for their help in completing PwS. In particular, special thanks go to
Paulo Marques (code porting), Farhan Feroz and Philip Graff for their
insightful contributions and discussions. PC is supported by a
Portuguese fellowship (ref: SFRH/BD/42366/2007) from the Fundacao para a
Ciencia e Tecnologia (FCT).; GR gratefully acknowledges support by the
NASA Science Mission Directorate via the US Planck Project. The research
described in this paper was partially carried out at the Jet propulsion
Laboratory, California Institute of Technology, under a contract with
NASA.
NR 50
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U1 0
U2 5
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 DEC
PY 2012
VL 427
IS 2
BP 1384
EP 1400
DI 10.1111/j.1365-2966.2012.22033.x
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 041PK
UT WOS:000311413500041
ER
PT J
AU Camera, S
Santos, MG
Bacon, DJ
Jarvis, MJ
McAlpine, K
Norris, RP
Raccanelli, A
Rottgering, H
AF Camera, Stefano
Santos, Mario G.
Bacon, David J.
Jarvis, Matt J.
McAlpine, Kim
Norris, Ray P.
Raccanelli, Alvise
Roettgering, Huub
TI Impact of redshift information on cosmological applications with
next-generation radio surveys
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE cosmological parameters; cosmology: observations; large-scale structure
of universe; radio continuum: galaxies
ID ESTIMATING PHOTOMETRIC REDSHIFTS; ARTIFICIAL NEURAL-NETWORKS; VLA SKY
SURVEY; DEEP FIELD; TELESCOPE; GALAXIES; COSMOS; SIMULATION; UNIVERSE;
CATALOG
AB In this paper, we explore how the forthcoming generation of large-scale radio continuum surveys, with the inclusion of some degree of redshift information, can constrain cosmological parameters. By cross-matching these radio surveys with shallow optical to near-infrared surveys, we can essentially separate the source distribution into a low- and a high-redshift sample, thus providing a constraint on the evolution of cosmological parameters such as those related to dark energy. We examine two radio surveys, the Evolutionary Map of the Universe (EMU) and the Westerbork Observations of the Deep APERTIF Northern sky (WODAN). A crucial advantage is their combined potential to provide a deep, full-sky survey. The surveys used for the cross-identifications are SkyMapper and Sloan Digital Sky Survey, for the southern and northern skies, respectively. We concentrate on the galaxy clustering angular power spectrum as our benchmark observable, and find that the possibility of including such low-redshift information yields major improvements in the determination of cosmological parameters. With this approach, and provided a good knowledge of the galaxy bias evolution, we are able to put strict constraints on the dark energy parameters, i.e. w0 = -0.9 +/- 0.041 and wa = -0.24 +/- 0.13, with Type Ia supernovae and cosmic microwave background priors (with a one-parameter bias in this case); this corresponds to a Figure of Merit (FoM) >600, which is twice better than what is obtained by using only the cross-identified sources and greater than four time better than the case without any redshift information at all.
C1 [Camera, Stefano; Santos, Mario G.] Univ Tecn Lisboa, CENTRA, Inst Super Tecn, P-1049001 Lisbon, Portugal.
[Bacon, David J.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth P01 3FX, Hants, England.
[Jarvis, Matt J.] Univ Hertfordshire, STRI, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Jarvis, Matt J.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa.
[McAlpine, Kim] Rhodes Univ, Dept Phys & Elect, ZA-6139 Grahamstown, South Africa.
[Norris, Ray P.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Raccanelli, Alvise] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Raccanelli, Alvise] CALTECH, Pasadena, CA 91125 USA.
[Roettgering, Huub] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Camera, S (reprint author), Univ Tecn Lisboa, CENTRA, Inst Super Tecn, Av Rovisco Pais 1, P-1049001 Lisbon, Portugal.
EM stefano.camera@ist.utl.pt; mgrsantos@ist.utl.pt; david.bacon@port.ac.uk
RI Camera, Stefano/N-2456-2013; Norris, Ray/A-1316-2008; Santos,
Mario/F-2484-2011;
OI Camera, Stefano/0000-0003-3399-3574; Norris, Ray/0000-0002-4597-1906;
Santos, Mario/0000-0003-3892-3073; Raccanelli,
Alvise/0000-0001-6726-0438
FU FCT-Portugal [PTDC/FIS/100170/2008, SFRH/BPD/80274/2011]
FX We thank the referee for a careful reading of our manuscript and very
insightful comments. SC and MGS acknowledge support from FCT-Portugal
under grant PTDC/FIS/100170/2008. SC's work is funded by FCT-Portugal
under Post-Doctoral Grant SFRH/BPD/80274/2011. Part of the research
described in this paper was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. The authors would
also like to thank Gong-Bo Zhao for his friendly and gratuitous
contribution.
NR 50
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Z9 10
U1 0
U2 5
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD DEC
PY 2012
VL 427
IS 3
BP 2079
EP 2088
DI 10.1111/j.1365-2966.2012.22073.x
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 041PX
UT WOS:000311414800018
ER
PT J
AU Lakew, B
Aslam, S
Brasunas, J
Cao, N
Costen, N
La, A
Nguyen, L
Stevenson, T
Waczynski, A
AF Lakew, B.
Aslam, S.
Brasunas, J.
Cao, N.
Costen, N.
La, A.
Nguyen, L.
Stevenson, T.
Waczynski, A.
TI MgB2 thin-film bolometer for applications in far-infrared instruments on
future planetary missions
SO PHYSICA C-SUPERCONDUCTIVITY AND ITS APPLICATIONS
LA English
DT Article
DE MgB2 thin-film; Bolometer; Thermal detector; D*; NEP
ID HIGH-T-C; SILICON-NITRIDE FILMS; SUPERCONDUCTING BOLOMETER; MEMBRANE;
PERFORMANCE; FABRICATION; RADIATION; TRANSPORT; SAPPHIRE; DETECTOR
AB A SiN membrane based MgB2 thin-film bolometer, with a non-optimized absorber, has been fabricated that shows an electrical noise equivalent power of 2.56 x 10 (13) W/root Hz operating at 30 Hz and a responsivity of 702 kV/W. It is predicted that with the inclusion of a gold black absorber that an optical specific detectivity of 8.3 x 10(10) cm/root Hz/W at an operational frequency of 10 Hz, can be realized for integration into future planetary exploration instrumentation where high sensitivity is required in the 17-250 mu m spectral wavelength range. (C) 2012 Published by Elsevier B.V.
C1 [Lakew, B.; Aslam, S.; Brasunas, J.] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA.
[Cao, N.; Costen, N.; La, A.; Nguyen, L.; Stevenson, T.; Waczynski, A.] NASA, Goddard Space Flight Ctr, Detector Syst Branch, Greenbelt, MD 20771 USA.
[Cao, N.; Costen, N.] MEI Technol Inc, Houston, TX 77058 USA.
RP Aslam, S (reprint author), NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Code 693, Greenbelt, MD 20771 USA.
EM shahid.aslam-1@nasa.gov
RI brasunas, john/I-2798-2013; Aslam, Shahid/D-1099-2012
FU NASA GSFC Internal Research and Development (IRAD) program; NASA HQ
Planetary Instrument Definition and Development (PIDD) program
FX The authors wish to thank Dr. Simon Bandler (University of Maryland) for
enlightening conversations regarding ac impedance measurements on
superconducting films. The NASA GSFC Internal Research and Development
(IRAD) and the NASA HQ Planetary Instrument Definition and Development
(PIDD) programs supported this work.
NR 42
TC 0
Z9 0
U1 1
U2 16
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0921-4534
J9 PHYSICA C
JI Physica C
PD DEC
PY 2012
VL 483
BP 119
EP 126
DI 10.1016/j.physc.2012.08.007
PG 8
WC Physics, Applied
SC Physics
GA 040UC
UT WOS:000311348800026
ER
PT J
AU Aliu, E
Archambault, S
Arlen, T
Aune, T
Beilicke, M
Benbow, W
Bouvier, A
Buckley, JH
Bugaev, V
Byrum, K
Cesarini, A
Ciupik, L
Collins-Hughes, E
Connolly, MP
Cui, W
Dickherber, R
Duke, C
Dumm, J
Falcone, A
Federici, S
Feng, Q
Finley, JP
Finnegan, G
Fortson, L
Furniss, A
Galante, N
Gall, D
Gillanders, GH
Godambe, S
Griffin, S
Grube, J
Gyuk, G
Hanna, D
Holder, J
Huan, H
Hughes, G
Humensky, TB
Kaaret, P
Karlsson, N
Khassen, Y
Kieda, D
Krawczynski, H
Krennrich, F
Lang, MJ
LeBohec, S
Lee, K
Lyutikov, M
Madhavan, AS
Maier, G
Majumdar, P
McArthur, S
McCann, A
Moriarty, P
Mukherjee, R
Nelson, T
de Bhroithe, AO
Ong, RA
Orr, M
Otte, AN
Park, N
Perkins, JS
Pohl, M
Prokoph, H
Quinn, J
Ragan, K
Reyes, LC
Reynolds, PT
Roache, E
Saxon, DB
Schroedter, M
Sembroski, GH
Senturk, GD
Smith, AW
Staszak, D
Telezhinsky, I
Tesic, G
Theiling, M
Thibadeau, S
Tsurusaki, K
Varlotta, A
Vincent, S
Vivier, M
Wagner, RG
Wakely, SP
Weekes, TC
Weinstein, A
Welsing, R
Williams, DA
Zitzer, B
Kondratiev, V
AF Aliu, E.
Archambault, S.
Arlen, T.
Aune, T.
Beilicke, M.
Benbow, W.
Bouvier, A.
Buckley, J. H.
Bugaev, V.
Byrum, K.
Cesarini, A.
Ciupik, L.
Collins-Hughes, E.
Connolly, M. P.
Cui, W.
Dickherber, R.
Duke, C.
Dumm, J.
Falcone, A.
Federici, S.
Feng, Q.
Finley, J. P.
Finnegan, G.
Fortson, L.
Furniss, A.
Galante, N.
Gall, D.
Gillanders, G. H.
Godambe, S.
Griffin, S.
Grube, J.
Gyuk, G.
Hanna, D.
Holder, J.
Huan, H.
Hughes, G.
Humensky, T. B.
Kaaret, P.
Karlsson, N.
Khassen, Y.
Kieda, D.
Krawczynski, H.
Krennrich, F.
Lang, M. J.
LeBohec, S.
Lee, K.
Lyutikov, M.
Madhavan, A. S.
Maier, G.
Majumdar, P.
McArthur, S.
McCann, A.
Moriarty, P.
Mukherjee, R.
Nelson, T.
de Bhroithe, A. O'Faolain
Ong, R. A.
Orr, M.
Otte, A. N.
Park, N.
Perkins, J. S.
Pohl, M.
Prokoph, H.
Quinn, J.
Ragan, K.
Reyes, L. C.
Reynolds, P. T.
Roache, E.
Saxon, D. B.
Schroedter, M.
Sembroski, G. H.
Sentuerk, G. D.
Smith, A. W.
Staszak, D.
Telezhinsky, I.
Tesic, G.
Theiling, M.
Thibadeau, S.
Tsurusaki, K.
Varlotta, A.
Vincent, S.
Vivier, M.
Wagner, R. G.
Wakely, S. P.
Weekes, T. C.
Weinstein, A.
Welsing, R.
Williams, D. A.
Zitzer, B.
Kondratiev, V.
TI SEARCH FOR A CORRELATION BETWEEN VERY-HIGH-ENERGY GAMMA RAYS AND GIANT
RADIO PULSES IN THE CRAB PULSAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE rays: stars; pulsars: individual: B0531+21
ID EMISSION; TELESCOPES; UNIVERSE; PHOTONS; GEMINGA; NEBULA; RANGE; MODEL
AB We present the results of a joint observational campaign between the Green Bank radio telescope and the VERITAS gamma-ray telescope, which searched for a correlation between the emission of very-high-energy (VHE) gamma rays (E-gamma > 150 GeV) and giant radio pulses (GRPs) from the Crab pulsar at 8.9 GHz. A total of 15,366 GRPs were recorded during 11.6 hr of simultaneous observations, which were made across four nights in 2008 December and in 2009 November and December. We searched for an enhancement of the pulsed gamma-ray emission within time windows placed around the arrival time of the GRP events. In total, eight different time windows with durations ranging from 0.033 ms to 72 s were positioned at three different locations relative to the GRP to search for enhanced gamma-ray emission which lagged, led, or was concurrent with, the GRP event. Furthermore, we performed separate searches on main pulse GRPs and interpulse GRPs and on the most energetic GRPs in our data sample. No significant enhancement of pulsed VHE emission was found in any of the preformed searches. We set upper limits of 5-10 times the average VHE flux of the Crab pulsar on the flux simultaneous with interpulse GRPs on single-rotation-period timescales. On similar to 8 s timescales around interpulse GRPs, we set an upper limit of 2-3 times the average VHE flux. Within the framework of recent models for pulsed VHE emission from the Crab pulsar, the expected VHE-GRP emission correlations are below the derived limits.
C1 [Aliu, E.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Staszak, D.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Arlen, T.; Majumdar, P.; Ong, R. A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Aune, T.; Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Aune, T.; Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; Lee, K.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Benbow, W.; Galante, N.; Roache, E.; Schroedter, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Byrum, K.; Wagner, R. G.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cesarini, A.; Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Collins-Hughes, E.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Cui, W.; Feng, Q.; Finley, J. P.; Lyutikov, M.; Sembroski, G. H.; Theiling, M.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA.
[Dumm, J.; Fortson, L.; Karlsson, N.; Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Federici, S.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.; Welsing, R.] DESY, D-15738 Zeuthen, Germany.
[Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Finnegan, G.; Godambe, S.; Kieda, D.; LeBohec, S.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Gall, D.; Kaaret, P.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Huan, H.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Humensky, T. B.; Sentuerk, G. D.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Otte, A. N.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Otte, A. N.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA.
[Perkins, J. S.] NASA, GSFC, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Perkins, J. S.] Univ Maryland, Baltimore, MD 21250 USA.
[Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
[Kondratiev, V.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Kondratiev, V.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia.
RP Aliu, E (reprint author), Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
EM mccann@kicp.uchicago.edu; nepomuk.otte@gmail.com;
schroedter@veritas.sao.arizona.edu
RI Khassen, Yerbol/I-3806-2015; Kondratiev, Vladislav/N-1105-2015;
OI Cesarini, Andrea/0000-0002-8611-8610; Khassen,
Yerbol/0000-0002-7296-3100; Lang, Mark/0000-0003-4641-4201; Kondratiev,
Vladislav/0000-0001-8864-7471; Cui, Wei/0000-0002-6324-5772
FU U.S. Department of Energy Office of Science; U.S. National Science
Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation
Ireland [SFI 10/RFP/AST2748]; STFC in the UK
FX This research is supported by grants from the U.S. Department of Energy
Office of Science, the U.S. National Science Foundation, and the
Smithsonian Institution, by NSERC in Canada, by Science Foundation
Ireland (SFI 10/RFP/AST2748), and by STFC in the UK. We acknowledge the
excellent work of the technical support staff at the Fred Lawrence
Whipple Observatory and at the collaborating institutions in the
construction and operation of the instrument. The National Radio
Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc.
NR 35
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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 DEC 1
PY 2012
VL 760
IS 2
AR 136
DI 10.1088/0004-637X/760/2/136
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 039BE
UT WOS:000311217000040
ER
PT J
AU Araujo, D
Bischoff, C
Brizius, A
Buder, I
Chinone, Y
Cleary, K
Dumoulin, RN
Kusaka, A
Monsalve, R
Kaess, S
Newburgh, LB
Reeves, R
Wehus, IK
Zwart, JTL
Bronfman, L
Bustos, R
Church, SE
Dickinson, C
Eriksen, HK
Gaier, T
Gundersen, JO
Hasegawa, M
Hazumi, M
Huffenberger, KM
Ishidoshiro, K
Jones, ME
Kangaslahti, P
Kapner, DJ
Kubik, D
Lawrence, CR
Limon, M
McMahon, JJ
Miller, AD
Nagai, M
Nguyen, H
Nixon, G
Pearson, TJ
Piccirillo, L
Radford, SJE
Readhead, ACS
Richards, JL
Samtleben, D
Seiffert, M
Shepherd, MC
Smith, KM
Staggs, ST
Tajima, O
Thompson, KL
Vanderlinde, K
Williamson, R
AF Araujo, D.
Bischoff, C.
Brizius, A.
Buder, I.
Chinone, Y.
Cleary, K.
Dumoulin, R. N.
Kusaka, A.
Monsalve, R.
Kaess, S.
Newburgh, L. B.
Reeves, R.
Wehus, I. K.
Zwart, J. T. L.
Bronfman, L.
Bustos, R.
Church, S. E.
Dickinson, C.
Eriksen, H. K.
Gaier, T.
Gundersen, J. O.
Hasegawa, M.
Hazumi, M.
Huffenberger, K. M.
Ishidoshiro, K.
Jones, M. E.
Kangaslahti, P.
Kapner, D. J.
Kubik, D.
Lawrence, C. R.
Limon, M.
McMahon, J. J.
Miller, A. D.
Nagai, M.
Nguyen, H.
Nixon, G.
Pearson, T. J.
Piccirillo, L.
Radford, S. J. E.
Readhead, A. C. S.
Richards, J. L.
Samtleben, D.
Seiffert, M.
Shepherd, M. C.
Smith, K. M.
Staggs, S. T.
Tajima, O.
Thompson, K. L.
Vanderlinde, K.
Williamson, R.
CA QUIET Collaboration
TI SECOND SEASON QUIET OBSERVATIONS: MEASUREMENTS OF THE COSMIC MICROWAVE
BACKGROUND POLARIZATION POWER SPECTRUM AT 95 GHz
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; gravitational
waves; inflation; polarization
ID CMB POLARIZATION; COSMOLOGICAL PARAMETERS; GRAVITY-WAVES; PROBE;
CONSTRAINTS; TEMPERATURE; TELESCOPE; IMAGER
AB The Q/U Imaging ExperimenT (QUIET) has observed the cosmic microwave background (CMB) at 43 and 95 GHz. The 43 GHz results have been published in a previous paper, and here we report the measurement of CMB polarization power spectra using the 95 GHz data. This data set comprises 5337 hr of observations recorded by an array of 84 polarized coherent receivers with a total array sensitivity of 87 mu K root s. Four low-foreground fields were observed, covering a total of similar to 1000 deg(2) with an effective angular resolution of 12.'8, allowing for constraints on primordial gravitational waves and high signal-to-noise measurements of the E-modes across three acoustic peaks. The data reduction was performed using two independent analysis pipelines, one based on a pseudo-C-l (PCL) cross-correlation approach, and the other on a maximum-likelihood (ML) approach. All data selection criteria and filters were modified until a predefined set of null tests had been satisfied before inspecting any non-null power spectrum. The results derived by the two pipelines are in good agreement. We characterize the EE, EB, and BB power spectra between l = 25 and 975 and find that the EE spectrum is consistent with Lambda CDM, while the BB power spectrum is consistent with zero. Based on these measurements, we constrain the tensor-to-scalar ratio to r = 1.1(-0.8)(+0.9) (r < 2.8 at 95% C. L.) as derived by the ML pipeline, and r = 1.2(-0.8)(+0.9) (r < 2.7 at 95% C. L.) as derived by the PCL pipeline. In one of the fields, we find a correlation with the dust component of the Planck Sky Model, though the corresponding excess power is small compared to statistical errors. Finally, we derive limits on all known systematic errors, and demonstrate that these correspond to a tensor-to-scalar ratio smaller than r = 0.01, the lowest level yet reported in the literature.
C1 [Araujo, D.; Dumoulin, R. N.; Newburgh, L. B.; Zwart, J. T. L.; Limon, M.; Miller, A. D.; Williamson, R.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Dumoulin, R. N.; Newburgh, L. B.; Zwart, J. T. L.; Limon, M.; Miller, A. D.; Williamson, R.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Bischoff, C.; Brizius, A.; Buder, I.; Kusaka, A.; Kapner, D. J.; Smith, K. M.; Tajima, O.; Vanderlinde, K.; Williamson, R.] Univ Chicago, Dept Phys, Kavli Inst Cosmol Phys, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Bischoff, C.; Buder, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brizius, A.; Samtleben, D.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Chinone, Y.; Hasegawa, M.; Hazumi, M.; Ishidoshiro, K.; Nagai, M.; Tajima, O.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki 3050801, Japan.
[Chinone, Y.] Tohoku Univ, Grad Sch Sci, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
[Cleary, K.; Reeves, R.; Pearson, T. J.; Radford, S. J. E.; Readhead, A. C. S.; Richards, J. L.; Shepherd, M. C.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Kusaka, A.; Newburgh, L. B.; Nixon, G.; Smith, K. M.; Staggs, S. T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
[Monsalve, R.; Bustos, R.; Gundersen, J. O.; Huffenberger, K. M.] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA.
[Monsalve, R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Kaess, S.; Eriksen, H. K.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway.
[Wehus, I. K.; Jones, M. E.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Wehus, I. K.] Univ Oslo, Dept Phys, NO-0316 Oslo, Norway.
[Zwart, J. T. L.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa.
[Bronfman, L.; Bustos, R.] Univ Chile, Dept Astron, Santiago, Chile.
[Bustos, R.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Church, S. E.; Thompson, K. L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Church, S. E.; Thompson, K. L.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Dickinson, C.; Piccirillo, L.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Eriksen, H. K.] Univ Oslo, Ctr Math Applicat, NO-0316 Oslo, Norway.
[Gaier, T.; Kangaslahti, P.; Lawrence, C. R.; Seiffert, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kapner, D. J.] Micro Encoder Inc, Kirkland, WA 98034 USA.
[Kubik, D.; Nguyen, H.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Nixon, G.] Tradeworx Inc, Red Bank, NJ 07701 USA.
[Samtleben, D.] Nikhef, Amsterdam, Netherlands.
[Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
RP Araujo, D (reprint author), Columbia Univ, Dept Phys, 538 W 120th St, New York, NY 10027 USA.
EM ibuder@uchicago.edu
RI Bronfman, Leonardo/H-9544-2013; Reeves, Rodrigo/H-2812-2014; Williamson,
Ross/H-1734-2015; Pearson, Timothy/N-2376-2015;
OI Huffenberger, Kevin/0000-0001-7109-0099; Bronfman,
Leonardo/0000-0002-9574-8454; Bischoff, Colin/0000-0001-9185-6514;
Reeves, Rodrigo/0000-0001-5704-271X; Williamson,
Ross/0000-0002-6945-2975; Pearson, Timothy/0000-0001-5213-6231; Limon,
Michele/0000-0002-5900-2698; radford, simon/0000-0001-9113-1660; Zwart,
Jonathan/0000-0002-4967-946X
FU NSF [AST-0506648, PHY-0355328, AST-0448909, PHY-0551142, PHY-0855887,
AST-1010016]; KAKENHI [20244041, 20740158, 21111002]; PRODEX [C90284];
KIPAC Enterprise grant; Strategic Alliance for the Implementation of New
Technologies (SAINT); Fermilab; Kavli Institute for Cosmological
Physics; University of Chicago; Office of Science of the U.S. Department
of Energy [DE-AC02-05CH11231]; JPL RTD program; STFC; ERC IRG grant
under FP7; CONICYT [Basal PFB-06]; ALMA-Conicyt [31070015]; Sloan
foundation; ERC
FX Support for the QUIET instrument and operation comes through the NSF
cooperative agreement AST-0506648. Support was also provided by NSF
awards PHY-0355328, AST-0448909, PHY-0551142, PHY-0855887, and
AST-1010016; KAKENHI 20244041, 20740158, and 21111002; PRODEX C90284; a
KIPAC Enterprise grant; and by the Strategic Alliance for the
Implementation of New Technologies (SAINT).; Some work was performed on
the Joint Fermilab-KICP Supercomputing Cluster, supported by grants from
Fermilab, the Kavli Institute for Cosmological Physics, and the
University of Chicago. Some work was performed on the Titan Cluster,
owned and maintained by the University of Oslo and NOTUR (the Norwegian
High Performance Computing Consortium), and on the Central Computing
System, owned and operated by the Computing Research Center at KEK. 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 No. DE-AC02-05CH11231. Portions
of this work were performed at the Jet Propulsion Laboratory (JPL) and
California Institute of Technology, operating under a contract with the
National Aeronautics and Space Administration. The Q-band modules were
developed using funding from the JPL R&TD program. We acknowledge the
Northrop Grumman Corporation for collaboration in the development and
fabrication of HEMT-based cryogenic temperature-compatible MMICs. We
acknowledge the use of the Planck Sky Model, developed by the Component
Separation Working Group (WG2) of the Planck Collaboration. Some of the
results in this paper have been derived using the HEALPix (Gorski et al.
2005) software and analysis package.; C.D. acknowledges an STFC Advanced
Fellowship and an ERC IRG grant under FP7. R.B. acknowledges support
from CONICYT project Basal PFB-06 and ALMA-Conicyt 31070015. A.D.M.
acknowledges a Sloan foundation fellowship. H.K.E. acknowledges an ERC
Starting Grant under FP7.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2012
VL 760
IS 2
AR 145
DI 10.1088/0004-637X/760/2/145
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 039BE
UT WOS:000311217000049
ER
PT J
AU Bampasidis, G
Coustenis, A
Achterberg, RK
Vinatier, S
Lavvas, P
Nixon, CA
Jennings, DE
Teanby, NA
Flasar, FM
Carlson, RC
Moussas, X
Preka-Papadema, P
Romani, PN
Guandique, EA
Stamogiorgos, S
AF Bampasidis, Georgios
Coustenis, A.
Achterberg, R. K.
Vinatier, S.
Lavvas, P.
Nixon, C. A.
Jennings, D. E.
Teanby, N. A.
Flasar, F. M.
Carlson, R. C.
Moussas, X.
Preka-Papadema, P.
Romani, P. N.
Guandique, E. A.
Stamogiorgos, S.
TI THERMAL AND CHEMICAL STRUCTURE VARIATIONS IN TITAN'S STRATOSPHERE DURING
THE CASSINI MISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: planetary systems; planets and satellites: atmospheres;
planets and satellites: composition; planets and satellites: individual
(Titan); radiation mechanisms: thermal; radiative transfer
ID COMPOSITE INFRARED SPECTROMETER; ATMOSPHERIC TEMPERATURES; SPECTROSCOPIC
DATABASE; LATITUDINAL VARIATIONS; ISOTOPIC-RATIOS; HYDROCARBONS;
SPECTRA; CIRS; HC3N; PROFILES
AB We have developed a line-by-line Atmospheric Radiative Transfer for Titan code that includes the most recent laboratory spectroscopic data and haze descriptions relative to Titan's stratosphere. We use this code to model Cassini Composite Infrared Spectrometer data taken during the numerous Titan flybys from 2006 to 2012 at surface-intercepting geometry in the 600-1500 cm(-1) range for latitudes from 50 degrees S to 50 degrees N. We report variations in temperature and chemical composition in the stratosphere during the Cassini mission, before and after the Northern Spring Equinox (NSE). We find indication for a weakening of the temperature gradient with warming of the stratosphere and cooling of the lower mesosphere. In addition, we infer precise concentrations for the trace gases and their main isotopologues and find that the chemical composition in Titan's stratosphere varies significantly with latitude during the 6 years investigated here, with increased mixing ratios toward the northern latitudes. In particular, we monitor and quantify the amplitude of a maximum enhancement of several gases observed at northern latitudes up to 50 degrees N around mid-2009, at the time of the NSE. We find that this rise is followed by a rapid decrease in chemical inventory in 2010 probably due to a weakening north polar vortex with reduced lateral mixing across the vortex boundary.
C1 [Bampasidis, Georgios; Coustenis, A.; Vinatier, S.] Univ Paris Diderot, UPMC Univ Paris 06, CNRS, LESIA,Observ Paris, F-92195 Meudon, France.
[Bampasidis, Georgios; Moussas, X.; Preka-Papadema, P.; Stamogiorgos, S.] Univ Athens, Fac Phys, GR-15783 Athens, Greece.
[Achterberg, R. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Lavvas, P.] Univ Reims, GSMA, F-51687 Reims 2, France.
[Nixon, C. A.; Jennings, D. E.; Flasar, F. M.; Carlson, R. C.; Romani, P. N.; Guandique, E. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Teanby, N. A.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England.
[Carlson, R. C.] Catholic Univ Amer, IACS, Washington, DC 20064 USA.
[Guandique, E. A.] Adnet Syst Inc, Rockville, MD USA.
RP Bampasidis, G (reprint author), Univ Paris Diderot, UPMC Univ Paris 06, CNRS, LESIA,Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France.
EM gbabasid@phys.uoa.gr
RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012;
OI Nixon, Conor/0000-0001-9540-9121; Teanby, Nicholas/0000-0003-3108-5775
FU CNES Cassini program
FX We thank Nicolas Gorius, Marcia Segura, and Florence Henry for help with
the data acquisition and processing during this project. We also
acknowledge support from the CNES Cassini program.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2012
VL 760
IS 2
AR 144
DI 10.1088/0004-637X/760/2/144
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 039BE
UT WOS:000311217000048
ER
PT J
AU Cheung, E
Faber, SM
Koo, DC
Dutton, AA
Simard, L
McGrath, EJ
Huang, JS
Bell, EF
Dekel, A
Fang, JJ
Salim, S
Barro, G
Bundy, K
Coil, AL
Cooper, MC
Conselice, CJ
Davis, M
Dominguez, A
Kassin, SA
Kocevski, DD
Koekemoer, AM
Lin, LW
Lotz, JM
Newman, JA
Phillips, AC
Rosario, DJ
Weiner, BJ
Willmer, CNA
AF Cheung, Edmond
Faber, S. M.
Koo, David C.
Dutton, Aaron A.
Simard, Luc
McGrath, Elizabeth J.
Huang, J. -S.
Bell, Eric F.
Dekel, Avishai
Fang, Jerome J.
Salim, Samir
Barro, G.
Bundy, K.
Coil, A. L.
Cooper, Michael C.
Conselice, C. J.
Davis, M.
Dominguez, A.
Kassin, Susan A.
Kocevski, Dale D.
Koekemoer, Anton M.
Lin, Lihwai
Lotz, Jennifer M.
Newman, J. A.
Phillips, Andrew C.
Rosario, D. J.
Weiner, Benjamin J.
Willmer, C. N. A.
TI THE DEPENDENCE OF QUENCHING UPON THE INNER STRUCTURE OF GALAXIES AT 0.5
<= z < 0.8 IN THE DEEP2/AEGIS SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: bulges; galaxies: evolution; galaxies: formation; galaxies:
fundamental parameters; galaxies: structure
ID DEEP GROTH STRIP; ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; DIGITAL
SKY SURVEY; COLOR-MAGNITUDE DIAGRAM; HIGH-REDSHIFT GALAXIES; CENTRAL
BLACK-HOLES; ARECIBO SDSS SURVEY; MASSIVE GALAXIES; STELLAR MASS
AB The shutdown of star formation in galaxies is generally termed "quenching." Quenching may occur through a variety of processes, e.g., active galactic nucleus (AGN) feedback, stellar feedback, or the shock heating of gas in the dark matter halo. However, which mechanism(s) is, in fact, responsible for quenching is still in question. This paper addresses quenching by searching for traces of possible quenching processes through their effects on galaxy structural parameters such as stellar mass (M-*), M-*/r(e), surface stellar mass density (similar to M-*/r(e)(2)), and Sersic index (n). We analyze the rest-frame U - B color correlations versus these structural parameters using a sample of galaxies in the redshift range 0.5 <= z < 0.8 from the DEEP2/AEGIS survey. In addition to global radii, stellar masses, and Sersic parameters, we also use "bulge" and "disk" photometric measurements from GIM2D fits to HST/ACS V and I images. We assess the tightness of the color relationships by measuring their "overlap regions," defined as the area in color-parameter space in which red and blue galaxies overlap; the parameter that minimizes these overlap regions is considered to be the most effective color discriminator. We find that Sersic index (n) has the smallest overlap region among all tested parameters and resembles a step function with a threshold value of n = 2.3. There exists, however, a significant population of outliers with blue colors yet high n values that seem to contradict this behavior; they make up approximate to 40% of n > 2.3 galaxies. We hypothesize that their Sersic values may be distorted by bursts of star formation, AGNs, and/or poor fits, leading us to consider central surface stellar mass density, Sigma*(1) (kpc), as an alternative to Sersic index. Not only does Sigma*(1) (kpc) correct the outliers, but it also forms a tight relationship with color, suggesting that the innermost structure of galaxies is most physically linked with quenching. Furthermore, at z similar to 0.65, the majority of the blue cloud galaxies cannot simply fade onto the red sequence since their GIM2D bulge masses are only half as large on average as the bulge masses of similar red sequence galaxies, thus demonstrating that stellar mass must absolutely increase at the centers of galaxies as they quench. We discuss a two-stage model for quenching in which galaxy star formation rates are controlled by their dark halos while they are still in the blue cloud and a second quenching process sets in later, associated with the central stellar mass buildup. The mass buildup is naturally explained by any non-axisymmetric features in the potential, such as those induced by mergers and/or disk instabilities. However, the identity of the second quenching agent is still unknown. We have placed our data catalog online.
C1 [Cheung, Edmond; Faber, S. M.; Koo, David C.; McGrath, Elizabeth J.; Fang, Jerome J.; Barro, G.; Kocevski, Dale D.; Phillips, Andrew C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Faber, S. M.; Koo, David C.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Dutton, Aaron A.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada.
[Simard, Luc] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Huang, J. -S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
[Salim, Samir; Lotz, Jennifer M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Bundy, K.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778582, Japan.
[Coil, A. L.] Univ Calif San Diego, Ctr Astrophys & Space Sci, Dept Phys, San Diego, CA 92093 USA.
[Cooper, Michael C.] Univ Calif Irvine, Ctr Galaxy Evolut, Dept Phys & Astron, Irvine, CA 92697 USA.
[Conselice, C. J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Davis, M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Dominguez, A.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Kassin, Susan A.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Lin, Lihwai] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Newman, J. A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Rosario, D. J.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Weiner, Benjamin J.; Willmer, C. N. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Cheung, E (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA.
EM ec2250@gmail.com
RI Conselice, Christopher/B-4348-2013;
OI Conselice, Christopher/0000-0003-1949-7638; Cheung,
Edmond/0000-0001-8546-1428; Koekemoer, Anton/0000-0002-6610-2048; Bell,
Eric/0000-0002-5564-9873
FU National Science Foundation [AST 95-29098, 00-711098, 05-07483,
08-08133, AST 00-71048, 05-07428, 08-07630]; NASA [HST-AR-01947]
FX The DEEP2 survey was initiated under the auspices of the NSF Center for
Particle Astrophysics. Major grant support was provided by National
Science Foundation grants AST 95-29098, 00-711098, 05-07483, and
08-08133 to UCSC and AST 00-71048, 05-07428, and 08-07630 to UCB. The
DEEP2 survey has been made possible through the dedicated efforts of the
DEIMOS instrument team at UC Santa Cruz and support of the staff at Keck
Observatory. The HST ACS mosaic in EGS was constructed by Anton
Koekemoer and Jennifer Lotz and was funded by grant HST-AR-01947 from
NASA. Finally, we recognize and acknowledge the highly significant
cultural role and reverence that the summit of Mauna Kea has always had
within the indigenous Hawaiian community; it has been a privilege to be
given the opportunity to conduct observations from this mountain.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2012
VL 760
IS 2
AR 131
DI 10.1088/0004-637X/760/2/131
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 039BE
UT WOS:000311217000035
ER
PT J
AU Dong, RB
Hashimoto, J
Rafikov, R
Zhu, ZH
Whitney, B
Kudo, T
Muto, T
Brandt, T
McClure, MK
Wisniewski, J
Abe, L
Brandner, W
Carson, J
Egner, S
Feldt, M
Goto, M
Grady, C
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, S
Henning, T
Hodapp, KW
Ishii, M
Iye, M
Janson, M
Kandori, R
Knapp, GR
Kusakabe, N
Kuzuhara, M
Kwon, J
Matsuo, T
McElwain, M
Miyama, S
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, TS
Serabyn, E
Suto, H
Suzuki, R
Takami, M
Takato, N
Terada, H
Thalmann, C
Tomono, D
Turner, E
Watanabe, M
Yamada, T
Takami, H
Usuda, T
Tamura, M
AF Dong, Ruobing
Hashimoto, Jun
Rafikov, Roman
Zhu, Zhaohuan
Whitney, Barbara
Kudo, Tomoyuki
Muto, Takayuki
Brandt, Timothy
McClure, Melissa K.
Wisniewski, John
Abe, L.
Brandner, W.
Carson, J.
Egner, S.
Feldt, M.
Goto, M.
Grady, C.
Guyon, O.
Hayano, Y.
Hayashi, M.
Hayashi, S.
Henning, T.
Hodapp, K. W.
Ishii, M.
Iye, M.
Janson, M.
Kandori, R.
Knapp, G. R.
Kusakabe, N.
Kuzuhara, M.
Kwon, J.
Matsuo, T.
McElwain, M.
Miyama, S.
Morino, J. -I.
Moro-Martin, A.
Nishimura, T.
Pyo, T. -S.
Serabyn, E.
Suto, H.
Suzuki, R.
Takami, M.
Takato, N.
Terada, H.
Thalmann, C.
Tomono, D.
Turner, E.
Watanabe, M.
Yamada, T.
Takami, H.
Usuda, T.
Tamura, M.
TI THE STRUCTURE OF PRE-TRANSITIONAL PROTOPLANETARY DISKS. I. RADIATIVE
TRANSFER MODELING OF THE DISK plus CAVITY IN THE PDS 70 SYSTEM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; protoplanetary disks; radiative transfer; stars:
individual (PDS 70); stars: pre-main sequence
ID T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; YOUNG STELLAR OBJECTS;
MAIN-SEQUENCE STARS; HERBIG AE/BE STARS; TRANSITIONAL DISKS; GG TAURI;
PROTOSTELLAR ENVELOPES; IMAGING POLARIMETRY; SIZE DISTRIBUTION
AB Through detailed radiative transfer modeling, we present a disk+cavity model to simultaneously explain both the spectral energy distribution (SED) and SubaruH-band polarized light imaging for the pre-transitional protoplanetary disk PDS 70. In particular, we are able to match not only the radial dependence but also the absolute scale of the surface brightness of the scattered light. Our disk model has a cavity 65AU in radius, which is heavily depleted of sub-micron-sized dust grains, and a small residual inner disk that produces a weak but still optically thick near-IR excess in the SED. To explain the contrast of the cavity's edge in the Subaru image, a factor of similar to 1000 depletion for the sub-micron-sized dust inside the cavity is required. The total dust mass of the disk may be on the order of 10(-4) M-circle dot, only weakly constrained due to the lack of long-wavelength observations and the uncertainties in the dust model. The scale height of the sub-micron-sized dust is similar to 6AU at the cavity edge, and the cavity wall is optically thick in the vertical direction at H-band. PDS 70 is not a member of the class of (pre-) transitional disks identified by Dong et al., whose members only show evidence of the cavity in the millimeter-size dust but not the sub-micron-sized dust in resolved images. The two classes of (pre-) transitional disks may form through different mechanisms, or they may simply be at different evolution stages in the disk-clearing process.
C1 [Dong, Ruobing; Rafikov, Roman; Zhu, Zhaohuan; Brandt, Timothy; Janson, M.; Knapp, G. R.; Turner, E.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Hashimoto, Jun; Iye, M.; Kandori, R.; Kusakabe, N.; Kuzuhara, M.; Kwon, J.; Morino, J. -I.; Suto, H.; Tamura, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Whitney, Barbara] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Kudo, Tomoyuki; Egner, S.; Guyon, O.; Hayano, Y.; Hayashi, S.; Ishii, M.; Nishimura, T.; Pyo, T. -S.; Takato, N.; Terada, H.; Tomono, D.; Takami, H.; Usuda, T.] Subaru Telescope, Hilo, HI 96720 USA.
[Muto, Takayuki] Kogakuin Univ, Div Liberal Arts, Shinjuku Ku, Tokyo 1638677, Japan.
[McClure, Melissa K.] Univ Michigan, Dept Astron, Ann Arbor, MI 48105 USA.
[Wisniewski, John] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Abe, L.] Univ Nice Sophia Antipolis, CNRS, UMR7293, Lab Lagrange,Observ Cote Azur, F-06300 Nice, France.
[Brandner, W.; Feldt, M.; Goto, M.; Henning, T.; Thalmann, C.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Carson, J.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Grady, C.; McElwain, M.] Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Grady, C.] Eureka Sci, Oakland, CA 96002 USA.
[Hayashi, M.] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Hodapp, K. W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Matsuo, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Miyama, S.] Hiroshima Univ, Off President, Higashihiroshima 7398511, Japan.
[Moro-Martin, A.] CAB INTA CSIC, Dept Astrofis, E-28850 Madrid, Spain.
CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Suzuki, R.] TMT Observ Corp, Pasadena, CA 91105 USA.
[Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Turner, E.] Univ Tokyo, Kavli Inst Phys & Math Univ, Kashiwa, Chiba 2278568, Japan.
[Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido 0600810, Japan.
[Yamada, T.] Tohoku Univ, Astron Inst, Sendai, Miyagi 9808578, Japan.
RP Dong, RB (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
EM rdong@astro.princeton.edu
RI Turner, Edwin/A-4295-2011; MIYAMA, Shoken/A-3598-2015
FU NSF [AST 0908269, AST 1008440, AST 1009314, AST 1009203]; NASA
[NNX22SK53G]; Sloan Fellowship; World Premier International Research
Center Initiative (WPI Initiative), MEXT, Japan
FX R.D. thanks Edwin Bergin, Tilman Birnstiel, Brendan Bowler, Nuria
Calvet, L. Ilsedore Cleeves, Bruce Draine, Catherine Espaillat, Lee
Hartmann, Shu-ichiro Inutsuka, Andrea Isella, James Owen, Thomas P.
Robitaille, Fredrik Windmark, and Yanqin Wu for useful discussions. The
authors are also grateful to the anonymous referee who helped improve
the manuscript. This work is partially supported by NSF grant AST
0908269 (R.D., Z.Z., and R.R.), AST 1008440 (C.G.), AST 1009314 (J.W.),
AST 1009203 (J.C.), NASA grant NNX22SK53G (L.H.), Sloan Fellowship
(R.R.), and World Premier International Research Center Initiative (WPI
Initiative), MEXT, Japan (E.L.T.). 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.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2012
VL 760
IS 2
AR 111
DI 10.1088/0004-637X/760/2/111
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 039BE
UT WOS:000311217000015
ER
PT J
AU Frisch, PC
Andersson, BG
Berdyugin, A
Piirola, V
DeMajistre, R
Funsten, HO
Magalhaes, AM
Seriacopi, DB
McComas, DJ
Schwadron, NA
Slavin, JD
Wiktorowicz, SJ
AF Frisch, P. C.
Andersson, B-G
Berdyugin, A.
Piirola, V.
DeMajistre, R.
Funsten, H. O.
Magalhaes, A. M.
Seriacopi, D. B.
McComas, D. J.
Schwadron, N. A.
Slavin, J. D.
Wiktorowicz, S. J.
TI THE INTERSTELLAR MAGNETIC FIELD CLOSE TO THE SUN. II.
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: bubbles; ISM: magnetic fields; local interstellar matter; methods:
data analysis; polarization; Sun: heliosphere
ID BOUNDARY-EXPLORER RIBBON; NEUTRAL ATOM MAPS; LOCAL BUBBLE; IBEX RIBBON;
LINEAR-POLARIZATION; OUTER HELIOSHEATH; GRAIN ALIGNMENT; COSMIC-RAYS;
OPTICAL POLARIZATION; STELLAR POLARIZATION
AB The magnetic field in the local interstellar medium (ISM) provides a key indicator of the galactic environment of the Sun and influences the shape of the heliosphere. We have studied the interstellar magnetic field (ISMF) in the solar vicinity using polarized starlight for stars within 40 pc of the Sun and 90 degrees of the heliosphere nose. In Frisch et al. (Paper I), we developed a method for determining the local ISMF direction by finding the best match to a group of interstellar polarization position angles obtained toward nearby stars, based on the assumption that the polarization is parallel to the ISMF. In this paper, we extend the analysis by utilizing weighted fits to the position angles and by including new observations acquired for this study. We find that the local ISMF is pointed toward the galactic coordinates l, b = 47 degrees +/- 20 degrees, 25 degrees +/- 20 degrees. This direction is close to the direction of the ISMF that shapes the heliosphere, l, b = 33 degrees +/- 4 degrees, 55 degrees +/- 4 degrees, as traced by the center of the "Ribbon" of energetic neutral atoms discovered by the Interstellar Boundary Explorer (IBEX) mission. Both the magnetic field direction and the kinematics of the local ISM are consistent with a scenario where the local ISM is a fragment of the Loop I superbubble. A nearby ordered component of the local ISMF has been identified in the region l approximate to 0 degrees -> 80 degrees and b approximate to 0 degrees -> 30 degrees, where PlanetPol data show a distance-dependent increase of polarization strength. The ordered component extends to within 8 pc of the Sun and implies a weak curvature in the nearby ISMF of +/- 0 degrees.25 pc(-1). This conclusion is conditioned on the small sample of stars available for defining this rotation. Variations from the ordered component suggest a turbulent component of +/- 23 degrees. The ordered component and standard relations between polarization, color excess, and H-o column density predict a reasonable increase of N(H) with distance in the local ISM. The similarity of the ISMF directions traced by the polarizations, the IBEX Ribbon, and pulsars inside the Local Bubble in the third galactic quadrant suggest that the ISMF is relatively uniform over spatial scales of 8-200 pc and is more similar to interarm than spiral-arm magnetic fields. The ISMF direction from the polarization data is also consistent with small-scale spatial asymmetries detected in GeV-TeV cosmic rays with a galactic origin. The peculiar geometrical relation found earlier between the cosmic microwave background dipole moment, the heliosphere nose, and the ISMF direction is supported by this study. The interstellar radiation field at +/- 975 angstrom does not appear to play a role in grain alignment for the low-density ISM studied here.
C1 [Frisch, P. C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Andersson, B-G] NASA, Ames Res Ctr, Univ Space Res Assoc, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
[Berdyugin, A.; Piirola, V.] Univ Turku, Finnish Ctr Astron ESO, SF-20500 Turku, Finland.
[DeMajistre, R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Funsten, H. O.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Magalhaes, A. M.; Seriacopi, D. B.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508 Sao Paulo, Brazil.
[McComas, D. J.] SW Res Inst, San Antonio, TX USA.
[Schwadron, N. A.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Slavin, J. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Wiktorowicz, S. J.] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA.
[McComas, D. J.] Univ Texas San Antonio, San Antonio, TX USA.
RP Frisch, PC (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
RI 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013; Magalhaes, Antonio
Mario/K-9532-2013; Funsten, Herbert/A-5702-2015;
OI Funsten, Herbert/0000-0002-6817-1039; Andersson, B-G/0000-0001-6717-0686
FU IBEX mission; NASA's Explorer Program; NASA [NNX09AH50G, NNX08AJ33G]
FX This work was supported by the IBEX mission as part of NASA's Explorer
Program, and by NASA grants NNX09AH50G and NNX08AJ33G to the University
of Chicago. We are grateful for observations made with the Nordic
Optical Telescope, operated on the island of La Palma jointly by
Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish
Observatorio del Roque de los Muchachos of the Instituto de Astrofisica
de Canarias. We are also grateful for observations made with telescopes
at the Observatorio do Pico dos Dias of the Laboratorio Nacional de
Astrofisica of Brazil.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2012
VL 760
IS 2
AR 106
DI 10.1088/0004-637X/760/2/106
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 039BE
UT WOS:000311217000010
ER
PT J
AU Linares, M
Connaughton, V
Jenke, P
van der Horst, AJ
Camero-Arranz, A
Kouveliotou, C
Chakrabarty, D
Beklen, E
Bhat, PN
Briggs, MS
Finger, M
Paciesas, WS
Preece, R
von Kienlin, A
Wilson-Hodge, CA
AF Linares, M.
Connaughton, V.
Jenke, P.
van der Horst, A. J.
Camero-Arranz, A.
Kouveliotou, C.
Chakrabarty, D.
Beklen, E.
Bhat, P. N.
Briggs, M. S.
Finger, M.
Paciesas, W. S.
Preece, R.
von Kienlin, A.
Wilson-Hodge, C. A.
TI THE FERMI-GBM X-RAY BURST MONITOR: THERMONUCLEAR BURSTS FROM 4U 0614+09
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; binaries: close; stars: neutron; X-rays:
binaries; X-rays: bursts; X-rays: individual (4U 0614+09)
ID NEUTRON-STAR; BINARY 4U-0614+091; TIMING-EXPLORER; 2S-0918-549
AB Thermonuclear bursts from slowly accreting neutron stars (NSs) have proven difficult to detect, yet they are potential probes of the thermal properties of the NS interior. During the first year of a systematic all-sky search for X-ray bursts using the Gamma-ray Burst Monitor aboard the Fermi Gamma-ray Space Telescope we have detected 15 thermonuclear bursts from the NS low-mass X-ray binary 4U 0614+09 when it was accreting at nearly 1% of the Eddington limit. We measured an average burst recurrence time of 12 +/- 3 days (68% confidence interval) between 2010 March and 2011 March, classified all bursts as normal duration bursts and placed a lower limit on the recurrence time of long/intermediate bursts of 62 days (95% confidence level). We discuss how observations of thermonuclear bursts in the hard X-ray band compare to pointed soft X-ray observations and quantify such bandpass effects on measurements of burst radiated energy and duration. We put our results for 4U 0614+09 in the context of other bursters and briefly discuss the constraints on ignition models. Interestingly, we find that the burst energies in 4U 0614+09 are on average between those of normal duration bursts and those measured in long/intermediate bursts. Such a continuous distribution in burst energy provides a new observational link between normal and long/intermediate bursts. We suggest that the apparent bimodal distribution that defined normal and long/intermediate duration bursts during the last decade could be due to an observational bias toward detecting only the longest and most energetic bursts from slowly accreting NSs.
C1 [Linares, M.; Chakrabarty, D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Connaughton, V.; Bhat, P. N.; Briggs, M. S.; Preece, R.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Jenke, P.; Kouveliotou, C.; Wilson-Hodge, C. A.] NASA, Space Sci Off, VP62, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[van der Horst, A. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Camero-Arranz, A.; Finger, M.; Paciesas, W. S.] Univ Space Res Assoc, Huntsville, AL 35805 USA.
[Beklen, E.] Suleyman Demirel Univ, Dept Phys, TR-32260 Isparta, Turkey.
[von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Connaughton, V.; Bhat, P. N.; Briggs, M. S.; Preece, R.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
RP Linares, M (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
OI Preece, Robert/0000-0003-1626-7335
FU NWO; NASA [NNX11AO19G]
FX Quick-look ASM results were provided by the RXTE/ASM team. Swift/BAT
transient monitor results were provided by the Swift/BAT team. This
paper utilizes preliminary analysis results from the Multi-INstrument
Burst ARchive (MINBAR; http://users.monash.edu.au/similar to
dgallow/minbar). Data from previous bursts were kindly provided by E.
Kuulkers. We thank A. Cumming for providing ignition models and for
stimulating discussions and V. Chaplin for clarifications on detector
geometries during some of the bursts. We also thank the anonymous
referee for constructive comments. M.L. is grateful to the International
Space Science Institute in Bern, where part of this work was completed,
and acknowledges support from the NWO Rubicon fellowship. This research
was partly funded by NASA's Fermi Guest Investigation program under
grant NNX11AO19G.
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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 DEC 1
PY 2012
VL 760
IS 2
AR 133
DI 10.1088/0004-637X/760/2/133
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 039BE
UT WOS:000311217000037
ER
PT J
AU Mallery, RP
Mobasher, B
Capak, P
Kakazu, Y
Masters, D
Ilbert, O
Hemmati, S
Scarlata, C
Salvato, M
McCracken, H
LeFevre, O
Scoville, N
AF Mallery, Ryan P.
Mobasher, Bahram
Capak, Peter
Kakazu, Yuko
Masters, Dan
Ilbert, Olivier
Hemmati, Shoubaneh
Scarlata, Claudia
Salvato, Mara
McCracken, Henry
LeFevre, Olivier
Scoville, Nick
TI Ly alpha EMISSION FROM HIGH-REDSHIFT SOURCES IN COSMOS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; galaxies: ISM
ID LYMAN-BREAK GALAXIES; STAR-FORMING GALAXIES; SUBARU DEEP FIELD;
SIMILAR-TO 3; LUMINOSITY FUNCTION; STELLAR POPULATIONS; EMITTING
GALAXIES; SPECTROSCOPIC CONFIRMATION; PHOTOMETRIC PROPERTIES;
BUILDING-BLOCKS
AB We investigate spectroscopically measured Ly alpha equivalent widths (EWs) and escape fractions of 244 sources of which 95 are Lyman break galaxies (LBGs) and 106 Lyman alpha emitters (LAEs) at z similar to 4.2, z similar to 4.8, and z similar to 5.6 selected from intermediate and narrowband observations. The sources were selected from the Cosmic Evolution Survey and observed with the DEIMOS spectrograph. We find that the distribution of EWs shows no evolution with redshift for both the LBG selected sources and the intermediate/narrowband LAEs. We also find that the Ly alpha escape fraction of intermediate/narrowband LAEs is on average higher and has a larger variation than the escape fraction of LBG selected sources. The escape fraction does not show a dependence with redshift. Similar to what has been found for LAEs at low redshifts, the sources with the highest extinctions show the lowest escape fractions. The range of escape fractions increases with decreasing extinction. This is evidence that the dust extinction is the most important factor affecting the escape of Ly alpha photons, but at low extinctions other factors, such as the H I covering fraction and gas kinematics, can be just as effective at inhibiting the escape of Ly alpha photons.
C1 [Mallery, Ryan P.; Mobasher, Bahram; Hemmati, Shoubaneh] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92507 USA.
[Capak, Peter; Kakazu, Yuko; Masters, Dan; Scoville, Nick] CALTECH, NASA, JPL Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Ilbert, Olivier; LeFevre, Olivier] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France.
[Scarlata, Claudia] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Salvato, Mara] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[McCracken, Henry] Univ Paris 06, CNRS UMR7095, Inst Astrophys Paris, F-75014 Paris, France.
RP Mallery, RP (reprint author), Univ Calif Riverside, Dept Phys & Astron, 900 Univ Ave, Riverside, CA 92507 USA.
FU W. M. Keck Foundation
FX Based in part on data obtained at the W. M. Keck Observatory, which is
operated as a scientific partnership among the California Institute of
Technology, the University of California, and NASA and was made possible
by the generous financial support of the W. M. Keck Foundation.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2012
VL 760
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AR 128
DI 10.1088/0004-637X/760/2/128
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 039BE
UT WOS:000311217000032
ER
PT J
AU Muinonen, K
Mishchenko, MI
Dlugach, JM
Zubko, E
Penttila, A
Videen, G
AF Muinonen, K.
Mishchenko, M. I.
Dlugach, J. M.
Zubko, E.
Penttila, A.
Videen, G.
TI COHERENT BACKSCATTERING VERIFIED NUMERICALLY FOR A FINITE VOLUME OF
SPHERICAL PARTICLES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE minor planets, asteroids: general; planets and satellites: surfaces;
polarization radiative transfer; scattering
ID MULTIPLE-SCATTERING; RADIATIVE-TRANSFER; LIGHT-SCATTERING; T-MATRIX;
INTERFACE; OBJECT; SYSTEM; SPHERES; MEDIA
AB We consider electromagnetic scattering by a spherical volume sparsely and randomly populated by spherical particles of equal size and optical properties. The far-field scattering matrix of the entire volume is computed using an exact method and an approximate method. The former is a direct computer solver of the Maxwell equations called the superposition T-matrix method (STMM). The latter is a solver based on numerical Monte Carlo integration of the ladder and cyclical diagrams appearing in the microphysical theory of radiative transfer and coherent backscattering (RT-CB). The quantitative agreement between the STMM and RT-CB computations provides verification of the RT-CB theory. Prominent backscattering features exhibited by the STMM data cannot be reproduced by keeping only the ladder diagrams of RT. Our results strongly support the CB explanation of opposition brightness and polarization phenomena observed for a class of atmosphereless solar-system objects. Further research is necessary to determine the range of quantitative applicability of the RT-CB theory to densely packed particulate media.
C1 [Muinonen, K.; Zubko, E.; Penttila, A.] Univ Helsinki, Dept Phys, FI-00014 U Helsinki, Finland.
[Mishchenko, M. I.] NASA Goddard Inst Space Studies, New York, NY 10025 USA.
[Dlugach, J. M.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine.
[Videen, G.] Army Res Lab, Adelphi, MD 20783 USA.
[Muinonen, K.] Finnish Geodet Inst, FI-02431 Masala, Finland.
[Zubko, E.] Kharkov Natl Univ, Inst Astron, UA-61022 Kharkov, Ukraine.
RP Muinonen, K (reprint author), Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2A, FI-00014 U Helsinki, Finland.
EM karri.muinonen@helsinki.fi; michael.i.mishchenko@nasa.gov;
dl@mao.kiev.ua; evgenij.zubko@helsinki.fi; antti.i.penttila@helsinki.fi;
gorden.videen@gmail.com
RI Penttila, Antti/C-4886-2012; Mishchenko, Michael/D-4426-2012
OI Penttila, Antti/0000-0001-7403-1721;
FU Academy of Finland [127461]; NASA Outer Planets Research Program
[NNX10AP93G]; NASA Lunar Advanced Science and Exploration Research
Program [NNX11AB25G]; NASA Radiation Sciences Program; NASA Remote
Sensing Theory Program; National Academy of Sciences of Ukraine under
the Main Astronomical Observatory GRAPE/GPU/GRID Computing Cluster
Project
FX This research has been partially funded by the Academy of Finland
(contract 127461), NASA Outer Planets Research Program (contract
NNX10AP93G), and NASA Lunar Advanced Science and Exploration Research
Program (contract NNX11AB25G), as well as by the NASA Radiation Sciences
Program managed by Hal Maring and by the NASA Remote Sensing Theory
Program managed by Lucia Tsaoussi. M.I.M. and J.M.D. also acknowledge
support from the National Academy of Sciences of Ukraine under the Main
Astronomical Observatory GRAPE/GPU/GRID Computing Cluster Project.
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SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2012
VL 760
IS 2
AR 118
DI 10.1088/0004-637X/760/2/118
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SC Astronomy & Astrophysics
GA 039BE
UT WOS:000311217000022
ER
PT J
AU Qian, L
Li, D
Goldsmith, PF
AF Qian, Lei
Li, Di
Goldsmith, Paul F.
TI (CO)-C-13 CORES IN THE TAURUS MOLECULAR CLOUD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; ISM: individual objects (Taurus); ISM: molecules;
turbulence
ID INITIAL MASS FUNCTION; STAR-FORMATION; DENSE CORES; CLUMP DISTRIBUTION;
SUBMILLIMETER CLUMPS; 850 MICRONS; ORION; PERSEUS; ORIGIN; EXTINCTION
AB Young stars form in molecular cores, which are dense condensations within molecular clouds. We have searched for molecular cores traced by (CO)-C-13 J = 1 -> 0 emission in the Taurus molecular cloud and studied their properties. Our data set has a spatial dynamic range (the ratio of linear map size to the pixel size) of about 1000 and spectrally resolved velocity information, which together allow a systematic examination of the distribution and dynamic state of (CO)-C-13 cores in a large contiguous region. We use empirical fit to the CO and CO2 ice to correct for depletion of gas-phase CO. The (CO)-C-13 core mass function ((CO)-C-13 CMF) can be fitted better with a log-normal function than with a power-law function. We also extract cores and calculate the (CO)-C-13 CMF based on the integrated intensity of (CO)-C-13 and the CMF from Two Micron All Sky Survey. We demonstrate that core blending exists, i.e., combined structures that are incoherent in velocity but continuous in column density. The core velocity dispersion (CVD), which is the variance of the core velocity difference delta nu, exhibits a power-law behavior as a function of the apparent separation L: CVD (km s(-1)) proportional to L(pc)(0.7). This is similar to Larson's law for the velocity dispersion of the gas. The peak velocities of (CO)-C-13 cores do not deviate from the centroid velocities of the ambient (CO)-C-12 gas by more than half of the line width. The low velocity dispersion among cores, the close similarity between CVD and Larson's law, and the small separation between core centroid velocities and the ambient gas all suggest that molecular cores condense out of the diffuse gas without additional energy from star formation or significant impact from converging flows.
C1 [Qian, Lei; Li, Di] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Li, Di] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Li, Di] Space Sci Inst, Boulder, CO USA.
RP Qian, L (reprint author), Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
EM lqian@nao.cas.cn; ithaca.li@gmail.com
RI Goldsmith, Paul/H-3159-2016
FU China Ministry of Science and Technology [2012CB821800]; General Program
of National Natural Science Foundation of China [11073028]; Young
Researcher Grant of National Astronomical Observatories, Chinese Academy
of Sciences; Chinese Academy of Sciences
FX This work is partly supported by the China Ministry of Science and
Technology under State Key Development Program for Basic Research
(2012CB821800) and partly supported by the General Program of National
Natural Science Foundation of China (11073028). L. Q. is partly
supported by the Young Researcher Grant of National Astronomical
Observatories, Chinese Academy of Sciences and partly supported by M.
Zhu with his funding from the One Hundred Person Project of the Chinese
Academy of Sciences. This work was carried out in part at the Jet
Propulsion Laboratory, operated by the California Institute of
Technology.
NR 58
TC 16
Z9 17
U1 1
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 DEC 1
PY 2012
VL 760
IS 2
AR 147
DI 10.1088/0004-637X/760/2/147
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 039BE
UT WOS:000311217000051
ER
PT J
AU Smail, I
Blundell, KM
Lehmer, BD
Alexander, DM
AF Smail, Ian
Blundell, Katherine M.
Lehmer, B. D.
Alexander, D. M.
TI INVERSE COMPTON X-RAY HALOS AROUND HIGH-z RADIO GALAXIES: A FEEDBACK
MECHANISM POWERED BY FAR-INFRARED STARBURSTS OR THE COSMIC MICROWAVE
BACKGROUND?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: evolution; galaxies: formation;
galaxies: individual (4C03.24, 4C19.71)
ID JET-CLOUD INTERACTIONS; DEEP-FIELD-NORTH; STAR-FORMATION; ELLIPTIC
GALAXIES; AGN FEEDBACK; 4C 60.07; HDF 130; EMISSION; CHANDRA; EVOLUTION
AB We report the detection of extended X-ray emission around two powerful radio galaxies at z similar to 3.6 (4C 03.24 and 4C 19.71) and use these to investigate the origin of extended, inverse Compton (IC) powered X-ray halos at high redshifts. The halos have X-ray luminosities of L-X similar to 3 x 10(44) erg s(-1) and sizes of similar to 60 kpc. Their morphologies are broadly similar to the similar to 60 kpc long radio lobes around these galaxies suggesting they are formed from IC scattering by relativistic electrons in the radio lobes, of either cosmic microwave background (CMB) photons or far-infrared photons from the dust-obscured starbursts in these galaxies. These observations double the number of z > 3 radio galaxies with X-ray-detected IC halos. We compare the IC X-ray-to-radio luminosity ratios for the two new detections to the two previously detected z similar to 3.8 radio galaxies. Given the similar redshifts, we would expect comparable X-ray IC luminosities if millimeter photons from the CMB are the dominant seed field for the IC emission (assuming all four galaxies have similar ages and jet powers). Instead we see that the two z similar to 3.6 radio galaxies, which are similar to 4x fainter in the far-infrared than those at z similar to 3.8, also have similar to 4x fainter X-ray IC emission. Including data for a further six z greater than or similar to 2 radio sources with detected IC X-ray halos from the literature, we suggest that in the more compact, majority of radio sources, those with lobe sizes less than or similar to 100-200 kpc, the bulk of the IC emission may be driven by scattering of locally produced far-infrared photons from luminous, dust-obscured starbursts within these galaxies, rather than millimeter photons from the CMB. The resulting X-ray emission appears sufficient to ionize the gas on similar to 100-200 kpc scales around these systems and thus helps form the extended, kinematically quiescent Ly alpha emission line halos found around some of these systems. The starburst and active galactic nucleus activity in these galaxies are thus combining to produce an even more effective and widespread "feedback" process, acting on the long-term gas reservoir for the galaxy, than either individually could achieve. If episodic radio activity and coeval starbursts are common in massive, high-redshift galaxies, then this IC-feedback mechanism may play a role in affecting the star formation histories of the most massive galaxies at the present day.
C1 [Smail, Ian] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England.
[Blundell, Katherine M.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Lehmer, B. D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Lehmer, B. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
RP Smail, I (reprint author), Univ Durham, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England.
RI Smail, Ian/M-5161-2013;
OI Smail, Ian/0000-0003-3037-257X; Alexander, David/0000-0002-5896-6313
FU Leverhulme Trust; STFC; Einstein Fellowship; CXC [G01-12173X]
FX We thank for Nick Seymour for generously checking his data prior to
publication and Rob Ivison, Richard Bower, Caleb Scharf, Wil van
Breugel, Mark Dickinson, Arjun Dey, Hy Spinrad, and Dan Stern for help
and useful conversations. I. R. S. acknowledges a Leverhulme Trust
Fellowship and I. R. S., K. M. B., and D. M. A. acknowledge support from
the STFC. B. D. L. acknowledges support from an Einstein Fellowship and
CXC grant G01-12173X. This work has used data from the NASA
Extragalactic Database (NED), and from the NRAO VLA, Hubble Space
Telescope, and Spitzer Space Telescope data archives.
NR 49
TC 4
Z9 4
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 DEC 1
PY 2012
VL 760
IS 2
AR 132
DI 10.1088/0004-637X/760/2/132
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 039BE
UT WOS:000311217000036
ER
PT J
AU Goosse, H
Crespin, E
Dubinkina, S
Loutre, MF
Mann, ME
Renssen, H
Sallaz-Damaz, Y
Shindell, D
AF Goosse, Hugues
Crespin, Elisabeth
Dubinkina, Svetlana
Loutre, Marie-France
Mann, Michael E.
Renssen, Hans
Sallaz-Damaz, Yoann
Shindell, Drew
TI The role of forcing and internal dynamics in explaining the "Medieval
Climate Anomaly"
SO CLIMATE DYNAMICS
LA English
DT Article
DE Paleoclimate; Last millennium; Medieval Climate Anomaly; Climate
modelling; Data assimilation; Atmospheric and ocean dynamics; Radiative
forcing
ID NORTH-ATLANTIC OSCILLATION; LAST MILLENNIUM; PAST MILLENNIUM;
CARBON-CYCLE; GULF-STREAM; RADIONUCLIDE RECORDS; SOLAR-ACTIVITY; SYSTEM
MODEL; WARM PERIOD; VARIABILITY
AB Proxy reconstructions suggest that peak global temperature during the past warm interval known as the Medieval Climate Anomaly (MCA, roughly 950-1250 AD) has been exceeded only during the most recent decades. To better understand the origin of this warm period, we use model simulations constrained by data assimilation establishing the spatial pattern of temperature changes that is most consistent with forcing estimates, model physics and the empirical information contained in paleoclimate proxy records. These numerical experiments demonstrate that the reconstructed spatial temperature pattern of the MCA can be explained by a simple thermodynamical response of the climate system to relatively weak changes in radiative forcing combined with a modification of the atmospheric circulation, displaying some similarities with the positive phase of the so-called Arctic Oscillation, and with northward shifts in the position of the Gulf Stream and Kuroshio currents. The mechanisms underlying the MCA are thus quite different from anthropogenic mechanisms responsible for modern global warming.
C1 [Goosse, Hugues; Crespin, Elisabeth; Dubinkina, Svetlana; Loutre, Marie-France; Sallaz-Damaz, Yoann] Catholic Univ Louvain, Earth & Life Inst, Georges Lemaitre Ctr Earth & Climate Res, B-1348 Louvain, Belgium.
[Mann, Michael E.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Mann, Michael E.] Penn State Univ, Earth & Environm Syst Inst, University Pk, PA 16802 USA.
[Renssen, Hans] Vrije Univ Amsterdam, Dept Earth Sci, Sect Climate Change & Landscape Dynam, Amsterdam, Netherlands.
[Shindell, Drew] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Goosse, H (reprint author), Catholic Univ Louvain, Earth & Life Inst, Georges Lemaitre Ctr Earth & Climate Res, Chemin Cyclotron 2, B-1348 Louvain, Belgium.
EM hugues.goosse@uclouvain.be
RI Shindell, Drew/D-4636-2012; Mann, Michael/B-8472-2017;
OI Mann, Michael/0000-0003-3067-296X; Loutre,
Marie-France/0000-0001-6944-4038
FU FRS-FNRS; Belgian Federal Science Policy Office; EU; NSF [ATM-0902133];
Fond de la Recherche Scientifique de Belgique (FRS-FNRS)
FX We thank E. Zorita and R. Wilson for comments and all the scientists
that collected and analysed the proxy data used in this work. H. G. is
Senior Research Associate with the Fonds National de la Recherche
Scientifique (FRS-FNRS-Belgium). This work is supported by the FRS-FNRS
and by the Belgian Federal Science Policy Office (Research Program on
Science for a Sustainable Development) and by EU (project Past4future).
M. E. M. acknowledges support from the NSF Paleoclimate program (grant
number ATM-0902133). Aurelien Mairesse helped in the design of Fig. 1.
Computational resources have been provided by the super-computing
facilities of the Universite Catholique de Louvain (CISM/UCL) and the
Consortium des Equipements de Calcul Intensif en Federation Wallonie
Bruxelles (CECI) funded by the Fond de la Recherche Scientifique de
Belgique (FRS-FNRS).
NR 60
TC 43
Z9 43
U1 1
U2 48
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
J9 CLIM DYNAM
JI Clim. Dyn.
PD DEC
PY 2012
VL 39
IS 12
BP 2847
EP 2866
DI 10.1007/s00382-012-1297-0
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 038VV
UT WOS:000311203100007
ER
PT J
AU Torres-Perez, JL
Armstrong, RA
AF Torres-Perez, J. L.
Armstrong, R. A.
TI Effects of UV radiation on the growth, photosynthetic and
photoprotective components, and reproduction of the Caribbean
shallow-water coral Porites furcata
SO CORAL REEFS
LA English
DT Article
DE Ultraviolet radiation; Coral growth; Mycosporine-like amino acids; Coral
reproduction; Porites furcata
ID AMINO-ACIDS MAAS; REEF-BUILDING CORAL; SOLAR ULTRAVIOLET-RADIATION;
GREAT-BARRIER-REEF; POCILLOPORA-DAMICORNIS; STYLOPHORA-PISTILLATA;
ABSORBING COMPOUNDS; ACROPORA-CERVICORNIS; SEXUAL REPRODUCTION;
CLIMATE-CHANGE
AB Shallow reef corals can frequently be subjected to high doses of ultraviolet radiation [280-400 nm (UVR)] and have developed mechanisms to cope with this. Nevertheless, slight changes in this stressor may impact their physiology and ultimately their survival. Here, we present results on the effects of artificially enhanced UVR on the growth, reproduction, production of photosynthetic pigments and photoprotective compounds of the Caribbean shallow-water branching coral Porites furcata. Corals were randomly located in one of the three different treatments: normal photosynthetically active radiation (PAR) + UVR; normal PAR+ enhanced UVR; normal PAR+ depleted UVR. Growth rates were measured using the Alizarin red staining method, photosynthetic pigments as well as mycosporine-like amino acids (MAAs) were quantified through high-performance liquid chromatography, and fecundity was estimated after histological analyses. Growth and photosynthetic pigment concentration were negatively correlated with increased UVR, compared to controls exposed to normal UVR. A significant increase in MAAs was also found in colonies under enhanced UVR. Based on their respective concentrations, the primary mycosporine-glycine (lambda(max) = 310 nm) and shinorine (lambda(max) = 333 nm) are the main contributors to UVR absorption in this species, while the levels of the secondary MAA palythine (lambda(max) = 320 nm) tripled toward the end of the 128 days of the experimental period. While several physical factors may influence reef coral physiology, the results suggest that slight increases in UVR can debilitate the skeletal constitution and severely reduce the fecundity of corals living in shallow waters.
C1 [Torres-Perez, J. L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Torres-Perez, J. L.; Armstrong, R. A.] Univ Puerto Rico, Dept Marine Sci, Mayaguez, PR 00708 USA.
RP Torres-Perez, JL (reprint author), NASA, Ames Res Ctr, MS 245-4,Bldg 245 Rm 120,POB 1, Moffett Field, CA 94035 USA.
EM juanltorresperez@gmail.com
FU Department of Marine Sciences, University of Puerto Rico; Alliance for
Graduate Education Professoriate (AGEP); National Science Foundation;
NASA [NCCW-0088]
FX We would like to acknowledge the help and support from the Department of
Marine Sciences, University of Puerto Rico. This research was supported
by fellowships from the Alliance for Graduate Education Professoriate
(AGEP) and from the National Science Foundation's Puerto Rico Graduate
Teaching Fellows in K-12 Education to the corresponding author, and a
NASA grant (NCCW-0088) to RAA. We are grateful to the Puerto Rico
Department of Natural and Environmental Resources particularly the
Marine Fisheries Laboratory for facilitating their histology laboratory.
This manuscript was greatly improved by the comments of two anonymous
reviewers.
NR 84
TC 7
Z9 7
U1 3
U2 46
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0722-4028
J9 CORAL REEFS
JI Coral Reefs
PD DEC
PY 2012
VL 31
IS 4
BP 1077
EP 1091
DI 10.1007/s00338-012-0927-7
PG 15
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 036AS
UT WOS:000310999300018
ER
PT J
AU Sheard, BS
Heinzel, G
Danzmann, K
Shaddock, DA
Klipstein, WM
Folkner, WM
AF Sheard, B. S.
Heinzel, G.
Danzmann, K.
Shaddock, D. A.
Klipstein, W. M.
Folkner, W. M.
TI Intersatellite laser ranging instrument for the GRACE follow-on mission
SO JOURNAL OF GEODESY
LA English
DT Article
DE GRACE; Intersatellite ranging; Laser interferometry
ID FREQUENCY STABILIZATION; OPTICAL INTERFEROMETERS; AUTOMATIC ALIGNMENT;
GRAVITY RECOVERY; MASS VARIABILITY; PHASEMETER; SYSTEM; IMPACT
AB The Gravity Recovery and Climate Experiment (GRACE) has demonstrated that low-low satellite-to-satellite tracking enables monitoring the time variations of the Earth's gravity field on a global scale, in particular those caused by mass-transport within the hydrosphere. Due to the importance of long-term continued monitoring of the variations of the Earth's gravitational field and the limited lifetime of GRACE, a follow-on mission is currently planned to be launched in 2017. In order to minimise risk and the time to launch, the follow-on mission will be basically a rebuild of GRACE with microwave ranging as the primary instrument for measuring changes of the intersatellite distance. Laser interferometry has been proposed as a method to achieve improved ranging precision for future GRACE-like missions and is therefore foreseen to be included as demonstrator experiment in the follow-on mission now under development. This paper presents the top-level architecture of an interferometric laser ranging system designed to demonstrate the technology which can also operate in parallel with the microwave ranging system of the GRACE follow-on mission.
C1 [Sheard, B. S.; Heinzel, G.; Danzmann, K.] Leibniz Univ Hannover, Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-30167 Hannover, Germany.
[Sheard, B. S.; Heinzel, G.; Danzmann, K.] Leibniz Univ Hannover, Inst Gravitat Phys, D-30167 Hannover, Germany.
[Shaddock, D. A.] Australian Natl Univ, Dept Quantum Sci, Acton, ACT 0200, Australia.
[Klipstein, W. M.; Folkner, W. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sheard, BS (reprint author), Leibniz Univ Hannover, Albert Einstein Inst, Max Planck Inst Gravitat Phys, Callinstr 38, D-30167 Hannover, Germany.
EM benjamin.sheard@aei.mpg.de; gerhard.heinzel@aei.mpg.de;
karsten.danzmann@aei.mpg.de; daniel.shaddock@anu.edu.au
RI Shaddock, Daniel/A-7534-2011
OI Shaddock, Daniel/0000-0002-6885-3494
FU "Deutsche Forschungsgemeinschaft" (DFG) within the Cluster of Excellence
QUEST (Centre for Quantum Engineering and Space-Time Research);
Australian Government's Australian Space Research Program
FX This work was partly funded by the "Deutsche Forschungsgemeinschaft"
(DFG) within the Cluster of Excellence QUEST (Centre for Quantum
Engineering and Space-Time Research). Parts of the research described in
this publication were carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. This work was also supported under
the Australian Government's Australian Space Research Program.
NR 48
TC 84
Z9 87
U1 4
U2 20
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0949-7714
EI 1432-1394
J9 J GEODESY
JI J. Geodesy
PD DEC
PY 2012
VL 86
IS 12
BP 1083
EP 1095
DI 10.1007/s00190-012-0566-3
PG 13
WC Geochemistry & Geophysics; Remote Sensing
SC Geochemistry & Geophysics; Remote Sensing
GA 035RG
UT WOS:000310964800001
ER
PT J
AU Li, YF
Wang, ML
Carra, C
Cucinotta, FA
AF Li, Yongfeng
Wang, Minli
Carra, Claudio
Cucinotta, Francis A.
TI Modularized Smad-regulated TGF beta signaling pathway
SO MATHEMATICAL BIOSCIENCES
LA English
DT Article
DE Ionizing radiation; Transforming growth factor beta (TGF beta); Smad;
Signaling pathway; Modularization; Stability
ID GROWTH-FACTOR-BETA; UBIQUITIN-DEPENDENT DEGRADATION; KINETIC-ANALYSIS;
CELL-MEMBRANE; RECEPTOR; DYNAMICS; FIBROSIS; NUCLEUS; FIBROBLASTS;
INHIBITION
AB The transforming Growth Factor beta (TGF beta) signaling pathway is a prominent regulatory signaling pathway controlling various important cellular processes. TGF beta signaling can be induced by several factors including ionizing radiation. The pathway is regulated in a negative feedback loop through promoting the nuclear import of the regulatory Smads and a subsequent expression of inhibitory Smad7, that forms ubiquitin ligase with Smurf2, targeting active TGF beta receptors for degradation. In this work, we proposed a mathematical model to study the Smad-regulated TGF beta signaling pathway. By modularization, we are able to analyze mathematically each component subsystem and recover the nonlinear dynamics of the entire network system. Meanwhile the excitability, a common feature observed in the biological systems, in the TGF beta signaling pathway is discussed and supported as well by numerical simulation, indicating the robustness of the model. Published by Elsevier Inc.
C1 [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Li, Yongfeng; Wang, Minli; Carra, Claudio] 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 francis.a.cucinotta@nasa.gov
NR 42
TC 2
Z9 3
U1 0
U2 6
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0025-5564
EI 1879-3134
J9 MATH BIOSCI
JI Math. Biosci.
PD DEC
PY 2012
VL 240
IS 2
BP 187
EP 200
DI 10.1016/j.mbs.2012.07.005
PG 14
WC Biology; Mathematical & Computational Biology
SC Life Sciences & Biomedicine - Other Topics; Mathematical & Computational
Biology
GA 036ZK
UT WOS:000311070600011
PM 22892478
ER
PT J
AU Yu, Y
van Dyk, DA
Kashyap, VL
Young, CA
AF Yu, Y.
van Dyk, D. A.
Kashyap, V. L.
Young, C. A.
TI A Bayesian Analysis of the Correlations Among Sunspot Cycles
SO SOLAR PHYSICS
LA English
DT Article
ID SOLAR-CYCLE; STOCHASTIC FLUCTUATIONS; PREDICTION; MAXIMUM; NUMBERS;
RESTORATION; AMPLITUDE; SPECTRA; DYNAMO; MODEL
AB Sunspot numbers form a comprehensive, long-duration proxy of solar activity and have been used numerous times to empirically investigate the properties of the solar cycle. A number of correlations have been discovered over the 24 cycles for which observational records are available. Here we carry out a sophisticated statistical analysis of the sunspot record that reaffirms these correlations, and sets up an empirical predictive framework for future cycles. An advantage of our approach is that it allows for rigorous assessment of both the statistical significance of various cycle features and the uncertainty associated with predictions. We summarize the data into three sequential relations that estimate the amplitude, duration, and time of rise to maximum for any cycle, given the values from the previous cycle. We find that there is no indication of a persistence in predictive power beyond one cycle, and we conclude that the dynamo does not retain memory beyond one cycle. Based on sunspot records up to October 2011, we obtain, for Cycle 24, an estimated maximum smoothed monthly sunspot number of 97 +/- 15, to occur in January-February 2014 +/- six months.
C1 [Yu, Y.] Univ Calif Irvine, Irvine, CA 92717 USA.
[van Dyk, D. A.] Univ London Imperial Coll Sci Technol & Med, London, England.
[Kashyap, V. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Young, C. A.] NASA, ADNET Syst Inc, GSFC, Greenbelt, MD USA.
RP Yu, Y (reprint author), Univ Calif Irvine, Irvine, CA 92717 USA.
EM yamingy@uci.edu; dvandyk@imperial.ac.uk; vkashyap@cfa.harvard.edu;
c.alex.young@gsfc.nasa.gov
OI Van Dyk, David/0000-0002-0816-331X
FU CXC NASA [NAS 8-39073]; NSF [DMS 04-06085, DMS 09-07522]
FX This work was supported by CXC NASA contract NAS 8-39073 (VLK) and NSF
grants DMS 04-06085 and DMS 09-07522 (DvD, YY).
NR 42
TC 3
Z9 3
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 DEC
PY 2012
VL 281
IS 2
BP 847
EP 862
DI 10.1007/s11207-012-0090-x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 035UD
UT WOS:000310974000020
ER
PT J
AU Johnson, L
Young, R
Barnes, N
Friedman, L
Lappas, V
McInnes, C
AF Johnson, Les
Young, Roy
Barnes, Nathan
Friedman, Louis
Lappas, Vaios
McInnes, Colin
TI Solar Sails: Technology And Demonstration Status
SO INTERNATIONAL JOURNAL OF AERONAUTICAL AND SPACE SCIENCES
LA English
DT Review
DE Solar Sail; In-Space Propulsion; IKAROS; Sunjammer; NanoSail-D;
CubeSail; LightSail-1
AB Solar Sail propulsion has been validated in space (IKAROS, 2010) and soon several more solar-sail propelled spacecraft will be flown. Using sunlight for spacecraft propulsion is not a new idea. First proposed by Frederick Tsander and Konstantin Tsiolkovsky in the 1920' s, NASA's Echo 1 balloon, launched in 1960, was the first spacecraft for which the effects of solar photon pressure were measured. Solar sails reflect sunlight to achieve thrust, thus eliminating the need for costly and often very-heavy fuel. Such "propellantless" propulsion will enable whole new classes of space science and exploration missions previously not considered possible due to the propulsive-intense maneuvers and operations required.
C1 [Johnson, Les; Young, Roy] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Barnes, Nathan] LGarde Inc, Tustin, CA 92780 USA.
[Friedman, Louis] Planetary Soc, Execut Director Emeritus, Pasadena, CA 91107 USA.
[Lappas, Vaios] Univ Surrey, Space Vehicle Control, Guildford GU2 5XH, Surrey, England.
[McInnes, Colin] Univ Strathclyde, Dept Mech & Aerosp Engn, Adv Space Concepts Lab, Glasgow G1 1XJ, Lanark, Scotland.
RP Johnson, L (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM charles.l.johnson-1@nasa.gov
NR 16
TC 6
Z9 6
U1 6
U2 12
PU KOREAN SOC AERONAUTICAL & SPACE SCIENCES
PI SEOULD
PA 635-4, YEOGSAM-DONG, KANGNAM-KU, SEOULD, 135-703, SOUTH KOREA
SN 2093-274X
EI 2093-2480
J9 INT J AERONAUT SPACE
JI Int. J. Aeronaut. Space Sci.
PD DEC
PY 2012
VL 13
IS 4
BP 421
EP 427
DI 10.5139/IJASS.2012.13.4.421
PG 7
WC Engineering, Aerospace
SC Engineering
GA V35WZ
UT WOS:000209177200002
ER
PT J
AU Lillibridge, J
Bonekamp, H
Willis, J
Bonnefond, P
AF Lillibridge, John
Bonekamp, Hans
Willis, Josh
Bonnefond, Pascal
TI Special Issue: OSTM/Jason-2 Applications-Part 3 Preface
SO MARINE GEODESY
LA English
DT Editorial Material
C1 [Lillibridge, John] NOAA, Lab Satellite Altimetry, College Pk, MD USA.
[Bonekamp, Hans] EUMETSAT, Darmstadt, Germany.
[Willis, Josh] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Bonnefond, Pascal] Geoazur Observ Cote Azur, Grasse, France.
RP Lillibridge, J (reprint author), NOAA, Lab Satellite Altimetry, College Pk, MD USA.
RI Lillibridge, John/F-5606-2010
OI Lillibridge, John/0000-0001-9102-171X
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PI PHILADELPHIA
PA 520 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 0149-0419
EI 1521-060X
J9 MAR GEOD
JI Mar. Geod.
PD DEC 1
PY 2012
VL 35
SU 1
SI SI
BP 1
EP 2
DI 10.1080/01490419.2012.721634
PG 2
WC Geochemistry & Geophysics; Oceanography; Remote Sensing
SC Geochemistry & Geophysics; Oceanography; Remote Sensing
GA 066RT
UT WOS:000313238600001
ER
PT J
AU Masters, D
Nerem, RS
Choe, C
Leuliette, E
Beckley, B
White, N
Ablain, M
AF Masters, D.
Nerem, R. S.
Choe, C.
Leuliette, E.
Beckley, B.
White, N.
Ablain, M.
TI Comparison of Global Mean Sea Level Time Series from TOPEX/Poseidon,
Jason-1, and Jason-2
SO MARINE GEODESY
LA English
DT Article
DE Global mean sea level; climate data record; altimetry; interannual
variability
ID ALTIMETER DATA; TOPEX; BUDGET; TIDES; RISE; MISSIONS
AB In the interest of improving the sea level climate data record, we compare the 19-year global mean sea level (GMSL) time series derived from TOPEX-Poseidon, Jason-1, and Jason-2 and produced by different research institutions. The GMSL time series are each produced using varying techniques and different applied corrections, and subsequently, the time series exhibit unique characteristics and sensitivity to seasonal and interannual signals. We find that the different applied corrections affect the time series variability much less than the technique for computing the GMSL from along-track versus gridded sea surface height anomalies and the choice of a minimum depth criteria.
C1 [Masters, D.; Nerem, R. S.; Choe, C.] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA.
[Leuliette, E.] NOAA, Lab Satellite Altimetry, Silver Spring, MD USA.
[Beckley, B.] NASA, Goddard Space Flight Ctr, SGT Inc, Greenbelt, MD 20771 USA.
[White, N.] CSIRO Marine & Atmospher Res, Ctr Australian Weather & Climate Res & Wealth Oce, Hobart, Tas, Australia.
[Ablain, M.] CLS, Ramonville St Agne, France.
RP Masters, D (reprint author), Univ Colorado, Colorado Ctr Astrodynam Res, 431UCB, Boulder, CO 80309 USA.
EM dallas.masters@colorado.edu
RI Leuliette, Eric/D-1527-2010
OI Leuliette, Eric/0000-0002-3425-4039
FU NASA; GSFC; NOAA; CNES; CLS; CSIRO
FX This work was supported by two grants from NASA (Ocean Surface
Topography Science Team and the MEaSUREs Project). Additional support
from GSFC, NOAA, CNES, CLS, and CSIRO is also acknowledged.
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SN 0149-0419
EI 1521-060X
J9 MAR GEOD
JI Mar. Geod.
PD DEC 1
PY 2012
VL 35
SU 1
SI SI
BP 20
EP 41
DI 10.1080/01490419.2012.717862
PG 22
WC Geochemistry & Geophysics; Oceanography; Remote Sensing
SC Geochemistry & Geophysics; Oceanography; Remote Sensing
GA 066RT
UT WOS:000313238600003
ER
PT J
AU Cazenave, A
Henry, O
Munier, S
Delcroix, T
Gordon, AL
Meyssignac, B
Llovel, W
Palanisamy, H
Becker, M
AF Cazenave, A.
Henry, O.
Munier, S.
Delcroix, T.
Gordon, A. L.
Meyssignac, B.
Llovel, W.
Palanisamy, H.
Becker, M.
TI Estimating ENSO Influence on the Global Mean Sea Level, 1993-2010
SO MARINE GEODESY
LA English
DT Article
DE Sea level; ENSO; land waters; steric sea level; ocean mass
ID INDONESIAN THROUGHFLOW; MAKASSAR STRAIT; PRECIPITATION; PROJECT; OCEAN;
VARIABILITY; EVOLUTION; TRANSPORT; MODEL; WATER
AB Interannual global mean sea level (GMSL) variations and El Nino-Southern Oscillation (ENSO) are highly correlated, with positive/negative GMSL anomalies during El Nino/La Nina events. In a previous study, we showed that interannual GMSL and total land water storage variations are inversely correlated, with lower-than-average total water storage on land and higher-than-average GMSL during El Nino. This result is in agreement with the observed rainfall deficit/excess over land/oceans during El Nino (and vice versa during La Nina). It suggests that the positive GMSL anomaly observed during El Nino is likely due to an ocean mass rather than thermal expansion increase. Here, we analyze the respective contribution of the Atlantic, Indian, and Pacific oceans to the interannual (ENSO-related) GMSL anomalies observed during the altimetry era (i.e., since 1993) with an emphasis on the 1997/1998 El Nino event. For each oceanic region, we compute the steric contribution, and remove it from the altimetry-based mean sea level to estimate the ocean mass component. We find that mass changes of the tropical Pacific Ocean, mainly in the region within 025 degrees N, are mostly responsible for the observed 1997/1998 ENSO-related GMSL anomaly. The ocean mass excess of this region almost perfectly compensates the total land water deficit during the 1997/1998 El Nino. An estimate of the ocean-atmosphere water balance of this region shows that the time derivative of the ocean mass component is well correlated with net P-E (precipitation minus evaporation) over most of the study period, except during the 1997/1998 ENSO event, where there is a temporary ocean mass increase, not compensated by the net P-E. We thus propose that the 1997/1998 ocean mass increase of this north tropical Pacific area be linked to an imbalance between the inflow/outflow entering/leaving the north tropical Pacific. A preliminary qualitative analysis indicates that a significant reduction of the Makassar Strait transport, (about 80% of the total Indonesian throughflow), as previously reported in the literature during the strong 1997/1998 El Nino event, could explain the north tropical Pacific Ocean mass excess reported in this study, hence the observed positive GMSL anomaly.
C1 [Cazenave, A.; Henry, O.; Munier, S.; Delcroix, T.; Meyssignac, B.; Palanisamy, H.] LEGOS, OMP, F-31401 Toulouse 9, France.
[Llovel, W.] JPL, Pasadena, CA USA.
[Gordon, A. L.] Columbia Univ, LDEO, New York, NY USA.
[Becker, M.] UMR Espace DEV UAG, Cayenne, French Guiana.
RP Cazenave, A (reprint author), LEGOS, OMP, 18 Ave Edouard Belin, F-31401 Toulouse 9, France.
EM anny.cazenave@legos.obs-mip.fr
RI Delcroix, Thierry/I-6103-2016; Munier, Simon/D-3849-2011; BECKER,
Melanie/B-3658-2012; Gordon, Arnold/H-1049-2011; Meyssignac,
Benoit/O-1910-2015; LLOVEL, William/G-6930-2016
OI Delcroix, Thierry/0000-0002-8850-4865; BECKER,
Melanie/0000-0002-0263-5558; Gordon, Arnold/0000-0001-6480-6095;
FU European grant in the context of the Monarch Project; CNES; JPL/NASA;
French ANR CECILE project; National Science Foundation [OCE-0725935]
FX O. Henry, S. Munier, W. Llovel, and H. Palanisamy are supported,
respectively, by a European grant in the context of the Monarch Project,
a postdoctoral grant from CNES, a postdoctoral grant from JPL/NASA, and
the French ANR CECILE project. A. L. Gordon research is supported by the
National Science Foundation grant OCE-0725935. This is Lamont-Doherty
contribution number 7545.
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PI PHILADELPHIA
PA 520 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 0149-0419
EI 1521-060X
J9 MAR GEOD
JI Mar. Geod.
PD DEC 1
PY 2012
VL 35
SU 1
SI SI
BP 82
EP 97
DI 10.1080/01490419.2012.718209
PG 16
WC Geochemistry & Geophysics; Oceanography; Remote Sensing
SC Geochemistry & Geophysics; Oceanography; Remote Sensing
GA 066RT
UT WOS:000313238600006
ER
PT J
AU Ray, RD
Beckley, BD
AF Ray, R. D.
Beckley, B. D.
TI Calibration of Ocean Wave Measurements by the TOPEX, Jason-1, and
Jason-2 Satellites
SO MARINE GEODESY
LA English
DT Article
DE Ocean waves; satellite altimetry; significant wave height; Jason-2
validation
ID WIND-SPEED; ALTIMETER; HEIGHT; BUOY; VALIDATION; ERROR
AB The calibration and validation of ocean wave height measurements by the TOPEX, Jason-1, and Jason-2 satellite altimeters are addressed by comparing the measurements internally among themselves and against independent wave measurements at moored buoys. The two six-month verification campaigns, when two of the satellites made near-simultaneous measurements along the same ground track, show the two Jason satellites to be remarkably consistent, while Topex reports waves generally 12% larger. External calibration is complicated by some systematic errors in the buoy data. We confirm that Canadian buoys underestimate significant wave heights by about 10% relative to U.S. buoys. Wave heights from all three altimetric satellites require scaling upwards by 56% to be consistent with U.S. buoys.
C1 [Ray, R. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Beckley, B. D.] SGT Inc, Greenbelt, MD 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 U. S. National Aeronautics and Space Administration
FX This work was funded by the U. S. National Aeronautics and Space
Administration under the Ocean Surface Topography program and the
MEaSUREs program. Buoy data were obtained from the National Data Buoy
Center, a part of the National Oceanic and Atmospheric Administration,
and from Fisheries and Oceans Canada.
NR 35
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PI PHILADELPHIA
PA 520 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 0149-0419
EI 1521-060X
J9 MAR GEOD
JI Mar. Geod.
PD DEC 1
PY 2012
VL 35
SU 1
SI SI
BP 238
EP 257
DI 10.1080/01490419.2012.718611
PG 20
WC Geochemistry & Geophysics; Oceanography; Remote Sensing
SC Geochemistry & Geophysics; Oceanography; Remote Sensing
GA 066RT
UT WOS:000313238600014
ER
PT J
AU Crago, RD
Okello, W
Jasinski, MF
AF Crago, Richard D.
Okello, Winnie
Jasinski, Michael F.
TI Equations for the Drag Force and Aerodynamic Roughness Length of Urban
Areas with Random Building Heights
SO BOUNDARY-LAYER METEOROLOGY
LA English
DT Article
DE Buildings; Aerodynamic roughness length; Shear stress; Urban
ID VEGETATION; CANOPY; ARRAYS; MODEL; FLOW; DISPERSION; TURBULENCE;
OBSTACLES; SURFACES; FIELDS
AB We use a conceptual model to investigate how randomly varying building heights within a city affect the atmospheric drag forces and the aerodynamic roughness length of the city. The model is based on the assumptions regarding wake spreading and mutual sheltering effects proposed by Raupach (Boundary-Layer Meteorol 60:375-395, 1992). It is applied both to canopies having uniform building heights and to those having the same building density and mean height, but with variability about the mean. For each simulated urban area, a correction is determined, due to height variability, to the shear stress predicted for the uniform building height case. It is found that u (*)/u (*R) , where u (*) is the friction velocity and u (*R) is the friction velocity from the uniform building height case, is expressed well as an algebraic function of lambda and sigma (h) /h (m) , where lambda is the frontal area index, sigma (h) is the standard deviation of the building height, and h (m) is the mean building height. The simulations also resulted in a simple algebraic relation for z (0)/z (0R) as a function of lambda and sigma (h) /h (m) , where z (0) is the aerodynamic roughness length and z (0R) is z (0) found from the original Raupach formulation for a uniform canopy. Model results are in keeping with those of several previous studies.
C1 [Crago, Richard D.; Okello, Winnie] Bucknell Univ, Dept Civil & Environm Engn, Lewisburg, PA 17837 USA.
[Jasinski, Michael F.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
RP Crago, RD (reprint author), Bucknell Univ, Dept Civil & Environm Engn, Lewisburg, PA 17837 USA.
EM rcrago@bucknell.edu
FU National Aeronautics and Space Administration [NNX08AY39G]
FX This work was funded in part by the National Aeronautics and Space
Administration through grant number NNX08AY39G.
NR 32
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U1 1
U2 18
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0006-8314
J9 BOUND-LAY METEOROL
JI Bound.-Layer Meteor.
PD DEC
PY 2012
VL 145
IS 3
BP 423
EP 437
DI 10.1007/s10546-012-9747-0
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 027UA
UT WOS:000310378100002
ER
PT J
AU Fereres, S
Lautenberger, C
Fernandez-Pello, AC
Urban, DL
Ruff, GA
AF Fereres, Sonia
Lautenberger, Chris
Fernandez-Pello, A. Carlos
Urban, David L.
Ruff, Gary A.
TI Understanding ambient pressure effects on piloted ignition through
numerical modeling
SO COMBUSTION AND FLAME
LA English
DT Article
DE Piloted ignition; Reduced pressure; Ignition delay; Critical mass flux;
FDS
ID POLYMERIC MATERIALS; MASS FLUX
AB This work presents a numerical modeling investigation of the mechanisms controlling the dependence on ambient pressure of the piloted ignition of a solid fuel under external radiant heating. The focus is to confirm the hypotheses and phenomenological arguments generated by previous experimental studies of the problem. For this purpose, the effect of ambient pressure on the piloted ignition of thermally irradiated samples of PMMA is modeled using the Fire Dynamics Simulator (FDS5) code. Two-dimensional simulations were performed using finite-rate single-step combustion kinetics in the gas-phase and a single-step Arrhenius reaction rate for the solid phase decomposition. Oxidative pyrolysis is not considered and the in-depth formed pyrolyzate is assumed to flow unrestricted through the PMMA. The objective is to understand the thermo-physical mechanisms leading to ignition and how they may be affected by a reduction in ambient pressure. The model is able to reproduce the main physical aspects of the piloted ignition of a solid fuel and confirms previous phenomenological explanations developed to describe recent experimental results at a range of ambient pressures. Reduced pressure environments result in: (1) shorter ignition times mainly due to reduced convective heat losses from the heated material to the surroundings, allowing for the material to heat more rapidly and pyrolyze faster; (2) a lower fuel mass flux at ignition, due primarily to a thicker thermal boundary layer and a thicker fuel species profile. The appearance of a premixed flame at the pilot, its propagation through the combustible mixture above the solid surface, and the subsequent sustained burning conditions are also explored in this work. The calculated ignition times and mass loss rates at ignition are compared to those measured experimentally in a laboratory-scale combustion wind tunnel. It is shown that with appropriate kinetic parameters the model qualitatively agrees with the experimental data. (C) 2012 The Combustion Institute. Published by Elsevier Inc. All rights reserved.
C1 [Fereres, Sonia] Abengoa Res, Seville 41014, Spain.
[Lautenberger, Chris; Fernandez-Pello, A. Carlos] Univ Calif Berkeley, Dept Mech Engn, Berkeley, CA 94720 USA.
[Urban, David L.; Ruff, Gary A.] NASA John H Glenn Res Ctr, Cleveland, OH 44256 USA.
RP Fereres, S (reprint author), Abengoa Res, C Energia Solar 1, Seville 41014, Spain.
EM sonia.fereres@research.abengoa.com
FU NASA [NNX08BA77A, NNX10AE01G]
FX The authors would like to thank David Rich, Andres Osorio and Amanda
Dodd for their comments and insightful discussions. This work was
supported by NASA Grants NNX08BA77A and NNX10AE01G.
NR 28
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U1 3
U2 31
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0010-2180
J9 COMBUST FLAME
JI Combust. Flame
PD DEC
PY 2012
VL 159
IS 12
BP 3544
EP 3553
DI 10.1016/j.combustflame.2012.08.006
PG 10
WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary;
Engineering, Chemical; Engineering, Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA 031QI
UT WOS:000310656600009
ER
PT J
AU Nayagam, V
Dietrich, DL
Ferkul, PV
Hicks, MC
Williams, FA
AF Nayagam, Vedha
Dietrich, Daniel L.
Ferkul, Paul V.
Hicks, Michael C.
Williams, Forman A.
TI Can cool flames support quasi-steady alkane droplet burning?
SO COMBUSTION AND FLAME
LA English
DT Article
DE Droplet combustion; Cool flames; Alkane chemistry; Microgravity;
Extinction
ID N-HEPTANE OXIDATION; ATMOSPHERIC-PRESSURE; FUEL DROPLETS; COMBUSTION;
IGNITION; MICROGRAVITY; CONVECTION; EXTINCTION; MIXTURES
AB Experimental observations of anomalous combustion of n-heptane droplets burning in microgravity are reported. Following ignition, a relatively large n-heptane droplet first undergoes radiative extinction, that is, the visible flame ceases to exist because of radiant energy loss. But the droplet continues to experience vigorous vaporization for an extended period according to a quasi-steady droplet-burning law, ending in a secondary extinction at a finite droplet diameter, after which a vapor cloud rapidly appears surrounding the droplet. We hypothesize that the second-stage vaporization is sustained by low-temperature, soot-free, "cool-flame" chemical heat release. Measured droplet burning rates and extinction diameters are used to extract an effective heat release, overall activation energy, and pre-exponential factor for this low-temperature chemistry, and the values of the resulting parameters are found to be closer to those of "cool-flame" overall reaction-rate parameters, found in the literature, than to corresponding hot-flame parameters. (C) 2012 The Combustion Institute. Published by Elsevier Inc. All rights reserved.
C1 [Nayagam, Vedha; Ferkul, Paul V.] Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA.
[Dietrich, Daniel L.; Hicks, Michael C.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Williams, Forman A.] Univ Calif San Diego, Dept Mech & Aerosp Engn, La Jolla, CA 92093 USA.
RP Nayagam, V (reprint author), Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA.
EM v.nayagam@grc.nasa.gov
FU NASA; International Space Station
FX This work was supported by the NASA Space Life and Physical Sciences
Research and Applications Program and the International Space Station
Program. We would like to thank our other FLEX team members, C.T.
Avedisian, M.Y. Choi, F.L. Dryer, and B.D. Shaw, as well as the
reviewers for their very critical comments and N. Peters for recent
insights.
NR 27
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0010-2180
J9 COMBUST FLAME
JI Combust. Flame
PD DEC
PY 2012
VL 159
IS 12
BP 3583
EP 3588
DI 10.1016/j.combustflame.2012.07.012
PG 6
WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary;
Engineering, Chemical; Engineering, Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA 031QI
UT WOS:000310656600013
ER
PT J
AU Benafan, O
Noebe, RD
Padula, SA
Vaidyanathan, R
AF Benafan, O.
Noebe, R. D.
Padula, S. A., II
Vaidyanathan, R.
TI Microstructural Response During Isothermal and Isobaric Loading of a
Precipitation-Strengthened Ni-29.7Ti-20Hf High-Temperature Shape Memory
Alloy
SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND
MATERIALS SCIENCE
LA English
DT Article
ID SEVERE PLASTIC-DEFORMATION; ACQUIRED IN-SITU; DIFFRACTION SPECTRA;
RIETVELD REFINEMENT; CYCLIC REVERSIBILITY; TRANSFORMATION; MARTENSITE;
PHASE; BEHAVIOR; STRAIN
AB A stable Ni-rich Ni-29.7Ti-20Hf (at. pct) shape memory alloy, with relatively high transformation temperatures, was shown to exhibit promising properties at lower raw material cost when compared to typical NiTi-X (X = Pt, Pd, Au) high-temperature shape memory alloys (HTSMAs). The excellent dimensional stability and high work output for this alloy were attributed to a coherent, nanometer size precipitate phase observed using transmission electron microscopy. To establish an understanding of the role of these precipitates on the microstructure and ensuing stability of the NiTiHf alloy, a detailed study of the micromechanical and microstructural behaviors was performed. In-situ neutron diffraction at stress and temperature was used to obtain quantitative information on phase-specific internal strain, texture, and phase volume fractions during both isothermal and isobaric testing of the alloy. During isothermal testing, the alloy exhibited low isothermal strains due to limited detwinning, consistent with direct measurements of the bulk texture through neutron diffraction. This limited detwinning was attributed to the pinning of twin and variant boundaries by the dispersion of fine precipitates. During isobaric thermal cycling at 400 MPa, the high work output and near-perfect dimensional stability was attributed to the presence of the precipitates that act as homogeneous sources for the nucleation of martensite throughout the material, while providing resistance to irrecoverable processes such as plastic deformation.
C1 [Vaidyanathan, R.] Univ Cent Florida, Mech Mat & Aerosp Engn Dept, Adv Mat Proc & Anal Ctr AMPAC, Orlando, FL 32816 USA.
[Noebe, R. D.; Padula, S. A., II] Univ Cent Florida, Mech Mat & Aerosp Engn Dept, Adv Mat Proc & Anal Ctr AMPAC, Orlando, FL 32816 USA.
RP Benafan, O (reprint author), NASA Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
EM raj@ucf.edu
FU NASA Fundamental Aeronautics Program, Supersonics Project [NNX08A-B51A];
Office of Basic Energy Sciences, United States Department of Energy; Los
Alamos National Security LLC under the United States Department of
Energy [DE-AC52-06NA25396]
FX Funding from the NASA Fundamental Aeronautics Program, Supersonics
Project (Grant No. NNX08A-B51A), is gratefully acknowledged. The authors
thank D. W. Brown, B. Clausen, and T. Sisneros (LANL) and D. Gaydosh, G.
Bigelow, and A. Garg (NASA GRC) for technical support and helpful
discussions. D. E. Nicholson's help in performing the neutron
diffraction experiments is gratefully acknowledged. This work benefited
from the use of the Lujan Neutron Scattering Center, LANSCE, which is
funded by the Office of Basic Energy Sciences, United States Department
of Energy. LANL is operated by Los Alamos National Security LLC under
the United States Department of Energy Contract No. DE-AC52-06NA25396.
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U1 2
U2 30
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1073-5623
J9 METALL MATER TRANS A
JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci.
PD DEC
PY 2012
VL 43A
IS 12
BP 4539
EP 4552
DI 10.1007/s11661-012-1297-z
PG 14
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA 022FH
UT WOS:000309940500013
ER
PT J
AU Padula, S
Qiu, SP
Gaydosh, D
Noebe, R
Bigelow, G
Garg, A
Vaidyanathan, R
AF Padula, Santo, II
Qiu, Shipeng
Gaydosh, Darrell
Noebe, Ronald
Bigelow, Glen
Garg, Anita
Vaidyanathan, Raj
TI Effect of Upper-Cycle Temperature on the Load-Biased, Strain-Temperature
Response of NiTi
SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND
MATERIALS SCIENCE
LA English
DT Article
ID SHAPE-MEMORY ALLOY; NEUTRON-DIFFRACTION; SUPERELASTIC NITI; IN-SITU;
STRESS; TRANSFORMATION; TEXTURE
AB Over the past decade, interest in shape-memory-alloy based actuators has increased as the primary benefits of these solid-state devices have become more apparent. However, much is still unknown about the characteristic behavior of these materials when used in actuator applications. Recently, we showed that the maximum temperature reached during thermal cycling under isobaric conditions could significantly affect the observed mechanical response of NiTi (55 wt pct Ni), especially the amount of transformation strain available for actuation and thus work output. The investigation we report here extends that original work to (1) ascertain whether increases in the upper-cycle temperature would produce additional changes in the work output of the material, which has a stress-free austenite finish temperature of 386 K (113 A degrees C), and (2) determine the optimum cyclic conditions. Thus, isobaric, thermal-cycle experiments were conducted on the aforementioned alloy at various stresses from 50 to 300 MPa using upper-cycle temperatures of 438 K, 473 K, 503 K, 533 K, 563 K, 593 K, and 623 K (165 A degrees C, 200 A degrees C, 230 A degrees C, 260 A degrees C, 290 A degrees C, 320 A degrees C, and 350 A degrees C). The data indicated that the amount of applied stress influenced the transformation strain, as would be expected. However, the maximum temperature reached during the thermal excursion also plays an equally significant role in determining the transformation strain, with the maximum transformation strain observed during thermal cycling to 563 K (290 A degrees C). In situ neutron diffraction at stress and temperature showed that the differences in transformation strain were mostly related to changes in martensite texture when cycling to different upper-cycle temperatures. Hence, understanding this effect is important to optimizing the operation of SMA-based actuators and could lead to new methods for processing and training shape-memory alloys for optimal performance.
C1 [Padula, Santo, II; Noebe, Ronald; Bigelow, Glen] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Qiu, Shipeng; Vaidyanathan, Raj] Univ Cent Florida, Orlanda, FL 32816 USA.
[Gaydosh, Darrell] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Garg, Anita] Univ Toledo, Toledo, OH 43606 USA.
RP Padula, S (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Santo.A.Padula@nasa.gov
FU Fundamental Aeronautics Program, Supersonics Project,; Office of Basic
Energy Sciences (DOE); Los Alamos National Security LLC under DOE
[DE-AC52-06NA25396]
FX This work was supported by the Fundamental Aeronautics Program,
Supersonics Project, API: Dale Hopkins. The authors thank B. Clausen, D.
Brown, and T. Sisneros at Los Alamos National Laboratory for
experimental assistance. This work has benefited from the use of the
Lujan Neutron Scattering Center at LANSCE, which is funded by the Office
of Basic Energy Sciences (DOE). LANL is operated by Los Alamos National
Security LLC under DOE Contract DE-AC52-06NA25396.
NR 20
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U1 0
U2 6
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1073-5623
J9 METALL MATER TRANS A
JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci.
PD DEC
PY 2012
VL 43A
IS 12
BP 4610
EP 4621
DI 10.1007/s11661-012-1267-5
PG 12
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA 022FH
UT WOS:000309940500018
ER
PT J
AU Van Hoose, JR
Grugel, RN
Tewari, SN
Brush, LN
Erdmann, RG
Poirier, DR
AF Van Hoose, J. R.
Grugel, R. N.
Tewari, S. N.
Brush, L. N.
Erdmann, R. G.
Poirier, D. R.
TI Observation of Misoriented Tertiary Dendrite Arms During Controlled
Directional Solidification in Aluminum-7 Wt pct Silicon Alloys
SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND
MATERIALS SCIENCE
LA English
DT Article
ID SINGLE-CRYSTAL SUPERALLOYS; CELLULAR ARRAY GROWTH; ZONE RAYLEIGH NUMBER;
AL-SI ALLOYS; PB-SN ALLOYS; IN-SITU; NUMERICAL-ANALYSIS; METALLIC
ALLOYS; MACROSEGREGATION; CU
AB Electron backscattered diffraction (EBSD) examination of transverse cross sections from a directionally solidified aluminum-7 wt pct silicon alloy revealed tertiary dendrite arms that appeared in place but in reality had orientations that significantly differed from their parent arm. The maximum extent of spuriously orientated arms occurred at an intermediate growth velocity and was more pronounced at subgrain boundaries that separated uniquely oriented dendritic arrays. Mechanisms for tertiary arm misorientations are discussed, and attention is called to the practical consequences of these in-situ defects.
C1 [Van Hoose, J. R.] Qualis Corp, Huntsville, AL 35806 USA.
[Grugel, R. N.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Tewari, S. N.] Cleveland State Univ, Chem & Biomed Engn Dept, Cleveland, OH 44115 USA.
[Brush, L. N.] Univ Washington, Dept Mat Sci & Engn, Seattle, WA 98195 USA.
[Erdmann, R. G.; Poirier, D. R.] Univ Arizona, Dept Mat Sci & Engn, Tucson, AZ 85721 USA.
RP Van Hoose, JR (reprint author), Siemens Corp, Orlando, FL 32826 USA.
EM Richard.N.Grugel@nasa.gov
FU NASA [NNX08AN49G]; Marshall Space Flight Center's Materials and
Processing Laboratory
FX The authors are grateful to Dr. Men G. Chu, Technical
Fellow-Solidification Technology, Alcoa Technical Center, for providing
the Al-7 wt pct Si as-cast feed bars. This research was supported, in
part, by NASA Grant No. NNX08AN49G. The support of the Marshall Space
Flight Center's Materials and Processing Laboratory is also gratefully
acknowledged.
NR 35
TC 1
Z9 1
U1 4
U2 26
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1073-5623
J9 METALL MATER TRANS A
JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci.
PD DEC
PY 2012
VL 43A
IS 12
BP 4724
EP 4731
DI 10.1007/s11661-012-1260-z
PG 8
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA 022FH
UT WOS:000309940500028
ER
PT J
AU Knight, GA
Hou, TH
Belcher, MA
Palmieri, FL
Wohl, CJ
Connell, JW
AF Knight, G. A.
Hou, T. H.
Belcher, M. A.
Palmieri, F. L.
Wohl, C. J.
Connell, J. W.
TI Hygrothermal aging of composite single lap shear specimens comprised of
AF-555M adhesive and T800H/3900-2 adherends
SO INTERNATIONAL JOURNAL OF ADHESION AND ADHESIVES
LA English
DT Article
DE AF-555M adhesive; T800H/3900-2 adherends; Temperature/humidity aging;
Composite lap shear specimens; Peel-ply surface treatment; Adhesion
failure mode analysis
AB Fiber reinforced resin matrix composites and structural adhesives have found increased usage on commercial and military aircraft. These structural materials offer weight savings without sacrificing strength and mechanical performance. Since service history and long-term aging performance of these relatively new material systems are not well established, a long-term environmental aging study was undertaken. Adhesive bonds were prepared by secondary bonding of 3M(TM) Scotch-Weld(TM) AF-555M between pre-cured, unidirectional composite adherends comprised of Toray(TM) T800H/3900-2 prepreg. Single lap shear specimens (SLS) were fabricated and subsequently aged in an unstressed configuration at 82 degrees C (180 degrees F) and 85% relative humidity for up to 772 days. The aging conditions are more severe than those expected to occur in service and were selected in order to observe some changes within a reasonable exposure time. The apparent shear strengths were measured periodically at both room temperature and 82 degrees C (180 degrees F), and failure modes were determined and compared to control specimens that had been stored for equal periods of time at room temperature under low humidity. With hygrothermal aging, apparent shear strengths decreased and some changes in the failure mode were observed relative to those of the control specimens. However, in spite of the severe aging conditions, no adhesive failures indicative of interfacial failures were observed. SLS specimens that were hygrothermally aged, subsequently dried, and then tested did not exhibit complete recovery of unaged apparent shear strengths indicating some irreversible changes. Published by Elsevier Ltd.
C1 [Knight, G. A.; Hou, T. H.; Wohl, C. J.; Connell, J. W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Belcher, M. A.] Boeing Co, Seattle, WA 98124 USA.
[Belcher, M. A.; Palmieri, F. L.] Natl Inst Aerosp, Hampton, VA 23666 USA.
RP Connell, JW (reprint author), NASA, Langley Res Ctr, 6 W Taylor St,MS 226, Hampton, VA 23681 USA.
EM john.w.connell@nasa.gov
NR 10
TC 8
Z9 8
U1 1
U2 22
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0143-7496
J9 INT J ADHES ADHES
JI Int. J. Adhes. Adhes.
PD DEC
PY 2012
VL 39
BP 1
EP 7
DI 10.1016/j.ijadhadh.2012.06.009
PG 7
WC Engineering, Chemical; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 018EW
UT WOS:000309643900001
ER
PT J
AU Lloyd, CW
AF Lloyd, Charles W.
TI IAC-11.E1-7.-A1.8.5 The Mission X: Train Like an Astronaut pilot study
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Education; Astronaut training; Health; Fitness; Obesity; Mission X
ID BODY-MASS INDEX; EARLY PHYSICAL-ACTIVITY; CHILDHOOD OBESITY; US
CHILDREN; ADOLESCENTS; PREVENTION; PREVALENCE
AB Mission X: Train Like an Astronaut is an international educational challenge focusing on fitness and nutrition as we encourage students to "train like an astronaut." Teams of students (aged 8-12) learn principles of healthy eating and exercise, compete for points by finishing training modules, and get excited about their future as "fit explorers." The 18 core exercises (targeting strength, endurance, coordination, balance, spatial awareness, and more) involve the same types of skills that astronauts learn in their training and use in spaceflight. This first-of-its-kind cooperative outreach program has allowed 11 space agencies and various partner institutions to work together to address quality health/fitness education, challenge students to be more physically active, increase awareness of the importance of lifelong health and fitness, teach students how fitness plays a vital role in human performance for exploration, and to inspire and motivate students to pursue careers in science, technology, engineering and math (STEM) fields. The project was initiated in 2009 in response to a request by the International Space Life Sciences Working Group. USA, Netherlands, Italy, France, Germany, Austria, Colombia, Spain, Belgium, Czech Republic and United Kingdom hosted teams for the pilot in the spring of 2010, and Japan held a modified version of the challenge. Several more agencies provided input into the preparations. Competing in 137 teams, more than 4000 students from over 40 cities worldwide participated in the first round of Mission X. Published by Elsevier Ltd.
C1 NASA, Houston, TX 77058 USA.
RP Lloyd, CW (reprint author), NASA, Houston, TX 77058 USA.
EM charles.w.lloyd@nasa.gov
NR 17
TC 3
Z9 3
U1 3
U2 23
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 DEC
PY 2012
VL 81
BP 77
EP 82
DI 10.1016/j.actaastro.2012.07.010
PG 6
WC Engineering, Aerospace
SC Engineering
GA 017CY
UT WOS:000309568900010
ER
PT J
AU Gehrels, N
Cannizzo, JK
AF Gehrels, N.
Cannizzo, J. K.
TI IAC-11.A7.2.1: Gamma-ray astronomy technology needs
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Gamma rays; General; Telescopes; Bursts; Blazars; Galactic transients
ID EXPERIMENT TELESCOPE EGRET; ACTIVE GALACTIC NUCLEI; LARGE-AREA
TELESCOPE; MISSION; CATALOG
AB In recent decades gamma-ray observations have become a valuable tool for studying the universe. Progress made in diverse areas such as gamma-ray bursts (GRBs), nucleosynthesis, and active galactic nuclei (AGNs) has complemented and enriched our astrophysical understanding in many ways. We present an overview of current and future planned space gamma-ray missions and discuss technology needs for the next generation of space gamma-ray instruments. (c) 2012 Elsevier Ltd. All rights reserved.
C1 [Cannizzo, J. K.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, JCA,CRESST,UMBC, Greenbelt, MD 20771 USA.
RP Cannizzo, JK (reprint author), NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, JCA,CRESST,UMBC, Greenbelt, MD 20771 USA.
EM neil.gehrels@nasa.gov; john.k.cannizzo@nasa.gov
NR 21
TC 0
Z9 0
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD DEC
PY 2012
VL 81
BP 83
EP 91
DI 10.1016/j.actaastro.2012.06.005
PG 9
WC Engineering, Aerospace
SC Engineering
GA 017CY
UT WOS:000309568900011
ER
PT J
AU Lee, D
Tippur, H
Bogert, P
AF Lee, Dongyeon
Tippur, Hareesh
Bogert, Phillip
TI Dynamic fracture of graphite/epoxy composites stiffened by buffer
strips: An experimental study
SO COMPOSITE STRUCTURES
LA English
DT Article
DE Graphite/epoxy; PETI-5/IM7; Stiffener; Dynamic fracture; Impact loading;
Digital image correlation
ID INDUCED LAMINATE FAILURE; IMAGE CORRELATION METHOD; HIGH-SPEED
PHOTOGRAPHY; CRACK
AB Fracture responses of unidirectional graphite/epoxy composite coupons enhanced by buffer strips are investigated under impact loading conditions using digital image correlation technique and high-speed photography. Composite coupons made of phenylethynyl terminated imide oligomer (PETI-5) as matrix and IM7 graphite fiber as reinforcement are studied. Buffer strips are made of the same material but with a different stacking sequence to attain quasi-isotropy. Edge-notched coupons are subjected to impact loading along the axis of symmetry. The effectiveness of methods used for attaching the buffer strip, namely, co-curing at elevated temperatures and adhesive bonding at room temperature, are also examined. The optically measured stress intensity factor histories reveal that both methods provide nearly identical fracture responses. However, the crack initiates much later in coupons stiffened using adhesive bonding method than its co-cured counterpart and thus shows higher stress intensity factor at initiation. The residual stresses are shown to be responsible for the difference in the fracture responses. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Lee, Dongyeon; Tippur, Hareesh] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
[Bogert, Phillip] NASA, Langley Res Ctr, Hampton, VA USA.
RP Tippur, H (reprint author), Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
EM htippur@eng.auburn.edu
FU NASA-LaRC [NNX07AC64B]
FX This research was sponsored by the NASA-LaRC under cooperative agreement
No. NNX07AC64B.
NR 22
TC 2
Z9 5
U1 0
U2 9
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 DEC
PY 2012
VL 94
IS 12
BP 3538
EP 3545
DI 10.1016/j.compstruct.2012.05.032
PG 8
WC Materials Science, Composites
SC Materials Science
GA 995XZ
UT WOS:000308049900012
ER
PT J
AU Delcourt, DC
Seki, K
Terada, N
Moore, TE
AF Delcourt, D. C.
Seki, K.
Terada, N.
Moore, T. E.
TI Centrifugally stimulated exospheric ion escape at Mercury
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MESSENGER OBSERVATIONS; ACCELERATION; FIELD; MODEL; MAGNETOSPHERE;
IONOSPHERE
AB We investigate the transport of ions in the low-altitude magnetosphere of Mercury. We show that, because of small spatial scales, the centrifugal effect due to curvature of the E X B drift paths can lead to significant particle energization in the parallel direction. We demonstrate that because of this effect, ions with initial speed smaller than the escape speed such as those produced via thermal desorption can overcome gravity and escape into the magnetosphere. The escape route of this low-energy exosphere originating material is largely controlled by the magnetospheric convection rate. This escape route spreads over a narrower range of altitudes when the convection rate increases. Bulk transport of low-energy planetary material thus occurs within a limited region of space once moderate magnetospheric convection is established. These results suggest that, via release of material otherwise gravitationally trapped, the E X B related centrifugal acceleration is an important mechanism for the net supply of plasma to the magnetosphere of Mercury. Citation: Delcourt, D. C., K. Seki, N. Terada, and T. E. Moore (2012), Centrifugally stimulated exospheric ion escape at Mercury, Geophys. Res. Lett., 39, L22105, doi:10.1029/2012GL054085.
C1 [Delcourt, D. C.] CNRS, LPP, FR-94107 St Maur Des Fosses, France.
[Seki, K.] Nagoya Univ, STELAB, Nagoya, Aichi 4648601, Japan.
[Terada, N.] Tohoku Univ, Dept Geophys, Sendai, Miyagi 980, Japan.
[Moore, T. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Delcourt, DC (reprint author), CNRS, LPP, 4 Ave Neptune, FR-94107 St Maur Des Fosses, France.
EM dominique.delcourt@lpp.polytechnique.fr
RI Moore, Thomas/D-4675-2012
OI Moore, Thomas/0000-0002-3150-1137
NR 20
TC 4
Z9 4
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD NOV 30
PY 2012
VL 39
AR L22105
DI 10.1029/2012GL054085
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 047LH
UT WOS:000311841800007
ER
PT J
AU Rodriguez, JAP
Bourke, M
Tanaka, KL
Miyamoto, H
Kargel, J
Baker, V
Fairen, AG
Davies, RJ
Bridget, L
Santiago, RL
Hernandez, MZ
Berman, DC
AF Rodriguez, J. A. P.
Bourke, Mary
Tanaka, Kenneth L.
Miyamoto, Hideaki
Kargel, Jeffrey
Baker, Victor
Fairen, Alberto G.
Davies, Richard J.
Bridget, Lynne
Linares Santiago, Rogelio
Zarroca Hernandez, Mario
Berman, Daniel C.
TI Infiltration of Martian outflow channel floodwaters into lowland
cavernous systems
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SOUTH CASPIAN BASIN; NORTHERN PLAINS; MUD VOLCANISM; MARS;
GEOMORPHOLOGY; EMPLACEMENT; RELEASE; HISTORY; OCEAN; WATER
AB The hydrosphere of Mars has remained mostly concealed within the subsurface for the past similar to 3.5 Gyr. Localized rupturing of the permafrost-capped crust led to voluminous groundwater discharges that carved some of the largest known channels in the solar system. However, our knowledge of the nature of the flows and their ultimate fate remains incomplete, partly because diagnostic landforms at outflow channel termini have been largely destroyed or buried. The Hebrus Valles outflow channels were excavated by fluid discharges that emanated from two point sources, and they mostly terminate in systems of fractures and depressions within the northern plains. Our investigation indicates that outflow channel floodwaters were captured and reabsorbed into the subsurface in zones where caverns developed within the northern plains. These findings imply that the study region comprises the only known location in the Martian northern lowlands where the fate of outflow channel discharges can be assessed with confidence. We propose that evacuation of subsurface materials via mud volcanism was an important process in cavern formation. Our conceptual model provides a hypothesis to account for the fate of sediments and fluids from some of the Martian outflow channels. It also reveals a mechanism for lowland cavern formation and upper crustal volatile enrichment after the development of the Martian global cryosphere. Citation: Rodriguez, J. A. P., et al. (2012), Infiltration of Martian outflow channel floodwaters into lowland cavernous systems, Geophys. Res. Lett., 39, L22201, doi: 10.1029/2012GL053225.
C1 [Rodriguez, J. A. P.; Bourke, Mary; Berman, Daniel C.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Bourke, Mary] Trinity Coll Dublin, Dept Geog, Dublin, Ireland.
[Tanaka, Kenneth L.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Miyamoto, Hideaki] Univ Tokyo, Univ Museum, Tokyo 1138654, Japan.
[Kargel, Jeffrey; Baker, Victor] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
[Fairen, Alberto G.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Davies, Richard J.] Univ Durham, Dept Earth Sci, Ctr Res Earth Energy Syst, Durham, England.
[Bridget, Lynne] Univ Auckland, Inst Earth Sci & Engn, Auckland 1, New Zealand.
[Linares Santiago, Rogelio; Zarroca Hernandez, Mario] Univ Autonoma Barcelona, Dept Geol, Unitat Geodinam Externa & Hidrogeol, E-08193 Barcelona, Spain.
RP Rodriguez, JAP (reprint author), Planetary Sci Inst, 1700 E Ft Lowell Rd,Ste 106, Tucson, AZ 85719 USA.
EM alexis@psi.edu
RI Miyamoto, Hideaki/B-9666-2008; Bourke, Mary/I-4387-2012;
OI Bourke, Mary/0000-0002-0424-0322; Zarroca, Mario/0000-0001-6907-1892
NR 47
TC 3
Z9 3
U1 0
U2 17
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 NOV 30
PY 2012
VL 39
AR L22201
DI 10.1029/2012GL053225
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 047LH
UT WOS:000311841800001
ER
PT J
AU Shepherd, A
Ivins, ER
Geruo, A
Barletta, VR
Bentley, MJ
Bettadpur, S
Briggs, KH
Bromwich, DH
Forsberg, R
Galin, N
Horwath, M
Jacobs, S
Joughin, I
King, MA
Lenaerts, JTM
Li, JL
Ligtenberg, SRM
Luckman, A
Luthcke, SB
McMillan, M
Meister, R
Milne, G
Mouginot, J
Muir, A
Nicolas, JP
Paden, J
Payne, AJ
Pritchard, H
Rignot, E
Rott, H
Sorensen, LS
Scambos, TA
Scheuchl, B
Schrama, EJO
Smith, B
Sundal, AV
van Angelen, JH
van de Berg, WJ
van den Broeke, MR
Vaughan, DG
Velicogna, I
Wahr, J
Whitehouse, PL
Wingham, DJ
Yi, DH
Young, D
Zwally, HJ
AF Shepherd, Andrew
Ivins, Erik R.
Geruo, A.
Barletta, Valentina R.
Bentley, Mike J.
Bettadpur, Srinivas
Briggs, Kate H.
Bromwich, David H.
Forsberg, Rene
Galin, Natalia
Horwath, Martin
Jacobs, Stan
Joughin, Ian
King, Matt A.
Lenaerts, Jan T. M.
Li, Jilu
Ligtenberg, Stefan R. M.
Luckman, Adrian
Luthcke, Scott B.
McMillan, Malcolm
Meister, Rakia
Milne, Glenn
Mouginot, Jeremie
Muir, Alan
Nicolas, Julien P.
Paden, John
Payne, Antony J.
Pritchard, Hamish
Rignot, Eric
Rott, Helmut
Sorensen, Louise Sandberg
Scambos, Ted A.
Scheuchl, Bernd
Schrama, Ernst J. O.
Smith, Ben
Sundal, Aud V.
van Angelen, Jan H.
van de Berg, Willem J.
van den Broeke, Michiel R.
Vaughan, David G.
Velicogna, Isabella
Wahr, John
Whitehouse, Pippa L.
Wingham, Duncan J.
Yi, Donghui
Young, Duncan
Zwally, H. Jay
TI A Reconciled Estimate of Ice-Sheet Mass Balance
SO SCIENCE
LA English
DT Article
ID PINE ISLAND GLACIER; RELATIVE SEA-LEVEL; ANTARCTIC PENINSULA; WEST
ANTARCTICA; ISOSTATIC-ADJUSTMENT; OCEAN CIRCULATION; ELEVATION CHANGE;
GREENLAND; MODEL; SHELF
AB We combined an ensemble of satellite altimetry, interferometry, and gravimetry data sets using common geographical regions, time intervals, and models of surface mass balance and glacial isostatic adjustment to estimate the mass balance of Earth's polar ice sheets. We find that there is good agreement between different satellite methods-especially in Greenland and West Antarctica-and that combining satellite data sets leads to greater certainty. Between 1992 and 2011, the ice sheets of Greenland, East Antarctica, West Antarctica, and the Antarctic Peninsula changed in mass by -142 +/- 49, +14 +/- 43, -65 +/- 26, and -20 +/- 14 gigatonnes year(-1), respectively. Since 1992, the polar ice sheets have contributed, on average, 0.59 +/- 0.20 millimeter year(-1) to the rate of global sea-level rise.
C1 [Shepherd, Andrew; Briggs, Kate H.; Sundal, Aud V.] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England.
[Ivins, Erik R.; Velicogna, Isabella] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Geruo, A.; Wahr, John] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Barletta, Valentina R.; Forsberg, Rene; Sorensen, Louise Sandberg] Tech Univ Denmark, DTU SPACE, Geodynam Dept, Natl Space Inst, DK-2880 Lyngby, Denmark.
[Bentley, Mike J.; Whitehouse, Pippa L.] Univ Durham, Dept Geog, Durham DH1 3LE, England.
[Bettadpur, Srinivas] Univ Texas Austin, Ctr Space Res, Austin, TX 78759 USA.
[Bromwich, David H.; Nicolas, Julien P.] Ohio State Univ, Byrd Polar Res Ctr, Polar Meteorol Grp, Columbus, OH 43210 USA.
[Bromwich, David H.; Nicolas, Julien P.] Ohio State Univ, Dept Geog, Atmospher Sci Program, Columbus, OH 43210 USA.
[Galin, Natalia; Meister, Rakia; Muir, Alan; Wingham, Duncan J.] UCL, Dept Earth Sci, Ctr Polar Observat & Modelling, London WC1E 6BT, England.
[Horwath, Martin] Tech Univ Munich, Inst Astron & Phys Geodasie, D-80333 Munich, Germany.
[Jacobs, Stan] Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Joughin, Ian; Smith, Ben] Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA.
[King, Matt A.] Newcastle Univ, Sch Civil Engn & Geosci, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England.
[Lenaerts, Jan T. M.; Ligtenberg, Stefan R. M.; van Angelen, Jan H.; van de Berg, Willem J.; van den Broeke, Michiel R.] Univ Utrecht, Inst Marine & Atmospher Res, Utrecht, Netherlands.
[Li, Jilu; Paden, John] Univ Kansas, Ctr Remote Sensing Ice Sheets, Lawrence, KS 66045 USA.
[Luckman, Adrian] Swansea Univ, Coll Sci, Dept Geog, Swansea SA2 8PP, W Glam, Wales.
[Luthcke, Scott B.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Milne, Glenn] Univ Ottawa, Dept Earth Sci, Ottawa, ON K1N 6N5, Canada.
[Mouginot, Jeremie; Rignot, Eric; Velicogna, Isabella] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Payne, Antony J.] Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England.
[Pritchard, Hamish; Vaughan, David G.] British Antarctic Survey, Cambridge CB3 0ET, England.
[Rott, Helmut] Univ Innsbruck, Inst Meteorol & Geophys, A-6020 Innsbruck, Austria.
[Scambos, Ted A.] Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA.
[Schrama, Ernst J. O.] Delft Univ Technol, Fac Aerosp Engn, NL-2629 HS Delft, Netherlands.
[Yi, Donghui] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, SGT Inc, Greenbelt, MD 20771 USA.
[Young, Duncan] Univ Texas Austin, Inst Geophys, Austin, TX 78759 USA.
[Zwally, H. Jay] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA.
[King, Matt A.] Univ Tasmania, Sch Geog & Environm Studies, Hobart, Tas 7001, Australia.
RP Shepherd, A (reprint author), Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England.
EM ashepherd@leeds.ac.uk; erik.r.ivins@jpl.nasa.gov
RI Bentley, Michael/F-7386-2011; King, Matt/B-4622-2008; payne,
antony/A-8916-2008; Horwath, Martin/F-9239-2011; van de Berg, Willem
Jan/H-4385-2011; Vaughan, David/C-8348-2011; Joughin, Ian/A-2998-2008;
Rignot, Eric/A-4560-2014; Van den Broeke, Michiel/F-7867-2011; Sorensen,
Louise/E-5282-2014; Young, Duncan/G-6256-2010; McMillan,
Malcolm/K-7712-2014; Bettadpur, Srinivas/M-3744-2014; Lenaerts,
Jan/D-9423-2012; Mouginot, Jeremie/G-7045-2015; Bromwich,
David/C-9225-2016
OI Bentley, Michael/0000-0002-2048-0019; King, Matt/0000-0001-5611-9498;
Luckman, Adrian/0000-0002-9618-5905; Whitehouse,
Pippa/0000-0002-9092-3444; payne, antony/0000-0001-8825-8425; Horwath,
Martin/0000-0001-5797-244X; Joughin, Ian/0000-0001-6229-679X; Rignot,
Eric/0000-0002-3366-0481; Van den Broeke, Michiel/0000-0003-4662-7565;
Sorensen, Louise/0000-0002-3771-4061; Young, Duncan/0000-0002-6866-8176;
Lenaerts, Jan/0000-0003-4309-4011;
FU Phillip Leverhulme Prize award; European Union [125]; NASA [NNX09AE47G,
NNX08AD64G]; Netherlands Organization for Scientific Research;
Netherlands Polar Program; UK Natural Environment Research Council; NSF;
Lamont Doherty Earth Observatory
FX This Ice Sheet Mass Balance Exercise (IMBIE) was facilitated by the
European Space Agency and NASA and by a Phillip Leverhulme Prize awarded
to A. S. The work was additionally supported by the European Union
Framework Programme 7 ice2sea program (ice2sea publication 125), the
Lamont Doherty Earth Observatory, NASA (grants NNX09AE47G and
NNX08AD64G), the Netherlands Organization for Scientific Research, the
Netherlands Polar Program, the UK Natural Environment Research Council,
and the NSF. Antarctic glacier ice thickness data used in the IOM
calculations were acquired by NASA IceBridge and the Centro de Estudios
Cientifico Chile, and additional estimates were provided by J. Bamber
and J. Griggs. E. van Meijgaard provided assistance with the RACMO
model.
NR 93
TC 475
Z9 479
U1 29
U2 410
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 NOV 30
PY 2012
VL 338
IS 6111
BP 1183
EP 1189
DI 10.1126/science.1228102
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 045AL
UT WOS:000311666200039
PM 23197528
ER
PT J
AU Ackermann, M
Ajello, M
Allafort, A
Schady, P
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bellazzini, R
Blandford, RD
Bloom, ED
Borgland, AW
Bottacini, E
Bouvier, A
Bregeon, J
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Cavazzuti, E
Cecchi, C
Charles, E
Chaves, RCG
Chekhtman, A
Cheung, CC
Chiang, J
Chiaro, G
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Cutini, S
D'Ammando, F
de Palma, F
Dermer, CD
Digel, SW
Silva, EDE
Domnguez, A
Drell, PS
Drlica-Wagner, A
Favuzzi, C
Fegan, SJ
Focke, WB
Franckowiak, A
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Grove, JE
Guiriec, S
Gustafsson, M
Hadasch, D
Hayashida, M
Hays, E
Jackson, MS
Jogler, T
Kataoka, J
Knodlseder, J
Kuss, M
Lande, J
Larsson, S
Latronico, L
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Mazziotta, MN
McEnery, JE
Mehault, J
Michelson, PF
Mizuno, T
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Tramacere, A
Nuss, E
Greiner, J
Ohno, M
Ohsugi, T
Omodei, N
Orienti, M
Orlando, E
Ormes, JF
Paneque, D
Perkins, JS
Pesce-Rollins, M
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Razzaque, S
Reimer, A
Reimer, O
Reyes, LC
Ritz, S
Rau, A
Romoli, C
Roth, M
Sanchez-Conde, M
Sanchez, DA
Scargle, JD
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Stawarz, L
Suson, DJ
Takahashi, H
Tanaka, T
Thayer, JG
Thompson, DJ
Tibaldo, L
Tinivella, M
Torres, DF
Tosti, G
Troja, E
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Waite, AP
Winer, BL
Wood, KS
Wood, M
AF Ackermann, M.
Ajello, M.
Allafort, A.
Schady, P.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bellazzini, R.
Blandford, R. D.
Bloom, E. D.
Borgland, A. W.
Bottacini, E.
Bouvier, A.
Bregeon, J.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Cavazzuti, E.
Cecchi, C.
Charles, E.
Chaves, R. C. G.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Chiaro, G.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Cutini, S.
D'Ammando, F.
de Palma, F.
Dermer, C. D.
Digel, S. W.
do Couto e Silva, E.
Domnguez, A.
Drell, P. S.
Drlica-Wagner, A.
Favuzzi, C.
Fegan, S. J.
Focke, W. B.
Franckowiak, A.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Grove, J. E.
Guiriec, S.
Gustafsson, M.
Hadasch, D.
Hayashida, M.
Hays, E.
Jackson, M. S.
Jogler, T.
Kataoka, J.
Knoedlseder, J.
Kuss, M.
Lande, J.
Larsson, S.
Latronico, L.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Mazziotta, M. N.
McEnery, J. E.
Mehault, J.
Michelson, P. F.
Mizuno, T.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Tramacere, A.
Nuss, E.
Greiner, J.
Ohno, M.
Ohsugi, T.
Omodei, N.
Orienti, M.
Orlando, E.
Ormes, J. F.
Paneque, D.
Perkins, J. S.
Pesce-Rollins, M.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Razzaque, S.
Reimer, A.
Reimer, O.
Reyes, L. C.
Ritz, S.
Rau, A.
Romoli, C.
Roth, M.
Sanchez-Conde, M.
Sanchez, D. A.
Scargle, J. D.
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Stawarz, Lukasz
Suson, D. J.
Takahashi, H.
Tanaka, T.
Thayer, J. G.
Thompson, D. J.
Tibaldo, L.
Tinivella, M.
Torres, D. F.
Tosti, G.
Troja, E.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Waite, A. P.
Winer, B. L.
Wood, K. S.
Wood, M.
TI The Imprint of the Extragalactic Background Light in the Gamma-Ray
Spectra of Blazars
SO SCIENCE
LA English
DT Article
ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; 1ST STARS;
RADIATIVE-TRANSFER; UNIVERSE; ABSORPTION; REDSHIFT; OPACITY; FIELDS;
GLAST
AB The light emitted by stars and accreting compact objects through the history of the universe is encoded in the intensity of the extragalactic background light (EBL). Knowledge of the EBL is important to understand the nature of star formation and galaxy evolution, but direct measurements of the EBL are limited by galactic and other foreground emissions. Here, we report an absorption feature seen in the combined spectra of a sample of gamma-ray blazars out to a redshift of z similar to 1.6. This feature is caused by attenuation of gamma rays by the EBL at optical to ultraviolet frequencies and allowed us to measure the EBL flux density in this frequency band.
C1 [Ajello, M.; Allafort, A.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Jogler, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Tanaka, T.; Thayer, J. G.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Ajello, M.; Allafort, A.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Jogler, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Tanaka, T.; Thayer, J. G.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Schady, P.; Greiner, J.; Rau, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Baldini, L.] Univ Pisa, I-56127 Pisa, Italy.
[Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Chaves, R. C. G.; Grenier, I. A.] Univ Paris Diderot, CNRS, CEA IRFU, Lab AIM,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Gustafsson, M.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Pivato, G.; Rando, R.; Romoli, C.; Tibaldo, L.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Bouvier, A.; Domnguez, A.; Porter, T. A.; Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Bouvier, A.; Domnguez, A.; Porter, T. A.; Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] CSIC, IEEE, Inst Ciencies Espai, Barcelona 08193, Spain.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cavazzuti, E.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy.
[Cecchi, C.; D'Ammando, F.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Chekhtman, A.; Razzaque, S.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Cheung, C. C.] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA.
[Chiaro, G.] Univ Padua, Ist Nazl Fis Nucl, I-35131 Padua, Italy.
[Chiaro, G.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Ciprini, S.] ASI Sci Data Ctr, I-00044 Rome, Italy.
[Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Universe & Particules Montpellier, Montpellier, France.
[Conrad, J.; Larsson, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Conrad, J.; Jackson, M. S.; Larsson, S.] Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Conrad, J.] Royal Swedish Acad Sci Res, SE-10691 Stockholm, Sweden.
[D'Ammando, F.] IASF Palermo, I-90146 Palermo, Italy.
[D'Ammando, F.] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy.
[Dermer, C. D.; Grove, J. E.; Lovellette, M. N.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Fukazawa, Y.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Gehrels, N.; Guiriec, S.; Hays, E.; McEnery, J. E.; Perkins, J. S.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Jackson, M. S.] Royal Inst Technol KTH, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Knoedlseder, J.] Univ Toulouse, UPS OMP, IRAP, GAHEC, Toulouse, France.
[Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Ohno, M.; Stawarz, Lukasz] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Perkins, J. S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Perkins, J. S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA.
[Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Perkins, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93401 USA.
[Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Sanchez, D. A.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Stawarz, Lukasz] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Vianello, G.] CIFS, I-10133 Turin, Italy.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
RP Ajello, M (reprint author), Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
EM majello@slac.stanford.edu; buehler@stanford.edu; anita.reimer@uibk.ac.at
RI Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Rando,
Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Funk,
Stefan/B-7629-2015; Loparco, Francesco/O-8847-2015; Gargano,
Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko,
Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro,
Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016;
OI Gasparrini, Dario/0000-0002-5064-9495; Tramacere,
Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726; Sgro',
Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864;
Dominguez, Alberto/0000-0002-3433-4610; Bastieri,
Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577;
Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti,
monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852;
Cutini, Sara/0000-0002-1271-2924; Reimer, Olaf/0000-0001-6953-1385;
Funk, Stefan/0000-0002-2012-0080; Loparco,
Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395;
giglietto, nicola/0000-0002-9021-2888; Moskalenko,
Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres,
Diego/0000-0002-1522-9065; Caraveo, Patrizia/0000-0003-2478-8018
FU K. A. Wallenberg Foundation; Fermi guest investigator program [31117,
51258]
FX M. A. acknowledges generous support from the Fermi guest investigator
program (proposals ID 31117 and 51258) and the Swift and the Gamma-Ray
Burst Optical/Near-Infrared Detector (GROND) teams for observing similar
to 100 Fermi blazars in an effort to constrain their redshifts. The
Fermi LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and the operation of the LAT as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States; the
Commissariat a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France; the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy; the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), High Energy
Accelerator Research Organization (KEK), and Japan Aerospace Exploration
Agency (JAXA) in Japan; and the K. A. Wallenberg Foundation, the Swedish
Research Council, and the Swedish National Space Board in Sweden.
Additional support for science analysis during the operations phase is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National d'Etudes Spatiales in France. J. Conrad is
funded by a grant from the K. A. Wallenberg Foundation. E. Troja is a
NASA Postdoctoral Program Fellow.
NR 45
TC 103
Z9 103
U1 1
U2 24
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 NOV 30
PY 2012
VL 338
IS 6111
BP 1190
EP 1192
DI 10.1126/science.1227160
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 045AL
UT WOS:000311666200040
PM 23118013
ER
PT J
AU Bowman, K
Henze, DK
AF Bowman, K.
Henze, D. K.
TI Attribution of direct ozone radiative forcing to spatially resolved
emissions
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SATELLITE MEASUREMENTS; TROPOSPHERIC OZONE; TRANSPORT; CHEMISTRY;
POLLUTION; SECTORS
AB Quantifying the dependence of ozone direct radiative forcing (DRF) on the mixture and spatial distribution of precursor emissions is a key step towards understanding the impact of air quality standards on climate. We use here a combination of satellite observations of ozone and its radiative effect in conjunction with an adjoint chemical transport model to determine the ozone DRF due to global, anthropogenic NOx, CO, and non-methane hydrocarbons (NMHC) emissions regionally at 2 degrees x 2.5 degrees regions resolution. We show that 8% of the ozone DRF from the sum of all these emissions can be attributed to 15 regions, which are predominantly located in China and the United States (US). To achieve an equivalent reduction in ozone DRF, necessary emission reductions for each precursor vary intra-continentally by a factor of 3-10 and globally by over an order of magnitude. The contribution of NOx emissions to ozone DRF relative to CO and NMHC emissions within individual regions varies globally by nearly a factor of two. Citation: Bowman, K., and D. K. Henze (2012), Attribution of direct ozone radiative forcing to spatially resolved emissions, Geophys. Res. Lett., 39, L22704, doi: 10.1029/2012GL053274.
C1 [Bowman, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Henze, D. K.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA.
RP Bowman, K (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM kevin.w.bowman@jpl.nasa.gov
FU NASA; NASA AQAST [NNX11AI54G]; AURA [NNH07ZDA001N]; New Investigator
Program [NNX10AR06G]; HEC
FX This research was carried out in part at the Jet Propulsion Laboratory,
California Institute of Technology, under contract from NASA. We would
like thank Helen Worden (NCAR) and the TES team for the IRK products. We
acknowledge sponsorship from NASA AQAST (NNX11AI54G), AURA
(NNH07ZDA001N), New Investigator Program (NNX10AR06G) and HEC computing
facilities.
NR 32
TC 15
Z9 15
U1 0
U2 31
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 NOV 29
PY 2012
VL 39
AR L22704
DI 10.1029/2012GL053274
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 047LG
UT WOS:000311841500001
ER
PT J
AU Wu, H
Kimball, JS
Elsner, MM
Mantua, N
Adler, RF
Stanford, J
AF Wu, Huan
Kimball, John S.
Elsner, Marketa M.
Mantua, Nate
Adler, Robert F.
Stanford, Jack
TI Projected climate change impacts on the hydrology and temperature of
Pacific Northwest rivers
SO WATER RESOURCES RESEARCH
LA English
DT Article
ID STREAM TEMPERATURE; WATER TEMPERATURE; GLOBAL OPTIMIZATION;
UNITED-STATES; MODEL; BASIN; FLOW; PRECIPITATION; VARIABILITY; RESOURCES
AB A dominant river-tracing-based streamflow and temperature (DRTT) model was developed by coupling stream thermal dynamics with a source-sink routing model. The DRTT model was applied using 1/16 degree (similar to 6 km) resolution gridded daily surface meteorology inputs over a similar to 988,000 km(2) Pacific Northwest (PNW) domain to produce regional daily streamflow and temperature simulations from 1996 to 2005. The DRTT results showed favorable performance for simulation of daily stream temperature (mean R-2 = 0.72 and root-mean-square error = 2.35 degrees C) and discharge (mean R-2 = 0.52 and annual relative error 14%) against observations from 12 PNW streams. The DRTT was then applied with a macroscale hydrologic model to predict streamflow and temperature changes under historical (1980s) and future (2020s, 2040s, and 2080s) climate change scenarios (IPCC AR4) as they may affect current and future patterns of freshwater salmon habitat and associated productivity of PNW streams. The model projected a 3.5% decrease in mean annual streamflow for the 2020s and 0.6% and 5.5% increases for the 2040s and 2080s, respectively, with projected increase in mean annual stream temperatures from 0.55 degrees C (2020s) to 1.68 degrees C (2080s). However, summer streamflow decreased from 19.3% (2020s) to 30.3% (2080s), while mean summer stream temperatures warmed from 0.92 degrees C to 2.10 degrees C. The simulations indicate that projected climate change will have greater impacts on snow dominant streams, with lower summer streamflows and warmer summer stream temperature changes relative to transient and rain dominant regimes. Lower summer flows combined with warmer stream temperatures suggest a future with widespread increased summertime thermal stress for coldwater fish in the PNW region.
C1 [Wu, Huan; Adler, Robert F.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20704 USA.
[Wu, Huan; Adler, Robert F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kimball, John S.] Univ Montana, Flathead Lake Biol Stn, Polson, MT 59860 USA.
[Kimball, John S.] Univ Montana, Coll Forestry & Conservat, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA.
[Elsner, Marketa M.; Mantua, Nate] Univ Washington, Climate Impacts Grp, Joint Inst Study Atmosphere & Ocean, Seattle, WA 98195 USA.
[Mantua, Nate] Univ Washington, Sch Aquat & Fisheries Sci, Seattle, WA 98195 USA.
RP Wu, H (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, 5825 Univ Ct,Ste 4001, College Pk, MD 20704 USA.
EM huanwu@umd.edu
RI Wu, Huan/K-1003-2013
OI Wu, Huan/0000-0003-2920-8860
FU Gordon and Betty Moore Foundation
FX This work was conducted at the University of Montana (UMT) with
financial support from the Gordon and Betty Moore Foundation. The
authors would like to thank Wilfred Wollheim and the two anonymous
reviewers for their very constructive comments and suggestions for
improving the paper. The authors would also like to thank John Lucotch
and Niels Maumenee for assistance in data processing.
NR 63
TC 28
Z9 28
U1 2
U2 75
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
J9 WATER RESOUR RES
JI Water Resour. Res.
PD NOV 29
PY 2012
VL 48
AR W11530
DI 10.1029/2012WR012082
PG 23
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 047OQ
UT WOS:000311850700001
ER
PT J
AU Rohling, EJ
Sluijs, A
Dijkstra, HA
Kohler, P
de Wal, RSWV
von der Heydt, AS
Beerling, DJ
Berger, A
Bijl, PK
Crucifix, M
DeConto, R
Drijfhout, SS
Fedorov, A
Foster, GL
Ganopolski, A
Hansen, J
Honisch, B
Hooghiemstra, H
Huber, M
Huybers, P
Knutti, R
Lea, DW
Lourens, LJ
Lunt, D
Masson-Demotte, V
Medina-Elizalde, M
Otto-Bliesner, B
Pagani, M
Palike, H
Renssen, H
Royer, DL
Siddall, M
Valdes, P
Zachos, JC
Zeebe, RE
AF Rohling, E. J.
Sluijs, A.
Dijkstra, H. A.
Koehler, P.
de Wal, R. S. W. van
von der Heydt, A. S.
Beerling, D. J.
Berger, A.
Bijl, P. K.
Crucifix, M.
DeConto, R.
Drijfhout, S. S.
Fedorov, A.
Foster, G. L.
Ganopolski, A.
Hansen, J.
Hoenisch, B.
Hooghiemstra, H.
Huber, M.
Huybers, P.
Knutti, R.
Lea, D. W.
Lourens, L. J.
Lunt, D.
Masson-Demotte, V.
Medina-Elizalde, M.
Otto-Bliesner, B.
Pagani, M.
Paelike, H.
Renssen, H.
Royer, D. L.
Siddall, M.
Valdes, P.
Zachos, J. C.
Zeebe, R. E.
CA PALAEOSENS Project Members
TI Making sense of palaeoclimate sensitivity
SO NATURE
LA English
DT Article
ID CARBON-DIOXIDE CONCENTRATION; GLOBAL CLIMATE SENSITIVITY; EOCENE
ATMOSPHERIC CO2; LAST GLACIAL MAXIMUM; PAST 800,000 YEARS; ICE-CORE;
TEMPERATURE-VARIATIONS; ANTARCTIC TEMPERATURE; POLAR AMPLIFICATION;
EARTHS TEMPERATURE
AB Many palaeoclimate studies have quantified pre-anthropogenic climate change to calculate climate sensitivity (equilibrium temperature change in response to radiative forcing change), but a lack of consistent methodologies produces a wide range of estimates and hinders comparability of results. Here we present a stricter approach, to improve intercomparison of palaeoclimate sensitivity estimates in a manner compatible with equilibrium projections for future climatechange. Over the past 65 million years, this reveals a climate sensitivity (in KW-1 m(2)) of 0.3-1.9 or 0.6-1.3 at 95% or 68% probability, respectively. The latter implies a warming of 2.2-4.8 K per doubling of atmospheric CO2, which agrees with IPCC estimates.
C1 [Rohling, E. J.; Foster, G. L.] Univ Southampton, Sch Ocean & Earth Sci, Natl Oceanog Ctr, Southampton SO14 3ZH, Hants, England.
[Rohling, E. J.] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia.
[Sluijs, A.; Bijl, P. K.; Lourens, L. J.] Univ Utrecht, Dept Earth Sci, Fac Geosci, NL-3584 CD Utrecht, Netherlands.
[Dijkstra, H. A.; de Wal, R. S. W. van; von der Heydt, A. S.] Univ Utrecht, Inst Marine & Atmospher Res Utrecht, NL-3584 CC Utrecht, Netherlands.
[Koehler, P.] Alfred Wegener Inst Polar & Marine Res AWI, D-27515 Bremerhaven, Germany.
[Beerling, D. J.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England.
[Berger, A.; Crucifix, M.] Catholic Univ Louvain, Georges Lemaitre Ctr Earth & Climate Res, Earth & Life Inst, B-1348 Louvain, Belgium.
[DeConto, R.] Univ Massachusetts, Dept Geosci, Morrill Sci Ctr 233, Amherst, MA 01003 USA.
[Drijfhout, S. S.] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands.
[Fedorov, A.] Yale Univ, Dept Geol & Geophys, New Haven, CT 06520 USA.
[Ganopolski, A.] Potsdam Inst Climate Impact Res PIK, D-14412 Potsdam, Germany.
[Hansen, J.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Hoenisch, B.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Hooghiemstra, H.] Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, NL-1098 XH Amsterdam, Netherlands.
[Huber, M.] Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA.
[Huybers, P.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Knutti, R.] ETH, Inst Atmospher andClimate Sci, CH-8092 Zurich, Switzerland.
[Lea, D. W.] Univ Calif Santa Barbara, Dept Earth Sci, Santa Barbara, CA 93106 USA.
[Lunt, D.; Valdes, P.] Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England.
[Masson-Demotte, V.] LCEA Saclay, LSCE IPSL CEA CNRS UVSQ, UMR 8212, F-91191 Gif Sur Yvette, France.
[Medina-Elizalde, M.] Ctr Invest Cient Yucatan, Unidad Ciencias Agua, Cancun 77500, Quintana Roo, Mexico.
[Otto-Bliesner, B.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Paelike, H.] Univ Bremen, MARUM, D-28359 Bremen, Germany.
[Renssen, H.] Free Univ Amsterdam, Dept Earth Sci, Fac Earth & Life Sci, NL-1081 HV Amsterdam, Netherlands.
[Royer, D. L.] Wesleyan Univ, Dept Earth & Environm Sci, Middletown, CT 06459 USA.
[Siddall, M.] Univ Bristol, Dept Earth Sci, Bristol BS8 1RJ, Avon, England.
[Zeebe, R. E.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Dept Oceanog, Honolulu, HI 96822 USA.
RP Rohling, EJ (reprint author), Univ Southampton, Sch Ocean & Earth Sci, Natl Oceanog Ctr, Southampton SO14 3ZH, Hants, England.
EM e.rohling@noc.soton.ac.uk
RI Palike, Heiko/A-6560-2008; Beerling, David/C-2840-2009; Drijfhout,
Sybren/I-4230-2016; Dijkstra , Henk /H-2559-2016; Sluijs,
Appy/B-3726-2009; Huber, Matthew/A-7677-2008; Kohler, Peter/F-7293-2010;
Masson-Delmotte, Valerie/G-1995-2011; van de wal, roderik/D-1705-2011;
Knutti, Reto/B-8763-2008; Lunt, Daniel/G-9451-2011; Pagani,
Mark/B-3233-2008; Valdes, Paul/C-4129-2013; Hoenisch,
Baerbel/C-7530-2013; Ganopolski, Andrey/F-6811-2013; Rohling,
Eelco/B-9736-2008; von der Heydt, Anna/B-9250-2008
OI Palike, Heiko/0000-0003-3386-0923; Beerling, David/0000-0003-1869-4314;
Sluijs, Appy/0000-0003-2382-0215; Royer, Dana/0000-0003-0976-953X;
Huber, Matthew/0000-0002-2771-9977; Kohler, Peter/0000-0003-0904-8484;
Masson-Delmotte, Valerie/0000-0001-8296-381X; Knutti,
Reto/0000-0001-8303-6700; Lunt, Daniel/0000-0003-3585-6928; Hoenisch,
Baerbel/0000-0001-5844-3398; Rohling, Eelco/0000-0001-5349-2158; von der
Heydt, Anna/0000-0002-5557-3282
FU Royal Netherlands Academy of Arts and Sciences (KNAW); UK-NERC
consortium iGlass [NE/I009906/1]; Australian Laureate Fellowship
[FL120100050]; Royal Society Wolfson Research Merit Awards; European
Research Council for ERC [259627]; NSF [0902882]; EU [243908]
FX This Perspective arose from the first PALAEOSENS workshop in March 2011.
We thank the Royal Netherlands Academy of Arts and Sciences (KNAW) for
funding and hosting this workshop in Amsterdam, PAGES for their support,
and J. Gregory for discussions. This study was supported by the UK-NERC
consortium iGlass (NE/I009906/1), and 2012 Australian Laureate
Fellowship FL120100050. D.J.B., E.J.R. and P.V. were supported by Royal
Society Wolfson Research Merit Awards. A.S. thanks the European Research
Council for ERC starting grant 259627, and M.H. acknowledges NSF P2C2
grant 0902882. Some of the work was supported by grant 243908
'Past4Future' of the EU's seventh framework programme; this is
Past4Future contribution number 30.
NR 99
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U1 21
U2 278
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 NOV 29
PY 2012
VL 491
IS 7426
BP 683
EP 691
DI 10.1038/nature11574
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 044FY
UT WOS:000311606000031
ER
PT J
AU Teanby, NA
Irwin, PGJ
Nixon, CA
de Kok, R
Vinatier, S
Coustenis, A
Sefton-Nash, E
Calcutt, SB
Flasar, FM
AF Teanby, Nicholas A.
Irwin, Patrick G. J.
Nixon, Conor A.
de Kok, Remco
Vinatier, Sandrine
Coustenis, Athena
Sefton-Nash, Elliot
Calcutt, Simon B.
Flasar, F. Michael
TI Active upper-atmosphere chemistry and dynamics from polar circulation
reversal on Titan
SO NATURE
LA English
DT Article
ID COMPOSITE INFRARED SPECTROMETER; CASSINI/CIRS DATA; TEMPERATURES; MODEL;
MESOSPHERE
AB Saturn's moon Titan has a nitrogen atmosphere comparable to Earth's, with a surface pressure of 1.4 bar. Numerical models reproduce the tropospheric conditions very well but have trouble explaining the observed middle-atmosphere temperatures, composition and winds(1,2). The top of the middle-atmosphere circulation has been thought to lie at an altitude of 450 to 500 kilometres, where there is a layer of haze that appears to be separated from the main haze deck(3). This 'detached' haze was previously explained as being due to the co-location of peak haze production and the limit of dynamical transport by the circulation's upper branch(4). Here we report a build-up of trace gases over the south pole approximately two years after observing the 2009 post-equinox circulation reversal, from which we conclude that middle-atmosphere circulation must extend to an altitude of at least 600 kilometres. The primary drivers of this circulation are summer-hemisphere heating of haze by absorption of solar radiation and winter-hemisphere cooling due to infrared emission by haze and trace gases(5); our results therefore imply that these effects are important well into the thermosphere (altitudes higher than 500 kilometres). This requires both active upper-atmosphere chemistry, consistent with the detection of high-complexity molecules and ions at altitudes greater than 950 kilometres(6,7), and an alternative explanation for the detached haze, such as a transition in haze particle growth from monomers to fractal structures(8).
C1 [Teanby, Nicholas A.; Sefton-Nash, Elliot] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England.
[Irwin, Patrick G. J.; Calcutt, Simon B.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England.
[Nixon, Conor A.; Flasar, F. Michael] NASA, Planetary Syst Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[de Kok, Remco] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Vinatier, Sandrine; Coustenis, Athena] Univ Paris Diderot, LESIA Observ Paris, CNRS, Univ Paris 06, F-92195 Meudon, France.
[Sefton-Nash, Elliot] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
RP Teanby, NA (reprint author), Univ Bristol, Sch Earth Sci, Wills Mem Bldg,Queens Rd, Bristol BS8 1RJ, Avon, England.
EM n.teanby@bristol.ac.uk
RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012;
OI Nixon, Conor/0000-0001-9540-9121; Calcutt, Simon/0000-0002-0102-3170;
Teanby, Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X
FU UK Science and Technology Facilities Council; Leverhulme Trust; NASA
Cassini mission
FX This work was funded by the UK Science and Technology Facilities
Council, the Leverhulme Trust and the NASA Cassini mission.
NR 30
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U1 1
U2 30
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 NOV 29
PY 2012
VL 491
IS 7426
BP 732
EP 735
DI 10.1038/nature11611
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 044FY
UT WOS:000311606000039
PM 23192150
ER
PT J
AU Cooper, OR
Gao, RS
Tarasick, D
Leblanc, T
Sweeney, C
AF Cooper, Owen R.
Gao, Ru-Shan
Tarasick, David
Leblanc, Thierry
Sweeney, Colm
TI Long-term ozone trends at rural ozone monitoring sites across the United
States, 1990-2010
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID STRATOSPHERE-TROPOSPHERE EXCHANGE; GROUND-LEVEL OZONE; TRANSPORTED
BACKGROUND OZONE; PARTICLE DISPERSION MODEL; ASIAN AIR-POLLUTION;
NORTH-AMERICA; SURFACE OZONE; WEST-COAST; METEOROLOGICAL CONTROLS;
15-YEAR CLIMATOLOGY
AB This analysis provides an up-to-date assessment of long-term (1990-2010) rural ozone trends using all available data in the western (12 sites) and eastern (41 sites) USA. Rather than focus solely on average ozone values or air quality standard violations, we consider the full range of ozone values, reporting trends for the 5th, 50th and 95th percentiles. Domestic ozone precursor emissions decreased strongly during 1990-2010. Accordingly 83%, 66% and 20% of summertime eastern U.S. sites experienced statistically significant ozone decreases in the 95th, 50th and 5th percentiles, respectively. During spring 43% of the eastern sites have statistically significant ozone decreases for the 95th percentile with no sites showing a significant increase. At the 50th percentile there is little overall change in the eastern U.S. In contrast, only 17% (2 sites) and 8% (1 site) of summertime western U.S. sites have statistically significant ozone decreases in the 95th and 50th percentiles, respectively. During spring no western site has a significant decrease, while 50% have a significant median increase. This dichotomy in U.S. ozone trends is discussed in terms of changing anthropogenic and biomass burning emissions. Consideration is given to the concept that increasing baseline ozone flowing into the western U.S. is counteracting ozone reductions due to domestic emission reductions. An update to the springtime free tropospheric ozone trend above western North America shows that ozone has increased significantly from 1995 to 2011 at the rate of 0.41 +/- 0.27 ppbv yr(-1). Finally, the ozone changes are examined in relation to regional temperature trends.
C1 [Cooper, Owen R.; Gao, Ru-Shan; Sweeney, Colm] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Cooper, Owen R.; Sweeney, Colm] Univ Colorado, NOAA, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Tarasick, David] Environm Canada, Expt Studies Res Div, Meteorol Serv Canada, Ottawa, ON K1A 0H3, Canada.
[Leblanc, Thierry] CALTECH, Jet Prop Lab, Table Mt Facil, Pasadena, CA USA.
RP Cooper, OR (reprint author), NOAA, Earth Syst Res Lab, CSD04,325 Broadway, Boulder, CO 80305 USA.
EM owen.r.cooper@noaa.gov
RI Cooper, Owen/H-4875-2013; Gao, Ru-Shan/H-7455-2013; Manager, CSD
Publications/B-2789-2015;
OI Tarasick, David/0000-0001-9869-0692
FU European Communities; EADS; Airbus; airlines (Lufthansa, Austrian, Air
France)
FX Ozone data from the National Park Service Gaseous Pollutant Monitoring
Program were collected by the National Park Service and downloaded from
the NPS Gaseous Pollutant and Meteorological Data Access Page:
http://ard-request.air-resource.com. Assistance in retrieving the data
was provided by Jessica Ward, Air Resource Specialists, Inc. and John
Ray, National Park Service Air Resources Division. Whiteface Mountain
Summit ozone data were collected by the University of Albany with
instrumentation provided by the New York State Department of
Environmental Conservation, and provided by James J. Schwab, Atmospheric
Sciences Research Center, University at Albany. Surface CO measurements
from Niwot Ridge measured and made available by the NOAA Earth System
Research Laboratory Carbon Cycle Group. We gratefully acknowledge the
strong support of the MOZAIC program by the European Communities, EADS,
Airbus and the airlines (Lufthansa, Austrian, Air France) who have
carried the MOZAIC equipment free of charge since 1994. Jean-Pierre
Cammas and Philippe Nedelec at CNRS - Laboratoire d'Aerologie, France,
provided access to the MOZAIC data. The EDGARv4.1 global NOx
emissions inventory was provided by European Commission, Joint Research
Centre (JRC)/Netherlands Environmental Assessment Agency (PBL): Emission
Database for Global Atmospheric Research (EDGAR), release version 4.1
http://edgar.jrc.ec.europa.eu, 2010. We acknowledge the free use of
tropospheric NO2 column data from the GOME and SCIAMACHY
sensors from www.temis.nl. The global topography data at 4 min
resolution were downloaded from: NOAA National Geophysical Data Center,
Boulder, www.ngdc.noaa.gov/mgg/global/global.html. Finally, we thank
three anonymous referees whose comments and suggestions improved the
analysis. Funding for the Trinidad Head ozonesondes was provided by the
NOAA ESRL Health of the Atmosphere Program.
NR 98
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U1 13
U2 144
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 NOV 28
PY 2012
VL 117
AR D22307
DI 10.1029/2012JD018261
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 047MH
UT WOS:000311844500005
ER
PT J
AU Martin, MV
Kahn, RA
Logan, JA
Paugam, R
Wooster, M
Ichoku, C
AF Martin, Maria Val
Kahn, Ralph A.
Logan, Jennifer A.
Paugam, Ronan
Wooster, Martin
Ichoku, Charles
TI Space-based observational constraints for 1-D fire smoke plume-rise
models
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID REMOTE-SENSING DATA; INJECTION HEIGHT; FOREST-FIRES; WRF-CHEM;
EMISSIONS; SATELLITE; TRANSPORT; SENSITIVITY; SIMULATION; WILDFIRES
AB We use a plume height climatology derived from space-based Multiangle Imaging Spectroradiometer (MISR) observations to evaluate the performance of a widely used plume-rise model. We initialize the model with assimilated meteorological fields from the NASA Goddard Earth Observing System and estimated fuel moisture content at the location and time of the MISR measurements. Fire properties that drive the plume-rise model are difficult to constrain, and we test the model with four estimates each of active fire area and total heat flux, obtained from Moderate Resolution Imaging Spectroradiometer (MODIS) fire radiative power (FRP) thermal anomalies available for each MISR plume and other empirical data. We demonstrate the degree to which the fire dynamical heat flux (related to active fire area and sensible heat flux) and atmospheric stability structure influence plume rise, although entrainment and possibly other less well constrained factors are also likely to be significant. Using atmospheric stability conditions, MODIS FRP, and MISR plume heights, we find that smoke plumes reaching high altitudes are characterized by higher FRP and weaker atmospheric stability conditions than those at low altitude, which tend to remain confined below the boundary layer, consistent with earlier results. However, over the diversity of conditions studied, the model simulations generally underestimate the plume height dynamic range observed by MISR and do not reliably identify plumes injected into the free troposphere, key information needed for atmospheric models to simulate smoke dispersion. We conclude that embedding in large-scale atmospheric studies an advanced plume-rise model using currently available fire constraints remains a difficult proposition, and we propose a simplified model that crudely constrains plume injection height based on two main physical factors for which some observational constraints often exist. Field experiments aimed at directly measuring fire and smoke plume properties in detail are likely to produce the next major advances in plume-rise modeling.
C1 [Martin, Maria Val; Logan, Jennifer A.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Kahn, Ralph A.; Ichoku, Charles] NASA, Climate & Radiat Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Paugam, Ronan; Wooster, Martin] Kings Coll London, Dept Geog, London WC2R 2LS, England.
RP Martin, MV (reprint author), Colorado State Univ, Dept Atmospher Sci, 3915 W Laporte Ave, Ft Collins, CO 80521 USA.
EM mval@atmos.colostate.edu
RI Val Martin, Maria/D-6955-2011; Ichoku, Charles/E-1857-2012; Kahn,
Ralph/D-5371-2012
OI Ichoku, Charles/0000-0003-3244-4549; Kahn, Ralph/0000-0002-5234-6359
FU National Science Foundation [ATM0554804]; NASA [NNX09AC51G]; NASA's
Climate and Radiation Research and Analysis Program; NASA's Atmospheric
Composition Program; NASA Earth Observing System MISR instrument project
FX This work was supported by grants from the National Science Foundation
(ATM0554804) and NASA (NNX09AC51G) to Harvard University (M.V.M. and
J.A.L.). The work of R.A.K. is supported in part by NASA's Climate and
Radiation Research and Analysis Program under H. Maring, NASA's
Atmospheric Composition Program under R. Eckman, and the NASA Earth
Observing System MISR instrument project. We thank Saulo Freitas for
providing and helping implement the 1-D plume-rise model, Nancy French
for helpful discussions about North American fuel beds, Alan Cantin for
access to the surface observations over Canada used to run CFWI. and
Martin Parker for providing the Alaska fuel bed map. The work of David
Nelson on the MISR plume climatology is gratefully acknowledged.
NR 75
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U1 2
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD NOV 28
PY 2012
VL 117
AR D22204
DI 10.1029/2012JD018370
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 047MH
UT WOS:000311844500006
ER
PT J
AU Hsu, TS
McPherron, RL
Angelopoulos, V
Ge, YS
Zhang, H
Russell, C
Chu, XN
Kissinger, J
AF Hsu, Tung-Shin
McPherron, R. L.
Angelopoulos, Vassilis
Ge, Yasong
Zhang, Hui
Russell, Christopher
Chu, Xiangning
Kissinger, Jennifer
TI A statistical analysis of the association between fast plasma flows and
Pi2 pulsations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID BURSTY BULK FLOWS; MAGNETOSPHERIC SUBSTORM; PI-2 PULSATIONS; LOW
LATITUDES; MAGNETOTAIL; MECHANISM; BRAKING; TRIGGER; EVENT; SHEET
AB What is the energy source for Pi2 pulsations? Some researchers have suggested that Pi2 pulsations are caused by plasma flows. Others have suggested that Pi2s are caused by a plasma instability initiated in the near-Earth region. In this study we use Time History of Events and Macroscale Interactions during Substorms (THEMIS) data to examine the relationship between plasma flows and Pi2s. We first identify plasma flows in the tail and then associate these flows with Pi2s. We find that the overall probability of association is nearly 70%. If we further examine the spatial distribution of association we find that in the near-Earth region (8-15 R-E) 90% of the flows are associated with Pi2s. This suggests either that plasma flow in the tail is the cause of Pi2 on the ground or that both are caused by the same process. More importantly, as the flows approach the Earth, the increasing magnetic field causes the flow speed to decrease, that is, the flows are decelerated. In this process of flow braking, the local magnetic field becomes more dipolar. The region of strongest flow braking corresponds to the region of strongest association between flows and Pi2s (8-15 R-E). The GSM X component of plasma flows become zero at around 8 R-E where the most significant magnetic dipolarization occurs. We also find that most plasma flows are associated with a sudden enhancement of the westward electrojet. These results suggest that plasma flows, Pi2 pulsations, and magnetic field dipolarization are essential components of the substorm expansion onset.
C1 [Hsu, Tung-Shin; McPherron, R. L.; Angelopoulos, Vassilis; Russell, Christopher; Chu, Xiangning] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Hsu, Tung-Shin; McPherron, R. L.; Angelopoulos, Vassilis; Russell, Christopher; Chu, Xiangning] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Ge, Yasong] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Zhang, Hui] Chinese Acad Sci, Inst Geol & Geophys, Beijing Natl Observ Space Environm, Beijing, Peoples R China.
[Kissinger, Jennifer] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hsu, TS (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
EM thsu@igpp.ucla.edu
RI Zhang, Hui/G-6600-2014
FU NSF [ATM-1003854, AGS-0720422]; [NASA-NNX07AG47G]; [NASA-NNX07AG16G];
[NASA-NNX07AF60G]
FX The authors would like to acknowledge support for this work from the
following grants: NASA-NNX07AG47G, NASA-NNX07AG16G, NASA-NNX07AF60G, NSF
ATM-1003854 and NSF AGS-0720422. We also thank the Principal
Investigators of the THEMIS spacecraft and ground stations for making
data from their instruments available for this study. Finally we thank
the Data Center for Geomagnetism at Kyoto, Japan for creation and
distribution of the AE indices.
NR 40
TC 11
Z9 11
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 NOV 28
PY 2012
VL 117
AR A11221
DI 10.1029/2012JA018173
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 047LY
UT WOS:000311843600003
ER
PT J
AU Bhatia, AK
Sinha, C
AF Bhatia, A. K.
Sinha, C.
TI Free-free transitions of the e-H system inside a dense plasma irradiated
by a laser field at very low incident-electron energies
SO PHYSICAL REVIEW A
LA English
DT Article
ID ION-SCATTERING; EXCITATION; COLLISIONS; HYDROGEN
AB The free-free transition is studied for an electron-hydrogen atom in ground state when a low-energy electron (external) is injected into hydrogenic plasma in the presence of an external homogenous, monochromatic, and linearly polarized laser field. The effect of plasma screening is considered in the Debye-Huckel approximation. The calculations are performed in the soft photon limit. The incident electron is considered to be dressed by the laser field in a nonperturbative manner by choosing the Volkov solutions in both the initial and final channels. The space part of the scattering wave function for the electron is solved numerically by taking into account the electron exchange. The laser-assisted differential and total cross sections are calculated for single-photon absorption or emission and no-photon exchange in the soft photon limit, the laser intensity being much less than the atomic field intensity. The calculations have been carried out for various values of Debye parameter, ranging from 0.005 to 0.12. A strong suppression is noted in the laser-assisted cross sections as compared to the field-free situation. A significant difference is noted for the singlet and triplet cross sections. The suppression is much more in the triplet states.
C1 [Bhatia, A. K.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Sinha, C.] Indian Assoc Cultivat Sci, Dept Theoret Phys, Kolkata 700032, India.
RP Bhatia, AK (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
NR 29
TC 6
Z9 6
U1 2
U2 5
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9926
EI 2469-9934
J9 PHYS REV A
JI Phys. Rev. A
PD NOV 28
PY 2012
VL 86
IS 5
AR 053421
DI 10.1103/PhysRevA.86.053421
PG 9
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 044FD
UT WOS:000311603900005
ER
PT J
AU Fuchs, EC
Cherukupally, A
Paulitsch-Fuchs, AH
Agostinho, LLF
Wexler, AD
Woisetschlager, J
Freund, FT
AF Fuchs, Elmar C.
Cherukupally, Anvesh
Paulitsch-Fuchs, Astrid H.
Agostinho, Luewton L. F.
Wexler, Adam D.
Woisetschlaeger, Jakob
Freund, Friedemann T.
TI Investigation of the mid-infrared emission of a floating water bridge
SO JOURNAL OF PHYSICS D-APPLIED PHYSICS
LA English
DT Article
ID SIMPLE IONIC HYDROXIDES; PROTON CONDUCTIVITY; ELECTRIC-FIELD;
TEMPERATURE-DEPENDENCE; INFRARED-SPECTROSCOPY; CARBON-DIOXIDE; LIQUID
WATER; TRANSMITTANCE; DYNAMICS; MG(OH)2
AB We report on the infrared emission of aqueous bridges under the application of high dc voltage (;'floating water bridge') over the range between 400 and 2500 cm(-1) (4.0-10.3 mu m). Comparison with bulk water of the same temperature reveals an additional broad peak at similar to 2200 cm(-1) as well as water vapour emission lines. Two complementary explanations are presented for the broad peak: first, a cooperative proton transfer comprising an orientational motion along the direction of conduction is suggested. Second, the electrolysis-less current flow is explained by a proton/defect-proton band mechanism, which is in line with the cooperative proton transfer. The water vapour emissions occur due to collision ionization of space charges with micro-and nano-droplets which are electrosprayed from the liquid/gas interface.
C1 [Fuchs, Elmar C.; Paulitsch-Fuchs, Astrid H.; Agostinho, Luewton L. F.; Wexler, Adam D.] Wetsus Ctr Excellence Sustainable Water Technol, Leeuwarden, Netherlands.
[Cherukupally, Anvesh] Univ Arizona, Dept Min & Geol Engn, Tucson, AZ 85721 USA.
[Woisetschlaeger, Jakob] Graz Univ Technol, Inst Thermal Turbomachinery & Machine Dynam, A-8010 Graz, Austria.
[Woisetschlaeger, Jakob] Carl Sagan Ctr, SETI Inst, Mountain View, CA USA.
[Freund, Friedemann T.] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA.
RP Fuchs, EC (reprint author), Wetsus Ctr Excellence Sustainable Water Technol, Leeuwarden, Netherlands.
EM elmar.fuchs@wetsus.nl
OI Woisetschlaeger, Jakob/0000-0002-7057-761X
FU Dutch Ministry of Economic Affairs; NASA Earth Surface and Interior
program
FX This work was performed in the TTIW-cooperation framework of Wetsus,
centre of excellence for sustainable water technology (www.wetsus.nl).
Wetsus is funded by the Dutch Ministry of Economic Affairs. The authors
like to thank the participants of the research theme 'Applied Water
Physics' for the fruitful discussions and their financial support. The
IR emission spectra were recorded at the NASA Ames Research Center,
Moffett Field, CA, USA, using an IR emission spectrometer provided by a
grant from the NASA Earth Surface and Interior program. The authors
thank Dr Dana Lynch for providing premier laboratory space for
conducting these experiments. The authors also would like to thank
Professors Huib Bakker (AMOLF Amsterdam), Cees Buisman (Wetsus), Karl
Gatterer (Graz University of Technology), Emilio Del Giudice (Universita
di Milano), Franz Heitmeir (Graz University of Technology), Jose
Teixeira (Laboratoire Leon Brillouin, CEA-CNRS/IRAMIS, CEA/Saclay), as
well as Cees Kamp (Wetsus), Lukasz Piatkowski (AMOLF) and Martina Sammer
(Wetsus) for ongoing discussions about the water bridge phenomenon (in
alphabetic order).
NR 52
TC 11
Z9 11
U1 0
U2 14
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0022-3727
J9 J PHYS D APPL PHYS
JI J. Phys. D-Appl. Phys.
PD NOV 28
PY 2012
VL 45
IS 47
AR 475401
DI 10.1088/0022-3727/45/47/475401
PG 10
WC Physics, Applied
SC Physics
GA 033ZK
UT WOS:000310839700016
ER
PT J
AU Elsila, JE
Glavin, DP
Dworkin, JP
Martins, Z
Bada, JL
AF Elsila, Jamie E.
Glavin, Daniel P.
Dworkin, Jason P.
Martins, Zita
Bada, Jeffrey L.
TI Inconclusive evidence for nonterrestrial isoleucine enantiomeric
excesses in primitive meteorites
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Letter
ID AMINO-ACIDS
C1 [Elsila, Jamie E.; Glavin, Daniel P.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Martins, Zita] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London SW7 2AZ, England.
[Bada, Jeffrey L.] Univ Calif San Diego, Scripps Inst Oceanog, Geosci Res Div, La Jolla, CA 92093 USA.
RP Elsila, JE (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
EM jamie.elsila@nasa.gov
RI Elsila, Jamie/C-9952-2012; Glavin, Daniel/D-6194-2012; Martins,
Zita/H-4860-2015; Dworkin, Jason/C-9417-2012
OI Glavin, Daniel/0000-0001-7779-7765; Martins, Zita/0000-0002-5420-1081;
Dworkin, Jason/0000-0002-3961-8997
NR 5
TC 7
Z9 7
U1 0
U2 11
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 NOV 27
PY 2012
VL 109
IS 48
BP E3288
EP E3288
DI 10.1073/pnas.1213261109
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 053ZN
UT WOS:000312313900001
PM 23064644
ER
PT J
AU Gluscevic, V
Hanson, D
Kamionkowski, M
Hirata, CM
AF Gluscevic, Vera
Hanson, Duncan
Kamionkowski, Marc
Hirata, Christopher M.
TI First CMB constraints on direction-dependent cosmological birefringence
from WMAP-7
SO PHYSICAL REVIEW D
LA English
DT Article
ID DISTANT RADIO-SOURCES; TESTING CPT SYMMETRY; POWER SPECTRA;
GRAVITY-WAVES; POLARIZATION; ANISOTROPY; PROBE; LIMITS; SIGNATURE;
GALAXIES
AB A Chern-Simons coupling of a new scalar field to electromagnetism may give rise to cosmological birefringence, a rotation of the linear polarization of electromagnetic waves as they propagate over cosmological distances. Prior work has sought this rotation, assuming the rotation angle to be uniform across the sky, by looking for the parity-violating TB and EB correlations that a uniform rotation produces in the cosmic microwave background temperature/polarization. However, if the scalar field that gives rise to cosmological birefringence has spatial fluctuations, then the rotation angle may vary across the sky. Here we search for direction-dependent cosmological birefringence in the WMAP-7 data. We report the first cosmic microwave background constraint on the rotation-angle power spectrum C-L(alpha alpha) for multipoles between L = 0 and L = 512. We also obtain a 68% confidence-level upper limit of root C-2(alpha alpha)/(4 pi) less than or similar to 1 degrees on the quadrupole of a scale-invariant rotation-angle power spectrum.
C1 [Gluscevic, Vera; Hanson, Duncan; Kamionkowski, Marc; Hirata, Christopher M.] CALTECH, Pasadena, CA 91125 USA.
[Kamionkowski, Marc] Johns Hopkins Univ Hosp, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Hanson, Duncan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gluscevic, V (reprint author), CALTECH, Mail Code 350-17, Pasadena, CA 91125 USA.
OI Kamionkowski, Marc/0000-0001-7018-2055
FU DOE [DE-FG03-92-ER40701, DOE.DE-SC0006624]; NASADavid and Lucile Packard
Foundation [NNX12AE86G]
FX This work was supported by DOE DE-FG03-92-ER40701, NASA NNX12AE86G, DOE
(DOE.DE-SC0006624), and the David and Lucile Packard Foundation. Part of
the research described in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. Some of
the results in this paper have been derived using the HEALPix package
[31].
NR 49
TC 22
Z9 22
U1 0
U2 3
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD NOV 26
PY 2012
VL 86
IS 10
AR 103529
DI 10.1103/PhysRevD.86.103529
PG 14
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 043NA
UT WOS:000311549300005
ER
PT J
AU Sibeck, DG
Korotova, G
Turner, DL
Angelopoulos, V
Glassmeier, KH
McFadden, JP
AF Sibeck, D. G.
Korotova, G.
Turner, D. L.
Angelopoulos, V.
Glassmeier, K. -H.
McFadden, J. P.
TI Frequency doubling and field-aligned ion streaming in a long-period
poloidal pulsation
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID HIGH-BETA PLASMA; COMPRESSIONAL PC5 PULSATIONS; PITCH-ANGLE
DISTRIBUTIONS; MIRROR INSTABILITY; GEOMAGNETIC-PULSATIONS; ENERGETIC
PARTICLES; ULF PULSATIONS; RING CURRENT; PC-5 WAVES; MAGNETOSPHERE
AB We reexamine a long-period (10-18 min) poloidal pulsation observed by THEMIS-A in the outer dawn magnetosphere from 10: 00 to 12: 30 UT on 7 November 2007. The interval was originally reported by Korotova et al. (2009). Although the nonlinear compressional plasma and magnetic field perturbations observed by THEMIS-A during this interval agree well with model predictions for the linear perturbations associated with antisymmetric waves generated by the ballooning-mirror mode instability, the phase relationships between these perturbations indicates a complex frequency rather than the purely imaginary frequency that theory predicts for the outer dawnside magnetosphere. Variations in the radial plasma velocity confirm that a phase-locked north/south oscillation in the equatorial line of nodes associated with the ballooning-mirror mode waves doubles the frequency of the compressional component of the magnetic field during these pulsations. The same velocity and magnetic field perturbations exclude explanations for the frequency doubling in terms of spatial gradients sweeping back and forth across the spacecraft or drift-bounce resonances. Azimuthal electric fields associated with the pulsations generate field-aligned anisotropies in the pitch angle distributions that become more prominent with increasing ion energy due to the presence of drift-shell splitting and radial flux gradients that steepen with increasing energy. Although there was no evidence for drift-bounce interactions during this event, the role of such events in ion energization in other events and at other locations remains to be evaluated.
C1 [Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Korotova, G.] IZMIRAN, Troitsk 142092, Russia.
[Korotova, G.] Univ Maryland, IPST, College Pk, MD 20742 USA.
[Turner, D. L.; Angelopoulos, V.] Univ Calif Los Angeles, ESS, Los Angeles, CA USA.
[Glassmeier, K. -H.] TUB, Inst Geophys & Extraterr Phys, Braunschweig, Germany.
[McFadden, J. P.] Univ Calif Berkeley, SSL, Berkeley, CA 94720 USA.
RP Sibeck, DG (reprint author), NASA, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA.
EM david.g.sibeck@nasa.gov
RI Turner, Drew/G-3224-2012
FU NASA's THEMIS Program; NASA GSFC [NNX09AV52G]
FX Research at GSFC was funded by NASA's THEMIS Program. Research at the
University of Maryland was supported by NASA GSFC grant NNX09AV52G. D.
G. S. thanks both referees, C. Z. Cheng, and K. Takahashi for many
helpful suggestions and boundless patience. V. Kondratovich aided in
analyzing the pulsations.
NR 48
TC 7
Z9 7
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 NOV 21
PY 2012
VL 117
AR A11215
DI 10.1029/2011JA017473
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 043SD
UT WOS:000311567000001
ER
PT J
AU Jaramillo-Botero, A
An, Q
Cheng, MJ
Goddard, WA
Beegle, LW
Hodyss, R
AF Jaramillo-Botero, Andres
An, Qi
Cheng, Mu-Jeng
Goddard, William A., III
Beegle, Luther W.
Hodyss, Robert
TI Hypervelocity Impact Effect of Molecules from Enceladus' Plume and
Titan's Upper Atmosphere on NASA's Cassini Spectrometer from Reactive
Dynamics Simulation
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID FORCE-FIELD; REAXFF; IONS
AB The NASA/ESA Cassini probe of Saturn analyzed the molecular composition of plumes emanating from one of its moons, Enceladus, and the upper atmosphere of another, Titan. However, interpretation of this data is complicated by the hypervelocity (HV) flybys of up to similar to 18 km/sec that cause substantial molecular fragmentation. To interpret this data we use quantum mechanical based reactive force fields to simulate the HV impact of various molecular species and ice clathrates on oxidized titanium surfaces mimicking those in Cassini's neutral and ion mass spectrometer (INMS). The predicted velocity dependent fragmentation patterns and composition mixing ratios agree with INMS data providing the means for identifying the molecules in the plume. We used our simulations to predict the surface damage from the HV impacts on the INMS interior walls, which we suggest acts as a titanium sublimation pump that could alter the instrument's readings. These results show how the theory can identify chemical events from hypervelocity impacts in space plumes and atmospheres, providing in turn clues to the internal structure of the corresponding sources (e.g., Enceladus). This may be valuable in steering modifications in future missions.
C1 [Jaramillo-Botero, Andres; An, Qi; Cheng, Mu-Jeng; Goddard, William A., III] CALTECH, Mat & Proc Simulat Ctr, Pasadena, CA 91125 USA.
[Beegle, Luther W.; Hodyss, Robert] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Jaramillo-Botero, A (reprint author), CALTECH, Mat & Proc Simulat Ctr, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM ajaramil@caltech.edu; wag@wag.caltech.edu
RI An, Qi/I-6985-2012; Cheng, Mu-Jeng/I-7316-2012
FU Department of Energy National Nuclear Security Administration
[DE-FC52-08NA28613]
FX Thanks to Adri van Duin and colleagues for providing the basic
TiO2-H2O ReaxFF force field, Patrick L. Theofanis
for his suggestions on the manuscript, and Chi Feng (SURF Fellow at
Caltech) for his contributions to hexane simulations. This work was
performed at Caltech and JPL under a contract with the National
Aeronautics and Space Administration (NASA). Partial support was
provided by the Department of Energy National Nuclear Security
Administration under Contract No. DE-FC52-08NA28613 (Caltech PSAAP).
NR 17
TC 4
Z9 4
U1 2
U2 43
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 NOV 21
PY 2012
VL 109
IS 21
AR 213201
DI 10.1103/PhysRevLett.109.213201
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 041CT
UT WOS:000311374500003
PM 23215593
ER
PT J
AU Garry, WB
Robinson, MS
Zimbelman, JR
Bleacher, JE
Hawke, BR
Crumpler, LS
Braden, SE
Sato, H
AF Garry, W. B.
Robinson, M. S.
Zimbelman, J. R.
Bleacher, J. E.
Hawke, B. R.
Crumpler, L. S.
Braden, S. E.
Sato, H.
TI The origin of Ina: Evidence for inflated lava flows on the Moon
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MARTIAN FLOOD LAVAS; SNAKE RIVER PLAIN; STEEP-SIDED DOMES; BASALTIC
LAVA; LABORATORY SIMULATIONS; KILAUEA VOLCANO; THERMAL MODELS; MAGELLAN
DATA; PAHOEHOE; EMPLACEMENT
AB Ina is an enigmatic volcanic feature on the Moon known for its irregularly shaped mounds, the origin of which has been debated since the Apollo Missions. Three main units are observed on the floor of the depression (2.9 km across, <= 64 m deep) located at the summit of a low-shield volcano: irregularly shaped mounds up to 20 m tall, a lower unit 1 to 5 m in relief that surrounds the mounds, and blocky material. Analyses of Lunar Reconnaissance Orbiter Camera images and topography show that features in Ina are morphologically similar to terrestrial inflated lava flows. Comparison of these unusual lunar mounds and possible terrestrial analogs leads us to hypothesize that features in Ina were formed through lava flow inflation processes. While the source of the lava remains unclear, this new model suggests that as the mounds inflated, breakouts along their margins served as sources for surface flows that created the lower morphologic unit. Over time, mass wasting of both morphologic units has exposed fresh surfaces observed in the blocky unit. Ina is different than the terrestrial analogs presented in this study in that the lunar features formed within a depression, no vent sources are observed, and no cracks are observed on the mounds. However, lava flow inflation processes explain many of the morphologic relationships observed in Ina and are proposed to be analogous with inflated lava flows on Earth.
C1 [Garry, W. B.; Bleacher, J. E.] NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Garry, W. B.] Planetary Sci Inst, Tucson, AZ USA.
[Robinson, M. S.; Braden, S. E.; Sato, H.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
[Zimbelman, J. R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
[Hawke, B. R.] Univ Hawaii Manoa, SOEST, Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Crumpler, L. S.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM USA.
RP Garry, WB (reprint author), NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Code 698, Greenbelt, MD 20771 USA.
EM william.b.garry@nasa.gov
RI Garry, Brent/I-5920-2013; Bleacher, Jacob/D-1051-2012
OI Bleacher, Jacob/0000-0002-8499-4828
FU NASA [NNX11AG90G, NNX08AM77G]; LROC Science Operations; NASA Moon and
Mars Analog Mission Activities (MMAMA) [NNX08AR76G, NNX09AW15G,
08-MMAMA08-016]; NASA Planetary Geology and Geophysics (PGG)
[NNX09AD88G]; Smithsonian Scholarly Studies Program [FY11]
FX Lunar research was supported by the NASA Lunar Reconnaissance Orbiter
Participating Scientist Program grants NNX11AG90G (PI: Garry),
NNX08AM77G (PI: Hawke), and LROC Science Operations (PI: Robinson).
Field work in Hawai'i, Idaho, and New Mexico was supported by the
following grants: NASA Moon and Mars Analog Mission Activities (MMAMA)
NNX08AR76G and NNX09AW15G (PI: Garry), 08-MMAMA08-016 (PI: Bleacher),
NASA Planetary Geology and Geophysics (PGG) NNX09AD88G (PI: Zimbelman),
Smithsonian Scholarly Studies Program FY11 (PI: Zimbelman). The authors
would like to thank the Lunar Reconnaissance Orbiter Project Office at
NASA Goddard Space Flight Center, the LROC Science Operations Center at
Arizona State University, El Malpais National Monument in New Mexico,
Craters of the Moon National Monument in Idaho, plus William J. Clancey
and Maarten Sierhuis for their assistance with field work in Idaho and
New Mexico. Thank you to Lazlo Keszthelyi, Peter H. Schultz, and an
anonymous reviewer for their time and thorough reviews of the
manuscript.
NR 74
TC 6
Z9 7
U1 0
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD NOV 20
PY 2012
VL 117
AR E00H31
DI 10.1029/2011JE003981
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 043RR
UT WOS:000311565100001
ER
PT J
AU Abadie, J
Abbott, BP
Abbott, R
Abbott, TD
Abernathy, M
Accadia, T
Acernese, F
Adams, C
Adhikari, RX
Affeldt, C
Agathos, M
Agatsuma, K
Ajith, P
Allen, B
Ceron, EA
Amariutei, D
Anderson, SB
Anderson, WG
Arai, K
Arain, MA
Araya, MC
Aston, SM
Astone, P
Atkinson, D
Aufmuth, P
Aulbert, C
Aylott, BE
Babak, S
Baker, P
Ballardin, G
Ballmer, S
Barayoga, JCB
Barker, D
Barone, F
Barr, B
Barsotti, L
Barsuglia, M
Barton, MA
Bartos, I
Bassiri, R
Bastarrika, M
Basti, A
Batch, J
Bauchrowitz, J
Bauer, TS
Bebronne, M
Beck, D
Behnke, B
Bejger, M
Beker, MG
Bell, AS
Belopolski, I
Benacquista, M
Berliner, JM
Bertolini, A
Betzwieser, J
Beveridge, N
Beyersdorf, PT
Bilenko, IA
Billingsley, G
Birch, J
Biswas, R
Bitossi, M
Bizouard, MA
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CA LIGO Sci Collaboration Virgo Colla
TI SEARCH FOR GRAVITATIONAL WAVES ASSOCIATED WITH GAMMA-RAY BURSTS DURING
LIGO SCIENCE RUN 6 AND VIRGO SCIENCE RUNS 2 AND 3
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; gamma-ray burst: general; gravitational waves
ID NEUTRON STAR BINARIES; GIANT FLARE; JET BREAKS; APRIL 1998; REDSHIFT
DISTRIBUTION; PRECURSOR ACTIVITY; RELATIVISTIC JETS; UNUSUAL SUPERNOVA;
COMPACT BINARIES; LOCAL UNIVERSE
AB We present the results of a search for gravitational waves associated with 154 gamma-ray bursts (GRBs) that were detected by satellite-based gamma-ray experiments in 2009-2010, during the sixth LIGO science run and the second and third Virgo science runs. We perform two distinct searches: a modeled search for coalescences of either two neutron stars or a neutron star and black hole, and a search for generic, unmodeled gravitational-wave bursts. We find no evidence for gravitational-wave counterparts, either with any individual GRB in this sample or with the population as a whole. For all GRBs we place lower bounds on the distance to the progenitor, under the optimistic assumption of a gravitational-wave emission energy of 10(-2) M-circle dot c(2) at 150 Hz, with a median limit of 17 Mpc. For short-hard GRBs we place exclusion distances on binary neutron star and neutron-star-black-hole progenitors, using astrophysically motivated priors on the source parameters, with median values of 16 Mpc and 28 Mpc, respectively. These distance limits, while significantly larger than for a search that is not aided by GRB satellite observations, are not large enough to expect a coincidence with a GRB. However, projecting these exclusions to the sensitivities of Advanced LIGO and Virgo, which should begin operation in 2015, we find that the detection of gravitational waves associated with GRBs will become quite possible.
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Neri, Igor/0000-0002-9047-9822; Shaddock, Daniel/0000-0002-6885-3494;
Postiglione, Fabio/0000-0003-0628-3796; Rocchi,
Alessio/0000-0002-1382-9016; Martelli, Filippo/0000-0003-3761-8616;
Miao, Haixing/0000-0003-4101-9958; Nelson, John/0000-0002-6928-617X;
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Stefan/0000-0001-7758-7493; Lee, Chang-Hwan/0000-0003-3221-1171;
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Alberto/0000-0002-6254-1617; Steinlechner,
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Christian/0000-0003-4993-2055; mosca, simona/0000-0001-7869-8275;
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Isidoro/0000-0002-0083-7228; Prato, Mirko/0000-0002-2188-8059; Travasso,
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FU United States National Science Foundation; Science and Technology
Facilities Council of the United Kingdom; Max-Planck-Society; State of
Niedersachsen/Germany; Australian Research Council; International
Science Linkages program of the Commonwealth of Australia; Council of
Scientific and Industrial Research of India; Istituto Nazionale di
Fisica Nucleare of Italy; Spanish Ministerio de Economia y
Competitividad; Conselleria d'Economia Hisenda i Innovacio of the Govern
de les Illes Balears; Foundation for Fundamental Research on Matter;
Polish Ministry of Science and Higher Education; FOCUS Programme of
Foundation for Polish Science; Royal Society; Scottish Funding Council;
Scottish Universities Physics Alliance; National Aeronautics and Space
Administration; Carnegie Trust; Leverhulme Trust; David and Lucile
Packard Foundation; Research Corporation; Alfred P. Sloan Foundation;
Netherlands Organisation for Scientific Research
FX We are indebted to the observers of the electromagnetic events and the
Gamma-ray burst Coordinates Network for providing us with valuable data.
The authors gratefully acknowledge the support of the United States
National Science Foundation for the construction and operation of the
LIGO Laboratory, the Science and Technology Facilities Council of the
United Kingdom, the Max-Planck-Society, and the State of
Niedersachsen/Germany for support of the construction and operation of
the GEO600 detector, and the Italian Istituto Nazionale di Fisica
Nucleare and the French Centre National de la Recherche Scientifique for
the construction and operation of the Virgo detector. The authors also
gratefully acknowledge the support of the research by these agencies and
by the Australian Research Council, the International Science Linkages
program of the Commonwealth of Australia, the Council of Scientific and
Industrial Research of India, the Istituto Nazionale di Fisica Nucleare
of Italy, the Spanish Ministerio de Economia y Competitividad, the
Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes
Balears, the Foundation for Fundamental Research on Matter supported by
the Netherlands Organisation for Scientific Research, the Polish
Ministry of Science and Higher Education, the FOCUS Programme of
Foundation for Polish Science, the Royal Society, the Scottish Funding
Council, the Scottish Universities Physics Alliance, the National
Aeronautics and Space Administration, the Carnegie Trust, the Leverhulme
Trust, the David and Lucile Packard Foundation, the Research
Corporation, and the Alfred P. Sloan Foundation. This document has been
assigned LIGO Laboratory document number LIGO-P1000121-v10.
NR 144
TC 66
Z9 66
U1 7
U2 99
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 NOV 20
PY 2012
VL 760
IS 1
AR 12
DI 10.1088/0004-637X/760/1/12
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 035DD
UT WOS:000310922200012
ER
PT J
AU Barry, RK
Demory, BO
Segransan, D
Forveille, T
Danchi, WC
Di Folco, E
Queloz, D
Spooner, HR
Torres, G
Traub, WA
Delfosse, X
Mayor, M
Perrier, C
Udry, S
AF Barry, R. K.
Demory, B. -O.
Segransan, D.
Forveille, T.
Danchi, W. C.
Di Folco, E.
Queloz, D.
Spooner, H. R.
Torres, G.
Traub, W. A.
Delfosse, X.
Mayor, M.
Perrier, C.
Udry, S.
TI A PRECISE PHYSICAL ORBIT FOR THE M-DWARF BINARY GLIESE 268
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: general; stars: individual (Gliese 268); techniques:
interferometric; techniques: radial velocities
ID LOW-MASS STARS; ECLIPSING BINARY; ACCURATE MASSES; SPECTROSCOPIC
BINARIES; EVOLUTIONARY MODELS; LAMBDA-VIRGINIS; MAIN-SEQUENCE;
INTERFEROMETER; SYSTEM
AB We report high-precision interferometric and radial velocity (RV) observations of the M-dwarf binary Gl 268. Combining measurements conducted using the IOTA interferometer and the ELODIE and Harvard Center for Astrophysics RV instruments leads to a mass of 0.22596 +/- 0.00084 M-circle dot for component A and 0.19230 +/- 0.00071 M-circle dot for component B. The system parallax as determined by these observations is 0.1560 +/- 0.0030 arcsec-a measurement with 1.9% uncertainty in excellent agreement with Hipparcos (0.1572 +/- 0.0033). The absolute H-band magnitudes of the component stars are not well constrained by these measurements; however, we can place an approximate upper limit of 7.95 and 8.1 for Gl 268A and B, respectively. We test these physical parameters against the predictions of theoretical models that combine stellar evolution with high fidelity, non-gray atmospheric models. Measured and predicted values are compatible within 2 sigma. These results are among the most precise masses measured for visual binaries and compete with the best adaptive optics and eclipsing binary results.
C1 [Barry, R. K.; Danchi, W. C.] NASA, Goddard Space Flight Ctr, Lab Exoplanets & Stellar Astrophys, Greenbelt, MD 20771 USA.
[Demory, B. -O.; Segransan, D.; Di Folco, E.; Queloz, D.; Udry, S.] MIT, Cambridge, MA 02139 USA.
[Forveille, T.; Delfosse, X.; Mayor, M.; Perrier, C.] Univ Geneva, Observ Geneva, CH-1290 Versoix, Switzerland.
[Spooner, H. R.] Univ Maryland, College Pk, MD 20742 USA.
[Torres, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02136 USA.
[Traub, W. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Barry, RK (reprint author), NASA, Goddard Space Flight Ctr, Lab Exoplanets & Stellar Astrophys, Code 667, Greenbelt, MD 20771 USA.
EM Richard.K.Barry@nasa.gov
OI Demory, Brice-Olivier/0000-0002-9355-5165
FU National Aeronautics and Space Administration; University of Grenoble
Observatory; Jet Propulsion Laboratory; California Association for
Research in Astronomy; Harvard-Smithsonian Center for Astrophysics;
Fonds National Suisse de la Recherche Scientifique
FX We are grateful to the National Aeronautics and Space Administration,
the University of Grenoble Observatory, Jet Propulsion Laboratory, the
California Association for Research in Astronomy, and to the
Harvard-Smithsonian Center for Astrophysics for support of this
research. We are also grateful for the work on software to reduce the
interferometric data from IOTA by J. Monnier. B.O.D. acknowledges the
support of the Fonds National Suisse de la Recherche Scientifique.
R.K.B. acknowledges the technical editing assistance of C. M. Morales
Sabogal.
NR 46
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U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 20
PY 2012
VL 760
IS 1
AR 55
DI 10.1088/0004-637X/760/1/55
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 035DD
UT WOS:000310922200055
ER
PT J
AU Bryans, P
Pesnell, WD
AF Bryans, P.
Pesnell, W. D.
TI THE EXTREME-ULTRAVIOLET EMISSION FROM SUN-GRAZING COMETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets: general; comets: individual (C/2011 N3, C/2011 W3); Sun: corona;
Sun: general
ID PHOTOIONIZATION CROSS-SECTIONS; IONIZATION RATE COEFFICIENTS; X-RAY;
SUNGRAZING COMETS; ELEMENTS HYDROGEN; ATOMIC DATABASE; CHARGE-TRANSFER;
ANALYTIC FITS; SOLAR; SPECTRUM
AB The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory has observed two Sun-grazing comets as they passed through the solar atmosphere. Both passages resulted in a measurable enhancement of extreme-ultraviolet (EUV) radiance in several of the AIA bandpasses. We explain this EUV emission by considering the evolution of the cometary atmosphere as it interacts with the ambient solar atmosphere. Molecules in the comet rapidly sublimate as it approaches the Sun. They are then photodissociated by the solar radiation field to create atomic species. Subsequent ionization of these atoms produces a higher abundance of ions than normally present in the corona and results in EUV emission in the wavelength ranges of the AIA telescope passbands.
C1 [Bryans, P.] NASA, ADNET Syst Inc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Bryans, P (reprint author), NASA, ADNET Syst Inc, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
RI Pesnell, William/D-1062-2012
OI Pesnell, William/0000-0002-8306-2500
FU Solar Dynamics Observatory
FX Research was supported by the Solar Dynamics Observatory. We acknowledge
many helpful comments and suggestions from K. Battams, J.C. Brown, H.S.
Hudson, W. Liu, P. Saint-Hilaire, and C.J. Schrijver.
NR 39
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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 NOV 20
PY 2012
VL 760
IS 1
AR 18
DI 10.1088/0004-637X/760/1/18
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 035DD
UT WOS:000310922200018
ER
PT J
AU Gomez, HL
Krause, O
Barlow, MJ
Swinyard, BM
Owen, PJ
Clark, CJR
Matsuura, M
Gomez, EL
Rho, J
Besel, MA
Bouwman, J
Gear, WK
Henning, T
Ivison, RJ
Polehampton, ET
Sibthorpe, B
AF Gomez, H. L.
Krause, O.
Barlow, M. J.
Swinyard, B. M.
Owen, P. J.
Clark, C. J. R.
Matsuura, M.
Gomez, E. L.
Rho, J.
Besel, M. -A.
Bouwman, J.
Gear, W. K.
Henning, Th.
Ivison, R. J.
Polehampton, E. T.
Sibthorpe, B.
TI A COOL DUST FACTORY IN THE CRAB NEBULA: A HERSCHEL STUDY OF THE
FILAMENTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; ISM: individual objects (Crab Nebula); ISM: supernova
remnants; submillimeter: ISM
ID LASER MAGNETIC-RESONANCE; CORE-COLLAPSE SUPERNOVAE;
SPITZER-SPACE-TELESCOPE; LARGE-MAGELLANIC-CLOUD; CHEMICAL EVOLUTION;
OPTICAL-PROPERTIES; SPIRE INSTRUMENT; EARLY UNIVERSE; II SUPERNOVAE;
COLD DUST
AB Whether supernovae are major sources of dust in galaxies is a long-standing debate. We present infrared and submillimeter photometry and spectroscopy from the Herschel Space Observatory of the Crab Nebula between 51 and 670 mu m as part of the Mass Loss from Evolved StarS program. We compare the emission detected with Herschel with multiwavelength data including millimeter, radio, mid-infrared, and archive optical images. We carefully remove the synchrotron component using the Herschel and Planck fluxes measured in the same epoch. The contribution from line emission is removed using Herschel spectroscopy combined with Infrared Space Observatory archive data. Several forbidden lines of carbon, oxygen, and nitrogen are detected where multiple velocity components are resolved, deduced to be from the nitrogen-depleted, carbon-rich ejecta. No spectral lines are detected in the SPIRE wavebands; in the PACS bands, the line contribution is 5% and 10% at 70 and 100 mu m and negligible at 160 mu m. After subtracting the synchrotron and line emission, the remaining far-infrared continuum can be fit with two dust components. Assuming standard interstellar silicates, the mass of the cooler component is 0.24(-0.08)(+0.32)M(circle dot) for T = 28.1(-3.2)(+5.5)K. Amorphous carbon grains require 0.11 +/- 0.01M(circle dot) of dust with T = 33.8(-1.8)(+2.3)K. A single temperature modified blackbody with 0.14M(circle dot) and 0.08M(circle dot) for silicate and carbon dust, respectively, provides an adequate fit to the far-infrared region of the spectral energy distribution but is a poor fit at 24-500 mu m. The Crab Nebula has condensed most of the relevant refractory elements into dust, suggesting the formation of dust in core-collapse supernova ejecta is efficient.
C1 [Gomez, H. L.; Clark, C. J. R.; Gomez, E. L.; Gear, W. K.] Cardiff Univ, Sch Phys & Astron, The Parade, Cardiff CF24 3AA, S Glam, Wales.
[Krause, O.; Besel, M. -A.; Bouwman, J.; Henning, Th.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Barlow, M. J.; Swinyard, B. M.; Owen, P. J.; Matsuura, M.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Swinyard, B. M.; Polehampton, E. T.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England.
[Gomez, E. L.] Las Cumbres Obsevratory Global Telescope Network, Goleta, CA 93117 USA.
[Rho, J.] NASA, Ames Res Ctr, Univ Space Res Assoc, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
[Ivison, R. J.; Sibthorpe, B.] Royal Observ Edinburgh, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Polehampton, E. T.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1J 1B1, Canada.
RP Gomez, HL (reprint author), Cardiff Univ, Sch Phys & Astron, The Parade, Cardiff CF24 3AA, S Glam, Wales.
RI Barlow, Michael/A-5638-2009; Ivison, R./G-4450-2011
OI Barlow, Michael/0000-0002-3875-1171; Ivison, R./0000-0001-5118-1313
FU Las Cumbres Observatory; National Aeronautics and Space Administration;
BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany);
ASI/INAF (Italy); CICYT/MCYT(Spain); CSA (Canada); NAOC (China); CEA
(France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB
(Sweden); STFC (UK); UKSA (UK); NASA (USA)
FX We thank the referee Tea Temim for her constructive and helpful referee
report. This research made use of APLpy, an open-source plotting package
for Python hosted at http://aplpy.github.com. We thank Robbie Auld, Eli
Dwek, Stuart Lowe, Takaya Nozawa, and Matt Smith for informative
discussions and J D Armstrong for support with the Faulkes Telescope
North. H. L. G. acknowledges the support of Las Cumbres Observatory.
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. 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); INAF-IFSI/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 Univ.
(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); SNSB (Sweden);
STFC, UKSA (UK); and NASA (USA). HIPE is a joint development by the
Herschel Science Ground Segment Consortium, consisting of ESA, the NASA
Herschel Science Center and the HIFI, PACS and SPIRE consortia.
NR 95
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U1 0
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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 NOV 20
PY 2012
VL 760
IS 1
AR 96
DI 10.1088/0004-637X/760/1/96
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 035DD
UT WOS:000310922200096
ER
PT J
AU Hathaway, DH
AF Hathaway, David H.
TI SUPERGRANULES AS PROBES OF THE SUN'S MERIDIONAL CIRCULATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE convection; Sun: rotation
ID MICHELSON DOPPLER IMAGER; WAVE-LIKE PROPERTIES; DIFFERENTIAL ROTATION;
MAGNETIC-FIELDS; SOLAR CONVECTION; LOCAL HELIOSEISMOLOGY; VELOCITY
FIELDS; FLOW; EVOLUTION; TRANSPORT
AB Recent analysis revealed that supergranules (convection cells seen at the Sun's surface) are advected by the zonal flows at depths equal to the widths of the cells themselves. Here we probe the structure of the meridional circulation by cross-correlating maps of the Doppler velocity signal using a series of successively longer time lags between maps. We find that the poleward meridional flow decreases in amplitude with time lag and reverses direction to become an equatorward return flow at time lags >24 hr. These cross-correlation results are dominated by larger and deeper cells at longer time lags. (The smaller cells have shorter lifetimes and do not contribute to the correlated signal at longer time lags.) We determine the characteristic cell size associated with each time lag by comparing the equatorial zonal flows measured at different time lags with the zonal flows associated with different cell sizes from a Fourier analysis. This association gives a characteristic cell size of similar to 50 Mm at a 24 hr time lag. This indicates that the poleward meridional flow returns equatorward at depths >50 Mm-just below the base of the surface shear layer. A substantial and highly significant equatorward flow (4.6 +/- 0.4 m s(-1)) is found at a time lag of 28 hr corresponding to a depth of similar to 70 Mm. This represents one of the first positive detections of the Sun's meridional return flow and illustrates the power of using supergranules to probe the Sun's internal dynamics.
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 Heliophysics Causes and Consequences of the Minimum of Solar Cycle 23/24
Program; Living With a Star Program to NASA Marshall Space Flight Center
FX The author thanks NASA for its support of this research through grants
from the Heliophysics Causes and Consequences of the Minimum of Solar
Cycle 23/24 Program and the Living With a Star Program to NASA Marshall
Space Flight Center. He is indebted to Ron Moore and Lisa (Rightmire)
Upton and an anonymous referee whose comments greatly improved the
manuscript and to John Beck who produced the temporally filtered data
from the original MDI Doppler data. He also thanks the American
taxpayers who support scientific research in general and this research
in particular. SOHO is a project of international cooperation between
ESA and NASA.
NR 47
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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 NOV 20
PY 2012
VL 760
IS 1
AR 84
DI 10.1088/0004-637X/760/1/84
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 035DD
UT WOS:000310922200084
ER
PT J
AU Hesman, BE
Bjoraker, GL
Sada, PV
Achterberg, RK
Jennings, DE
Romani, PN
Lunsford, AW
Fletcher, LN
Boyle, RJ
Simon-Miller, AA
Nixon, CA
Irwin, PGJ
AF Hesman, B. E.
Bjoraker, G. L.
Sada, P. V.
Achterberg, R. K.
Jennings, D. E.
Romani, P. N.
Lunsford, A. W.
Fletcher, L. N.
Boyle, R. J.
Simon-Miller, A. A.
Nixon, C. A.
Irwin, P. G. J.
TI ELUSIVE ETHYLENE DETECTED IN SATURN'S NORTHERN STORM REGION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: individual
(Saturn)
ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; OUTER PLANETS; THERMAL STRUCTURE;
TEMPERATURES; ATMOSPHERE; PAIRS; STRATOSPHERE; DISTURBANCE; ABUNDANCE;
EMISSION
AB The massive eruption at 40 degrees N (planetographic latitude) on Saturn in 2010 December has produced significant and lasting effects in the northern hemisphere on temperature and species abundances. The northern storm region was observed on many occasions in 2011 by Cassini's Composite Infrared Spectrometer (CIRS). In 2011 May, temperatures in the stratosphere greater than 200 K were derived from CIRS spectra in the regions referred to as "beacons" (warm regions in the stratosphere). Ethylene has been detected in the beacon region in Saturn's northern storm region using CIRS. Ground-based observations using the high-resolution spectrometer Celeste on the McMath-Pierce Telescope on 2011 May 15 were used to confirm the detection and improve the altitude resolution in the retrieved profile. The derived ethylene profile from the CIRS data gives a C2H4 mole fraction of 5.9 +/- 4.5 x 10(-7) at 0.5 mbar, and from Celeste data it gives 2.7 +/- 0.45 x 10(-6) at 0.1 mbar. This is two orders of magnitude higher than the amount measured in the ultraviolet at other latitudes prior to the storm. It is also much higher than predicted by photochemical models, indicating that perhaps another production mechanism is required or a loss mechanism is being inhibited.
C1 [Hesman, B. E.; Achterberg, R. K.; Nixon, C. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Hesman, B. E.; Bjoraker, G. L.; Achterberg, R. K.; Jennings, D. E.; Romani, P. N.; Simon-Miller, A. A.; Nixon, C. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sada, P. V.] Univ Monterrey, Dept Fis & Matemat, Garza Garcia 66238, NL, Mexico.
[Lunsford, A. W.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Fletcher, L. N.] Clarendon Lab, Oxford OX1 3PU, England.
[Boyle, R. J.] Dickinson Coll, Dept Phys & Astron, Carlisle, PA 17013 USA.
[Hesman, B. E.; Achterberg, R. K.; Nixon, C. A.] CRESST, Greenbelt, MD 20771 USA.
RP Hesman, BE (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM brigette.e.hesman@nasa.gov
RI Nixon, Conor/A-8531-2009; Fletcher, Leigh/D-6093-2011; Simon,
Amy/C-8020-2012;
OI Nixon, Conor/0000-0001-9540-9121; Fletcher, Leigh/0000-0001-5834-9588;
Simon, Amy/0000-0003-4641-6186; Irwin, Patrick/0000-0002-6772-384X
FU NASA Cassini/CIRS project; NASA Planetary Astronomy (PAST) Program
[NNX11AJ47G]; NASA Cassini Data Analysis Participating Scientists
(CDAPS) Program [NNX12AC24G]
FX The authors thank the Cassini/CIRS calibration team for their assistance
in the calibration of these data sets. The authors also thank the
McMath-Pierce Telescope staff for their assistance during these
observations. This research was supported by the NASA Cassini/CIRS
project, by the NASA Planetary Astronomy (PAST) Program grant number
NNX11AJ47G, and the NASA Cassini Data Analysis Participating Scientists
(CDAPS) Program grant number NNX12AC24G. The National Solar Observatory
is operated by the Association of Universities for Research in Astronomy
under contract for the National Science Foundation.
NR 25
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U1 0
U2 24
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 NOV 20
PY 2012
VL 760
IS 1
AR 24
DI 10.1088/0004-637X/760/1/24
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 035DD
UT WOS:000310922200024
ER
PT J
AU Huber, D
Ireland, MJ
Bedding, TR
Brandao, IM
Piau, L
Maestro, V
White, TR
Bruntt, H
Casagrande, L
Molenda-Zakowicz, J
Aguirre, VS
Sousa, SG
Barclay, T
Burke, CJ
Chaplin, WJ
Christensen-Dalsgaard, J
Cunha, MS
De Ridder, J
Farrington, CD
Frasca, A
Garcia, RA
Gilliland, RL
Goldfinger, PJ
Hekker, S
Kawaler, SD
Kjeldsen, H
McAlister, HA
Metcalfe, TS
Miglio, A
Monteiro, MJPFG
Pinsonneault, MH
Schaefer, GH
Stello, D
Stumpe, MC
Sturmann, J
Sturmann, L
ten Brummelaar, TA
Thompson, MJ
Turner, N
Uytterhoeven, K
AF Huber, D.
Ireland, M. J.
Bedding, T. R.
Brandao, I. M.
Piau, L.
Maestro, V.
White, T. R.
Bruntt, H.
Casagrande, L.
Molenda-Zakowicz, J.
Aguirre, V. Silva
Sousa, S. G.
Barclay, T.
Burke, C. J.
Chaplin, W. J.
Christensen-Dalsgaard, J.
Cunha, M. S.
De Ridder, J.
Farrington, C. D.
Frasca, A.
Garcia, R. A.
Gilliland, R. L.
Goldfinger, P. J.
Hekker, S.
Kawaler, S. D.
Kjeldsen, H.
McAlister, H. A.
Metcalfe, T. S.
Miglio, A.
Monteiro, M. J. P. F. G.
Pinsonneault, M. H.
Schaefer, G. H.
Stello, D.
Stumpe, M. C.
Sturmann, J.
Sturmann, L.
ten Brummelaar, T. A.
Thompson, M. J.
Turner, N.
Uytterhoeven, K.
TI FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND
CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: late-type; stars: oscillations (including pulsations);
techniques: interferometric; techniques: photometric
ID SOLAR-LIKE OSCILLATIONS; RED GIANT STARS; EFFECTIVE TEMPERATURE SCALE;
EXOPLANET HOST STARS; ALPHA-CENTAURI-B; 1ST 4 MONTHS; BOLOMETRIC
CORRECTIONS; MAIN-SEQUENCE; SPECTROSCOPIC PARAMETERS; PHOTOMETRIC SYSTEM
AB We present results of a long-baseline interferometry campaign using the PAVO beam combiner at the CHARA Array to measure the angular sizes of five main-sequence stars, one subgiant and four red giant stars for which solar-like oscillations have been detected by either Kepler or CoRoT. By combining interferometric angular diameters, Hipparcos parallaxes, asteroseismic densities, bolometric fluxes, and high-resolution spectroscopy, we derive a full set of near-model-independent fundamental properties for the sample. We first use these properties to test asteroseismic scaling relations for the frequency of maximum power (nu(max)) and the large frequency separation (Delta nu). We find excellent agreement within the observational uncertainties, and empirically show that simple estimates of asteroseismic radii for main-sequence stars are accurate to less than or similar to 4%. We furthermore find good agreement of our measured effective temperatures with spectroscopic and photometric estimates with mean deviations for stars between T-eff = 4600-6200 K of -22 +/- 32 K (with a scatter of 97 K) and -58 +/- 31 K (with a scatter of 93 K), respectively. Finally, we present a first comparison with evolutionarymodels, and find differences between observed and theoretical properties for the metal-rich main-sequence star HD 173701. We conclude that the constraints presented in this study will have strong potential for testing stellar model physics, in particular when combined with detailed modeling of individual oscillation frequencies.
C1 [Huber, D.; Ireland, M. J.; Bedding, T. R.; Maestro, V.; White, T. R.; Stello, D.] Univ Sydney, Sch Phys, SIfA, Sydney, NSW 2006, Australia.
[Huber, D.; Barclay, T.] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ireland, M. J.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia.
[Ireland, M. J.] Australian Astron Observ, Epping, NSW 1710, Australia.
[Brandao, I. M.; Sousa, S. G.; Cunha, M. S.; Monteiro, M. J. P. F. G.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Brandao, I. M.; Sousa, S. G.; Cunha, M. S.; Monteiro, M. J. P. F. G.] Univ Porto, Fac Ciencias, P-4150762 Oporto, Portugal.
[Piau, L.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48823 USA.
[Bruntt, H.; Aguirre, V. Silva; Chaplin, W. J.; Christensen-Dalsgaard, J.; Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
[Casagrande, L.] Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Molenda-Zakowicz, J.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland.
[Burke, C. J.; Stumpe, M. C.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Chaplin, W. J.; Miglio, A.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[De Ridder, J.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Farrington, C. D.; Goldfinger, P. J.; McAlister, H. A.; Schaefer, G. H.; Sturmann, J.; Sturmann, L.; ten Brummelaar, T. A.; Turner, N.] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA.
[Frasca, A.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy.
[Garcia, R. A.] Univ Paris 07, CEA DSM CNRS, Lab AIM, Ctr Saclay,IRFU SAp, F-91191 Gif Sur Yvette, France.
[Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Metcalfe, T. S.] Space Sci Inst, Boulder, CO 80301 USA.
[Pinsonneault, M. H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Thompson, M. J.] NCAR, High Altitude Observ, Boulder, CO 80307 USA.
[Uytterhoeven, K.] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Uytterhoeven, K.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain.
RP Huber, D (reprint author), Univ Sydney, Sch Phys, SIfA, Sydney, NSW 2006, Australia.
EM daniel.huber@nasa.gov
RI Sousa, Sergio/I-7466-2013; Brandao, Isa/M-5172-2013; Monteiro, Mario
J.P.F.G./B-4715-2008;
OI Garcia, Rafael/0000-0002-8854-3776; Kawaler, Steven/0000-0002-6536-6367;
Sousa, Sergio/0000-0001-9047-2965; Brandao, Isa/0000-0002-1153-0942;
Monteiro, Mario J.P.F.G./0000-0003-0513-8116; Cunha,
Margarida/0000-0001-8237-7343; Frasca, Antonio/0000-0002-0474-0896;
Ireland, Michael/0000-0002-6194-043X; Bedding,
Timothy/0000-0001-5943-1460; Metcalfe, Travis/0000-0003-4034-0416;
Bedding, Tim/0000-0001-5222-4661
FU National Science Foundation through NSF [AST-0606958]; Georgia State
University through the College of Arts and Sciences; W. M. Keck
Foundation; FCT/MCTES, Portugal [SFRH/BD/41213/2007]; Polish Ministry [N
N203 405139]; Fundacao para a Ciencia e Tecnologia
[SFRH/BPD/47611/2008]; European Research Council [ERC-2009-StG-239953,
267864]; UK Science and Technology Facilities Council (STFC); FCT
(Portugal); POPH/FSE (EC); PTDC/CTE [AST/098754/2008]; Netherlands
Organisation for Scientific Research (NWO); Spanish National Plan of RD
[AYA2010-17803]; ASTERISK project; National Aeronautics and Space
Administration; National Science Foundation
FX The authors gratefully acknowledge the Kepler Science Office and
everyone involved in the Kepler mission for making this paper possible.
Funding for the Kepler mission is provided by NASA's Science Mission
Directorate. The CHARA Array is funded by the National Science
Foundation through NSF grant AST-0606958, by Georgia State University
through the College of Arts and Sciences, and by the W. M. Keck
Foundation. The CoRoT space mission, launched on 2006 December 27, has
been developed and is operated by CNES, with the contribution of
Austria, Belgium, Brazil, ESA (RSSD and Science Programme), Germany, and
Spain. D. H. is thankful to Karsten Brogaard, Pieter Degroote, and
Benoit Mosser for interesting discussions and comments on the paper. D.
H., T. R. B., and V. M. acknowledge support from the Access to Major
Research Facilities Program, administered by the Australian Nuclear
Science and Technology Organisation (ANSTO). D. H. is supported by an
appointment to the NASA Postdoctoral Program at Ames Research Center,
administered by Oak Ridge Associated Universities through a contract
with NASA. I. M. B. is supported by the grant SFRH/BD/41213/2007 from
FCT/MCTES, Portugal. J.M.-.Z. acknowledges the Polish Ministry grant
number N N203 405139. S. G. S. acknowledges the support from the
Fundacao para a Ciencia e Tecnologia (grant ref. SFRH/BPD/47611/2008)
and the European Research Council (grant ref. ERC-2009-StG-239953).
W.J.C. acknowledges financial support from the UK Science and Technology
Facilities Council (STFC). M. C. acknowledges funding from FCT
(Portugal) and POPH/FSE (EC), for funding through a Contrato Cincia 2007
and the project PTDC/CTE-AST/098754/2008. S. H. acknowledges financial
support from the Netherlands Organisation for Scientific Research (NWO).
K. U. acknowledges financial support by the Spanish National Plan of R&D
for 2010, project AYA2010-17803. Funding for the Stellar Astrophysics
Centre is provided by The Danish National Research Foundation. The
research is supported by the ASTERISK project (ASTERoseismic
Investigations with SONG and Kepler) funded by the European Research
Council (grant agreement No. 267864). 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.
NR 162
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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 NOV 20
PY 2012
VL 760
IS 1
AR 32
DI 10.1088/0004-637X/760/1/32
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 035DD
UT WOS:000310922200032
ER
PT J
AU Karpen, JT
Antiochos, SK
DeVore, CR
AF Karpen, J. T.
Antiochos, S. K.
DeVore, C. R.
TI THE MECHANISMS FOR THE ONSET AND EXPLOSIVE ERUPTION OF CORONAL MASS
EJECTIONS AND ERUPTIVE FLARES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic fields; magnetohydrodynamics (MHD); Sun: coronal mass ejections
(CMEs); Sun: flares
ID HOMOLOGOUS SOLAR-FLARES; MAGNETIC RECONNECTION; BREAKOUT MODEL; CURRENT
SHEETS; INTERNAL RECONNECTION; PARTICLE-ACCELERATION; EXTERNAL
RECONNECTION; QUIESCENT FILAMENT; 2-RIBBON FLARES; FLUX EMERGENCE
AB We have investigated the onset and acceleration of coronal mass ejections (CMEs) and eruptive flares. To isolate the eruption physics, our study uses the breakout model, which is insensitive to the energy buildup process leading to the eruption. We performed 2.5D simulations with adaptive mesh refinement that achieved the highest overall spatial resolution to date in a CME/eruptive flare simulation. The ultra-high resolution allows us to separate clearly the timing of the various phases of the eruption. Using new computational tools, we have determined the number and evolution of all X- and O-type nulls in the system, thereby tracking both the progress and the products of reconnection throughout the computational domain. Our results show definitively that CME onset is due to the start of fast reconnection at the breakout current sheet. Once this reconnection begins, eruption is inevitable; if this is the only reconnection in the system, however, the eruption will be slow. The explosive CME acceleration is triggered by fast reconnection at the flare current sheet. Our results indicate that the explosive eruption is caused by a resistive instability, not an ideal process. Moreover, both breakout and flare reconnections begin first as a form of weak tearing characterized by slowly evolving plasmoids, but eventually transition to a fast form with well-defined Alfvenic reconnection jets and rapid flux transfer. This transition to fast reconnection is required for both CME onset and explosive acceleration. We discuss the key implications of our results for CME/flare observations and for theories of magnetic reconnection.
C1 [Karpen, J. T.; Antiochos, S. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[DeVore, C. R.] NRL, Washington, DC 20375 USA.
RP Karpen, JT (reprint author), NASA, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA.
RI Antiochos, Spiro/D-4668-2012; DeVore, C/A-6067-2015
OI Antiochos, Spiro/0000-0003-0176-4312; DeVore, C/0000-0002-4668-591X
FU NASA's LWS research program; Heliophysics SR&T research program
FX We thank B. Dennis, D. Falconer, and K. D. Leka for helpful discussions,
and the referee for suggestions that have improved this paper. This work
was supported in part by NASA's LWS and Heliophysics SR&T research
programs. The computer resources were provided by the DoD HPCMP.
NR 98
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 20
PY 2012
VL 760
IS 1
AR 81
DI 10.1088/0004-637X/760/1/81
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 035DD
UT WOS:000310922200081
ER
PT J
AU Tassis, K
Hezareh, T
Willacy, K
AF Tassis, Konstantinos
Hezareh, Talayeh
Willacy, Karen
TI A SEARCH FOR CO-EVOLVING ION AND NEUTRAL GAS SPECIES IN PRESTELLAR
MOLECULAR CLOUD CORES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: abundances; ISM: clouds; ISM: magnetic fields; ISM: molecules;
magnetohydrodynamics (MHD); stars: formation
ID TURBULENT AMBIPOLAR DIFFUSION; MAGNETIC-FIELD; CHEMISTRY; SPECTRA;
DISSIPATION; 21(OH)
AB A comparison between the widths of ion and neutral molecule spectral lines has been recently used to estimate the strength of the magnetic field in turbulent star-forming regions. However, the ion (HCO+) and neutral (HCN) species used in such studies may not be necessarily co-evolving at every scale and density, and thus, may not trace the same regions. Here, we use coupled chemical/dynamical models of evolving prestellar molecular cloud cores including non-equilibrium chemistry, with and without magnetic fields, to study the spatial distribution of HCO+ and HCN, which have been used in observations of spectral line width differences to date. In addition, we seek new ion-neutral pairs that are good candidates for such observations, because they have similar evolution and are approximately co-spatial in our models. We identify three such good candidate pairs: HCO+/NO, HCO+/CO, and NO+/NO.
C1 [Tassis, Konstantinos; Hezareh, Talayeh] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Willacy, Karen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Tassis, K (reprint author), Max Planck Inst Radioastron, D-53121 Bonn, Germany.
RI Tassis, Konstantinos/C-3155-2011;
OI Tassis, Konstantinos/0000-0002-8831-2038
FU Alexander von Humboldt foundation; NASA
FX We thank Harold Yorke and Helmut Wiesemeyer for insightful and
constructive comments that improved this paper. T.H. is funded by the
Alexander von Humboldt foundation. The project was supported in part by
the NASA Origins of Solar Systems program. Part of this work was carried
out at the Jet Propulsion Laboratory, California Institute of Technology
under contract with the National Aeronautics and Space Administration.
NR 26
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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 NOV 20
PY 2012
VL 760
IS 1
AR 57
DI 10.1088/0004-637X/760/1/57
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 035DD
UT WOS:000310922200057
ER
PT J
AU Teets, WK
Weintraub, DA
Kastner, JH
Grosso, N
Hamaguchi, K
Richmond, M
AF Teets, William K.
Weintraub, David A.
Kastner, Joel H.
Grosso, Nicolas
Hamaguchi, Kenji
Richmond, Michael
TI DETECTION OF A COOL, ACCRETION-SHOCK-GENERATED X-RAY PLASMA IN EX LUPI
DURING THE 2008 OPTICAL ERUPTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: formation; stars: individual (EX Lupi); stars: pre-main sequence;
X-rays: stars
ID T-TAURI STARS; ILLUMINATING MCNEIL-NEBULA; FU-ORIONIS STARS; YOUNG STAR;
V1647 ORI; SPECTRAL VARIABILITY; EXTREME OUTBURST; SPACED DATA;
XMM-NEWTON; EMISSION
AB EX Lupi is the prototype for a class of young, pre-main-sequence stars which are observed to undergo irregular, presumably accretion-generated, optical outbursts that result in a several magnitude rise of the optical flux. EX Lupi was observed to optically erupt in 2008 January, triggering Chandra ACIS Target of Opportunity observations shortly thereafter. We find very strong evidence that most of the X-ray emission in the first few months after the optical outburst is generated by accretion of circumstellar material onto the stellar photosphere. Specifically, we find a strong correlation between the decreasing optical and X-ray fluxes following the peak of the outburst in the optical, which suggests that these observed declines in both the optical and X-ray fluxes are the result of declining accretion rate. In addition, in our models of the X-ray spectrum, we find strong evidence for a similar to 0.4 keV plasma component, as expected for accretion shocks on low-mass, pre-main-sequence stars. From 2008 March through October, this cool plasma component appeared to fade as EX Lupi returned to its quiescent level in the optical, consistent with a decrease in the overall emission measure of accretion-shock-generated plasma. The overall small increase of the X-ray flux during the optical outburst of EX Lupi is similar to what was observed in previous X-ray observations of the 2005 optical outburst of the EX Lupi-type star V1118 Ori but contrasts with the large increase of the X-ray flux from the erupting young star V1647 Ori during its 2003 and 2008 optical outbursts.
C1 [Teets, William K.; Weintraub, David A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Grosso, Nicolas] Univ Strasbourg, Observ Astron Strasbourg, CNRS, UMR 7550, F-67000 Strasbourg, France.
[Hamaguchi, Kenji] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kastner, Joel H.; Richmond, Michael] Rochester Inst Technol, Rochester, NY 14623 USA.
RP Teets, WK (reprint author), Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
NR 38
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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 NOV 20
PY 2012
VL 760
IS 1
AR 89
DI 10.1088/0004-637X/760/1/89
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 035DD
UT WOS:000310922200089
ER
PT J
AU Wang, FY
Bromm, V
Greif, TH
Stacy, A
Dai, ZG
Loeb, A
Cheng, KS
AF Wang, F. Y.
Bromm, Volker
Greif, Thomas H.
Stacy, Athena
Dai, Z. G.
Loeb, Abraham
Cheng, K. S.
TI PROBING PRE-GALACTIC METAL ENRICHMENT WITH HIGH-REDSHIFT GAMMA-RAY
BURSTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; cosmology: theory; galaxies: high-redshift;
gamma-ray burst: general; quasars: absorption lines
ID INITIAL MASS FUNCTION; POPULATION-III STARS; ATOMIC-ABSORPTION LINES;
1ST STARS; INTERGALACTIC MEDIUM; PRIMORDIAL GAS; EARLY UNIVERSE; LIGHT
CURVES; HII-REGIONS; PROTOSTELLAR FEEDBACK
AB We explore high-redshift gamma-ray bursts (GRBs) as promising tools to probe pre-galactic metal enrichment. We utilize the bright afterglow of a Population III (Pop III) GRB exploding in a primordial dwarf galaxy as a luminous background source, and calculate the strength of metal absorption lines that are imprinted by the first heavy elements in the intergalactic medium (IGM). To derive the GRB absorption line diagnostics, we use an existing highly resolved simulation of the formation of a first galaxy which is characterized by the onset of atomic hydrogen cooling in a halo with virial temperature greater than or similar to 10(4) K. We explore the unusual circumburst environment inside the systems that hosted Pop III stars, modeling the density evolution with the self-similar solution for a champagne flow. For minihalos close to the cooling threshold, the circumburst density is roughly proportional to (1 + z) with values of about a few cm(-3). In more massive halos, corresponding to the first galaxies, the density may be larger, n greater than or similar to 100 cm(-3). The resulting afterglow fluxes are weakly dependent on redshift at a fixed observed time, and may be detectable with the James Webb Space Telescope and Very Large Array in the near-IR and radio wavebands, respectively, out to redshift z greater than or similar to 20. We predict that the maximum of the afterglow emission shifts from near-IR to millimeter bands with peak fluxes from mJy to Jy at different observed times. The metal absorption line signature is expected to be detectable in the near future. GRBs are ideal tools for probing the metal enrichment in the early IGM, due to their high luminosities and featureless power-law spectra. The metals in the first galaxies produced by the first supernova (SN) explosions are likely to reside in low-ionization stages (C II, OI, Si II and Fe II). We show that, if the afterglow can be observed sufficiently early, analysis of the metal lines may distinguish whether the first heavy elements were produced in a pair-instability supernova or a core-collapse (Type II) SN, thus constraining the initial mass function of the first stars.
C1 [Wang, F. Y.; Dai, Z. G.] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Peoples R China.
[Wang, F. Y.; Bromm, Volker] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Bromm, Volker] Univ Texas Austin, Texas Cosmol Ctr, Austin, TX 78712 USA.
[Greif, Thomas H.] Max Planck Inst Astrophys, D-85740 Garching, Germany.
[Stacy, Athena] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Loeb, Abraham] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Cheng, K. S.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China.
RP Wang, FY (reprint author), Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Peoples R China.
RI Wang, Fayin/B-1479-2009; Cheng, Kwong Sang/D-3073-2009
OI Wang, Fayin/0000-0003-4157-7714;
FU National Natural Science Foundation of China [11103007, 11033002]; NSF
[AST-1009928]; NASA [NNX09AJ33G]; Government of the Hong Kong SAR [HKU
7011/09p]
FX We are indebted to Anna Frebel and Steve Finkelstein for helpful
discussions. This work is supported by the National Natural Science
Foundation of China (grants 11103007 and 11033002). V.B. acknowledges
support from NSF grant AST-1009928 and NASA ATFP grant NNX09AJ33G.
K.S.C. is supported by the GRF grants of the Government of the Hong Kong
SAR under HKU 7011/09p. The simulations presented here were carried out
at the Texas Advanced Computing Center (TACC).
NR 131
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 20
PY 2012
VL 760
IS 1
AR 27
DI 10.1088/0004-637X/760/1/27
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 035DD
UT WOS:000310922200027
ER
PT J
AU Xu, CK
Shupe, DL
Bethermin, M
Aussel, H
Berta, S
Bock, J
Bridge, C
Conley, A
Cooray, A
Elbaz, D
Franceschini, A
Le Floc'h, E
Lu, N
Lutz, D
Magnelli, B
Marsden, G
Oliver, SJ
Pozzi, F
Riguccini, L
Schulz, B
Scoville, N
Vaccari, M
Vieira, JD
Wang, L
Zemcov, M
AF Xu, C. K.
Shupe, D. L.
Bethermin, M.
Aussel, H.
Berta, S.
Bock, J.
Bridge, C.
Conley, A.
Cooray, A.
Elbaz, D.
Franceschini, A.
Le Floc'h, E.
Lu, N.
Lutz, D.
Magnelli, B.
Marsden, G.
Oliver, S. J.
Pozzi, F.
Riguccini, L.
Schulz, B.
Scoville, N.
Vaccari, M.
Vieira, J. D.
Wang, L.
Zemcov, M.
TI COSMIC EVOLUTION OF STAR FORMATION ENHANCEMENT IN CLOSE MAJOR-MERGER
GALAXY PAIRS SINCE z=1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: general; galaxies: interactions;
galaxies: starburst
ID DIGITAL SKY SURVEY; LUMINOUS INFRARED GALAXIES; HERSCHEL-SPIRE
INSTRUMENT; HIGH-REDSHIFT GALAXIES; SUBMILLIMETER GALAXIES; FIELD
GALAXIES; STELLAR MASS; EXTRAGALACTIC SURVEY; FORMING GALAXIES; S-COSMOS
AB The infrared (IR) emission of "M-* galaxies" (10(10.4) <= M-star <= 10(11.0) M-circle dot) in galaxy pairs, derived using data obtained in Herschel (PEP/HerMES) and Spitzer (S-COSMOS) surveys, is compared to that of single-disk galaxies in well-matched control samples to study the cosmic evolution of the star formation enhancement induced by galaxy-galaxy interaction. Both the mean IR spectral energy distribution and mean IR luminosity of star-forming galaxies (SFGs) in SFG+SFG (S+S) pairs in the redshift bin of 0.6 < z < 1 are consistent with no star formation enhancement. SFGs in S+S pairs in a lower redshift bin of 0.2 < z < 0.6 show marginal evidence for a weak star formation enhancement. Together with the significant and strong sSFR enhancement shown by SFGs in a local sample of S+S pairs (obtained using previously published Spitzer observations), our results reveal a trend for the star formation enhancement in S+S pairs to decrease with increasing redshift. Between z = 0 and z = 1, this decline of interaction-induced star formation enhancement occurs in parallel with the dramatic increase (by a factor of similar to 10) of the sSFR of single SFGs, both of which can be explained by the higher gas fraction in higher-z disks. SFGs in mixed pairs (S+E pairs) do not show any significant star formation enhancement at any redshift. The difference between SFGs in S+S pairs and in S+E pairs suggests a modulation of the sSFR by the intergalactic medium (IGM) in the dark matter halos hosting these pairs.
C1 [Xu, C. K.; Shupe, D. L.; Lu, N.; Schulz, B.; Zemcov, M.] CALTECH, Infrared Proc & Anal Ctr, JPL, Pasadena, CA 91125 USA.
[Bethermin, M.; Aussel, H.; Elbaz, D.; Le Floc'h, E.; Riguccini, L.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA DSM Irfu, CNRS,CE Saclay, F-91191 Gif Sur Yvette, France.
[Bethermin, M.] Univ Paris 11, IAS, F-91405 Orsay, France.
[Bethermin, M.] CNRS, UMR 8617, F-91405 Orsay, France.
[Berta, S.; Lutz, D.; Magnelli, B.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany.
[Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA.
[Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Franceschini, A.; Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Marsden, G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Oliver, S. J.; Wang, L.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
[Pozzi, F.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Vaccari, M.] Univ Western Cape, Astrophys Grp, Dept Phys, ZA-7535 Bellville, Cape Town, South Africa.
RP Xu, CK (reprint author), CALTECH, Infrared Proc & Anal Ctr, JPL, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
RI Oliver, Seb/A-2479-2013; Vaccari, Mattia/R-3431-2016;
OI Oliver, Seb/0000-0001-7862-1032; Vaccari, Mattia/0000-0002-6748-0577;
Bethermin, Matthieu/0000-0002-3915-2015
FU Science and Technology Facilities Council [ST/I000976/1]; BMVIT
(Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany);
ASI/INAF (Italy); CICYT/MCYT (Spain); CSA (Canada); NAOC (China); CEA
(France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB
(Sweden); STFC (UK); UKSA (UK); NASA (USA)
FX Dr. Xianzhong Zheng is thanked for kindly providing the software and
instructions for the "clean stacking." We acknowledge support from the
Science and Technology Facilities Council (grant No. ST/I000976/1). 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); INAF-IFSI/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:
the University of Lethbridge (Canada); NAOC (China); CEA, LAM (France);
IFSI, the University of Padua (Italy); IAC (Spain); Stockholm
Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, the
University of Sussex (UK); and Caltech, JPL, NHSC, the University of
Colorado (USA). This development has been supported by national funding
agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI
(Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).
The data presented in this paper will be released through the Herschel
Database in Marseille (HeDaM, http://hedam.oamp.fr/HerMES).
NR 79
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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 NOV 20
PY 2012
VL 760
IS 1
AR 72
DI 10.1088/0004-637X/760/1/72
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 035DD
UT WOS:000310922200072
ER
PT J
AU Mainzer, A
Grav, T
Masiero, J
Bauer, J
Cutri, RM
McMillan, RS
Nugent, CR
Tholen, D
Walker, R
Wright, EL
AF Mainzer, A.
Grav, T.
Masiero, J.
Bauer, J.
Cutri, R. M.
McMillan, R. S.
Nugent, C. R.
Tholen, D.
Walker, R.
Wright, E. L.
TI PHYSICAL PARAMETERS OF ASTEROIDS ESTIMATED FROM THE WISE 3-BAND DATA AND
NEOWISE POST-CRYOGENIC SURVEY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE atlases; catalogs; minor planets, asteroids: general; surveys
ID THERMAL-MODEL CALIBRATION; EARTH; DIAMETERS; ALBEDOS; OBJECTS
AB Enhancements to the science data processing pipeline of NASA's Wide-field Infrared Survey Explorer (WISE) mission, collectively known as NEOWISE, resulted in the detection of >158,000 minor planets in four infrared wavelengths during the fully cryogenic portion of the mission. Following the depletion of its cryogen, NASA's Planetary Science Directorate funded a four-month extension to complete the survey of the inner edge of the Main Asteroid Belt and to detect and discover near-Earth objects (NEOs). This extended survey phase, known as the NEOWISE Post-Cryogenic Survey, resulted in the detection of similar to 6500 large Main Belt asteroids and 86 NEOs in its 3.4 and 4.6 mu m channels. During the Post-Cryogenic Survey, NEOWISE discovered and detected a number of asteroids co-orbital with the Earth and Mars, including the first known Earth Trojan. We present preliminary thermal fits for these and other NEOs detected during the 3-Band Cryogenic and Post-Cryogenic Surveys.
C1 [Mainzer, A.; Masiero, J.; Bauer, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grav, T.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Bauer, J.; Cutri, R. M.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[McMillan, R. S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Nugent, C. R.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Tholen, D.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Walker, R.] Monterey Inst Res Astron, Monterey, CA 93933 USA.
[Wright, E. L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Mainzer, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM amainzer@jpl.nasa.gov
OI Masiero, Joseph/0000-0003-2638-720X
FU National Aeronautics and Space Administration; NSF [AST 1109940]
FX This publication makes use of data products from the Widefield Infrared
Survey Explorer, which is a joint project of the University of
California, Los Angeles, and the Jet Propulsion Laboratory/California
Institute of Technology, and NEOWISE, which is a project of the Jet
Propulsion Laboratory/California Institute of Technology. WISE and
NEOWISE are funded by the National Aeronautics and Space Administration.
We gratefully acknowledge the extraordinary services specific to NEOWISE
contributed by the International Astronomical Union's Minor Planet
Center, operated by the Harvard-Smithsonian Center for Astrophysics. We
thank the worldwide community of dedicated amateur and professional
astronomers devoted to minor planet follow-up observations. We thank our
referee for thoughtful comments. This research has made use of the
NASA/IPAC Infrared Science Archive, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. D.J.T.
acknowledges support from NSF Grant AST 1109940.
NR 13
TC 17
Z9 17
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 NOV 20
PY 2012
VL 760
IS 1
AR L12
DI 10.1088/2041-8205/760/1/L12
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 033ZE
UT WOS:000310839100012
ER
PT J
AU Ofman, L
Thompson, BJ
AF Ofman, L.
Thompson, B. J.
TI SDO/AIA OBSERVATION OF KELVIN-HELMHOLTZ INSTABILITY IN THE SOLAR CORONA
(vol 734, pg L11, 2011)
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Correction
C1 [Ofman, L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Ofman, L.; Thompson, B. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ofman, L (reprint author), Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel.
RI Thompson, Barbara/C-9429-2012
NR 3
TC 1
Z9 1
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD NOV 20
PY 2012
VL 760
IS 1
AR L19
DI 10.1088/2041-8205/760/1/L19
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 033ZE
UT WOS:000310839100019
ER
PT J
AU Perez, LM
Carpenter, JM
Chandler, CJ
Isella, A
Andrews, SM
Ricci, L
Calvet, N
Corder, SA
Deller, AT
Dullemond, CP
Greaves, JS
Harris, RJ
Henning, T
Kwon, W
Lazio, J
Linz, H
Mundy, LG
Sargent, AI
Storm, S
Testi, L
Wilner, DJ
AF Perez, Laura M.
Carpenter, John M.
Chandler, Claire J.
Isella, Andrea
Andrews, Sean M.
Ricci, Luca
Calvet, Nuria
Corder, Stuartt A.
Deller, Adam T.
Dullemond, Cornelis P.
Greaves, Jane S.
Harris, Robert J.
Henning, Thomas
Kwon, Woojin
Lazio, Joseph
Linz, Hendrik
Mundy, Lee G.
Sargent, Anneila I.
Storm, Shaye
Testi, Leonardo
Wilner, David J.
TI CONSTRAINTS ON THE RADIAL VARIATION OF GRAIN GROWTH IN THE AS 209
CIRCUMSTELLAR DISK
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE protoplanetary disks; stars: individual (AS 209)
ID T-TAURI STARS; PROTOPLANETARY DISKS; ACCRETION DISKS; OPTICAL-CONSTANTS;
CQ TAURI; EVOLUTION; OPACITIES; SIZE
AB We present dust continuum observations of the protoplanetary disk surrounding the pre-main-sequence star AS 209, spanning more than an order of magnitude in wavelength from 0.88 to 9.8 mm. The disk was observed with subarcsecond angular resolution (0 ''.2-0 ''.5) to investigate radial variations in its dust properties. At longer wavelengths, the disk emission structure is notably more compact, providing model-independent evidence for changes in the grain properties across the disk. We find that physical models which reproduce the disk emission require a radial dependence of the dust opacity kappa(nu) Assuming that the observed wavelength-dependent structure can be attributed to radial variations in the dust opacity spectral index (beta), we find that beta(R) increases from beta < 0.5 at similar to 20 AU to beta > 1.5 for R greater than or similar to 80 AU, inconsistent with a constant value of beta across the disk (at the 10 sigma level). Furthermore, if radial variations of kappa(nu) are caused by particle growth, we find that the maximum size of the particle-size distribution (a(max)) increases from submillimeter-sized grains in the outer disk (R greater than or similar to 70 AU) to millimeter- and centimeter-sized grains in the inner disk regions (R less than or similar to 70 AU). We compare our observational constraint on a(max)(R) with predictions from physical models of dust evolution in protoplanetary disks. For the dust composition and particle-size distribution investigated here, our observational constraints on a(max)(R) are consistent with models where the maximum grain size is limited by radial drift.
C1 [Perez, Laura M.; Carpenter, John M.; Isella, Andrea; Ricci, Luca; Sargent, Anneila I.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Chandler, Claire J.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Andrews, Sean M.; Harris, Robert J.; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Calvet, Nuria] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Corder, Stuartt A.] Joint ALMA Observ, Santiago, Chile.
[Deller, Adam T.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Dullemond, Cornelis P.; Linz, Hendrik] Univ Heidelberg, Ctr Astron, D-69120 Heidelberg, Germany.
[Greaves, Jane S.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Kwon, Woojin] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Lazio, Joseph] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
[Mundy, Lee G.; Storm, Shaye] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Testi, Leonardo] European So Observ, D-85748 Garching, Germany.
[Testi, Leonardo] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
RP Perez, LM (reprint author), CALTECH, Dept Astron, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
OI Dullemond, Cornelis/0000-0002-7078-5910; Deller,
Adam/0000-0001-9434-3837
FU NSF [AST-1109334]; Smithsonian Institution; Academia Sinica
FX We acknowledge T. Birnstiel for useful discussions. A.I., J.M.C., L.M.P
acknowledge support from NSF award AST-1109334. The National Radio
Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc.
Ongoing CARMA development and operations are supported by the National
Science Foundation under a cooperative agreement, and by the CARMA
partner universities. The SMA is a joint project between the Smithsonian
Astrophysical Observatory and the Academia Sinica Institute of Astronomy
and Astrophysics, funded by the Smithsonian Institution and Academia
Sinica. Part of this research was carried out at the Jet Propulsion
Laboratory, Caltech, under a contract with the National Aeronautics and
Space Administration.
NR 35
TC 74
Z9 74
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 NOV 20
PY 2012
VL 760
IS 1
AR L17
DI 10.1088/2041-8205/760/1/L17
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 033ZE
UT WOS:000310839100017
ER
PT J
AU Miyashita, Y
Machida, S
Nose, M
Liou, K
Saito, Y
Paterson, WR
AF Miyashita, Y.
Machida, S.
Nose, M.
Liou, K.
Saito, Y.
Paterson, W. R.
TI A statistical study of energy release and transport midway between the
magnetic reconnection and initial dipolarization regions in the
near-Earth magnetotail associated with substorm expansion onsets
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID CENTRAL PLASMA SHEET; GEOTAIL OBSERVATIONS; MIDDISTANT MAGNETOTAIL;
AURORAL BREAKUPS; FLUX TRANSPORT; BULK FLOWS; EVOLUTION; ION;
MAGNETOSPHERE; SPACECRAFT
AB Our previous study showed that the energy release associated with substorm expansion onsets is the most significant midway between the magnetic reconnection and initial dipolarization regions (- 12 > X > - 18 R-E in the premidnight sector) in the magnetotail. In the present paper, we have statistically studied the substorm-associated energy balance and transport in the magnetotail, focusing on the midway region as well as the near-Earth initial dipolarization region (X > similar to- 12 R-E). We find that a large amount of energy is released in the midway region, associated with onsets, but only a part of this energy is transported to the near-Earth initial dipolarization region mainly in the form of the thermal flux and the wave Poynting flux. It is possible that the energy carried by fast earthward flows and waves from the reconnection region is not sufficient for the thermal energy increase and the outward transported energy in the initial dipolarization region, although the magnetic flux may be sufficiently carried. A considerably large amount of the magnetic energy comes from the lobes in the form of the Poynting flux also in the initial dipolarization region.
C1 [Miyashita, Y.] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan.
[Machida, S.] Kyoto Univ, Dept Geophys, Kyoto, Japan.
[Nose, M.] Kyoto Univ, Grad Sch Sci, Data Anal Ctr Geomagnetism & Space Magnetism, Kyoto, Japan.
[Liou, K.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Saito, Y.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Paterson, W. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Miyashita, Y (reprint author), Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648601, Japan.
EM miyasita@stelab.nagoya-u.ac.jp
RI Nose, Masahito/B-1900-2015; Liou, Kan/C-2089-2016
OI Nose, Masahito/0000-0002-2789-3588; Liou, Kan/0000-0001-5277-7688
FU Japan Society for the Promotion of Science [22340145]; [22740321]
FX The Geotail MGF magnetic field data were provided by T. Nagai and S.
Kokubun. The Geotail EPIC-STICS high-energy particle data were provided
by A. T. Y. Lui, R. W. McEntire, and S. P. Christon. We also thank D.
Nagata for processing the EPIC-STICS data. This work was supported by a
Grant-in-Aid for Young Scientists (22740321) and a Grant-in-Aid for
Scientific Research (22340145) of Japan Society for the Promotion of
Science.
NR 42
TC 8
Z9 8
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 NOV 17
PY 2012
VL 117
AR A11214
DI 10.1029/2012JA017925
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 039NK
UT WOS:000311253100002
ER
PT J
AU Leahy, LV
Wood, R
Charlson, RJ
Hostetler, CA
Rogers, RR
Vaughan, MA
Winker, DM
AF Leahy, L. V.
Wood, R.
Charlson, R. J.
Hostetler, C. A.
Rogers, R. R.
Vaughan, M. A.
Winker, D. M.
TI On the nature and extent of optically thin marine low clouds
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SPECTRAL-RESOLUTION LIDAR; LIQUID WATER PATH; TRADE-WIND CUMULI;
STRATIFORM CLOUDS; CALIPSO LIDAR; SATELLITE-OBSERVATIONS; INSTRUMENT
SIMULATORS; RADIATION BUDGET; BOUNDARY-LAYER; SEA-SALT
AB Macrophysical properties of optically thin marine low clouds over the nonpolar oceans (60 degrees S-60 degrees N) are measured using 2 years of full-resolution nighttime data from the Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP). Optically thin clouds, defined as the subset of marine low clouds that do not fully attenuate the lidar signal, comprise almost half of the low clouds over the marine domain. Regionally, the fraction of low clouds that are optically thin (f(thin,cld)) exhibits a strong inverse relationship with the low-cloud cover, with maxima in the tropical trades (f(thin,cld) > 0.8) and minima in regions of persistent marine stratocumulus and in midlatitudes (f(thin,cld) < 0.3). Domain-wide, a power law fit describes the cloud length distribution, with exponent beta = 2.03 +/- 0.06 (+/- 95% confidence interval). On average, the fraction of a cloud that is optically thin decreases from similar to 1 for clouds smaller than 2 km to <0.3 for clouds larger than 30 km. This relationship is found to be independent of region, so that geographical variations in the cloud length distribution explain three quarters of the variance in f(thin,cld). Comparing collocated trade cumulus observations from CALIOP and the airborne High Spectral Resolution Lidar reveals that clouds with lengths smaller than are resolvable with CALIOP contribute approximately half of the low clouds in the region sampled. A bounded cascade model is constructed to match the observations from the trades. The model shows that the observed optically thin cloud behavior is consistent with a power law scaling of cloud optical depth and suggests that most optically thin clouds only partially fill the CALIOP footprint.
C1 [Leahy, L. V.; Wood, R.; Charlson, R. J.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Hostetler, C. A.; Rogers, R. R.; Vaughan, M. A.; Winker, D. M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Leahy, LV (reprint author), Univ Washington, Dept Atmospher Sci, Box 351640, Seattle, WA 98195 USA.
EM lleahy@atmos.washington.edu
RI Wood, Robert/A-2989-2008
OI Wood, Robert/0000-0002-1401-3828
FU NASA [NNX10AE59G, NNX10AN78G]
FX This work was supported by NASA award numbers NNX10AE59G and NNX10AN78G.
We wish to thank Sarah Doherty for insightful comments which contributed
greatly to the quality of this work and Roger Marchand for pointing out
an important flaw in our original application of the bounded cascade
model.
NR 67
TC 8
Z9 8
U1 1
U2 20
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD NOV 16
PY 2012
VL 117
AR D22201
DI 10.1029/2012JD017929
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 039LS
UT WOS:000311247900003
ER
PT J
AU Larour, E
Morlighem, M
Seroussi, H
Schiermeier, J
Rignot, E
AF Larour, E.
Morlighem, M.
Seroussi, H.
Schiermeier, J.
Rignot, E.
TI Ice flow sensitivity to geothermal heat flux of Pine Island Glacier,
Antarctica
SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE
LA English
DT Article
ID WEST ANTARCTICA; SATELLITE RADAR; SHEET MODEL; PART 1; SHELF; BASAL;
VELOCITY; RHEOLOGY; SURFACE
AB Model projections of ice flow in a changing climate are dependent on model inputs such as surface elevation, bedrock position or surface temperatures, among others. Of all these inputs, geothermal heat flux is the one for which uncertainty is greatest. In the area of Pine Island Glacier, Antarctica, available data sets differ by up to a factor of 2.5. Here, we evaluate the impact of such uncertainty on ice flow, using sampling analyses based on the Latin-Hypercube method. First, we quantify the impact of geothermal heat flux errors on ice hardness, a thermal parameter that critically controls the magnitude of ice flow. Second, we quantify the impact of the same errors on mass balance, specifically on the mass flux advecting through thirteen fluxgates distributed across Pine Island Glacier. We contrast our results with similar uncertainties generated by errors in the specification of ice thickness. Model outputs indicate that geothermal heat flux errors yield uncertainties on ice hardness on the order of 5-7%, with maximum uncertainty reaching 15%. Resulting uncertainties in mass balance remain however below 1%. We discuss the uncertainty distribution and its relationship to the amount of heat available at the base of the ice sheet from friction, viscous and geothermal heating. We also show that comparatively, errors in ice thickness contribute more to model uncertainty than errors in geothermal heat flux, especially for fast-flowing ice streams.
C1 [Larour, E.; Seroussi, H.; Schiermeier, J.; Rignot, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morlighem, M.; Rignot, E.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
RP Larour, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM eric.larour@jpl.nasa.gov
RI Rignot, Eric/A-4560-2014; Morlighem, Mathieu/O-9942-2014
OI Rignot, Eric/0000-0002-3366-0481; Morlighem, Mathieu/0000-0001-5219-1310
FU National Aeronautics and Space Administration; Cryospheric Sciences
Program; MAP Program; NSF [ANT-0424589]; NASA [NNX10AT68G]; NASA
Postdoctoral Program at the Jet Propulsion Laboratory, California
Institute of Technology
FX This work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, and the Department of Earth System Science,
University of California Irvine, under a contract with the National
Aeronautics and Space Administration, Cryospheric Sciences Program and
MAP Program. The authors would like to acknowledge Operation IceBridge
data used in the study, as well as CReSIS data generated from NSF grant
ANT-0424589 and NASA grant NNX10AT68G. Helene Seroussi was supported by
an appointment to the NASA Postdoctoral Program at the Jet Propulsion
Laboratory, California Institute of Technology, administered by Oak
Ridge Associated Universities through a contract with NASA. We would
also like to acknowledge R. Gladstone, the Associate Editor Poul
Christoffersen and the other anonymous reviewers for their review and
insights into the manuscript.
NR 56
TC 18
Z9 18
U1 1
U2 23
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9003
EI 2169-9011
J9 J GEOPHYS RES-EARTH
JI J. Geophys. Res.-Earth Surf.
PD NOV 16
PY 2012
VL 117
AR F04023
DI 10.1029/2012JF002371
PG 12
WC Geosciences, Multidisciplinary
SC Geology
GA 039OE
UT WOS:000311255400001
ER
PT J
AU Kitamura, N
Nishimura, Y
Chandler, MO
Moore, TE
Terada, N
Ono, T
Shinbori, A
Kumamoto, A
AF Kitamura, N.
Nishimura, Y.
Chandler, M. O.
Moore, T. E.
Terada, N.
Ono, T.
Shinbori, A.
Kumamoto, A.
TI Storm-time electron density enhancement in the cleft ion fountain
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID INTERPLANETARY MAGNETIC-FIELD; POLAR WIND; PLASMA SHEET; EARTHS
MAGNETOSPHERE; GEOMAGNETIC STORM; SOLAR-WIND; IONOSPHERIC OUTFLOWS;
COORDINATE SYSTEM; AURORAL-ZONE; OXYGEN IONS
AB To determine the characteristics and origin of observed storm-time electron density enhancements in the polar cap, and to investigate the spatial extent (noon-midnight direction) of associated O+ ion outflows, we analyzed nearly simultaneous observations of such electron density enhancements from the Akebono satellite and ion upflows from the Polar satellite during a geomagnetic storm occurring on 6 April 2000. The Akebono satellite observed substantial electron density enhancements by a factor of similar to 10-90 with a long duration of similar to 15 h at similar to 2 R-E in the southern polar region. The Polar satellite outflow measurements in the northern polar cap at similar to 7-4 R-E exhibited velocity filtering of the similar to 100 eV to similar to 0 eV (from the spacecraft potential) ion outflow from the cleft ion fountain, with resultant temperatures declining from similar to 3 eV to 0.03 eV with increasing distance from the cusp. Similar velocity filtering was detected in the southern polar cap at similar to 1.8-3.5 RE. The region of O+ ion outflows with fluxes exceeding 5 x 10(8) /cm(2)/s (mapped to 1000 km altitude) extended similar to 10 degrees MLAT (similar to 1000 km) at the ionosphere from the cusp/cleft into the dayside polar cap at similar to 2.5 RE. These coordinated Akebono-Polar observations are consistent with the development of storm-time electron density enhancements in the polar cap as a result of the bulk outflow of low-energy plasma as part of the cleft ion fountain. The large spatial scale, large ion fluxes, and the long duration indicate significant supply of very-low-energy O+ ions to the magnetosphere through this region.
C1 [Kitamura, N.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Nishimura, Y.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Chandler, M. O.] NASA, Nat Environm EV44, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Moore, T. E.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Terada, N.; Ono, T.; Kumamoto, A.] Tohoku Univ, Dept Geophys, Sendai, Miyagi 980, Japan.
[Shinbori, A.] Kyoto Univ, Res Inst Sustainable Humanosphere, Uji, Kyoto, Japan.
RP Kitamura, N (reprint author), Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
EM kitamura@stelab.nagoya-u.ac.jp
RI Moore, Thomas/D-4675-2012
OI Moore, Thomas/0000-0002-3150-1137
FU Global COE program "Global Education and Research Center for Earth and
Planetary Dynamics" at Tohoku University; Research Fellowship of the
Japan Society for the Promotion of Science (JSPS); JSPS KAKENHI
[22.1671]; Inter-university Upper atmosphere Global Observation NETwork
(IUGONET); Ministry of Education, Culture, Sports, Science and
Technology (MEXT), Japan
FX The Akebono satellite project has been managed by Institute of Space and
Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA).
The SYM-H index was provided by WDC for Geomagnetism, Kyoto. The OMNI
data set were obtained from the GSFC/SPDF OMNIWeb interface at
http://omniweb.gsfc.nasa.gov. This work was supported by the Global COE
program "Global Education and Research Center for Earth and Planetary
Dynamics" at Tohoku University, a Research Fellowship of the Japan
Society for the Promotion of Science (JSPS), and JSPS KAKENHI grant
22.1671. The Hydra data set were obtained from the Coordinated Data
Analysis Web at http://cdaweb.gsfc.nasa.gov. The authors would like to
thank J. Scudder and Hydra team for use of the data. A. Shinbori is
supported by the Inter-university Upper atmosphere Global Observation
NETwork (IUGONET) project funded by the Ministry of Education, Culture,
Sports, Science and Technology (MEXT), Japan.
NR 112
TC 4
Z9 4
U1 1
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 NOV 16
PY 2012
VL 117
AR A11212
DI 10.1029/2012JA017900
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 039NF
UT WOS:000311252500003
ER
PT J
AU Biaggi-Labiosa, A
Sola, F
Lebron-Colon, M
Evans, LJ
Xu, JC
Hunter, GW
Berger, GM
Gonzalez, JM
AF Biaggi-Labiosa, A.
Sola, F.
Lebron-Colon, M.
Evans, L. J.
Xu, J. C.
Hunter, G. W.
Berger, G. M.
Gonzalez, J. M.
TI A novel methane sensor based on porous SnO2 nanorods: room temperature
to high temperature detection
SO NANOTECHNOLOGY
LA English
DT Article
ID GAS SENSORS; OXIDE NANOSTRUCTURES; CARBON NANOTUBES; METAL-OXIDES; TIN
OXIDE; NANOWIRES; RESISTANCE; DEVICES
AB We report for the first time a novel room temperature methane (CH4) sensor fabricated using porous tin oxide (SnO2) nanorods as the sensing material. The porous SnO2 nanorods were synthesized by using multiwall carbon nanotubes (MWCNTs) as templates. Current versus time curves were obtained demonstrating the room temperature sensing capabilities of the sensor system when exposed to 0.25% CH4 in air. The sensor also exhibited a wide temperature range for different concentrations of CH4 (25-500 degrees C), making it useful in harsh environments as well.
C1 [Biaggi-Labiosa, A.; Berger, G. M.] NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA.
[Gonzalez, J. M.] NASA, Glenn Res Ctr, Gilcrest, Cleveland, OH 44135 USA.
RP Biaggi-Labiosa, A (reprint author), NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, 21000 Brookpark Rd, Cleveland, OH 44135 USA.
EM azlin.m.biaggi-labiosa@nasa.gov
FU Vehicle Systems Safety Technologies Project
FX The authors would like to acknowledge the contributions of Drs L Matus,
M Zeller, and C W Chang for discussions and critical review of the
manuscript. We also acknowledge the technical assistance of C Hampton, P
Lampard, and M Artale. This research is supported by the Vehicle Systems
Safety Technologies Project.
NR 35
TC 20
Z9 20
U1 2
U2 69
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
J9 NANOTECHNOLOGY
JI Nanotechnology
PD NOV 16
PY 2012
VL 23
IS 45
AR 455501
DI 10.1088/0957-4484/23/45/455501
PG 8
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 030OE
UT WOS:000310579200015
PM 23064120
ER
PT J
AU Roberts, JC
Harrigan, TP
Ward, EE
Taylor, TM
Annett, MS
Merkle, AC
AF Roberts, J. C.
Harrigan, T. P.
Ward, E. E.
Taylor, T. M.
Annett, M. S.
Merkle, A. C.
TI Human head-neck computational model for assessing blast injury
SO JOURNAL OF BIOMECHANICS
LA English
DT Article
DE Brain injury; Finite element models (FEM); Surrogate models; Blast;
Human models
ID IMPACT
AB A human head finite element model (HHFEM) was developed to study the effects of a blast to the head. To study both the kinetic and kinematic effects of a blast wave, the HHFEM was attached to a finite element model of a Hybrid III ATD neck. A physical human head surrogate model (HSHM) was developed from solid model files of the HHFEM, which was then attached to a physical Hybrid III ATD neck and exposed to shock tube overpressures. This allowed direct comparison between the HSHM and HHFEM. To develop the temporal and spatial pressures on the HHFEM that would simulate loading to the HSHM, a computational fluid dynamics (CFD) model of the HHFEM in front of a shock tube was generated. CFD simulations were made using loads equivalent to those seen in experimental studies of the HSHM for shock tube driver pressures of 517, 690 and 862 kPa. Using the selected brain material properties, the peak intracranial pressures, temporal and spatial histories of relative brain-skull displacements and the peak relative brain-skull displacements in the brain of the HHFEM compared favorably with results from the HSHM. The HSHM sensors measured the rotations of local areas of the brain as well as displacements, and the rotations of the sensors in the sagittal plane of the HSHM were, in general, correctly predicted from the HHFEM. Peak intracranial pressures were between 70 and 120 kPa, while the peak relative brain-skull displacements were between 0.5 and 3.0 mm. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Roberts, J. C.; Harrigan, T. P.; Ward, E. E.; Taylor, T. M.; Merkle, A. C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Annett, M. S.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Roberts, JC (reprint author), Johns Hopkins Univ, Appl Phys Lab, 10020 Johns Hopkins Rd, Laurel, MD 20723 USA.
EM jack.roberts@jhuapl.edu
FU Office of Naval Research (ONR) [N0001407PD20006]; Department of Defense
Congressionally Directed Medical Research Programs (CDMRP)
[W81XVVH-09-2-0168]
FX The authors would like to express their appreciation to the Office of
Naval Research (ONR) and the Department of Defense Congressionally
Directed Medical Research Programs (CDMRP) under contracts
N0001407PD20006 and W81XVVH-09-2-0168, respectively, for supporting this
work. The content included in this work does not necessarily reflect the
position or policy of the US Government.
NR 24
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PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0021-9290
J9 J BIOMECH
JI J. Biomech.
PD NOV 15
PY 2012
VL 45
IS 16
BP 2899
EP 2906
DI 10.1016/j.jbiomech.2012.07.027
PG 8
WC Biophysics; Engineering, Biomedical
SC Biophysics; Engineering
GA 050FS
UT WOS:000312039100026
PM 23010219
ER
PT J
AU Fazal, IM
Ahmed, N
Wang, J
Yang, JY
Yan, Y
Shamee, B
Huang, H
Yue, Y
Dolinar, S
Tur, M
Willner, AE
AF Fazal, Irfan M.
Ahmed, Nisar
Wang, Jian
Yang, Jeng-Yuan
Yan, Yan
Shamee, Bishara
Huang, Hao
Yue, Yang
Dolinar, Sam
Tur, Moshe
Willner, Alan E.
TI 2 Tbit/s free-space data transmission on two orthogonal
orbital-angular-momentum beams each carrying 25 WDM channels
SO OPTICS LETTERS
LA English
DT Article
ID DIVISION; SYSTEMS; LIGHT
AB We demonstrate a 2 Tbit/s free-space data link using two orthogonal orbital angular momentum beams each carrying 25 different wavelength-division-multiplexing channels. We measure the performance for different modulation formats, including directly detected 40 Gbit/s nonreturn-to-zero (NRZ) differential phase-shift keying, 40 Gbit/s NRZ on-off keying, and coherently-detected 10 Gbaud NRZ quadrature phase-shift keying, and achieve low bit error rates with penalties less than 5 dB. (C) 2012 Optical Society of America
C1 [Fazal, Irfan M.; Ahmed, Nisar; Wang, Jian; Yang, Jeng-Yuan; Yan, Yan; Shamee, Bishara; Huang, Hao; Yue, Yang; Willner, Alan E.] Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA.
[Dolinar, Sam] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tur, Moshe] Tel Aviv Univ, Sch Elect Engn, IL-69978 Tel Aviv, Israel.
RP Ahmed, N (reprint author), Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA.
EM nisarahm@usc.edu
RI Yue, Yang/A-3357-2012
FU DARPA under the InPho (Information in Photon) program
FX We acknowledge the support of DARPA under the InPho (Information in
Photon) program.
NR 14
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Z9 10
U1 0
U2 19
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 NOV 15
PY 2012
VL 37
IS 22
BP 4753
EP 4755
PG 3
WC Optics
SC Optics
GA 038JA
UT WOS:000311169800063
PM 23164902
ER
PT J
AU Jozwiak, LM
Head, JW
Zuber, MT
Smith, DE
Neumann, GA
AF Jozwiak, Lauren M.
Head, James W.
Zuber, Maria T.
Smith, David E.
Neumann, Gregory A.
TI Lunar floor-fractured craters: Classification, distribution, origin and
implications for magmatism and shallow crustal structure
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID IMPACT CRATERS; VISCOUS RELAXATION; EVOLUTION; GRAVITY; BASINS;
INTRUSIONS; VOLCANISM; ERUPTION; MERCURY; DEPTH
AB Floor-Fractured Craters (FFCs) are a class of lunar craters characterized by anomalously shallow floors cut by radial, concentric, and/or polygonal fractures; additional interior features are moats, ridges, and patches of mare material. Two formation mechanisms have been hypothesized-floor uplift in response to shallow magmatic intrusion and sill formation, and floor shallowing in response to thermally driven viscous relaxation. This study combines new Lunar Orbiter Laser Altimeter (LOLA) and Lunar Reconnaissance Orbiter Camera (LROC) data to characterize and categorize the population of FFCs and map their distribution on the Moon, and uses variations in floor-fractured crater morphology and regional distribution to investigate the proposed formation mechanisms. The population of FFCs was categorized according to the classes outlined by Schultz (1976). The distribution of these FFC categories shows an evolution of crater morphology from areas adjacent to lunar impact basins to areas in the lunar highlands. We propose that this trend is supportive of formation by shallow magmatic intrusion and sill formation-crustal thickness determines the magnitude of magmatic driving pressure, and thus either piston-like floor uplift for high magnitude, or a convex floor profile for low magnitude. Predictions from previous studies modeling viscous relaxation are inconsistent with the observed altimetric profiles of FFCs. Hence our analysis favors FFC formation by shallow magmatic intrusion, with the variety of FFC morphologies being intimately linked with location and crustal thickness, and the driving pressure of the intrusion. Data from the GRAIL (Gravity Recovery and Interior Laboratory) mission will help to test these conclusions.
C1 [Jozwiak, Lauren M.; Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Zuber, Maria T.; Smith, David E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA.
[Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
RP Jozwiak, LM (reprint author), Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
EM lauren_jozwiak@brown.edu
RI Neumann, Gregory/I-5591-2013; Jozwiak, Lauren/N-2474-2016
OI Neumann, Gregory/0000-0003-0644-9944; Jozwiak,
Lauren/0000-0001-7946-5633
FU LRO LOLA [NNX09AM54G]
FX Thanks are extended to the Lunar Reconnaissance Orbiter (LRO) mission
personnel and to the planning and operations teams for both LOLA and
LROC. This work was supported by the LRO LOLA team through grant
NNX09AM54G to JWH.
NR 43
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U1 0
U2 16
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 NOV 15
PY 2012
VL 117
AR E11005
DI 10.1029/2012JE004134
PG 23
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 039OJ
UT WOS:000311256000001
ER
PT J
AU Zhang, FF
Xu, HF
Konishi, H
Kemp, JM
Roden, EE
Shen, ZZ
AF Zhang, Fangfu
Xu, Huifang
Konishi, Hiromi
Kemp, Joshua M.
Roden, Eric E.
Shen, Zhizhang
TI Dissolved sulfide-catalyzed precipitation of disordered dolomite:
Implications for the formation mechanism of sedimentary dolomite
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID SULFATE-REDUCING BACTERIA; CONTINENTAL-MARGIN SEDIMENTS; ANAEROBIC
METHANE OXIDATION; LATEMAR CARBONATE BUILDUP; ORGANIC-RICH SEDIMENTS;
GULF-OF-CALIFORNIA; CALCIUM-CARBONATE; ORGANOGENIC DOLOMITIZATION;
ISOTOPE FRACTIONATION; MICROBIAL MEDIATION
AB Dolomite is a common mineral in the rock record. However, the rarity of modern dolomite and the notorious difficulty in synthesizing dolomite abiotically under normal Earth-surface conditions result in the long-standing "dolomite problem" in sedimentary geology. Some modern dolomites are associated with sediments where microbial sulfate reduction is active; however, the role of sulfate-reducing bacteria in dolomite formation is still under debate. In this study, we tested the effect of dissolved sulfide on the precipitation of Ca-Mg carbonates, which has been never explored before although dissolved sulfide is one of the major products of microbial sulfate reduction. Our results demonstrated that dissolved sulfide with a concentration of as low as several millimoles can enhance the Mg2+ incorporation into the calcitic structure, and promote the crystallization of high magnesian calcite and disordered dolomite. We also conducted seeded precipitation in experimental solutions containing dissolved sulfide, which showed that calcite seeds can inhibit the precipitation of aragonite and monohydrocalcite (CaCO3 center dot H2O), and induce more Mg2+ incorporation. We propose that accumulated dissolved sulfide in pore waters in organic-rich sediments may trigger the precipitation of disordered dolomite which can be considered as a precursor of some sedimentary dolomite. Our adsorption experiments revealed a strong adsorption of dissolved sulfide onto calcite faces. We suggest that adsorbed dissolved sulfide can lower the energy barrier to the dehydration of Mg2+-water complexes on the growing carbonate surfaces. This study sheds new light on understanding the role of sulfate-reducing bacteria in dolomite formation and the formation mechanism of sedimentary dolomite. (C) 2012 Published by Elsevier Ltd.
C1 [Zhang, Fangfu; Xu, Huifang; Konishi, Hiromi; Kemp, Joshua M.; Roden, Eric E.; Shen, Zhizhang] Univ Wisconsin, Dept Geosci, NASA Astrobiol Inst, Madison, WI 53706 USA.
RP Xu, HF (reprint author), Univ Wisconsin, Dept Geosci, NASA Astrobiol Inst, 1215 W Dayton St,A352 Weeks Hall, Madison, WI 53706 USA.
EM hfxu@geology.wisc.edu
RI Zhang, Fangfu/B-4295-2014
OI Zhang, Fangfu/0000-0001-7550-9483
FU NASA Astrobiology Institute [N07-5489]; NSF [EAR-095800]; U.S.
Department of Energy [DE-SC0001929]; Department of Geoscience,
University of Wisconsin-Madison; ExxonMobil; Geological Society of
America
FX This work is supported by NASA Astrobiology Institute (N07-5489), NSF
(EAR-095800), and U.S. Department of Energy (DE-SC0001929). We thank
Prof. Timothy W. Lyons for handling this paper and the three anonymous
reviewers for their fruitful suggestions which greatly improved this
paper. We thank Dr. John Fournelle for providing the dolomite standard.
Zhang thanks Department of Geoscience, University of Wisconsin-Madison
and ExxonMobil for 2008 Summer Research Grant, and Geological Society of
America for 2009 Graduate Research Grant.
NR 116
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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 NOV 15
PY 2012
VL 97
BP 148
EP 165
DI 10.1016/j.gca.2012.09.008
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 028MW
UT WOS:000310427400010
ER
PT J
AU Peslier, AH
Woodland, AB
Bell, DR
Lazarov, M
Lapen, TJ
AF Peslier, A. H.
Woodland, A. B.
Bell, D. R.
Lazarov, M.
Lapen, T. J.
TI Metasomatic control of water contents in the Kaapvaal cratonic mantle
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID NOMINALLY ANHYDROUS MINERALS; SOUTHERN AFRICAN KIMBERLITES; ARCHEAN
LITHOSPHERIC MANTLE; EARTHS UPPER-MANTLE; MELT-ROCK REACTION; RE-OS
ISOTOPE; TRACE-ELEMENT; PERIDOTITE XENOLITHS; ORTHO-PYROXENE; HYDROGEN
DIFFUSION
AB Water and trace element contents were measured by FTIR and laser ablation-ICPMS on minerals from peridotite xenoliths in kimberlites of the Kaapvaal craton from Finsch, Kimberley, Jagersfontein (South Africa), Letseng-La-Terae, and Liqhobong (Lesotho) mines. The peridotites record a wide range of pressure, temperature, oxygen fugacity, and metasomatic events. Correlations between water content or OH vibration bands with major, minor and trace elements in pyroxene and garnet precludes disturbance during xenolith entrainment by the host kimberlite magma and indicate preservation of mantle water contents. Clinopyroxene water contents (150-400 ppm H2O, by weight) correlate with those of orthopyroxene (40-250 ppm). Olivines (Peslier et al., 2008, 2010) and garnets have 0-86 and 0-20 ppm H2O, respectively. Relations in individual xenolith suites between the amount of water and that of incompatible elements Ti, Na, Fe3+ and rare earths in minerals suggests that metasomatism by oxidizing melts controls the water content of olivine, pyroxene and garnet. At pressures <= 5.5 GPa, hydrous, alkaline, siliceous fluids or melts metasomatized Liqhobong and Kimberley peridotites, producing high water contents in their olivine, pyroxenes and garnet. At higher pressures, the percolation of ultramafic melts reacting with peridotite resulted in co-variation of Ca, Ti and water at the edge of garnets at Jagersfontein, and the overall crystallization of garnet with lower water contents than those in the original peridotites. The upward migration of these ultramafic melts through the lithospheric mantle also increased the water content of olivines with decreasing pressure at Finsch Mine. H2O/Ce ratios of melts in equilibrium with Kaapvaal peridotites range from 100 to 20,000 and the larger values may indicate metasomatism in subduction zone settings. Metasomatic events in Kaapvaal peridotites are thought to have occurred from the Archean to the Mesozoic. However, circumstantial evidence suggest that the metasomatic events responsible for setting the water contents may date from the Archean at Kimberley and from the Proterozoic at Jagersfontein. Combined water with Lu-Hf and Sm-Nd isotopic data at Finsch (Lazarov et al., in press-a) and with Ar-Ar phlogopite ages at Liqhobong (Hopp et al., 2008) indicates that water addition by metasomatic melts occurred in the Proterozoic. Water contents of mantle minerals in Kaapvaal xenoliths measured here have been preserved since that time and can consequently be used in modelling viscosity and longevity of cratonic roots since at least the mid-Proterozoic. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Peslier, A. H.] Jacobs Technol, ESCG, Houston, TX 77058 USA.
[Peslier, A. H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Woodland, A. B.] Goethe Univ Frankfurt, Inst Geosci, D-60438 Frankfurt, Germany.
[Bell, D. R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Lazarov, M.] Leibniz Univ Hannover, Inst Mineral, D-30167 Hannover, Germany.
[Lapen, T. J.] Univ Houston, Houston, TX 77204 USA.
RP Peslier, AH (reprint author), Jacobs Technol, ESCG, Mail Code JE23,2224 Bay Area Blvd, Houston, TX 77058 USA.
EM anne.h.peslier@nasa.gov; woodland@em.uni-frankfurt.de;
David.R.Bell@asu.edu; m.lazarov@mineralogie.uni-hannover.de;
tjlapen@uh.edu
FU NSF [EAR-1118335, EAR-1129072, EAR-0743377]
FX This work was supported by NSF (Grants EAR-1118335, EAR-1129072, and
EAR-0743377). Thank you to L. Keller for letting AHP use his Nicolet
FTIR. We are very grateful to M. Gregoire and two anonymous reviewers
for their constructive comments which greatly improved this manuscript
and to M. Norman for his work as editor.
NR 213
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD NOV 15
PY 2012
VL 97
BP 213
EP 246
DI 10.1016/j.gca.2012.08.028
PG 34
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 028MW
UT WOS:000310427400014
ER
PT J
AU Garcia-Soto, C
Vazquez-Cuervo, J
Clemente-Colon, P
Hernandez, F
AF Garcia-Soto, Carlos
Vazquez-Cuervo, Jorge
Clemente-Colon, Pablo
Hernandez, Fabrice
TI Satellite oceanography and climate change
SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY
LA English
DT Article
DE Climate change; Satellite oceanography; Global warming; Sea level rise;
Polar regions; Natural climate variability
ID SEA-SURFACE TEMPERATURE; LEVEL RISE; VARIABILITY; ICE; CHLOROPHYLL;
OSCILLATION; PATTERNS; COLLAPSE; TRENDS; BUDGET
AB Satellites are essential tools in the present monitoring of climate change as they provide frequent measurements of the Earth over decades with significantly high spatial resolution. Satellite measurements of sea surface temperature are a key component in the analyses of global warming and its effects. Altimeters and gravity missions such as GRACE are used to measure sea level rise at global and regional scales. A variety of satellite sensors (microwave and visible radiometers, scatterometers, SAR, gravity sensors, altimeters, etc.) are used for tracking the melting of sea ice and continental ice over the Polar Regions and Greenland. Satellite techniques are used to monitor large scale natural climate oscillations such as El Nino and the influence of atmospheric teleconexions such as NAO. The present issue is the first one of a series of issues updating our knowledge of the satellite-observed variability related to climate change. A short introduction to the topic is presented. (c) 2012 Elsevier Ltd. All rights reserved.
C1 [Garcia-Soto, Carlos] IEO, Santander 39004, Spain.
[Garcia-Soto, Carlos] Plentziako Itsas Estazioa Euskalherriko Unibertsi, Plentzia 48620, Spain.
[Vazquez-Cuervo, Jorge] CALTECH, NASA Jet Prop Lab JPL, Pasadena, CA 91109 USA.
[Clemente-Colon, Pablo] NOAA NSOF, Natl Naval Ice Ctr, Washington, DC 20395 USA.
[Hernandez, Fabrice] MERCATOR Ocean IRD, F-31520 Ramonville St Agne, France.
RP Garcia-Soto, C (reprint author), IEO, Promontorio S Martin S-N, Santander 39004, Spain.
EM carlos.soto@st.ieo.es
RI Clemente-Colon, Pablo/F-5581-2010; Hernandez, Fabrice/F-6642-2013
OI Hernandez, Fabrice/0000-0003-2152-0657
NR 38
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U1 0
U2 45
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0645
EI 1879-0100
J9 DEEP-SEA RES PT II
JI Deep-Sea Res. Part II-Top. Stud. Oceanogr.
PD NOV 15
PY 2012
VL 77-80
SI SI
BP 1
EP 9
DI 10.1016/j.dsr2.2012.07.004
PG 9
WC Oceanography
SC Oceanography
GA 006TS
UT WOS:000308842500001
ER
PT J
AU Nghiem, SV
Clemente-Colon, P
Rigor, IG
Hall, DK
Neumann, G
AF Nghiem, S. V.
Clemente-Colon, P.
Rigor, I. G.
Hall, D. K.
Neumann, G.
TI Seafloor control on sea ice
SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY
LA English
DT Article
DE Sea ice; Bathymetry; Arctic; Scatterometer; IBCAO
ID GREENLAND SEA; POLAR FRONT; BARENTS SEA; OCEAN
AB The seafloor has a profound role in Arctic Sea ice formation and seasonal evolution. Ocean bathymetry controls the distribution and mixing of warm and cold waters, which may originate from different sources, thereby dictating the pattern of sea ice on the ocean surface. Sea ice dynamics, forced by surface winds, are also guided by seafloor features in preferential directions. Here, satellite mapping of sea ice together with buoy measurements are used to reveal the bathymetric control on sea ice growth and dynamics. Bathymetric effects on sea ice formation are clearly observed in the conformity between sea ice patterns and bathymetric characteristics in the peripheral seas. Beyond local features, bathymetric control appears over extensive regions of the sea ice cover across the Arctic Ocean. The large-scale conformity between bathymetry and patterns of different synoptic sea ice classes, including seasonal and perennial sea ice, is identified. An implication of the bathymetric influence is that the maximum extent of the total sea ice cover is relatively stable, as observed by scatterometer data in the decade of the 2000s, while the minimum ice extent has decreased drastically. Because of the geologic control, the sea ice cover can expand only as far as it reaches the seashore, the continental shelf break, or other pronounced bathymetric features in the peripheral seas. Since the seafloor does not change significantly for decades or centuries, sea ice patterns can be recurrent around certain bathymetric features, which, once identified, may help improve short-term forecast, seasonal outlook, and decadal prediction of the sea ice cover. Moreover, the seafloor can indirectly influence the cloud cover by its control on sea ice distribution, which differentially modulates the latent heat flux through ice covered and open water areas. (c) 2012 Elsevier Ltd. All rights reserved.
C1 [Nghiem, S. V.; Neumann, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Clemente-Colon, P.] Natl Naval Ice Ctr, Washington, DC 20395 USA.
[Rigor, I. G.] Univ Washington, Appl Phys Lab, Seattle, WA 98105 USA.
[Hall, D. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Nghiem, SV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM son.v.nghiem@jpl.nasa.gov
RI Clemente-Colon, Pablo/F-5581-2010
FU National Aeronautics and Space Administration (NASA) Cryospheric
Sciences Program (CSP); NASA CSP; NASA
FX The research carried out at the Jet Propulsion Laboratory, California
Institute of Technology, was supported by the National Aeronautics and
Space Administration (NASA) Cryospheric Sciences Program (CSP). The
research at the Goddard Space Flight Center is also supported by NASA
CSP. Rigor is funded by NASA, and the contributors to the International
Arctic Buoy Programme (IABP), which include the International Arctic
Research Center, NASA, NAVO, NIC, NOAA, NSF, ONR, and U.S. Coast Guard.
The views, opinions, and findings contained in this report are those of
the authors and should not be construed as an official National Oceanic
and Atmospheric Administration, or any other U.S. government position,
policy, or decision.
NR 40
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U1 0
U2 18
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0645
EI 1879-0100
J9 DEEP-SEA RES PT II
JI Deep-Sea Res. Part II-Top. Stud. Oceanogr.
PD NOV 15
PY 2012
VL 77-80
SI SI
BP 52
EP 61
DI 10.1016/j.dsr2.2012.04.004
PG 10
WC Oceanography
SC Oceanography
GA 006TS
UT WOS:000308842500006
ER
PT J
AU Dewitte, B
Vazquez-Cuervo, J
Goubanova, K
Illig, S
Takahashi, K
Cambon, G
Purca, S
Correa, D
Gutierrez, D
Sifeddine, A
Ortlieb, L
AF Dewitte, B.
Vazquez-Cuervo, J.
Goubanova, K.
Illig, S.
Takahashi, K.
Cambon, G.
Purca, S.
Correa, D.
Gutierrez, D.
Sifeddine, A.
Ortlieb, L.
TI Change in El Nino flavours over 1958-2008: Implications for the
long-term trend of the upwelling off Peru
SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY
LA English
DT Article
DE El Nino Modoki; Equatorial Kelvin wave; Climate change; Coastal
upwelling; Peru undercurrent
ID SEA-SURFACE TEMPERATURE; HIGH-RESOLUTION; CURRENT SYSTEM; PACIFIC RIM;
WARM POOL; OCEAN; MODEL; CLIMATE; ENSO; REANALYSIS
AB The tropical Pacific variability has experienced changes in its characteristics over the last decades. In particular, there is some evidence of an increased occurrence of El Nino events in the central Pacific (a.k.a. 'Central Pacific El Nino' (CP El Nino) or 'El Nino Modoki'), in contrast with the cold tongue or Eastern Pacific (EP) El Nino which develops in the eastern Pacific. Here we show that the different flavours of El Nino imply a contrasted Equatorial Kelvin Wave (EKW) characteristic and that their rectification on the mean upwelling condition off Peru through oceanic teleconnection is changed when the CP El Nino frequency of occurrence increases. The Simple Ocean Data Assimilation (SODA) reanalysis product is first used to document the seasonal evolution of the EKW during CP and EP El Nino. It is shown that the strong positive asymmetry of ENSO (El Nino Southern Oscillation) is mostly reflected into the EKW activity of the EP El Nino whereas during CP El Nino, the EKW is negatively skewed in the eastern Pacific. Along with slightly cooler conditions off Peru (shallow thermocline) during CP El Nino, this is favourable for the accumulation of cooler SST anomalies along the coast by the remotely forced coastal Kelvin wave. Such a process is observed in a high-resolution regional model of the Humboldt Current system using the SODA outputs as boundary conditions. In particular the model simulates a cooling trend of the SST off Peru although the wind stress forcing has no trend. The model is further used to document the vertical structure along the coast during the two types of El Nino. It is suggested that the increased occurrence of the CP El Nino may also lead to a reduction of mesoscale activity off Peru. (c) 2012 Elsevier Ltd. All rights reserved.
C1 [Dewitte, B.; Goubanova, K.; Illig, S.; Cambon, G.] IRD, LEGOS, Toulouse, France.
[Vazquez-Cuervo, J.] NASA, JPL, CALTECH, Pasadena, CA USA.
[Goubanova, K.] CNES, Toulouse, France.
[Illig, S.; Purca, S.; Gutierrez, D.] Inst Mar Peru, Callao, Peru.
[Takahashi, K.] Inst Geofis Peru, Lima, Peru.
[Correa, D.] Serv Nacl Meteorol & Hidrol Peru, Lima, Peru.
[Gutierrez, D.] Univ Peruana Cayetano Heredia, Programa Maestria Ciencias Mar, Lima, Peru.
[Sifeddine, A.; Ortlieb, L.] IRD, LOCEAN, Paris, France.
[Sifeddine, A.; Ortlieb, L.] IRD, LOCEAN, Bondy, France.
[Sifeddine, A.] Univ Fed Fluminense, LMI PALEOTRACES, Dept Geoquim, Niteroi, RJ, Brazil.
RP Dewitte, B (reprint author), IRD, LEGOS, Toulouse, France.
EM bxd@legos.obs-mip.fr
RI ORTLIEB, Luc/A-8801-2011; Takahashi, Ken/G-5321-2010; Cambon,
Gildas/A-1882-2016;
OI Takahashi, Ken/0000-0003-3670-2939; Cambon, Gildas/0000-0002-3899-1204;
Purca, Sara/0000-0001-8751-1476
FU National Aeronautics and Space Administration; CNES (Centre National
d'Etudes Spatiales, France); Peru Chile Climate Change (PCCC) program of
the Agence Nationale de la Recherche (ANR); CALMIP [2011-[1044]]
FX Most parts of this work were initiated while Boris Dewitte was at CIMOBP
(modelling centre at IMARPE, Peru). Katerina Goubanova was supported by
CNES (Centre National d'Etudes Spatiales, France). Jorge Vazquez-Cuervo
was supported under contract with the National Aeronautics and Space
Administration. We would like to thank the Peru Chile Climate Change
(PCCC) program of the Agence Nationale de la Recherche (ANR) for
financial support. This work was performed using HPC resources from
CALMIP (Grant 2011-[1044]). We are grateful to Dr. Ben Giese from Texas
A&M University for providing the SODA data. Pr. D. Gushchina (University
of Moscow) is also acknowledged for fruitful discussions on a previous
version of this manuscript.
NR 61
TC 24
Z9 24
U1 5
U2 83
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0645
EI 1879-0100
J9 DEEP-SEA RES PT II
JI Deep-Sea Res. Part II-Top. Stud. Oceanogr.
PD NOV 15
PY 2012
VL 77-80
SI SI
BP 143
EP 156
DI 10.1016/j.dsr2.2012.04.011
PG 14
WC Oceanography
SC Oceanography
GA 006TS
UT WOS:000308842500014
ER
PT J
AU Singh, G
West, WC
Soler, J
Katiyar, RS
AF Singh, Gurpreet
West, W. C.
Soler, J.
Katiyar, Ram S.
TI In situ Raman spectroscopy of layered solid solution Li2MnO3-LiMO2 (M =
Ni, Mn, Co)
SO JOURNAL OF POWER SOURCES
LA English
DT Article
DE Cathode; Solid solution; Lithium ion battery; Raman spectroscopy
ID ELECTROCHEMICAL ACTIVITY; IRREVERSIBLE CAPACITY; OXYGEN LOSS;
ELECTRODES; CATHODES; BATTERIES; OXIDE; LI
AB Lithium rich manganese oxide based materials are emerging as possible high energy density cathode materials for lithium ion batteries. In the present research, we have investigated the first charge/discharge profile behavior of Li1.2Ni0.175Co0.1Mn0.52O2 via in situ Raman spectroscopy. X-ray diffraction studies confirm the presence of cation ordering in the transition metal layers. Scanning electron microscopy shows the homogeneous distribution of highly dense spherical agglomerates of similar to 5 mu m size. Steady decrease in impedance up to similar to 4.5 V followed by a less steep increase as the cell voltage traversed the first charge cycle has been confirmed by electrochemical impedance spectroscopy. Raman spectroscopy shows that the extraction of lithium takes place from both the transition metal layers as well as lithium layers in the voltage range of 4.1-4.4 V. The oxygen removal becomes severe in the voltage range of 4.55-4.6 V, after which the diffusion of the transition metal ions to the vacant sites takes place. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Singh, Gurpreet; Katiyar, Ram S.] Univ Puerto Rico, Dept Phys, Inst Funct Nanomat, San Juan, PR 00936 USA.
[West, W. C.; Soler, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Singh, G (reprint author), Univ Puerto Rico, Dept Phys, Inst Funct Nanomat, San Juan, PR 00936 USA.
EM singhgurpreet268@yahoo.com
RI Singh, Gurpreet/B-5293-2012
OI Singh, Gurpreet/0000-0001-5496-6992
FU NASA-URC [NNX08BA48A]; NASA
FX The financial support from NASA-URC (NNX08BA48A) grant to University of
Puerto Rico is gratefully acknowledged.; This work was partially carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. The authors acknowledge the funding support of NASA's
Space Power Systems Program.
NR 21
TC 23
Z9 25
U1 7
U2 159
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-7753
EI 1873-2755
J9 J POWER SOURCES
JI J. Power Sources
PD NOV 15
PY 2012
VL 218
BP 34
EP 38
DI 10.1016/j.jpowsour.2012.06.083
PG 5
WC Chemistry, Physical; Electrochemistry; Energy & Fuels; Materials
Science, Multidisciplinary
SC Chemistry; Electrochemistry; Energy & Fuels; Materials Science
GA 009PQ
UT WOS:000309038100007
ER
PT J
AU Bell, SW
Thomson, BJ
Dyar, MD
Neish, CD
Cahill, JTS
Bussey, DBJ
AF Bell, Samuel W.
Thomson, Bradley J.
Dyar, M. Darby
Neish, Catherine D.
Cahill, Joshua T. S.
Bussey, D. B. J.
TI Dating small fresh lunar craters with Mini-RF radar observations of
ejecta blankets
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID IMPACT CRATERS; AGE; MATURITY; FARSIDE; SURFACE; EARTH; MOON
AB The ages of large impact craters on the Moon can be estimated by measuring the size-frequency distribution of smaller craters superimposed on their ejecta, but applying this method to individual craters under similar to 3 km in diameter remains difficult due to their limited areal extent. The ejecta blankets of fresh lunar impact craters are expressed as halos of optical and radar bright material that gradually fade with time. Although compositional differences make inferring crater ages from optical albedo problematic, radar is less sensitive to composition and thus may provide a more reliable means of estimating age. In this work, we use radar data from the Miniature Radio Frequency (Mini-RF) instrument on the Lunar Reconnaissance Orbiter (LRO) to characterize the radar backscatter of large numbers of ejecta blankets. By analyzing the size-frequency distribution of these craters, we show that the lifetime of the radar-bright discontinuous ejecta blanket varies with crater diameter in a predictable way for craters with diameters between 0.45 and 5 km. Absolute ages of individual craters can then be estimated by combining this empirically derived model with estimates of the relative degradation state of each individual crater. The lifetimes of radar-bright discontinuous ejecta blankets are significantly shorter in the highlands than the maria, although this is likely due to local topography, creating difficulties in applying the method to the highlands. The cosmic ray exposure age of South Ray Crater, a fresh crater visited by Apollo 16, provides confirmation of these results. This method therefore provides a new way to accurately date small, fresh craters using the Mini-RF data set.
C1 [Bell, Samuel W.] Brown Univ, Providence, RI 02912 USA.
[Thomson, Bradley J.] Boston Univ, Ctr Remote Sensing, Boston, MA 02215 USA.
[Dyar, M. Darby] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA.
[Neish, Catherine D.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Cahill, Joshua T. S.; Bussey, D. B. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
RP Bell, SW (reprint author), Brown Univ, 45 Prospect St, Providence, RI 02912 USA.
EM samuel_bell@brown.edu
RI Neish, Catherine/G-6321-2012; Cahill, Joshua/I-3656-2012;
OI Cahill, Joshua/0000-0001-6874-5533; Thomson, Bradley/0000-0001-8635-8932
NR 60
TC 11
Z9 11
U1 0
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 NOV 14
PY 2012
VL 117
AR E00H30
DI 10.1029/2011JE004007
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 039OG
UT WOS:000311255600001
ER
PT J
AU Harrison, KW
Kumar, SV
Peters-Lidard, CD
Santanello, JA
AF Harrison, Kenneth W.
Kumar, Sujay V.
Peters-Lidard, Christa D.
Santanello, Joseph A.
TI Quantifying the change in soil moisture modeling uncertainty from remote
sensing observations using Bayesian inference techniques
SO WATER RESOURCES RESEARCH
LA English
DT Article
ID CHAIN MONTE-CARLO; SATURATED HYDRAULIC CONDUCTIVITY; LAND
INFORMATION-SYSTEM; MESOSCALE ETA-MODEL; BOUNDARY-LAYER; UNITED-STATES;
DIFFERENTIAL EVOLUTION; PEDOTRANSFER FUNCTIONS; HETEROGENEOUS SOILS;
MAXIMUM-LIKELIHOOD
AB Operational land surface models (LSMs) compute hydrologic states such as soil moisture that are needed for a range of important applications (e. g., drought, flood, and weather prediction). The uncertainty in LSM parameters is sufficiently great that several researchers have proposed conducting parameter estimation using globally available remote sensing data to identify best fit local parameter sets. However, even with in situ data at fine modeling scales, there can be significant remaining uncertainty in LSM parameters and outputs. Here, using a new uncertainty estimation subsystem of the NASA Land Information System (LIS) (described herein), a Markov chain Monte Carlo (MCMC) technique is applied to conduct Bayesian analysis for the accounting of parameter uncertainties. The Differential Evolution Markov Chain (DE-MC) MCMC algorithm was applied, for which a new parallel implementation was developed. A case study is examined that builds on previous work in which the Noah LSM was calibrated to passive (L-band) microwave remote sensing estimates of soil moisture for the Walnut Gulch Experimental Watershed. In keeping with prior related studies, the parameters subjected to the analysis were restricted to the soil hydraulic properties (SHPs). The main goal is to estimate SHPs and soil moisture simulation uncertainty before and after consideration of the remote sensing data. The prior SHP uncertainty is based on the original source of the standard SHP lookup tables for the Noah LSM. Conclusions are drawn regarding the value and viability of Bayesian analysis over alternative approaches (e. g., parameter estimation, lookup tables) and further research needs are identified.
C1 [Harrison, Kenneth W.; Kumar, Sujay V.; Peters-Lidard, Christa D.; Santanello, Joseph A.] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kumar, Sujay V.] Sci Applicat Int Corp, Beltsville, MD USA.
[Harrison, Kenneth W.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Harrison, KW (reprint author), NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Code 617,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM ken.harrison@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 Earth Science Technology Office (ESTO) [AIST-08-077]
FX We gratefully acknowledge the financial support from the NASA Earth
Science Technology Office (ESTO) (Advanced Information System Technology
program award AIST-08-077). Thanks to David Mocko and Scott Rheingrover
for helpful comments. Also, we thank the anonymous reviewers who
suggestions improved the manuscript. Computing was supported by the
resources at the NASA Center for Climate Simulation.
NR 132
TC 14
Z9 14
U1 2
U2 34
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
EI 1944-7973
J9 WATER RESOUR RES
JI Water Resour. Res.
PD NOV 13
PY 2012
VL 48
AR W11514
DI 10.1029/2012WR012337
PG 22
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 039AW
UT WOS:000311216200003
ER
PT J
AU Gerin, M
Levrier, F
Falgarone, E
Godard, B
Hennebelle, P
Le Petit, F
De Luca, M
Neufeld, D
Sonnentrucker, P
Goldsmith, P
Flagey, N
Lis, DC
Persson, CM
Black, JH
Goicoechea, JR
Menten, KM
AF Gerin, M.
Levrier, F.
Falgarone, E.
Godard, B.
Hennebelle, P.
Le Petit, F.
De Luca, M.
Neufeld, D.
Sonnentrucker, P.
Goldsmith, P.
Flagey, N.
Lis, D. C.
Persson, C. M.
Black, J. H.
Goicoechea, J. R.
Menten, K. M.
TI Hydride spectroscopy of the diffuse interstellar medium: new clues on
the gas fraction in molecular form and cosmic ray ionization rate in
relation to H-3(+)
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL
AND ENGINEERING SCIENCES
LA English
DT Article
DE diffuse interstellar medium; W49N; W51
ID MEUDON PDR CODE; HERSCHEL/HIFI OBSERVATIONS; G10.6-0.4 W31C; NITROGEN
HYDRIDES; ABSORPTION-LINES; SIGHT-LINE; CLOUDS; REGIONS; W49N;
CHLORONIUM
AB The Herschel-guaranteed time key programme PRobing InterStellar Molecules with Absorption line Studies (PRISMAS)(1) is providing a survey of the interstellar hydrides containing the elements C, O, N, F and Cl. As the building blocks of interstellar molecules, hydrides provide key information on their formation pathways. They can also be used as tracers of important physical and chemical properties of the interstellar gas that are difficult to measure otherwise. This paper presents an analysis of two sight-lines investigated by the PRISMAS project, towards the star-forming regions W49N and W51. By combining the information extracted from the detected spectral lines, we present an analysis of the physical properties of the diffuse interstellar gas, including the electron abundance, the fraction of gas in molecular form, and constraints on the cosmic ray ionization rate and the gas density.
C1 [Gerin, M.; Levrier, F.; Falgarone, E.; Hennebelle, P.; De Luca, M.] Observ Paris, LERMA, CNRS UMR8112, F-75014 Paris, France.
[Gerin, M.; Levrier, F.; Falgarone, E.; Hennebelle, P.; De Luca, M.] ENS, F-75230 Paris 05, France.
[Godard, B.; Goicoechea, J. R.] Ctr Astrobiol CAB, Madrid 28850, Spain.
[Le Petit, F.] Observ Paris, LUTh, CNRS UMR8102, Meudon, France.
[Neufeld, D.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Sonnentrucker, P.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Goldsmith, P.; Flagey, N.] Jet Prop Lab, Pasadena, CA 91011 USA.
[Lis, D. C.] CALTECH, Pasadena, CA 91125 USA.
[Persson, C. M.; Black, J. H.] Chalmers, SE-43992 Onsala, Sweden.
[Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
RP Gerin, M (reprint author), Observ Paris, LERMA, CNRS UMR8112, F-75014 Paris, France.
EM maryvonne.gerin@lra.ens.fr
FU CNES; CNRS/INSU program PCMI; French Agence Nationale de la Recherche
[ANR-09-BLAN-0231-01]
FX HIFI has been designed and built by a consortium of institutes and
university departments from across Europe, Canada and the USA under the
leadership of the SRON Netherlands Institute for Space Research,
Groningen, The Netherlands, and with major contributions from Germany,
France and the USA. Consortium members are: Canada: CSA, U. Waterloo.
France: CESR, LAB, LERMA, IRAM. Germany: KOSMA, MPIfR, MPS. Ireland: NUI
Maynooth. Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di
Arcetri-INAF. The Netherlands: SRON, TUD. Poland: CAMK, CBK. Spain:
Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia
(CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS &
GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm
University-Stockholm Observatory. Switzerland: ETH Zurich, FHNW. USA:
Caltech, JPL, NHSC. M.G., F.L., E.F., P.H. and M.D.L. acknowledge
support from CNES and from the CNRS/INSU program PCMI. The chemical
modelling is partly funded by grant no. ANR-09-BLAN-0231-01 from the
French Agence Nationale de la Recherche as part of the SCHISM project.
NR 32
TC 13
Z9 13
U1 0
U2 5
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1364-503X
J9 PHILOS T R SOC A
JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci.
PD NOV 13
PY 2012
VL 370
IS 1978
BP 5174
EP 5185
DI 10.1098/rsta.2012.0023
PG 12
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 016MN
UT WOS:000309522800017
PM 23028164
ER
PT J
AU Beilicke, M
Baring, MG
Barthelmy, S
Binns, WR
Buckley, J
Cowsik, R
Dowkontt, P
Garson, A
Guo, Q
Haba, Y
Israel, MH
Kunieda, H
Lee, K
Matsumoto, H
Miyazawa, T
Okajima, T
Schnittman, J
Tamura, K
Tueller, J
Krawczynski, H
AF Beilicke, M.
Baring, M. G.
Barthelmy, S.
Binns, W. R.
Buckley, J.
Cowsik, R.
Dowkontt, P.
Garson, A.
Guo, Q.
Haba, Y.
Israel, M. H.
Kunieda, H.
Lee, K.
Matsumoto, H.
Miyazawa, T.
Okajima, T.
Schnittman, J.
Tamura, K.
Tueller, J.
Krawczynski, H.
TI Design and tests of the hard X-ray polarimeter X-Calibur
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article; Proceedings Paper
CT 3rd Roma International Conference on Astroparticle Physics (RICAP)
CY MAY 24-27, 2011
CL Roma Tre Univ, Roma, ITALY
SP Univ Sapienza, Univ Tor Vergata
HO Roma Tre Univ
DE X-rays; Polarization; Black hole; InFOC mu S; X-Calibur
ID EMISSION; CRAB
AB X-ray polarimetry will give qualitatively new information about high-energy astrophysical sources. We designed, built and tested a hard X-ray polarimeter X-Calibur to be used in the focal plane of the InFOC mu S grazing incidence hard X-ray telescope. X-Calibur combines a low-Z Compton scatterer with a CZT detector assembly to measure the polarization of 10-80 keV X-rays making use of the fact that polarized photons Compton scatter preferentially perpendicular to the electric field orientation. X-Calibur achieves a high detection efficiency of order unity. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Beilicke, M.; Binns, W. R.; Buckley, J.; Cowsik, R.; Dowkontt, P.; Garson, A.; Guo, Q.; Israel, M. H.; Lee, K.; Krawczynski, H.] Washington Univ, St Louis, MO 63130 USA.
[Baring, M. G.] Rice Univ, Houston, TX 77251 USA.
[Barthelmy, S.; Okajima, T.; Schnittman, J.; Tueller, J.] Goddard Space Flight Ctr, Greenbelt, MD USA.
[Haba, Y.; Kunieda, H.; Matsumoto, H.; Miyazawa, T.; Tamura, K.] Nagoya Univ, Nagoya, Aichi 4648601, Japan.
RP Beilicke, M (reprint author), Washington Univ, St Louis, MO 63130 USA.
EM beilicke@physics.wustl.edu
NR 8
TC 1
Z9 1
U1 1
U2 2
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 NOV 11
PY 2012
VL 692
BP 283
EP 284
DI 10.1016/j.nima.2011.12.111
PG 2
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 020CJ
UT WOS:000309786000058
ER
PT J
AU Aliu, E
Archambault, S
Arlen, T
Aune, T
Beilicke, M
Benbow, W
Bottcher, M
Bouvier, A
Buckley, JH
Bugaev, V
Cesarini, A
Ciupik, L
Collins-Hughes, E
Connolly, MP
Cui, W
Dickherber, R
Duke, C
Dumm, J
Errando, M
Falcone, A
Federici, S
Feng, Q
Finley, JP
Finnegan, G
Fortson, L
Furniss, A
Galante, N
Gall, D
Godambe, S
Griffin, S
Grube, J
Gyuk, G
Hanna, D
Holder, J
Huan, H
Kaaret, P
Karlsson, N
Khassen, Y
Kieda, D
Krawczynski, H
Krennrich, F
Lee, K
Madhavan, AS
Maier, G
Majumdar, P
McArthur, S
McCann, A
Moriarty, P
Mukherjee, R
Nelson, T
de Bhroithe, AO
Ong, RA
Orr, M
Otte, AN
Park, N
Perkins, JS
Pichel, A
Pohl, M
Prokoph, H
Quinn, J
Ragan, K
Reyes, LC
Reynolds, PT
Roache, E
Saxon, DB
Sembroski, GH
Staszak, D
Telezhinsky, I
Tesic, G
Theiling, M
Thibadeau, S
Tsurusaki, K
Varlotta, A
Vassiliev, VV
Vincent, S
Vivier, M
Wakely, SP
Weekes, TC
Weinstein, A
Welsing, R
Williams, DA
Zitzer, B
Fortin, P
Horan, D
Fumagalli, M
Kaplan, K
Prochaska, JX
AF Aliu, E.
Archambault, S.
Arlen, T.
Aune, T.
Beilicke, M.
Benbow, W.
Boettcher, M.
Bouvier, A.
Buckley, J. H.
Bugaev, V.
Cesarini, A.
Ciupik, L.
Collins-Hughes, E.
Connolly, M. P.
Cui, W.
Dickherber, R.
Duke, C.
Dumm, J.
Errando, M.
Falcone, A.
Federici, S.
Feng, Q.
Finley, J. P.
Finnegan, G.
Fortson, L.
Furniss, A.
Galante, N.
Gall, D.
Godambe, S.
Griffin, S.
Grube, J.
Gyuk, G.
Hanna, D.
Holder, J.
Huan, H.
Kaaret, P.
Karlsson, N.
Khassen, Y.
Kieda, D.
Krawczynski, H.
Krennrich, F.
Lee, K.
Madhavan, A. S.
Maier, G.
Majumdar, P.
McArthur, S.
McCann, A.
Moriarty, P.
Mukherjee, R.
Nelson, T.
de Bhroithe, A. O'Faolain
Ong, R. A.
Orr, M.
Otte, A. N.
Park, N.
Perkins, J. S.
Pichel, A.
Pohl, M.
Prokoph, H.
Quinn, J.
Ragan, K.
Reyes, L. C.
Reynolds, P. T.
Roache, E.
Saxon, D. B.
Sembroski, G. H.
Staszak, D.
Telezhinsky, I.
Tesic, G.
Theiling, M.
Thibadeau, S.
Tsurusaki, K.
Varlotta, A.
Vassiliev, V. V.
Vincent, S.
Vivier, M.
Wakely, S. P.
Weekes, T. C.
Weinstein, A.
Welsing, R.
Williams, D. A.
Zitzer, B.
Fortin, P.
Horan, D.
Fumagalli, M.
Kaplan, K.
Prochaska, J. X.
CA VERITAS Collaboration
TI VERITAS OBSERVATIONS OF SIX BRIGHT, HARD-SPECTRUM FERMI-LAT BLAZARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: general; gamma rays: galaxies
ID EXTRAGALACTIC BACKGROUND LIGHT; BL-LACERTAE OBJECTS; ALL-SKY SURVEY;
LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; ENERGY GAMMA-RAYS;
MULTIWAVELENGTH OBSERVATIONS; RELATIVISTIC JET; COMPLETE SAMPLE; SOURCE
CATALOG
AB We report on VERITAS very high energy (VHE; E >= 100 GeV) observations of six blazars selected from the Fermi Large Area Telescope First Source Catalog (1FGL). The gamma-ray emission from 1FGL sources was extrapolated up to the VHE band, taking gamma-ray absorption by the extragalactic background light into account. This allowed the selection of six bright, hard-spectrum blazars that were good candidate TeV emitters. Spectroscopic redshift measurements were attempted with the Keck Telescope for the targets without Sloan Digital Sky Survey spectroscopic data. No VHE emission is detected during the observations of the six sources described here. Corresponding TeV upper limits are presented, along with contemporaneous Fermi observations and non-concurrent Swift UVOT and X-Ray Telescope data. The blazar broadband spectral energy distributions (SEDs) are assembled and modeled with a single-zone synchrotron self-Compton model. The SED built for each of the six blazars shows a synchrotron peak bordering between the intermediate-and high-spectrum-peak classifications, with four of the six resulting in particle-dominated emission regions.
C1 [Aune, T.; Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Aune, T.; Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA.
[Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Staszak, D.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Arlen, T.; Majumdar, P.; Ong, R. A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; Lee, K.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Benbow, W.; Galante, N.; Roache, E.; Weekes, T. C.; Fortin, P.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Boettcher, M.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA.
[Cesarini, A.; Connolly, M. P.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Collins-Hughes, E.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Natl Univ Ireland Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA.
[Dumm, J.; Fortson, L.; Karlsson, N.; Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Falcone, A.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Federici, S.; Maier, G.; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.; Welsing, R.] DESY, D-15738 Zeuthen, Germany.
[Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Finnegan, G.; Godambe, S.; Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Gall, D.; Kaaret, P.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Huan, H.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Otte, A. N.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Otte, A. N.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA.
[Perkins, J. S.] NASA, Astroparticle Phys Lab, GSFC, Greenbelt, MD 20771 USA.
[Perkins, J. S.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina.
[Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
[Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Prochaska, J. X.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Boettcher, M.] North West Univ, Ctr Space Res, ZA-2531 Potchefstroom, South Africa.
RP Furniss, A (reprint author), Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
EM afurniss@ucsc.edu; pafortin@cfa.harvard.edu; deirdre@llr.in2p3.fr
RI Khassen, Yerbol/I-3806-2015; Fumagalli, Michele/K-9510-2015;
OI Khassen, Yerbol/0000-0002-7296-3100; Fumagalli,
Michele/0000-0001-6676-3842; Cui, Wei/0000-0002-6324-5772; Cesarini,
Andrea/0000-0002-8611-8610
FU U.S. Department of Energy Office of Science; U.S. National Science
Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation
Ireland [SFI 10/RFP/AST2748]; STFC in the U.K; NSF [AST-0548180]; Alfred
P. Sloan Foundation; U.S. Department of Energy; National Aeronautics and
Space Administration; Japanese Monbukagakusho; Max Planck Society;
Higher Education Funding Council for England; Istituto Nazionale di
Astrofisica in Italy; Centre National d'Etudes Spatiales in France
FX This research is supported by grants from the U.S. Department of Energy
Office of Science, the U.S. National Science Foundation, and the
Smithsonian Institution, by NSERC in Canada, by Science Foundation
Ireland (SFI 10/RFP/AST2748), and by STFC in the U.K. We acknowledge the
excellent work of the technical support staff at the Fred Lawrence
Whipple Observatory and at the collaborating institutions in the
construction and operation of the instrument. The Fermi-LAT
Collaboration acknowledges generous support from a number of agencies
and institutes that have supported the development and the operation of
the LAT as well as scientific data analysis. These include the National
Aeronautics and Space Administration and the Department of Energy in the
United States, the Commissariat a l'Energie Atomique and the Centre
National de la Recherche Scientifique/Institut National de Physique
Nucleaire et de Physique des Particules in France, the Agenzia Spaziale
Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the
Ministry of Education, Culture, Sports, Science and Technology (MEXT),
High Energy Accelerator Research Organization (KEK), and Japan Aerospace
Exploration Agency (JAXA) in Japan, and the K.A. Wallenberg Foundation,
the Swedish Research Council, and the Swedish National Space Board in
Sweden. Additional support for science analysis during the operations
phase is acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National d'Etudes Spatiales in France. J.X.P.
acknowledges funding through an NSF CAREER grant (AST-0548180). Funding
for the SDSS and SDSS-II has been provided by the Alfred P. Sloan
Foundation, the Participating Institutions, the National Science
Foundation, the U.S. 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
Web site is http://www.sdss.org/. This research has made use of the
NASA/IPAC Extragalactic Database (NED) which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration.
NR 91
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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 NOV 10
PY 2012
VL 759
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AR 102
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PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034ZL
UT WOS:000310911300025
ER
PT J
AU Hewitt, JW
Grondin, MH
Lemoine-Goumard, M
Reposeur, T
Ballet, J
Tanaka, T
AF Hewitt, J. W.
Grondin, M. -H.
Lemoine-Goumard, M.
Reposeur, T.
Ballet, J.
Tanaka, T.
TI FERMI-LAT AND WMAP OBSERVATIONS OF THE PUPPIS A SUPERNOVA REMNANT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; cosmic rays; ISM: individual objects (Puppis
A); radiation mechanisms: non-thermal
ID LARGE-AREA TELESCOPE; GAMMA-RAY EMISSION; MOLECULAR CLOUDS; NEUTRAL
HYDROGEN; VLA OBSERVATIONS; EMITTING EJECTA; DISCOVERY; PULSAR;
CASSIOPEIA; DIRECTION
AB We report the detection of GeV gamma-ray emission from the supernova remnant (SNR) Puppis A with the Fermi Gamma-Ray Space Telescope. Puppis A is among the faintest SNRs yet detected at GeV energies, with a luminosity of only 2.7 x 10(34) (D/2.2 kpc)(2) erg s(-1) between 1 and 100 GeV. The gamma-ray emission from the remnant is spatially extended, with a morphology matching that of the radio and X-ray emission, and is well described by a simple power law with an index of 2.1. We attempt to model the broadband spectral energy distribution (SED), from radio to gamma-rays, using standard nonthermal emission mechanisms. To constrain the relativistic electron population we use 7 years of Wilkinson Microwave Anisotropy Probe data to extend the radio spectrum up to 93 GHz. Both leptonic- and hadronic-dominated models can reproduce the nonthermal SED, requiring a total content of cosmic-ray electrons and protons accelerated in Puppis A of at least W-CR approximate to (1-5) x 10(49) erg.
C1 [Hewitt, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Grondin, M. -H.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Grondin, M. -H.] Univ Heidelberg, Landessternwarte, D-69117 Heidelberg, Germany.
[Lemoine-Goumard, M.; Reposeur, T.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Ballet, J.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France.
[Tanaka, T.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA.
[Tanaka, T.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
RP Hewitt, JW (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM john.w.hewitt@nasa.gov; marie-helene.grondin@mpi-hd.mpg.de;
lemoine@cenbg.in2p3.fr
FU Istituto Nazionale di Astrofisica in Italy; Centre National d' Etudes
Spatiales in France; Commonwealth Government; Science Mission
Directorate Office at NASA Headquarters; NASA Postdoctoral Program at
the Goddard Space Flight Center; NASA; Fermi Guest Investigator Program;
Alexander von Humboldt Foundation; European Community [ERC-StG-259391]
FX 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 Parkes
radio telescope is part of the Australia Telescope which is funded by
the Commonwealth Government for operation as a National Facility managed
by CSIRO. We thank our colleagues for their assistance with the radio
timing observations.; The WMAP mission is made possible by the support
of the Science Mission Directorate Office at NASA Headquarters. This
research has made use of NASA's Astrophysics Data System Bibliographic
Services, and data obtained from the High Energy Astrophysics Science
Archive Research Center (HEASARC), provided by NASA's Goddard Space
Flight Center. We thank Nils Odegard for assisting us with analysis of
WMAP data, and Gloria Dubner for providing us with the 1.4 GHz radio
image of Puppis A. J.W.H. acknowledges support 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, and also by a grant from the Fermi Guest Investigator
Program. M.H.G. acknowledges support from the Alexander von Humboldt
Foundation. M.L.G. acknowledges funding by contract ERC-StG-259391 from
the European Community.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 10
PY 2012
VL 759
IS 2
AR 89
DI 10.1088/0004-637X/759/2/89
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034ZL
UT WOS:000310911300012
ER
PT J
AU Jenke, PA
Finger, MH
Wilson-Hodge, CA
Camero-Arranz, A
AF Jenke, P. A.
Finger, M. H.
Wilson-Hodge, C. A.
Camero-Arranz, A.
TI ORBITAL DECAY AND EVIDENCE OF DISK FORMATION IN THE X-RAY BINARY PULSAR
OAO 1657-415
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; pulsars: individual (OAO 1657-415); stars:
neutron; stars: winds, outflows; X-rays: binaries
ID NEUTRON STAR STRUCTURE; ACCRETION TORQUES; BURST MONITOR; OAO-1657-415;
OAO1657-415; EVOLUTION; COMPANION
AB OAO 1657-415 is an eclipsing X-ray binary wind-fed pulsar that has exhibited smooth spin-up/spin-down episodes and has undergone several torque reversals throughout its long history of observation. We present a frequency history spanning nearly 19 years of observations from the Burst and Transient Source Experiment and from the Gamma-Ray Burst Monitor (Fermi/GBM). Our analysis suggests two modes of accretion: one resulting in steady spin-up correlated with flux during which we believe a stable accretion disk is present and one in which the neutron star is spinning down at a lesser rate which is uncorrelated with flux. Orbital elements of the pulsar system are determined at several intervals throughout this history. With these ephemerides, statistically significant orbital decay with a P-orb = (-9.74 +/- 0.78) x 10(-8) is established.
C1 [Jenke, P. A.] MSFC NPP, Huntsville, AL 35812 USA.
[Finger, M. H.] Univ Space Res Assoc, Huntsville, AL 35806 USA.
[Wilson-Hodge, C. A.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
[Camero-Arranz, A.] Fac Ciencies, Inst Ciencies Espai CSIC IEEC, E-08193 Barcelona, Spain.
RP Jenke, PA (reprint author), MSFC NPP, Huntsville, AL 35812 USA.
FU NASA [NNX08AW06G, NNX11AE24G]; NASA Postdoctoral Program at the Marshall
Space Flight Center; Fermi Guest Investigator program; Astrophysics Data
Analysis Program (ADAP)
FX We acknowledge Slawomir Suchy for the use of his results from his
observations of OAO 1657-415 by RXTE. M.F. and A.C. acknowledge support
from NASA grants NNX08AW06G and NNX11AE24G. P. Jenke was supported by an
appointment to the NASA Postdoctoral Program at the Marshall Space
Flight Center, administered by Oak Ridge Associated Universities through
a contract with NASA. This work was supported by the Fermi Guest
Investigator program and by the Astrophysics Data Analysis Program
(ADAP).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 10
PY 2012
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PG 8
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SC Astronomy & Astrophysics
GA 034ZL
UT WOS:000310911300047
ER
PT J
AU Monson, AJ
Freedman, WL
Madore, BF
Persson, SE
Scowcroft, V
Seibert, M
Rigby, JR
AF Monson, Andrew J.
Freedman, Wendy L.
Madore, Barry F.
Persson, S. E.
Scowcroft, Victoria
Seibert, Mark
Rigby, Jane R.
TI THE CARNEGIE HUBBLE PROGRAM: THE LEAVITT LAW AT 3.6 AND 4.5 mu m IN THE
MILKY WAY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: stars; stars: variables: Cepheids
ID CEPHEID PERIOD-LUMINOSITY; LARGE-MAGELLANIC-CLOUD;
SPITZER-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; CLASSICAL CEPHEIDS;
GALACTIC CEPHEIDS; TRIGONOMETRIC PARALLAXES; INTERSTELLAR EXTINCTION;
SUPERNOVA PROJECT; COLOR RELATIONS
AB The Carnegie Hubble Program (CHP) is designed to calibrate the extragalactic distance scale using data from the post-cryogenic era of the Spitzer Space Telescope. The ultimate goal of the CHP is a systematic improvement in the distance scale leading to a determination of the Hubble constant to within an accuracy of 2%. This paper focuses on the measurement and calibration of the Galactic Cepheid period-luminosity (PL, Leavitt) relation using the warm Spitzer/IRAC 1 and 2 bands at 3.6 and 4.5 mu m. We present photometric measurements covering the period range 4-70 days for 37 Galactic Cepheids. Data at 24 phase points were collected for each star. Three PL relations of the form M = a(log(P)- 1)+b are derived. The method adopted here takes the slope a to be -3.31, as determined from the Spitzer Large Magellanic Cloud (LMC) data of Scowcroft et al. Using the geometric Hubble Space Telescope guide-star distances to 10 Galactic Cepheids, we find a calibrated 3.6 mu m PL zero point of -5.80 +/- 0.03. Together with our value for the LMC zero point, we determine a reddening-corrected distance modulus of 18.48 +/- 0.04 mag to the LMC. The mid-IR period-color diagram and the [3.6]-[4.5] color variation with phase are interpreted in terms of CO absorption at 4.5 mu m. This situation compromises the use of the 4.5 mu m data for distance determinations.
C1 [Monson, Andrew J.; Freedman, Wendy L.; Madore, Barry F.; Persson, S. E.; Scowcroft, Victoria; Seibert, Mark] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
RP Monson, AJ (reprint author), Observ Carnegie Inst Washington, 813 Santa Barbara St, Pasadena, CA 91101 USA.
EM amonson@obs.carnegiescience.edu; wendy@obs.carnegiescience.edu;
barry@obs.carnegiescience.edu; persson@obs.carnegiescience.edu;
vs@obs.carnegiescience.edu; mseibert@obs.carnegiescience.edu;
Jane.R.Rigby@nasa.gov
RI Rigby, Jane/D-4588-2012
OI Rigby, Jane/0000-0002-7627-6551
FU Jet Propulsion Laboratory, California Institute of Technology; NASA
FX We thank the staff of the Spitzer Science Center for their assistance
with scheduling such a large and complex project as well as the support
received to make these analyses. This work is based (in part) on
observations made with the Spitzer Space Telescope, which is operated by
the Jet Propulsion Laboratory, California Institute of Technology under
a contract with NASA. Support for this work was provided by NASA through
an award issued by JPL/Caltech. We also thank the anonymous referee for
constructive comments regarding the form and content of this work.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 10
PY 2012
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PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034ZL
UT WOS:000310911300069
ER
PT J
AU Nakauchi, D
Suwa, Y
Sakamoto, T
Kashiyama, K
Nakamura, T
AF Nakauchi, Daisuke
Suwa, Yudai
Sakamoto, Takanori
Kashiyama, Kazumi
Nakamura, Takashi
TI LONG-DURATION X-RAY FLASH AND X-RAY-RICH GAMMA-RAY BURSTS FROM LOW-MASS
POPULATION III STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE early universe; gamma rays: general; stars: Population III
ID 1ST STARS; LUMINOSITY RELATION; EVOLUTION; JETS; CONSTRAINTS;
SUPERNOVAE; COLLAPSARS; ACCRETION; REDSHIFT; TRANSIENTS
AB Recent numerical simulations suggest that Population III (Pop III) stars were born with masses not larger than similar to 100 M-circle dot and typically similar to 40 M-circle dot. By self-consistently considering the jet generation and propagation in the envelope of these low-mass Pop III stars, we find that a Pop III blue supergiant star has the possibility of giving rise to a gamma-ray burst (GRB) even though it keeps a massive hydrogen envelope. We evaluate observational characteristics of Pop III GRBs and predict that Pop III GRBs have a duration of similar to 10(5) s in the observer frame and a peak luminosity of similar to 5 x 10(50) erg s(-1). Assuming that the E-p-L-p (or E-p-E-gamma,E-iso) correlation holds for Pop III GRBs, we find that the spectrum peak energy falls at approximately a few keV (or similar to 100 keV) in the observer frame. We discuss the detectability of Pop III GRBs by future satellite missions such as EXIST and Lobster. If the E-p-E-gamma,E-iso correlation holds, we have the possibility to detect Pop III GRBs at z similar to 9 as long-duration X-ray-rich GRBs by EXIST. Conversely, if the E-p-L-p correlation holds, we have the possibility to detect Pop III GRBs up to z similar to 19 as long-duration X-ray flashes by Lobster.
C1 [Nakauchi, Daisuke; Kashiyama, Kazumi; Nakamura, Takashi] Kyoto Univ, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan.
[Suwa, Yudai] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan.
[Sakamoto, Takanori] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Sakamoto, Takanori] Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
[Kashiyama, Kazumi] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
RP Nakauchi, D (reprint author), Kyoto Univ, Dept Phys, Sakyo Ku, Oiwake Cho, Kyoto 6068502, Japan.
RI Suwa, Yudai/G-9711-2012
FU Ministry of Education, Culture, Sports, Science and Technology (MEXT) of
Japan [23540305, 24103006, 23840023]; Universality and Emergence at
Kyoto University
FX We thank A. Heger for kindly providing us his stellar model data. We
thank D. Yonetoku and R. Yamazaki for fruitful discussion and
suggestions about GRB observations. We also thank K. Omukai for fruitful
discussions about Population III stars and the anonymous referee for
fruitful comments. This work is supported in part by the Grant-in-Aid
from the Ministry of Education, Culture, Sports, Science and Technology
(MEXT) of Japan, Nos. 23540305 (T.N.), 24103006 (T.N.), 23840023 (Y.S.)
and by the Grant-in-Aid for the global COE program The Next Generation
of Physics, Spun from Universality and Emergence at Kyoto University.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 10
PY 2012
VL 759
IS 2
AR 128
DI 10.1088/0004-637X/759/2/128
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034ZL
UT WOS:000310911300051
ER
PT J
AU Peacock, MB
Zepf, SE
Kundu, A
Maccarone, TJ
Rhode, KL
Salzer, JJ
Waters, CZ
Ciardullo, R
Gronwall, C
Stern, D
AF Peacock, Mark B.
Zepf, Stephen E.
Kundu, Arunav
Maccarone, Thomas J.
Rhode, Katherine L.
Salzer, John J.
Waters, Christopher Z.
Ciardullo, Robin
Gronwall, Caryl
Stern, Daniel
TI SPATIALLY RESOLVED SPECTROSCOPY OF THE GLOBULAR CLUSTER RZ 2109 AND THE
NATURE OF ITS BLACK HOLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (NGC 4472); galaxies: star clusters: general;
galaxies: star clusters: individual: RZ 2109; globular clusters:
general; X-rays: binaries; X-rays: galaxies: clusters
ID X-RAY BINARIES; HUBBLE-SPACE-TELESCOPE; EARLY-TYPE GALAXIES; LUMINOUS O
III; ELLIPTIC GALAXIES; STAR-CLUSTERS; NGC 4472; N II; MASS; EMISSION
AB We present optical Hubble Space Telescope/Space Telescope Imaging Spectrograph (HST/STIS) spectroscopy of RZ 2109, a globular cluster (GC) in the elliptical galaxy NGC 4472. This GC is notable for hosting an ultraluminous X-ray source as well as associated strong and broad [O III] lambda lambda 4959, 5007 emission. We show that the HST/STIS spectroscopy spatially resolves the [O III] emission in RZ 2109. While we are unable to make a precise determination of the morphology of the emission-line nebula, the best-fitting models all require that the [O III] lambda 5007 emission has a half-light radius in the range 3-7 pc. The extended nature of the [O III] lambda 5007 emission is inconsistent with published models that invoke an intermediate-mass black hole origin. It is also inconsistent with the ionization of ejecta from a nova in the cluster. The spatial scale of the nebula could be produced via the photoionization of a strong wind driven from a stellar mass black hole accreting at roughly its Eddington rate.
C1 [Peacock, Mark B.; Zepf, Stephen E.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Kundu, Arunav] Eureka Sci Inc, Oakland, CA 94602 USA.
[Maccarone, Thomas J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Rhode, Katherine L.; Salzer, John J.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA.
[Waters, Christopher Z.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Ciardullo, Robin; Gronwall, Caryl] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Ciardullo, Robin; Gronwall, Caryl] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Peacock, MB (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
EM mpeacock@msu.edu
FU NASA from the Space Telescope Science Institute [HST-GO-11703,
HST-GO-11029]; AURA, Inc., under NASA [NAS 5-26555]; NASA through
Chandra [GO1-12112X, GO0-11111A]; NASA [NAS8-03060]; NSF Faculty Early
Career Development (CAREER) award [AST-0847109]
FX We thank the anonymous referee for considering this paper and for
helpful comments. We are grateful for the assistance of the HST STIS
helpdesk team, who provided very useful answers and suggestions in
relation to the analysis of these data. Support for this work was
provided by NASA through grant numbers HST-GO-11703 (M.B.P. and S.E.Z.)
and HST-GO-11029 (S.E.Z. and C.Z.W.) from the Space Telescope Science
Institute, which is operated by AURA, Inc., under NASA contract NAS
5-26555. Support for A.K.'s work was provided by NASA through Chandra
grant Numbers GO1-12112X and GO0-11111A issued by the Chandra X-ray
Observatory Center, which is operated by the SAO for and on behalf of
the NASA under contract NAS8-03060. K.L.R. is supported by an NSF
Faculty Early Career Development (CAREER) award (AST-0847109). The work
of D.S. was carried out at Jet Propulsion Laboratory, California
Institute of Technology, under a contract with NASA.; STScI is operated
by the Association of Universities for Research in Astronomy, Inc. under
NASA contract NAS 5-26555.
NR 40
TC 4
Z9 4
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 NOV 10
PY 2012
VL 759
IS 2
AR 126
DI 10.1088/0004-637X/759/2/126
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034ZL
UT WOS:000310911300049
ER
PT J
AU Savani, NP
Shiota, D
Kusano, K
Vourlidas, A
Lugaz, N
AF Savani, N. P.
Shiota, D.
Kusano, K.
Vourlidas, A.
Lugaz, N.
TI A STUDY OF THE HELIOCENTRIC DEPENDENCE OF SHOCK STANDOFF DISTANCE AND
GEOMETRY USING 2.5D MAGNETOHYDRODYNAMIC SIMULATIONS OF CORONAL MASS
EJECTION DRIVEN SHOCKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetohydrodynamics (MHD); solar-terrestrial relations; Sun: coronal
mass ejections (CMEs); Sun: heliosphere
ID MAGNETIC-FIELD; SOLAR-WIND; FLUX ROPE; LASCO OBSERVATIONS; TRIGGER
MECHANISM; STEREO MISSION; IMAGER SMEI; BOW SHOCKS; 1 AU; EVOLUTION
AB We perform four numerical magnetohydrodynamic simulations in 2.5 dimensions ( 2.5D) of fast coronal mass ejections (CMEs) and their associated shock fronts between 10 Rs and 300 Rs. We investigate the relative change in the shock standoff distance, Delta, as a fraction of the CME radial half-width, D-OB (i.e., Delta/D-OB). Previous hydrodynamic studies have related the shock standoff distance for Earth's magnetosphere to the density compression ratio (DR; rho(u)/rho(d)) measured across the bow shock. The DR coefficient, k(dr), which is the proportionality constant between the relative standoff distance (Delta/D-OB) and the compression ratio, was semi-empirically estimated as 1.1. For CMEs, we show that this value varies linearly as a function of heliocentric distance and changes significantly for different radii of curvature of the CME's leading edge. We find that a value of 0.8 +/- 0.1 is more appropriate for small heliocentric distances (<30 Rs) which corresponds to the spherical geometry of a magnetosphere presented by Seiff. As the CME propagates its cross section becomes more oblate and the k(dr) value increases linearly with heliocentric distance, such that k(dr) = 1.1 is most appropriate at a heliocentric distance of about 80 Rs. For terrestrial distances (215 Rs) we estimate k(dr) = 1.8 +/- 0.3, which also indicates that the CME cross-sectional structure is generally more oblate than that of Earth's magnetosphere. These alterations to the proportionality coefficients may serve to improve investigations into the estimates of the magnetic field in the corona upstream of a CME as well as the aspect ratio of CMEs as measured in situ.
C1 [Savani, N. P.] UCAR, Boulder, CO 80307 USA.
[Savani, N. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Shiota, D.] RIKEN, Computat Astrophys Lab, Adv Sci Inst, Wako, Saitama 3510198, Japan.
[Kusano, K.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Kusano, K.] Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa 2360001, Japan.
[Vourlidas, A.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Lugaz, N.] Univ New Hampshire, Expt Space Plasma Grp, Durham, NH 03824 USA.
RP Savani, NP (reprint author), UCAR, Boulder, CO 80307 USA.
EM neel.savani02@imperial.ac.uk
RI Lugaz, Noe/C-1284-2008; Savani, Neel/G-4066-2014; Vourlidas,
Angelos/C-8231-2009;
OI Lugaz, Noe/0000-0002-1890-6156; Savani, Neel/0000-0002-1916-7877;
Vourlidas, Angelos/0000-0002-8164-5948; Shiota,
Daikou/0000-0002-9032-8792
FU NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program; NASA;
office of Naval Research; JSPS fellowship at Nagoya University
FX N.P.S. was supported by the NASA Living With a Star Jack Eddy
Postdoctoral Fellowship Program, administered by the UCAR Visiting
Scientist Programs and hosted by the Naval Research Laboratory. N.P.S.
and A.V. were supported by NASA and the office of Naval Research. The
numerical calculations were made using the supercomputing cluster at the
Solar-Terrestrial Environment Laboratory, Nagoya University. This work
of N.P.S. was in part performed during a JSPS fellowship at Nagoya
University.
NR 75
TC 9
Z9 9
U1 0
U2 14
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 NOV 10
PY 2012
VL 759
IS 2
AR 103
DI 10.1088/0004-637X/759/2/103
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034ZL
UT WOS:000310911300026
ER
PT J
AU Stevenson, R
Kramer, EA
Bauer, JM
Masiero, JR
Mainzer, AK
AF Stevenson, R.
Kramer, E. A.
Bauer, J. M.
Masiero, J. R.
Mainzer, A. K.
TI CHARACTERIZATION OF ACTIVE MAIN BELT OBJECT P/2012 F5 (GIBBS): A
POSSIBLE IMPACTED ASTEROID
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets: individual (P/2012 F5 (Gibbs)); minor planets, asteroids:
individual (P/2012 F5)
ID INFRARED-SURVEY-EXPLORER; NEAR-EARTH ASTEROIDS; R2 LA SAGRA; 596
SCHEILA; THERMAL-MODEL; PHYSICAL-PROPERTIES; SOLAR-SYSTEM; 1999 KW4;
COMET; 133P/ELST-PIZARRO
AB In this work, we characterize the recently discovered active main belt object P/2012 F5 (Gibbs), which was discovered with a dust trail > 7' in length in the outer main belt, 7 months prior to aphelion. We use optical imaging obtained on UT 2012 March 27 to analyze the central condensation and the long trail. We find B-band and R-band apparent magnitudes of 20.96 +/- 0.04 mag and 19.93 +/- 0.02 mag, respectively, which give an upper limit on the radius of the nucleus of 2.1 km. The geometric scattering cross-section of material in the trail was similar to 4 x 10(8) m(2), corresponding to a mass of similar to 5 x 10(7) kg. Analysis of infrared images taken by the Wide-field Infrared Survey Explorer in 2010 September reveals that the object was below the detection limit, suggesting that it was less active than it was during 2012, or possibly inactive, just six months after it passed through perihelion. We set a 1 sigma upper limit on its radius during this time of 2.9 km. P/2012 F5 (Gibbs) is dynamically stable in the outer main belt on timescales of similar to 1 Gyr, pointing toward an asteroidal origin. We find that the morphology of the ejected dust is consistent with it being produced by a single event that occurred on UT 2011 July 7 +/- 20 days, possibly as the result of a collision with a small impactor.
C1 [Stevenson, R.; Kramer, E. A.; Bauer, J. M.; Masiero, J. R.; Mainzer, A. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kramer, E. A.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA.
RP Stevenson, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Rachel.A.Stevenson@jpl.nasa.gov
OI Masiero, Joseph/0000-0003-2638-720X
FU National Aeronautics and Space Administration; NASA Postdoctoral
Fellowship Program; JPL Graduate Fellowship Program; NASA through the
Near Earth Object observing programs; JPL Office of the Chief
Information Officer
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 work was based on observations obtained at the Hale
Telescope, Palomar Observatory as part of a continuing collaboration
between the California Institute of Technology, NASA/JPL, and Cornell
University. The authors thank Henry Hsieh for bringing the discovery of
P/2012 F5 to their attention. They also thank Kevin Rykoski, Carolyn
Heffner, and Jean Mueller for assistance with the observations at
Palomar Observatory. R.S. and J.M. acknowledge support from the NASA
Postdoctoral Fellowship Program. E.K. was supported by the JPL Graduate
Fellowship Program. This research was funded in part by a grant from
NASA through the Near Earth Object observing programs, for the NEOWISE
project. The supercomputer used in this investigation was provided by
funding from the JPL Office of the Chief Information Officer.
NR 53
TC 19
Z9 19
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 NOV 10
PY 2012
VL 759
IS 2
AR 142
DI 10.1088/0004-637X/759/2/142
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034ZL
UT WOS:000310911300065
ER
PT J
AU Tian, H
McIntosh, SW
Wang, TJ
Ofman, L
De Pontieu, B
Innes, DE
Peter, H
AF Tian, Hui
McIntosh, Scott W.
Wang, Tongjiang
Ofman, Leon
De Pontieu, Bart
Innes, Davina E.
Peter, Hardi
TI PERSISTENT DOPPLER SHIFT OSCILLATIONS OBSERVED WITH HINODE/EIS IN THE
SOLAR CORONA: SPECTROSCOPIC SIGNATURES OF ALFVENIC WAVES AND RECURRING
UPFLOWS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE line: profiles; solar wind; Sun: corona; Sun: oscillations; waves
ID SLOW MAGNETOACOUSTIC WAVES; ACTIVE-REGION LOOPS; EUV IMAGING
SPECTROMETER; TRANSITION-REGION; TRANSVERSE OSCILLATIONS; PROPAGATING
WAVES; MAGNETIC-FIELD; KINK WAVES; INTENSITY OSCILLATIONS;
EMISSION-LINES
AB Using data obtained by the EUV Imaging Spectrometer on board Hinode, we have performed a survey of obvious and persistent (without significant damping) Doppler shift oscillations in the corona. We have found mainly two types of oscillations from February to April in 2007. One type is found at loop footpoint regions, with a dominant period around 10 minutes. They are characterized by coherent behavior of all line parameters (line intensity, Doppler shift, line width, and profile asymmetry), and apparent blueshift and blueward asymmetry throughout almost the entire duration. Such oscillations are likely to be signatures of quasi-periodic upflows (small-scale jets, or coronal counterpart of type-II spicules), which may play an important role in the supply of mass and energy to the hot corona. The other type of oscillation is usually associated with the upper part of loops. They are most clearly seen in the Doppler shift of coronal lines with formation temperatures between one and two million degrees. The global wavelets of these oscillations usually peak sharply around a period in the range of three to six minutes. No obvious profile asymmetry is found and the variation of the line width is typically very small. The intensity variation is often less than 2%. These oscillations are more likely to be signatures of kink/Alfven waves rather than flows. In a few cases, there seems to be a pi/2 phase shift between the intensity and Doppler shift oscillations, which may suggest the presence of slow-mode standing waves according to wave theories. However, we demonstrate that such a phase shift could also be produced by loops moving into and out of a spatial pixel as a result of Alfvenic oscillations. In this scenario, the intensity oscillations associated with Alfvenic waves are caused by loop displacement rather than density change. These coronal waves may be used to investigate properties of the coronal plasma and magnetic field.
C1 [Tian, Hui; McIntosh, Scott W.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Wang, Tongjiang; Ofman, Leon] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Wang, Tongjiang; Ofman, Leon] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[De Pontieu, Bart] Lockheed Martin Solar & Astrophys Lab, Org ADBS, Palo Alto, CA 94304 USA.
[Innes, Davina E.; Peter, Hardi] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
RP Tian, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM htian@ucar.edu
FU NASA [NNX08AL22G, NNX08BA99G, NNX10AN10G, NNX12AB34G]; NSF [ATM-0541567,
ATM-0925177]; ASP Postdoctoral Fellowship Program of National Center for
Atmospheric Research; National Science Foundation
FX EIS is an instrument on board Hinode, a Japanese mission developed and
launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC
(UK) as international partners. It is operated by these agencies in
cooperation with ESA and NSC (Norway). S. W. McIntosh is supported by
NASA (NNX08AL22G and NNX08BA99G) and NSF (ATM-0541567, ATM-0925177). T.
Wang and L. Ofman acknowledge supports by NASA grants NNX10AN10G and
NNX12AB34G. H. Tian is supported by the ASP Postdoctoral Fellowship
Program of National Center for Atmospheric Research, which is sponsored
by the National Science Foundation. H. Tian thanks I. De Moortel, G. R.
Gupta, and L. Teriaca for helpful discussions.
NR 188
TC 36
Z9 36
U1 12
U2 29
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 NOV 10
PY 2012
VL 759
IS 2
AR 144
DI 10.1088/0004-637X/759/2/144
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034ZL
UT WOS:000310911300067
ER
PT J
AU Warren, HP
Winebarger, AR
Brooks, DH
AF Warren, Harry P.
Winebarger, Amy R.
Brooks, David H.
TI A SYSTEMATIC SURVEY OF HIGH-TEMPERATURE EMISSION IN SOLAR ACTIVE REGIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona
ID ULTRAVIOLET IMAGING SPECTROMETER; TRANSITION-REGION; ATOMIC DATA; X-RAY;
FUNDAMENTAL LIMITATIONS; PLASMA TEMPERATURE; HINODE EIS; HOT PLASMA;
FE-XVIII; CORONA
AB The recent analysis of observations taken with the EUV Imaging Spectrometer and X-Ray Telescope instruments on Hinode suggests that well-constrained measurements of the temperature distribution in solar active regions can finally be made. Such measurements are critical for constraining theories of coronal heating. Past analysis, however, has suffered from limited sample sizes and large uncertainties at temperatures between 5 and 10 MK. Here we present a systematic study of the differential emission measure distribution in 15 active region cores. We focus on measurements in the "inter-moss" region, that is, the region between the loop footpoints, where the observations are easier to interpret. To reduce the uncertainties at the highest temperatures we present a new method for isolating the Fe XVIII emission in the AIA/SDO 94 angstrom channel. The resulting differential emission measure distributions confirm our previous analysis showing that the temperature distribution in an active region core is often strongly peaked near 4 MK. We characterize the properties of the emission distribution as a function of the total unsigned magnetic flux. We find that the amount of high-temperature emission in the active region core is correlated with the total unsigned magnetic flux, while the emission at lower temperatures, in contrast, is inversely related. These results provide compelling evidence that high-temperature active region emission is often close to equilibrium, although weaker active regions may be dominated by evolving million degree loops in the core.
C1 [Warren, Harry P.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Winebarger, Amy R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Brooks, David H.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
RP Warren, HP (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
FU NASA
FX This research was supported by NASA. Hinode is a Japanese mission
developed and launched by ISAS/JAXA, with NAOJ as domestic partner and
NASA and STFC (UK) as international partners. It is operated by these
agencies in co-operation with ESA and NSC (Norway). H.P.W. benefited
greatly from discussions at an International Space Science Institute
meeting on coronal heating led by Steve Bradshaw and Helen Mason.
NR 51
TC 65
Z9 65
U1 1
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 10
PY 2012
VL 759
IS 2
AR 141
DI 10.1088/0004-637X/759/2/141
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034ZL
UT WOS:000310911300064
ER
PT J
AU Werner, MW
Murphy, DW
Livingston, JH
Gorjian, V
Jones, DL
Meier, DL
Lawrence, CR
AF Werner, Michael W.
Murphy, David W.
Livingston, John H.
Gorjian, Varoujan
Jones, Dayton L.
Meier, David L.
Lawrence, Charles R.
TI SPITZER OBSERVATIONS OF HOTSPOTS IN RADIO LOBES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; radiation mechanisms: non-thermal
ID X-RAY-EMISSION; HOT-SPOTS; CYGNUS-A; CHANDRA OBSERVATIONS;
SPACE-TELESCOPE; COSMIC-RAYS; GALAXIES; RESOLUTION; JETS; ACCELERATION
AB We have carried out a systematic search with Spitzer Warm Mission and archival data for infrared emission from the hotspots in radio lobes that have been described by Hardcastle et al. These hotspots have been detected with both radio and X-ray observations, but an observation at an intermediate frequency in the infrared can be critical to distinguish between competing models for particle acceleration and radiation processes in these objects. Between the archival and warm mission data, we report detections of 18 hotspots; the archival data generally include detections at all four IRAC bands, the Warm Mission data only at 3.6 mu m. Using a theoretical formalism adopted from Godfrey et al., we fit both archival and warm mission spectral energy distributions (SEDs)-including radio, X-ray, and optical data from Hardcastle as well as the Spitzer data-with a synchrotron self-Compton (SSC) model, in which the X-rays are produced by Compton scattering of the radio frequency photons by the energetic electrons which radiate them. With one exception, an SSC model requires that the magnetic field be less or much less than the equipartition value which minimizes total energy and has comparable amounts of energy in the magnetic field and in the energetic particles. This conclusion agrees with those of comparable recent studies of hotspots, and with the analysis presented by Hardcastle et al. We also show that the infrared data rule out the simplest synchrotron-only models for the SEDs. We briefly discuss the implications of these results and of alternate interpretations of the data.
C1 [Werner, Michael W.; Murphy, David W.; Livingston, John H.; Gorjian, Varoujan; Jones, Dayton L.; Meier, David L.; Lawrence, Charles R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Werner, MW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU Jet Propulsion Laboratory, California Institute of Technology under a
contract with NASA; NASA
FX We thank the referee and Martin Hardcastle for their thoughtful
commentswhich improved the paper significantly. This work is based on
observations made with the Spitzer Space Telescope, which is operated by
the Jet Propulsion Laboratory, California Institute of Technology under
a contract with NASA. Support for this work was provided by NASA through
an award issued by JPL/Caltech.
NR 23
TC 6
Z9 6
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 NOV 10
PY 2012
VL 759
IS 2
AR 86
DI 10.1088/0004-637X/759/2/86
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034ZL
UT WOS:000310911300009
ER
PT J
AU Gebregiorgis, AS
Tian, YD
Peters-Lidard, CD
Hossain, F
AF Gebregiorgis, Abebe S.
Tian, Yudong
Peters-Lidard, Christa D.
Hossain, Faisal
TI Tracing hydrologic model simulation error as a function of satellite
rainfall estimation bias components and land use and land cover
conditions
SO WATER RESOURCES RESEARCH
LA English
DT Article
ID PRECIPITATION ANALYSIS TMPA; GLOBAL PRECIPITATION; PASSIVE MICROWAVE;
UNITED-STATES; PRODUCTS; SYSTEM; RESOLUTION; SCALES; DATASET; FLUXES
AB The key question that is asked in this study is "how are the three independent bias components of satellite rainfall estimation, comprising hit bias, missed, and false precipitation, physically related to the estimation uncertainty of soil moisture and runoff for a physically based hydrologic model?" The study also investigated the performance of different satellite rainfall products as a function of land use and land cover (LULC) type. Using the entire Mississippi river basin as the study region and the variable infiltration capacity (VIC)-3L as the distributed hydrologic model, the study of the satellite products (CMORPH, 3B42RT, and PERSIANN-CCS) yielded two key findings. First, during the winter season, more than 40% of the rainfall total bias is dominated by missed precipitation in forest and woodland regions (southeast of Mississippi). During the summer season, 51% of the total bias is governed by the hit bias, and about 42% by the false precipitation in grassland-savanna region (western part of Mississippi basin). Second, a strong dependence is observed between hit bias and runoff error, and missed precipitation and soil moisture error. High correlation with runoff error is observed with hit bias (similar to 0.85), indicating the need for improving the satellite rainfall product's ability to detect rainfall more consistently for flood prediction. For soil moisture error, it is the total bias that correlated significantly (similar to 0.78), indicating that a satellite product needed to be minimized of total bias for long-term monitoring of watershed conditions for drought through continuous simulation.
C1 [Gebregiorgis, Abebe S.; Hossain, Faisal] Tennessee Technol Univ, Dept Civil & Environm Engn, Cookeville, TN 38505 USA.
[Tian, Yudong; Peters-Lidard, Christa D.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
[Tian, Yudong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Hossain, F (reprint author), Tennessee Technol Univ, Dept Civil & Environm Engn, 1020 Stadium Dr,Box 5015, Cookeville, TN 38505 USA.
EM fhossain@tntech.edu
RI Gebregiorgis, Abebe/C-7947-2016; Peters-Lidard, Christa/E-1429-2012;
Measurement, Global/C-4698-2015
OI Gebregiorgis, Abebe/0000-0002-2975-9104; Peters-Lidard,
Christa/0000-0003-1255-2876;
FU NASA New Investigator Program (NIP) [NNX08AR32G]; Center for Management,
Utilization and Protection of Water Resources at TN Technological
University
FX The study and the first author (Gebregiorgis) were supported by NASA New
Investigator Program (NIP) grant NNX08AR32G of Faisal Hossain and the
Center for Management, Utilization and Protection of Water Resources at
TN Technological University. A major component of the research was also
generously supported by the Goddard Earth Sciences and Technology (GEST)
Center of University of MD Baltimore County through its Graduate Student
Summer Program (GSSP) during summer 2011 awarded to the first author
under the able supervision of Dr. Christa Peters-Lidard and Dr. Yudong
Tian. The authors are also grateful for the guidance received from the
associate editor and the three anonymous reviewers that helped to
improve the quality of the study and manuscript considerably.
NR 38
TC 17
Z9 17
U1 0
U2 21
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
J9 WATER RESOUR RES
JI Water Resour. Res.
PD NOV 10
PY 2012
VL 48
AR W11509
DI 10.1029/2011WR011643
PG 17
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 035QI
UT WOS:000310962200001
ER
PT J
AU Dragomir, D
Matthews, JM
Howard, AW
Antoci, V
Henry, GW
Guenther, DB
Johnson, JA
Kuschnig, R
Marcy, GW
Moffat, AFJ
Rowe, JF
Rucinski, SM
Sasselov, D
Weiss, WW
AF Dragomir, Diana
Matthews, Jaymie M.
Howard, Andrew W.
Antoci, Victoria
Henry, Gregory W.
Guenther, David B.
Johnson, John A.
Kuschnig, Rainer
Marcy, Geoffrey W.
Moffat, Anthony F. J.
Rowe, Jason F.
Rucinski, Slavek M.
Sasselov, Dimitar
Weiss, Werner W.
TI NON-DETECTION OF PREVIOUSLY REPORTED TRANSITS OF HD 97658b WITH MOST
PHOTOMETRY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planetary systems; stars: individual (HD 97658); techniques: photometric
ID EXTRASOLAR PLANETS; SPACED DATA; ORBITS
AB The radial velocity-discovered exoplanet HD 97658b was recently announced to transit, with a derived planetary radius of 2.93 +/- 0.28 R-circle plus. As a transiting super-Earth orbiting a bright star, this planet would make an attractive candidate for additional observations, including studies of its atmospheric properties. We present and analyze follow-up photometric observations of the HD 97658 system acquired with the Microvariability and Oscillations of STars space telescope. Our results show no transit with the depth and ephemeris reported in the announcement paper. For the same ephemeris, we rule out transits for a planet with radius larger than 2.09 R-circle plus, corresponding to the reported 3 sigma lower limit. We also report new radial velocity measurements which continue to support the existence of an exoplanet with a period of 9.5 days, and obtain improved orbital parameters.
C1 [Dragomir, Diana; Matthews, Jaymie M.; Antoci, Victoria] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Howard, Andrew W.; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Howard, Andrew W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Antoci, Victoria] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr SAC, DK-8000 Aarhus C, Denmark.
[Antoci, Victoria; Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Henry, Gregory W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA.
[Guenther, David B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Johnson, John A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Johnson, John A.] NASA, Exoplanet Sci Inst NExScI, Pasadena, CA 91125 USA.
[Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rucinski, Slavek M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Dragomir, D (reprint author), Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
EM diana@phas.ubc.ca
RI Howard, Andrew/D-4148-2015;
OI Howard, Andrew/0000-0001-8638-0320; Dragomir, Diana/0000-0003-2313-467X;
Antoci, Victoria/0000-0002-0865-3650
FU University of British Columbia Four Year Fellowship; Danish National
Research Foundation; ASTERISK project; European Research Council
[267864]; Natural Sciences and Engineering Research Council of Canada;
FQRNT (Quebec); Austrian Science Fund [P22691-N16]; Austrian Research
Promotion Agency-ALR
FX D.D. is supported by a University of British Columbia Four Year
Fellowship. Funding for the Stellar Astrophysics Centre (SAC) is
provided by The Danish National Research Foundation and research is
supported by the ASTERISK project (ASTERoseismic Investigations with
SONG and Kepler) funded by the European Research Council (grant
agreement No. 267864). The Natural Sciences and Engineering Research
Council of Canada supports the research of D. B. G., J.M.M., A.F.J.M.,
and S. M. R. Additional support for A.F.J.M. comes from FQRNT (Quebec).
R. K. and W. W. W. were supported by the Austrian Science Fund
(P22691-N16) and by the Austrian Research Promotion Agency-ALR.
NR 19
TC 3
Z9 3
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 NOV 10
PY 2012
VL 759
IS 2
AR L41
DI 10.1088/2041-8205/759/2/L41
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030PC
UT WOS:000310581600015
ER
PT J
AU Redford, JA
Castro, IP
Coleman, GN
AF Redford, John A.
Castro, Ian P.
Coleman, Gary N.
TI On the universality of turbulent axisymmetric wakes
SO JOURNAL OF FLUID MECHANICS
LA English
DT Article
DE shear layer turbulence; turbulence simulation; wakes
ID DIRECT NUMERICAL-SIMULATION; EVOLVING PLANE WAKES; INITIAL CONDITIONS;
REYNOLDS-NUMBER; EQUILIBRIUM; SIMILARITY; FLOW; EVOLUTION; MEMORY
AB Direct numerical simulations (DNS) of two time-dependent, axially homogeneous, axisymmetric turbulent wakes having very different initial conditions are presented in order to assess whether they reach a universal self-similar state as classically hypothesized by Townsend. It is shown that an extensive early-time period exists during which the two wakes are individually self-similar with wake widths growing like delta proportional to t(1/3), as predicted by classical dimensional analysis, but have very different growth rates and are thus not universal. Subsequently, however, the turbulence adjusts to yield, eventually, wakes that are structurally identical and have the same growth rate (also with delta proportional to t(1/3)) so provide clear evidence of a universal, self-similar state. The former non-universal but self-similar state extends, in terms of a spatially equivalent flow behind a spherical body of diameter d, to a distance of O(3000d) whereas the final universal state does not appear before O(5000d) (and exists despite relatively low values of the Reynolds number and no evidence of a spectral kappa (5/3) inertial subrange). Universal wake evolution is therefore likely to be rare in practice. Despite its low Reynolds number, the flow does not exhibit the sometime-suggested alternative self-similar behaviour with delta proportional to t(1/2) (as for the genuinely laminar case) at large times (or, equivalently, distances), since the eddy viscosity remains large compared to the molecular viscosity and its temporal variations are not negligible.
C1 [Redford, John A.; Castro, Ian P.; Coleman, Gary N.] Univ Southampton, Aerodynam & Flight Mech Res Grp, Southampton SO17 1BJ, Hants, England.
RP Coleman, GN (reprint author), NASA Langley Res Ctr, Computat Aerosci Branch, Hampton, VA 23681 USA.
EM Gary.N.Coleman@nasa.gov
FU UK Ministry of Defence [RD027-02854]; UK Turbulence Consortium; EPSRC
[EP/D044073/1, EP/G069581/1]; Office of Science and Technology through
EPSRC
FX This work was supported by the UK Ministry of Defence (Dstl project
RD027-02854, managed by Dr R. P. Hornby), and the UK Turbulence
Consortium, funded by the EPSRC under Grants EP/D044073/1 and
EP/G069581/1. It made use of the facilities of HPCx and HECToR, the UK's
national high-performance computing service, which is provided by UoE
HPCx Ltd at the University of Edinburgh, Cray Inc and NAG Ltd, and
funded by the Office of Science and Technology through EPSRC's High End
Computing Programme. We are indebted to Drs P. J. Archer, T. S. Lund, E.
Rind, K. Shariff and T. G. Thomas, and Professors S. Chernyshenko, B.
Ganapathisumbramani, R. D. Sandberg and N. D. Sandham for their advice
and encouragement along the way. Professors P. Bradshaw and R. Narasimha
made useful comments on the manuscript. Thanks are due Dr C. P. Yorke
for the substantial role he played in developing the vortex-ring
initialization strategy, and to Dr Lund for proposing the procedure used
to expand the lateral domain. The explanation in 3 regarding the
relationship between the radius of the vortex rings and the half-width
of the initial mean profile was provided by Dr Shariff. We have also
benefited from timely discussions with Professor W. K. George, Professor
J. C. R. Hunt, Dr M. M. Rogers and especially Dr P. R. Spalart.
NR 29
TC 15
Z9 15
U1 0
U2 8
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0022-1120
J9 J FLUID MECH
JI J. Fluid Mech.
PD NOV 10
PY 2012
VL 710
BP 419
EP 452
DI 10.1017/jfm.2012.371
PG 34
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA 029AJ
UT WOS:000310466900017
ER
PT J
AU Hanna, KLD
Thomas, IR
Bowles, NE
Greenhagen, BT
Pieters, CM
Mustard, JF
Jackson, CRM
Wyatt, MB
AF Hanna, K. L. Donaldson
Thomas, I. R.
Bowles, N. E.
Greenhagen, B. T.
Pieters, C. M.
Mustard, J. F.
Jackson, C. R. M.
Wyatt, M. B.
TI Laboratory emissivity measurements of the plagioclase solid solution
series under varying environmental conditions
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID SPECTROSCOPY; ANORTHOSITE; FELDSPARS; MINERALS; SPECTRA; MOON; MARS
AB New laboratory thermal infrared emissivity measurements of the plagioclase solid solution series over the 1700 similar to 400 cm(-1) (6-25 mu m) spectral range are presented. Thermal infrared (TIR) spectral changes for fine-particulate samples (0-25 mu m) are characterized for the first time under different laboratory environmental conditions: ambient (terrestrial-like), half-vacuum (Mars-like), vacuum, and vacuum with cooled chamber (lunar-like). Under all environmental conditions the Christiansen Feature (CF) is observed to vary in a systematic way with Na-rich end-member (albite) having a CF position at the highest wave number (shortest wavelength) and the Ca-rich end-member (anorthite) having a CF position with the lowest wave number (longest wavelength). As pressure decreases to <10(-3) mbar four observations are made: (1) the CF position shifts to higher wave numbers, (2) the spectral contrast of the CF increases relative to the RB, (3) the spectral contrast of the RB in the similar to 1200-900 spectral range decreases while the spectral contrast of the RB in the similar to 800-400 spectral range either increases or remains the same and (4) the TF disappears. A relationship between the wavelength position of the CF measured under simulated lunar conditions and plagioclase composition (An#) is developed. Although its exact form may evolve with additional data, this linear relationship should be applied to current and future TIR data sets of the Moon. Our new spectral measurements demonstrate how sensitive thermal infrared emissivity spectra of plagioclase feldspars are to the environmental conditions under which they are measured and provide important constraints for interpreting current and future thermal infrared data sets.
C1 [Hanna, K. L. Donaldson; Pieters, C. M.; Mustard, J. F.; Jackson, C. R. M.; Wyatt, M. B.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Thomas, I. R.; Bowles, N. E.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England.
[Greenhagen, B. T.] CALTECH, Jet Prop Lab, Geophys & Planetary Geosci Grp, Pasadena, CA USA.
RP Hanna, KLD (reprint author), Brown Univ, Dept Geol Sci, Box 1846, Providence, RI 02912 USA.
EM ri_donaldson_hanna@brown.edu
RI Greenhagen, Benjamin/C-3760-2016
FU NASA [NNX08AM75G]; NLSI [NNA09DB34A]
FX We would like to extend our appreciation to Phil Christensen and Arizona
State University for donating samples used in this study. A special
thanks to Nilanjan Chatterjee at the MIT Electron Microprobe Facility
for sample analyses. The authors would also like to thank Steve Ruff and
the other anonymous reviewers for the thorough comments and suggestions
that greatly improved this manuscript. K. L. Donaldson Hanna was
supported by NASA grant ID NNX08AM75G. This research was supported in
part by NLSI grant ID NNA09DB34A.
NR 28
TC 10
Z9 10
U1 0
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD NOV 8
PY 2012
VL 117
AR E11004
DI 10.1029/2012JE004184
PG 7
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 035PP
UT WOS:000310960100001
ER
PT J
AU Lindsay, R
Haas, C
Hendricks, S
Hunkeler, P
Kurtz, N
Paden, J
Panzer, B
Sonntag, J
Yungel, J
Zhang, J
AF Lindsay, R.
Haas, C.
Hendricks, S.
Hunkeler, P.
Kurtz, N.
Paden, J.
Panzer, B.
Sonntag, J.
Yungel, J.
Zhang, J.
TI Seasonal forecasts of Arctic sea ice initialized with observations of
ice thickness
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MODEL
AB Seasonal forecasts of the September 2012 Arctic sea ice thickness and extent are conducted starting from 1 June 2012. An ensemble of forecasts is made with a coupled ice-ocean model. For the first time, observations of the ice thickness are used to correct the initial ice thickness distribution to improve the initial conditions. Data from two airborne campaigns are used: NASA Operation IceBridge and SIZONet. The model was advanced through April and May using reanalysis data from 2012 and for June-September it was forced with reanalysis data from the previous seven summers. The ice extent in the corrected runs averaged lower in the Pacific sector and higher in the Atlantic sector compared to control runs with no corrections. The predicted total ice extent is 4.4 +/- 0.5 M km(2), 0.2 M km(2) less than that made with the control runs but 0.8 M km(2) higher than the observed September extent. Citation: Lindsay, R., C. Haas, S. Hendricks, P. Hunkeler, N. Kurtz, J. Paden, B. Panzer, J. Sonntag, J. Yungel, and J. Zhang (2012), Seasonal forecasts of Arctic sea ice initialized with observations of ice thickness, Geophys. Res. Lett., 39, L21502, doi:10.1029/2012GL053576.
C1 [Lindsay, R.; Zhang, J.] Univ Washington, Polar Sci Ctr, Appl Phys Lab, Seattle, WA 98105 USA.
[Haas, C.] York Univ, Dept Earth & Space Sci & Engn, Toronto, ON M3J 2R7, Canada.
[Hendricks, S.; Hunkeler, P.] Alfred Wegener Inst Polar & Marine Res, Bremerhaven, Germany.
[Kurtz, N.] NASA, Cryospher Sci Program, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Paden, J.; Panzer, B.] Univ Kansas, Ctr Remote Sensing Ice Sheets, Lawrence, KS 66045 USA.
[Sonntag, J.; Yungel, J.] NASA, Wallops Flight Facil, Goddard Space Flight Ctr, Wallops Isl, VA USA.
RP Lindsay, R (reprint author), Univ Washington, Polar Sci Ctr, Appl Phys Lab, 1013 NE 40th St, Seattle, WA 98105 USA.
EM lindsay@apl.washington.edu
RI Hendricks, Stefan/D-5168-2011; Haas, Christian/L-5279-2016; Lindsay,
Ron/S-9083-2016
OI Hendricks, Stefan/0000-0002-1412-3146; Haas,
Christian/0000-0002-7674-3500;
FU National Science Foundation Office of Polar Programs; National
Aeronautics and Space Administration Cryosphere Program and Operation
IceBridge; Office of Naval Research; Center for Remote Sensing of Ice
Sheets
FX This study was conducted with support from the National Science
Foundation Office of Polar Programs, the National Aeronautics and Space
Administration Cryosphere Program and Operation IceBridge, the Office of
Naval Research, and the Center for Remote Sensing of Ice Sheets.
NR 17
TC 21
Z9 21
U1 0
U2 28
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 NOV 8
PY 2012
VL 39
AR L21502
DI 10.1029/2012GL053576
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 035QQ
UT WOS:000310963000002
ER
PT J
AU Jin, D
Murtugudde, R
Waliser, DE
AF Jin, Daeho
Murtugudde, Raghu
Waliser, Duane E.
TI Tropical Indo-Pacific Ocean chlorophyll response to MJO forcing
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID ATMOSPHERIC INTRASEASONAL VARIABILITY; MADDEN-JULIAN OSCILLATION;
GENERAL-CIRCULATION MODEL; MIXED-LAYER MODEL; ARABIAN SEA; PENETRATIVE
RADIATION; SOLAR-RADIATION; INDIAN-OCEAN; CLIMATE; PHYTOPLANKTON
AB Previous studies that analyzed ocean color satellite data have suggested that the primary mechanism of surface chlorophyll (Chl) response to the MJO is wind-induced turbulent mixing and the corresponding mixed layer entrainment. In this study, this notion is examined with an ocean biophysical model in an ensemble framework, focusing on upper ocean processes (z < 200 m). As a whole, the model's mean Chl state is lower than observations except in the tropical Pacific basin, but its seasonal variation is acceptable, particularly in the tropical Indian Ocean. In this basin, the model can simulate surface Chl responses to the MJO consistent with the observations in terms of the phase-by-phase anomaly evolution patterns. These Chl responses are mostly induced by surface wind forcing, which is consistent with previous studies. Further investigation of subsurface variations is performed at select grid points, and it is revealed that (1) entrained nutrients are the primary source of enhancement for surface Chl concentration and detrainment blooms are relatively less common; (2) in limited regions, Ekman pumping can effectively reduce Chl concentration; and (3) both entrainment/detrainment and Ekman pumping mechanisms rely on background states of nutrient availability, so the same forcing can result in completely different Chl responses depending on the background state.
C1 [Jin, Daeho; Murtugudde, Raghu] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Jin, D (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, 5825 Univ Res Ct,Ste 4001, College Pk, MD 20740 USA.
EM daehojin@umd.edu
FU NASA PO grant [NNX09AF43G]; Divecha Center for Climate Change;
IITM-Pune; National Aeronautics and Space Administration
FX D.J., R. M., and D. W. acknowledge support from NASA PO grant
NNX09AF43G. R. M. acknowledges the support by the Divecha Center for
Climate Change and IITM-Pune for their support and hospitality. R. M.
also acknowledges the ONR DYNAMO grant. D.W.'s contribution to this
study was carried out on behalf of the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. Associated with the observations
data, CMAP Precipitation data provided by the NOAA/OAR/ESRL PSD,
Boulder, Colorado, USA, from their Web site at
http://www.esrl.noaa.gov/psd/.ECMWF ERA-Interim data used in this study
have been obtained from the ECMWF data server. The CFSR data was
developed by NOAA's NCEP. The data for this study are from NOAA's
National Operational Model Archive and Distribution System (NOMADS),
which is maintained at NOAA's National Climate Data Center (NCDC).
NR 58
TC 5
Z9 5
U1 0
U2 16
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 NOV 8
PY 2012
VL 117
AR C11008
DI 10.1029/2012JC008015
PG 20
WC Oceanography
SC Oceanography
GA 035RS
UT WOS:000310966300001
ER
PT J
AU Sibanda, P
Moldwin, MB
Galvan, DA
Sandel, BR
Forrester, T
AF Sibanda, Patrick
Moldwin, Mark B.
Galvan, David A.
Sandel, Bill R.
Forrester, Terry
TI Quantifying the azimuthal plasmaspheric density structure and dynamics
inferred from IMAGE EUV
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID EXTREME-ULTRAVIOLET IMAGER; 17 APRIL 2002; INNER MAGNETOSPHERE; CRRES
OBSERVATIONS; PLASMAPAUSE; CONVECTION; EVOLUTION; FEATURES; PLUMES;
STORMS
AB The extreme ultraviolet (EUV) imager on the IMAGE satellite provided the first global images of the plasmasphere leading to enhanced understanding of plasmapause structure and dynamics. However, few studies have investigated the structure and dynamics of the inner plasmasphere (regions interior to the plasmapause), which previous in situ observations have shown to often be highly structured. This study is the first to systematically analyze global images of the density structure of the inner plasmasphere by using data from the EUV imager on the IMAGE satellite. We find that the inner plasmasphere exhibits both fine and meso-scale structure characterized by rapid density fluctuations and density enhancements of varying amplitudes (factors of similar to 2-5) and spatial scales (from 10 s of minutes to 6 hours MLT) that occur regularly in the aftermath of geomagnetic storms. The level of variability within the azimuthal structure was found to increase with increasing geomagnetic activity. The observations suggest that some meso-scale azimuthal density structure observed in the inner plasmasphere is from "fossil" plasmapause features entrained inside the expanding and refilling plasmasphere.
C1 [Sibanda, Patrick; Moldwin, Mark B.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Sibanda, Patrick] Univ Zambia, Dept Phys, Lusaka, Zambia.
[Galvan, David A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Sandel, Bill R.; Forrester, Terry] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
RP Sibanda, P (reprint author), Univ Michigan, Ann Arbor, MI 48109 USA.
EM sibandapatrick.ps@gmail.com
RI Moldwin, Mark/F-8785-2011
OI Moldwin, Mark/0000-0003-0954-1770
FU NASA [NNX09AI62G, NNX10AC82G, NNH09ZDA001-LWSSTRT, NNX07AG46G]
FX This work was done while Patrick Sibanda worked as a Post-doc under the
guidance of Mark Moldwin at the University of Michigan and was supported
by NASA grants NNX09AI62G, NNX10AC82G and NNH09ZDA001-LWSSTRT. The IDL
EUV analysis tools developed by the University of Arizona are available
at http://euv.lpl.arizona.edu/euv/index. Work at the University of
Arizona was supported under NASA Grant NNX07AG46G from the Heliospheric
Guest Investigator Program.
NR 31
TC 2
Z9 2
U1 0
U2 9
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 NOV 8
PY 2012
VL 117
AR A11204
DI 10.1029/2012JA017522
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 035RX
UT WOS:000310967000001
ER
PT J
AU Simoes, F
Klenzing, J
Ivanov, S
Pfaff, R
Freudenreich, H
Bilitza, D
Rowland, D
Bromund, K
Liebrecht, MC
Martin, S
Schuck, P
Uribe, P
Yokoyama, T
AF Simoes, Fernando
Klenzing, Jeffrey
Ivanov, Stoyan
Pfaff, Robert
Freudenreich, Henry
Bilitza, Dieter
Rowland, Douglas
Bromund, Kenneth
Liebrecht, Maria Carmen
Martin, Steven
Schuck, Peter
Uribe, Paulo
Yokoyama, Tatsuhiro
TI Detection of ionospheric Alfven resonator signatures in the equatorial
ionosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID SCHUMANN RESONANCE; BACKGROUND-NOISE; PROPAGATION; MODEL; GENERATION;
EXCITATION; ATMOSPHERE; WAVES; RANGE; FIELD
AB The ionosphere response resulting from minimum solar activity during cycle 23/24 was unusual and offered unique opportunities for investigating space weather in the near-Earth environment. We report ultra low frequency electric field signatures related to the ionospheric Alfven resonator detected by the Communications/Navigation Outage Forecasting System (C/NOFS) satellite in the equatorial region. These signatures are used to constrain ionospheric empirical models and offer a new approach for monitoring ionosphere dynamics and space weather phenomena, namely aeronomy processes, Alfven wave propagation, and troposphere-ionosphere-magnetosphere coupling mechanisms.
C1 [Simoes, Fernando; Klenzing, Jeffrey; Pfaff, Robert; Freudenreich, Henry; Rowland, Douglas; Bromund, Kenneth; Liebrecht, Maria Carmen; Martin, Steven; Schuck, Peter; Uribe, Paulo; Yokoyama, Tatsuhiro] NASA, Goddard Space Flight Ctr, Space Weather Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Ivanov, Stoyan] Georgia Inst Technol, Dept Phys, Atlanta, GA 30332 USA.
[Bilitza, Dieter] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Bilitza, Dieter] George Mason Univ, Space Weather Lab, Fairfax, VA 22030 USA.
RP Simoes, F (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA.
EM fernando.a.simoes@nasa.gov
RI Klenzing, Jeff/E-2406-2011; Pfaff, Robert/F-5703-2012; Rowland,
Douglas/F-5589-2012
OI Klenzing, Jeff/0000-0001-8321-6074; Pfaff, Robert/0000-0002-4881-9715;
Rowland, Douglas/0000-0003-0948-6257
FU USAF; Air Force Office of Scientific Research; NASA
FX The Communication/Navigation Outage Forecast System (C/NOFS) mission,
conceived and developed by the U.S. Air Force Research Laboratory, is
sponsored and executed by the USAF Space Test Program. We acknowledge
support from the Air Force Office of Scientific Research. FS and JK are
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 work performed by SI at
Goddard Space Flight Center was made possible by the NASA Education
Office through the Undergraduate Student Research Program managed by the
Universities Space Research Association.
NR 42
TC 8
Z9 8
U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD NOV 8
PY 2012
VL 117
AR A11305
DI 10.1029/2012JA017709
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 035RX
UT WOS:000310967000002
ER
PT J
AU Perri, S
Goldstein, ML
Dorelli, JC
Sahraoui, F
AF Perri, S.
Goldstein, M. L.
Dorelli, J. C.
Sahraoui, F.
TI Detection of Small-Scale Structures in the Dissipation Regime of
Solar-Wind Turbulence
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID MAGNETOHYDRODYNAMIC TURBULENCE; MAGNETIC RECONNECTION; RANGE SPECTRUM;
FLUCTUATIONS; CASCADES; DYNAMICS; WAVES; AU
AB Recent observations of the solar wind have pointed out the existence of a cascade of magnetic energy from the scale of the proton Larmor radius rho(p) down to the electron Larmor radius rho(e) scale. In this Letter we study the spatial properties of magnetic field fluctuations in the solar wind and find that at small scales the magnetic field does not resemble a sea of homogeneous fluctuations, but rather a two-dimensional plane containing thin current sheets and discontinuities with spatial sizes ranging from l greater than or similar to rho(p) down to rho(e) and below. These isolated structures may be manifestations of intermittency that localize sites of turbulent dissipation. Studying the relationship between turbulent dissipation, reconnection, and intermittency is crucial for understanding the dynamics of laboratory and astrophysical plasmas.
C1 [Perri, S.] Univ Calabria, Dipartmento Fis, I-87036 Arcavacata Di Rende, CS, Italy.
[Goldstein, M. L.; Dorelli, J. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sahraoui, F.] UPMC, Lab Phys Plasmas, CNRS, Ecole Polytech,Observ St Maur, F-94107 St Maur Des Fosses, France.
RP Perri, S (reprint author), Univ Calabria, Dipartmento Fis, I-87036 Arcavacata Di Rende, CS, Italy.
RI Dorelli, John/C-9488-2012
FU Borsa Post-doc POR Calabria FSE Asse IV Capitale Umano-Obiettivo
Operativo M.2; ISSI team "Dispersive cascade and dissipation in
collisionless space plasma turbulence-observations and simulations"
[185]; Marie Curie Project FP7 [PIRSES-2010-269297-"Turboplasmas''];
Magnetospheric Multiscale Mission Interdisciplinary Science program at
the Goddard Space Flight Center; French ANR project, THESOW
FX S. P.'s research was supported by "Borsa Post-doc POR Calabria FSE
2007/2013 Asse IV Capitale Umano-Obiettivo Operativo M.2''. S. P. and F.
S. acknowledge their participation in the ISSI team 185 "Dispersive
cascade and dissipation in collisionless space plasma
turbulence-observations and simulations.'' S. P. further acknowledges
the Marie Curie Project FP7 PIRSES-2010-269297-"Turboplasmas''. M. L. G.
and J. C. D. acknowledge support from the Magnetospheric Multiscale
Mission Interdisciplinary Science program at the Goddard Space Flight
Center. F. S. acknowledges support from the French ANR project, THESOW.
NR 35
TC 46
Z9 46
U1 5
U2 16
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD NOV 8
PY 2012
VL 109
IS 19
AR 191101
DI 10.1103/PhysRevLett.109.191101
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 034EL
UT WOS:000310853100004
PM 23215371
ER
PT J
AU Jordan, PM
Saccomandi, G
AF Jordan, P. M.
Saccomandi, G.
TI Compact acoustic travelling waves in a class of fluids with nonlinear
material dispersion
SO PROCEEDINGS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING
SCIENCES
LA English
DT Article
DE nonlinear acoustics; compact travelling waves; nonlinear dispersion
ID EQUATIONS; MODEL; FLOW; SOLIDS; GREEN
AB We apply a phenomenological theory of continua put forth by Rubin, Rosenau and Gottlieb in 1995 to an important class of compressible media. Regarding the material characteristic length coefficient, a, not as constant, but instead as a quadratic function of the velocity gradient, we carry out an in-depth analysis of one-dimensional acoustic travelling waves in inviscid, non-thermally conducting fluids. Analytical and numerical methods are employed to study the resulting waveforms, a special case of which exhibits compact support. In particular, a phase plane analysis is performed; simplified approximate/asymptotic expressions are presented; and a weakly nonlinear, KdV-like model that admits compact travelling wave solutions (TWSs), but which is not of the class K(m, n), is derived and analysed. Most significantly, our formulation allows for compact, pulse-type, acoustic waveforms in both gases and liquids.
C1 [Jordan, P. M.] USN, Acoust Div, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA.
[Saccomandi, G.] Univ Perugia, Dipartimento Ingn Ind, I-06125 Perugia, Italy.
RP Jordan, PM (reprint author), USN, Acoust Div, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA.
EM pjordan@nrlssc.navy.mil
RI Saccomandi, Giuseppe/F-8690-2010
OI Saccomandi, Giuseppe/0000-0001-7987-8892
FU ONR
FX The authors thank Dr Len G. Margolin for his constructive comments and
suggestions, and Dr Josette P. Fabre for her careful proofreading of an
earlier version of this article. P.M.J. was supported by ONR funding. G.
S. acknowledges GNFM of INdAM and by PRIN 2009 'Matematica e meccanica
dei sistemi biologici e dei tessuti molli.' All figures were generated
using the software package MATHEMATICA (v. 5.2).
NR 31
TC 8
Z9 8
U1 2
U2 10
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1364-5021
J9 P ROY SOC A-MATH PHY
JI Proc. R. Soc. A-Math. Phys. Eng. Sci.
PD NOV 8
PY 2012
VL 468
IS 2147
BP 3441
EP 3457
DI 10.1098/rspa.2012.0321
PG 17
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 016XA
UT WOS:000309551900011
ER
PT J
AU Khazanov, GV
Khabibrakhmanov, IK
Glocer, A
AF Khazanov, George V.
Khabibrakhmanov, Ildar K.
Glocer, Alex
TI Kinetic description of ionospheric outflows based on the exact form of
Fokker-Planck collision operator: Electrons
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID POLAR WIND; MONTE-CARLO; TRANSPORT-EQUATIONS; SUPERTHERMAL ELECTRONS;
TEMPERATURE ANISOTROPY; VELOCITY DISTRIBUTION; MODEL; PLASMA; ION;
SIMULATION
AB We present the results of a finite difference implementation of the kinetic Fokker-Planck model with an exact form of the nonlinear collisional operator. The model is time dependent and three-dimensional; one spatial dimension and two in velocity space. The spatial dimension is aligned with the local magnetic field, and the velocity space is defined by the magnitude of the velocity and the cosine of pitch angle. An important new feature of model, the concept of integration along the particle trajectories, is discussed in detail. Integration along the trajectories combined with the operator time splitting technique results in a solution scheme which accurately accounts for both the fast convection of the particles along the magnetic field lines and relatively slow collisional process. We present several tests of the model's performance and also discuss simulation results of the evolution of the plasma distribution for realistic conditions in Earth's plasmasphere under different scenarios.
C1 [Glocer, Alex] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Khabibrakhmanov, Ildar K.] IBM Corp, Thomas J Watson Res Ctr, Yorktown Hts, NY 10598 USA.
RP Glocer, A (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Mail Code 673, Greenbelt, MD 20771 USA.
EM alex.glocer-1@nasa.gov
RI Glocer, Alex/C-9512-2012; feggans, john/F-5370-2012
OI Glocer, Alex/0000-0001-9843-9094;
FU NASA [UPN 370 16 10]; NASA HQ POLAR Project; NASA LWS Program
FX Funding in support of this study was provided by NASA grant UPN 370 16
10, NASA HQ POLAR Project, and the NASA LWS Program. We are grateful to
the reviewers for their helpful comments.
NR 59
TC 2
Z9 2
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD NOV 7
PY 2012
VL 117
AR A11203
DI 10.1029/2012JA018082
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 035RW
UT WOS:000310966800002
ER
PT J
AU Velez, JCR
Blanco-Cano, X
Aguilar-Rodriguez, E
Russell, CT
Kajdic, P
Jian, LK
Luhmann, JG
AF Ramirez Velez, J. C.
Blanco-Cano, X.
Aguilar-Rodriguez, E.
Russell, C. T.
Kajdic, P.
Jian, L. K.
Luhmann, J. G.
TI Whistler waves associated with weak interplanetary shocks
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID QUASI-PARALLEL SHOCKS; EARTHS BOW SHOCK; MACH NUMBER; ISEE-2
OBSERVATIONS; OBSERVED UPSTREAM; SOLAR-WIND; PLASMA; IONS; INSTABILITY;
BETA
AB We analyze the properties of 98 weak interplanetary shocks measured by the dual STEREO spacecraft over approximately 3 years during the past solar minimum. We study the occurrence of whistler waves associated with these shocks, which on average are high beta shocks (0.2 < beta < 10). We have compared the waves properties upstream and downstream of the shocks. In the upstream region the waves are mainly circularly polarized, and in most of the cases (similar to 75%) they propagate almost parallel to the ambient magnetic field (<30 degrees). In contrast, the propagation angle with respect to the shock normal varies in a broad range of values (20 degrees to 90 degrees), suggesting that they are not phase standing. We find that the whistler waves can extend up to 100,000 km in the upstream region but in most cases (88%) are contained in a distance within 30,000 km from the shock. This corresponds to a larger region with upstream whistlers associated with IP shocks than previously reported in the literature. The maximum amplitudes of the waves are observed next to the shock interface, and they decrease as the distance to the shock increases. In most cases the wave propagation direction becomes more aligned with the magnetic field as the distance to the shock increases. These two facts suggest that most of the waves in the upstream region are Landau damping as they move away from the shock. From the analysis we also conclude that it is likely that the generation mechanism of the upstream whistler waves is taking place at the shock interface. In the downstream region, the waves are irregularly polarized, and the fluctuations are very compressive; that is, the compressive component of the wave clearly dominates over the transverse one. The majority of waves in the downstream region (95%) propagate at oblique angles with respect to the ambient magnetic field (>60 degrees). The wave propagation with respect to the shock-normal direction has no preferred direction and varies similarly to the upstream case. It is possible that downstream fluctuations are generated by ion relaxation as suggested in previous hybrid simulation shocks.
C1 [Ramirez Velez, J. C.] Univ Nacl Autonoma Mexico, Inst Astron, Unidad Ensenada, Ensenada, Baja California, Mexico.
[Blanco-Cano, X.; Kajdic, P.] Univ Nacl Autonoma Mexico, Inst Geofis, Mexico City 04510, DF, Mexico.
[Aguilar-Rodriguez, E.] Univ Nacl Autonoma Mexico, Inst Geofis, Unidad Michoacan, Morelia, Michoacan, Mexico.
[Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Jian, L. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Jian, L. K.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Velez, JCR (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Unidad Ensenada, Ensenada, Baja California, Mexico.
EM julio@astrosen.unam.mx
RI Russell, Christopher/E-7745-2012; Jian, Lan/B-4053-2010; Ramirez-Velez,
Robinson/D-5311-2016
OI Russell, Christopher/0000-0003-1639-8298; Jian, Lan/0000-0002-6849-5527;
Ramirez-Velez, Robinson/0000-0003-3075-6960
FU PAPIIT [IN109112]; CONACyT [101625, 81154]; NASA STEREO program
[NAS5-03131]; DGAPA [110511-3]; PAPIT [IN-110511-3]
FX J. C. Ramirez Velez and E. Aguilar-Rodriguez thank PAPIIT project grant
IN109112 and CONACyT project grant 101625. L. K. Jian is supported by
the NASA STEREO program through grant NAS5-03131 administered by UC
Berkeley. X. Blanco-Cano thanks CONACyT project grant 81154 and DGAPA
grant 110511-3. P. Kajdic thanks CONACyT project grants 101625 and 81154
and PAPIT grant IN-110511-3.
NR 31
TC 4
Z9 4
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-SPACE
JI J. Geophys. Res-Space Phys.
PD NOV 6
PY 2012
VL 117
AR A11103
DI 10.1029/2012JA017573
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 035RV
UT WOS:000310966600001
ER
PT J
AU Eckermann, SD
Wu, DL
AF Eckermann, S. D.
Wu, D. L.
TI Satellite detection of orographic gravity-wave activity in the winter
subtropical stratosphere over Australia and Africa
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MOUNTAIN WAVES; RADIANCES; VARIANCES; LIMB
AB Orographic gravity-wave (OGW) parameterizations in models produce waves over subtropical mountain ranges in Australia and Africa that propagate into the stratosphere during austral winter and deposit momentum, affecting weather and climate. Satellite sensors have measured stratospheric GWs for over a decade, yet find no evidence of these waves. So are parameterizations failing here? Here we argue that the short wavelengths of subtropical OGWs place them near or below the detection limits of satellite sensors. To test this hypothesis, we reanalyze nine years of stratospheric radiances from the Atmospheric Infrared Sounder (AIRS) on NASA's Aqua satellite during austral winter, applying new averaging techniques to maximize signal-to-noise and improve thresholds for OGW detection. Deep climatological enhancements in stratospheric OGW variance over specific mountain ranges in Australia and southern Africa are revealed for the first time, which exhibit temporal and vertical variations consistent with predicted OGW responses to varying background winds. Citation: Eckermann, S. D., and D. L. Wu (2012), Satellite detection of orographic gravity-wave activity in the winter subtropical stratosphere over Australia and Africa, Geophys. Res. Lett., 39, L21807, doi:10.1029/2012GL053791.
C1 [Eckermann, S. D.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
[Wu, D. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Eckermann, SD (reprint author), USN, Div Space Sci, Res Lab, Code 7631,4555 Overlook Ave SW, Washington, DC 20375 USA.
EM stephen.eckermann@nrl.navy.mil
FU NASA through the NRA [NNH09ZDA001N-TERRAQUA, NNH11AQ99I]
FX This work was partially supported by NASA through the NRA
NNH09ZDA001N-TERRAQUA (The Science of Terra and Aqua), grant NNH11AQ99I.
NR 14
TC 9
Z9 9
U1 0
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD NOV 6
PY 2012
VL 39
AR L21807
DI 10.1029/2012GL053791
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 035QK
UT WOS:000310962400005
ER
PT J
AU Baars, H
Ansmann, A
Althausen, D
Engelmann, R
Heese, B
Muller, D
Artaxo, P
Paixao, M
Pauliquevis, T
Souza, R
AF Baars, H.
Ansmann, A.
Althausen, D.
Engelmann, R.
Heese, B.
Mueller, D.
Artaxo, P.
Paixao, M.
Pauliquevis, T.
Souza, R.
TI Aerosol profiling with lidar in the Amazon Basin during the wet and dry
season
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID MICROPHYSICAL PARTICLE PARAMETERS; FOREST-FIRE SMOKE;
OPTICAL-PROPERTIES; PHYSICAL-PROPERTIES; BACKSCATTER LIDAR; RAMAN-LIDAR;
RAIN-FOREST; SUBMICROMETER AEROSOL; SIZE DISTRIBUTION; FREE TROPOSPHERE
AB For the first time, multiwavelength polarization Raman lidar observations of optical and microphysical particle properties over the Amazon Basin are presented. The fully automated advanced Raman lidar was deployed 60 km north of Manaus, Brazil (2.5 degrees S, 60 degrees W) in the Amazon rain forest from January to November 2008. The measurements thus cover both the wet season (Dec-June) and the dry or burning season (July-Nov). Two cases studies of young and aged smoke plumes are discussed in terms of spectrally resolved optical properties (355, 532, and 1064 nm) and further lidar products such as particle effective radius and single-scattering albedo. These measurement examples confirm that biomass burning aerosols show a broad spectrum of optical, microphysical, and chemical properties. The statistical analysis of the entire measurement period revealed strong differences between the pristine wet and the polluted dry season. African smoke and dust advection frequently interrupt the pristine phases during the wet season. Compared to pristine wet season conditions, the particle scattering coefficients in the lowermost 2 km of the atmosphere were found to be enhanced, on average, by a factor of 4 during periods of African aerosol intrusion and by a factor of 6 during the dry (burning) season. Under pristine conditions, the particle extinction coefficients and optical depth for 532 nm wavelength were frequently as low as 10-30 Mm(-1) and <0.05, respectively. During the dry season, biomass burning smoke plumes reached to 3-5 km height and caused a mean optical depth at 532 nm of 0.26. On average during that season, particle extinction coefficients (532 nm) were of the order of 100 Mm(-1) in the main pollution layer (up to 2 km height). Angstrom exponents were mainly between 1.0 and 1.5, and the majority of the observed lidar ratios were between 50-80 sr.
C1 [Baars, H.; Ansmann, A.; Althausen, D.; Engelmann, R.; Heese, B.; Mueller, D.; Paixao, M.] Leibniz Inst Tropospher Res, DE-04318 Leipzig, Germany.
[Mueller, D.] NASA, Langley Res Ctr, Sci Syst & Applicat Inc, Hampton, VA 23665 USA.
[Artaxo, P.; Paixao, M.] Univ Sao Paulo, Inst Phys, Sao Paulo, Brazil.
[Pauliquevis, T.] Univ Fed Sao Paulo, Dept Earth & Nat Sci, Diadema, Brazil.
[Souza, R.] Univ State Amazonas, Manaus, Amazonas, Brazil.
RP Baars, H (reprint author), Leibniz Inst Tropospher Res, Permoserstr 15, DE-04318 Leipzig, Germany.
EM baars@tropos.de
RI MUELLER, DETLEF/F-1010-2015; Baars, Holger/I-3308-2015; Pauliquevis,
Theotonio/B-9408-2012; Artaxo, Paulo/E-8874-2010
OI MUELLER, DETLEF/0000-0002-0203-7654; Baars, Holger/0000-0002-2316-8960;
Artaxo, Paulo/0000-0001-7754-3036
FU National Institute for Amazonia Research (INPA); AMAZE-08 team; European
Union (FP7) [036833-2]; CNPq; FAPESP Thematic Project AEROCLIMA
[2008/58100-2]; EU FP6 project EUCAARI [34684]
FX We thank the National Institute for Amazonia Research (INPA) and the
AMAZE-08 team, especially Scot Martin, for their support. EUCAARI was
funded by the European Union (FP7, grant 036833-2). Paulo Artaxo
acknowledges CNPq and FAPESP Thematic Project AEROCLIMA 2008/58100-2.
This project was also funded by the EU FP6 project EUCAARI (contract
34684). Some analyses and visualizations used in this paper were
produced with the Giovanni online data system, developed and maintained
by the NASA GES DISC. We also acknowledge the MODIS mission scientists
and associated NASA personnel for the production of the data used in
this research effort. We thank Mika Komppula for providing ECMWF data.
NR 68
TC 29
Z9 29
U1 1
U2 42
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 NOV 3
PY 2012
VL 117
AR D21201
DI 10.1029/2012JD018338
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 032BE
UT WOS:000310686000001
ER
PT J
AU Li, LM
Baines, KH
Smith, MA
West, RA
Perez-Hoyos, S
Trammell, HJ
Simon-Miller, AA
Conrath, BJ
Gierasch, PJ
Orton, GS
Nixon, CA
Filacchione, G
Fry, PM
Momary, TW
AF Li, Liming
Baines, Kevin H.
Smith, Mark A.
West, Robert A.
Perez-Hoyos, Santiago
Trammell, Harold J.
Simon-Miller, Amy A.
Conrath, Barney J.
Gierasch, Peter J.
Orton, Glenn S.
Nixon, Conor A.
Filacchione, Gianrico
Fry, Patrick M.
Momary, Thomas W.
TI Emitted power of Jupiter based on Cassini CIRS and VIMS observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID QUASI-BIENNIAL OSCILLATION; MERIDIONAL ENERGY-BALANCE; INFRARED
SPECTROMETER; SPATIAL-ORGANIZATION; MOIST CONVECTION; TIME-DEPENDENCE;
INTERNAL HEAT; ATMOSPHERE; STRATOSPHERE; TEMPERATURES
AB The emitted power of Jupiter and its meridional distribution are determined from observations by the Composite Infrared Spectrometer and Visual and Infrared Mapping Spectrometer onboard Cassini during its flyby en route to Saturn in late 2000 and early 2001. Jupiter's global-average emitted power and effective temperature are measured to be 14.10 +/- 0.03 Wm(-2) and 125.57 +/- 0.07 K, respectively. Jupiter's 5 mm thermal emission contributes 0.7 +/- 0.1% to the total emitted power at the global scale, but it can reach 1.9 +/- 0.6% at 15 degrees N. The meridional distribution of emitted power shows a significant asymmetry between the two hemispheres with the emitted power in the northern hemisphere 3.0 +/- 0.3% larger than that in the southern hemisphere. Such an asymmetry shown in the Cassini epoch (2000-2001) is not present in the Voyager epoch (1979). In addition, the global-average emitted power increased 3.8 +/- 1.0% between the two epochs. The temporal variation of Jupiter's total emitted power is mainly due to the warming of atmospheric layers around the pressure level of 200 mbar.
The temporal variation of emitted power was also discovered on Saturn. Therefore, we suggest that the varying emitted power is a common phenomenon on the giant planets.
C1 [Li, Liming; Smith, Mark A.; Trammell, Harold J.] Univ Houston, Coll Nat Sci & Math, Houston, TX 77004 USA.
[Baines, Kevin H.; West, Robert A.; Orton, Glenn S.; Momary, Thomas W.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Perez-Hoyos, Santiago] Univ Basque Country, ETS Ingn, Dept Fis Aplicada 1, Bilbao, Spain.
[Simon-Miller, Amy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Conrath, Barney J.; Gierasch, Peter J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Nixon, Conor A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Filacchione, Gianrico] Area Ric Tor Vergata, Ist Astrofis & Planetol Spaziali, INAF IAPS, Rome, Italy.
[Fry, Patrick M.] Univ Wisconsin Madison, Ctr Space Sci & Engn, Madison, WI USA.
RP Li, LM (reprint author), Univ Houston, Coll Nat Sci & Math, 4800 Calhoun Rd, Houston, TX 77004 USA.
EM lli13@uh.edu
RI Nixon, Conor/A-8531-2009; Perez-Hoyos, Santiago/L-7543-2014; Simon,
Amy/C-8020-2012;
OI Nixon, Conor/0000-0001-9540-9121; Perez-Hoyos,
Santiago/0000-0002-2587-4682; Simon, Amy/0000-0003-4641-6186;
Filacchione, Gianrico/0000-0001-9567-0055
NR 43
TC 7
Z9 7
U1 0
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD NOV 3
PY 2012
VL 117
AR E11002
DI 10.1029/2012JE004191
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 032CU
UT WOS:000310690400001
ER
PT J
AU Norvig, P
AF Norvig, Peter
TI THE COMING SUPERINTELLIGENCE
SO NEW SCIENTIST
LA English
DT Editorial Material
C1 [Norvig, Peter] Stanford Univ, Stanford, CA 94305 USA.
[Norvig, Peter] NASA, Ames Res Ctr, Computat Sci Div, Washington, DC USA.
NR 0
TC 0
Z9 0
U1 2
U2 10
PU REED BUSINESS INFORMATION LTD
PI SUTTON
PA QUADRANT HOUSE THE QUADRANT, SUTTON SM2 5AS, SURREY, ENGLAND
SN 0262-4079
J9 NEW SCI
JI New Sci.
PD NOV 3
PY 2012
VL 216
IS 2889
BP VIII
EP VIII
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 034HI
UT WOS:000310863100036
ER
PT J
AU Boening, C
Lebsock, M
Landerer, F
Stephens, G
AF Boening, Carmen
Lebsock, Matthew
Landerer, Felix
Stephens, Graeme
TI Snowfall-driven mass change on the East Antarctic ice sheet
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID GRACE; VARIABILITY; REANALYSIS; BALANCE; SYSTEM
AB An improved understanding of processes dominating the sensitive balance between mass loss primarily due to glacial discharge and mass gain through precipitation is essential for determining the future behavior of the Antarctic ice sheet and its contribution to sea level rise. While satellite observations of Antarctica indicate that West Antarctica experiences dramatic mass loss along the Antarctic Peninsula and Pine Island Glacier, East Antarctica has remained comparably stable. In this study, we describe the causes and magnitude of recent extreme precipitation events along the East Antarctic coast that led to significant regional mass accumulations that partially compensate for some of the recent global ice mass losses that contribute to global sea level rise. The gain of almost 350 Gt from 2009 to 2011 is equivalent to a decrease in global mean sea level at a rate of 0.32 mm/yr over this three-year period. Citation: Boening, C., M. Lebsock, F. Landerer, and G. Stephens (2012), Snowfall-driven mass change on the East Antarctic ice sheet, Geophys. Res. Lett., 39, L21501, doi:10.1029/2012GL053316.
C1 [Boening, Carmen; Lebsock, Matthew; Landerer, Felix; Stephens, Graeme] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Boening, C (reprint author), CALTECH, Jet Prop Lab, MS 300-323,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM carmen.boening@jpl.nasa.gov
OI Landerer, Felix/0000-0003-2678-095X
FU NASA [NMO710771]
FX We would like to thank two anonymous reviewers for their helpful
comments and suggestions. The work was performed at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with NASA
and is partially supported through NASA contract NMO710771 to JPL. We
thank the GRACE analysis centers at University of Texas, JPL, and
Geoforschungszentrum Potsdam, and the German Space Operations Center
(GSOC) of the German Aerospace Center (DLR).
NR 31
TC 39
Z9 40
U1 2
U2 47
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 NOV 2
PY 2012
VL 39
AR L21501
DI 10.1029/2012GL053316
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 032DA
UT WOS:000310691000001
ER
PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Untitled
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Editorial Material
C1 [Siegel, Peter H.] CALTECH, Pasadena, CA 91125 USA.
[Siegel, Peter H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Siegel, PH (reprint author), CALTECH, Pasadena, CA 91125 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD NOV
PY 2012
VL 2
IS 6
BP 573
EP 574
DI 10.1109/TTHZ.2012.2224234
PG 2
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 142AU
UT WOS:000318769000001
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, Pasadena, CA 91125 USA.
[Siegel, Peter H.] JPL, Pasadena, CA 91125 USA.
RP Siegel, PH (reprint author), CALTECH, Pasadena, CA 91125 USA.
NR 12
TC 1
Z9 1
U1 1
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD NOV
PY 2012
VL 2
IS 6
BP 577
EP 577
DI 10.1109/TTHZ.2012.2222637
PG 1
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 142AU
UT WOS:000318769000002
ER
PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Terahertz Pioneer: Frank C. De Lucia "The Numbers Count"
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Editorial Material
ID MILLIMETER-WAVE; ROTATIONAL SPECTRUM; HYDROGEN-PEROXIDE; INDIUM
ANTIMONIDE; ANALYTICAL TOOL; BEAM MASER; GAS-PHASE; SPECTROSCOPY;
REGION; PRESSURE
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 91109 USA.
RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91125 USA.
EM phs@cal-tech.edu
NR 62
TC 0
Z9 0
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 NOV
PY 2012
VL 2
IS 6
BP 578
EP 583
DI 10.1109/TTHZ.2012.2222638
PG 6
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 142AU
UT WOS:000318769000003
ER
PT J
AU Morales, W
Street, KW
Richard, RM
Valco, DJ
AF Morales, Wilfredo
Street, Kenneth W.
Richard, Ryan M.
Valco, Daniel J.
TI Tribological Testing and Thermal Analysis of an Alkyl Sulfate Series of
Ionic Liquids for Use as Aerospace Lubricants
SO TRIBOLOGY TRANSACTIONS
LA English
DT Article
DE Ionic Liquids; Spiral Orbit Tribometry; Vapor Pressure;
Thermogravimetric Analysis
ID MELTING-POINT DEPRESSION; SPIRAL ORBIT TRIBOMETRY; VACUUM; PRESSURE
AB Due to their low vapor pressures, low melting points, high boiling points, high radiation resistance, and high thermal stability, room-temperature ionic liquids (ILs) appear to be suitable candidates as new aerospace lubricants for the upcoming return to the Moon and eventual Mars missions and for air and rotorcraft applications. In this study, three ILs with the same cation, 1-butyl-3-methylimidazolium, but different sulfate anions were tested using an ultra-high vacuum spiral orbit tribometer (SOT) and their thermal properties were determined by thermogravimetric analysis (TGA). Specifically, 1-butyl-3-methylimidazolium methyl sulfate, 1-butyl-3-methylimidazolium ethyl sulfate, and 1-butyl-3-methylimidazolium octyl sulfate were tested. The SOT experiments revealed that the lifetimes of the three ILs decreased with increasing alkyl substituent length on the sulfate anion. Infrared and Raman spectra were taken to detect unused ILs and graphitic degradation products, respectively, on worn parts. Post-run spectroscopic analysis indicated residual degraded, but still usable, ILs in all runs, coupled with varying amounts of amorphous graphitic material produced as the final degradation product of all ILs. SOT testing indicated that these ILs have lower friction coefficients and lifetimes greater than those of two commonly used perfluoropolyalkylether (PFPE) space lubricants. TGA showed that the methyl sulfate IL had the highest thermal stability in air and nitrogen. The vapor pressure of the methyl sulfate IL is as at least as low as Fomblin 815Z at 20 degrees C.
C1 [Morales, Wilfredo; Street, Kenneth W.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Richard, Ryan M.] Cleveland State Univ, Cleveland, OH 44115 USA.
[Valco, Daniel J.] Ohio State Univ, Columbus, OH 43210 USA.
RP Morales, W (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
NR 16
TC 14
Z9 14
U1 3
U2 24
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA
SN 1040-2004
J9 TRIBOL T
JI Tribol. Trans.
PD NOV 1
PY 2012
VL 55
IS 6
BP 815
EP 821
DI 10.1080/10402004.2012.715322
PG 7
WC Engineering, Mechanical
SC Engineering
GA 089LS
UT WOS:000314912600012
ER
PT J
AU Kudryavtsev, VA
Spooner, NJC
Gluyas, J
Fung, C
Coleman, M
AF Kudryavtsev, Vitaly A.
Spooner, Neil J. C.
Gluyas, Jon
Fung, Cora
Coleman, Max
TI Monitoring subsurface CO2 emplacement and security of storage using muon
tomography
SO INTERNATIONAL JOURNAL OF GREENHOUSE GAS CONTROL
LA English
DT Article
DE Carbon capture; Carbon storage monitoring; Muon tomography; Cosmic-ray
muons
ID CARBON-DIOXIDE; MUSIC; JAPAN
AB Storage of supercritical carbon dioxide in the deep subsurface is arguably the most viable industrial scale process available to stop increase of atmospheric CO2. Today, monitoring CO2 emplacement and possible leakage is a major challenge; methods are episodic and expensive. Cosmic-ray muon tomography has been used to investigate hidden archaeological and geological features. We developed a model to test if this approach would work for monitoring CO2 storage and show that muon detection is a viable method. Our results indicate that we could detect as little as 0.4% change in the mean reservoir density at about 1 km depth (equivalent to 7% of pore volume). Hence, cosmic ray muon detection could monitor migration of injected CO2 continuously and inexpensively and help rapid introduction of this essential technology. (c) 2012 Elsevier Ltd. All rights reserved.
C1 [Kudryavtsev, Vitaly A.; Spooner, Neil J. C.; Fung, Cora] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England.
[Gluyas, Jon] Univ Durham, Dept Earth Sci, Ctr Res Earth Energy Syst, Durham DH1 3LE, England.
[Coleman, Max] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kudryavtsev, VA (reprint author), Univ Sheffield, Dept Phys & Astron, Hounsfield Rd, Sheffield S3 7RH, S Yorkshire, England.
EM v.kudryavtsev@sheffield.ac.uk
RI Gluyas, Jon/B-8808-2014
OI Gluyas, Jon/0000-0002-9386-7206
FU University of Sheffield; EPSRC through the E-Futures Doctoral Training
Centre at the University of Sheffield; National Aeronautics and Space
Administration (NASA)
FX We are grateful to S. M. Paling, L. F. Thompson, J. Cripps, T. Bennett,
D. Lerner, C. Shelbourn, D. A. French and I. Phillips for useful
discussions, and to D. H. Rodgers, who alerted MC to the existence of
muon tomography. VAK and NJCS are grateful to the University of
Sheffield for the financial support of the Ph.D. network related to muon
tomography. CF's project work was funded by EPSRC through the E-Futures
Doctoral Training Centre at the University of Sheffield. JG thanks DONG
and Ikon Science for supporting carbon capture and storage research at
Durham University. The contribution of MC was carried out at the Jet
Propulsion Laboratory (JPL), California Institute of Technology, under
contract with the National Aeronautics and Space Administration (NASA).
NR 22
TC 14
Z9 14
U1 0
U2 17
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1750-5836
J9 INT J GREENH GAS CON
JI Int. J. Greenh. Gas Control
PD NOV
PY 2012
VL 11
BP 21
EP 24
DI 10.1016/j.ijggc.2012.07.023
PG 4
WC GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY; Energy & Fuels; Engineering,
Environmental
SC Science & Technology - Other Topics; Energy & Fuels; Engineering
GA 070AW
UT WOS:000313479200003
ER
PT J
AU Rickman, D
Immer, C
Metzger, P
Dixon, E
Pendleton, M
Edmunson, J
AF Rickman, Doug
Immer, Christopher
Metzger, Philip
Dixon, Emily
Pendleton, Matthew
Edmunson, Jennifer
TI PARTICLE SHAPE IN SIMULANTS OF THE LUNAR REGOLITH
SO JOURNAL OF SEDIMENTARY RESEARCH
LA English
DT Article
AB Shape is an important property of lunar regolith particles. It substantially affects the regolith's strength, the angle of repose, the packing density, and the ability of regolith particles to attach to and abrade spacecraft materials or clog air filters. For these reasons, simulants are needed to reproduce regolith particle shapes for testing spacecraft that interacts with the lunar surface. Difficulties in assessing "how good" a simulant reproduces the shape of lunar particles stem from the lack of shape measurements obtained on lunar particles, compounded by the lack of a strict definition of shape or a way to quantifiably measure shape. This paper presents a general method for measuring and comparing particle shapes, and provides shape measurements for six lunar-regolith simulants.
The method of evaluating particle shape presented here involves Fine Particle Analysis and corresponding image analysis to extract the maximum Feret diameter, Feret diameter of the minor axis of the inertial ellipse, mean diameter, sieve diameter, area, and perimeter length from images with an approximately 4.4 mu m pixel resolution. From those, aspect ratio and Heywood factor are computed. Data processing involves calculating the frequency distributions of particle shapes according to their sieve diameter, aspect ratio, and Heywood factor. The resulting graphical representations indicate that the majority of the lunar regolith simulant particles, in two-dimensional projection, can be well represented by a mixture of ellipses and rectangles of varying aspect ratios. The differences between simulant particle shapes, and lunar regolith particle shapes measured in the future, can be quantified by differencing the accumulated distributions. Thus, this paper presents a new method of particle shape analysis and a new way to quantifiably compare particle shapes.
C1 [Rickman, Doug] NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35812 USA.
[Immer, Christopher] GE Global Res, Electromagnet & Superconduct Lab, Niskayuna, NY 12309 USA.
[Metzger, Philip] NASA, Granular Mech & Regolith Operat Lab, Kennedy Space Ctr, FL 32899 USA.
[Dixon, Emily] Univ Oklahoma, Dept Geol, Norman, OK 73019 USA.
[Pendleton, Matthew] Univ Minnesota, Dept Geol & Geophys, Minneapolis, MN 55440 USA.
[Edmunson, Jennifer] BAE Syst, Huntsville, AL 35806 USA.
RP Rickman, D (reprint author), NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35812 USA.
RI Metzger, Philip/R-3136-2016;
OI Metzger, Philip/0000-0002-6871-5358; Rickman, Doug/0000-0003-3409-2882
NR 18
TC 3
Z9 3
U1 0
U2 7
PU SEPM-SOC SEDIMENTARY GEOLOGY
PI TULSA
PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA
SN 1527-1404
J9 J SEDIMENT RES
JI J. Sediment. Res.
PD NOV-DEC
PY 2012
VL 82
IS 11-12
BP 823
EP 832
DI 10.2110/jsr.2012.69
PG 10
WC Geology
SC Geology
GA 078FZ
UT WOS:000314085400002
ER
PT J
AU Gietzen, KM
Lacy, CHS
Ostrowski, DR
Sears, DWG
AF Gietzen, Katherine M.
Lacy, Claud H. S.
Ostrowski, Daniel R.
Sears, Derek W. G.
TI IRTF observations of S complex and other asteroids: Implications for
surface compositions, the presence of clinopyroxenes, and their
relationship to meteorites
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID MODIFIED GAUSSIAN MODEL; NEAR-EARTH OBJECTS; SPECTROSCOPIC SURVEY;
SPECTRAL PROPERTIES; ORDINARY CHONDRITES; PYROXENE MIXTURES; THERMAL
HISTORIES; INFRARED-SPECTRA; VESTA; CONNECTION
AB We have obtained near-infrared spectra for near-Earth asteroids (NEA) and Main Belt asteroids by using NASA's Infrared Telescope Facility. Most of the S complex classes of the Tholen-Bus-DeMeo scheme and the S(I)-S(VII) classes are represented. To help interpret the results, we examined visible/near-IR spectra for ordinary chondrites. The unequilibrated ordinary chondrites (UOC) spectra contain a 2.3 mu m feature which is absent in the spectra of the equilibrated ordinary chondrites (EOC). On the basis of literature data and new spectra low-Ca clinopyroxenes, we suggest that the 2.3 mu m in UOC is due to the presence of low-Ca clinopyroxene in the UOC which is absent in EOC. While this difference can be seen in the raw spectra, we confirmed this observation using a modified Gaussian model (MGM) for spectral analysis. Both the UOC and the EOC plot in the S(IV) field of the band area ratio plot for asteroids. We suggest that many or most S(IV) asteroids have material resembling UOC on their surfaces. An internally heated ordinary chondrite parent object would have EOC material at depth and UOC material on the surface. Cosmic ray exposure ages, and K-Ar ages for L chondrites, indicate that most EOC came from relatively few objects; however, the age distributions for UOC are unlike those of EOC. We suggest that while EOC come from the interiors of a limited number of S(IV) asteroids, the UOC come from the surfaces of a large number of S(IV) asteroids.
C1 [Gietzen, Katherine M.; Lacy, Claud H. S.; Ostrowski, Daniel R.; Sears, Derek W. G.] Univ Arkansas, Arkansas Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA.
[Lacy, Claud H. S.] Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA.
[Sears, Derek W. G.] Univ Arkansas, Dept Chem & Biochem, Fayetteville, AR 72701 USA.
RP Sears, DWG (reprint author), NASA, Space Sci & Astrobiol Div, Ames Res Ctr, MS245-3, Mountain View, CA 94035 USA.
EM derek.sears@nasa.gov
FU NASA
FX Without implying endorsement of our views, we gratefully acknowledge the
many colleagues who have commented on our work over the last few years
or otherwise helped as we evolved our thoughts and ideas: Paul Abell,
Rick Binzel, Vincent Chevrier, Mike Gaffey, Paul Hardersen, Tim McCoy,
Andy Rivkin, Ludolf Schultz, and Jessica Sunshine. We are also grateful
to NASA for access to the IRTF and for funding, to Bobby Bus for
hospitality and help in obtaining the data, Dan Britt for advice using
the facility, Takahiro Hiroi for obtaining spectra for terrestrial
clinopyroxenes, and Tom Burbine, Beth Clark Joseph, and Hazel Sears for
very helpful reviews, and Hazel Sears for proofing the paper.
NR 74
TC 5
Z9 5
U1 0
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD NOV
PY 2012
VL 47
IS 11
BP 1789
EP 1808
DI 10.1111/maps.12013
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 076UW
UT WOS:000313985100008
ER
PT J
AU Clark, BE
AF Clark, Beth Ellen
TI ASTEROIDS Dark and stormy weather
SO NATURE
LA English
DT Editorial Material
ID SPACE; SURFACE
C1 [Clark, Beth Ellen] Ithaca Coll, Dept Phys, Ithaca, NY 14850 USA.
[Clark, Beth Ellen] Univ Arizona, NASA, OSIRIS REx Asteroid Sample Return Mission, Tucson, AZ 85721 USA.
RP Clark, BE (reprint author), Ithaca Coll, Dept Phys, Ithaca, NY 14850 USA.
EM bclark@ithaca.edu
NR 14
TC 0
Z9 0
U1 0
U2 0
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD NOV 1
PY 2012
VL 491
IS 7422
BP 45
EP 46
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 028PM
UT WOS:000310434500025
PM 23128222
ER
PT J
AU Pieters, CM
Ammannito, E
Blewett, DT
Denevi, BW
De Sanctis, MC
Gaffey, MJ
Le Corre, L
Li, JY
Marchi, S
McCord, TB
McFadden, LA
Mittlefehldt, DW
Nathues, A
Palmer, E
Reddy, V
Raymond, CA
Russell, CT
AF Pieters, C. M.
Ammannito, E.
Blewett, D. T.
Denevi, B. W.
De Sanctis, M. C.
Gaffey, M. J.
Le Corre, L.
Li, J. -Y.
Marchi, S.
McCord, T. B.
McFadden, L. A.
Mittlefehldt, D. W.
Nathues, A.
Palmer, E.
Reddy, V.
Raymond, C. A.
Russell, C. T.
TI Distinctive space weathering on Vesta from regolith mixing processes
SO NATURE
LA English
DT Article
ID ITOKAWA DUST PARTICLES; ASTEROID 4 VESTA; ORDINARY CHONDRITES;
IRRADIATION; MORPHOLOGY; MINERALOGY; SURFACE; ALBEDO; BELT; DAWN
AB The surface of the asteroid Vesta has prominent near-infrared absorption bands characteristic of a range of pyroxenes, confirming a direct link to the basaltic howardite-eucrite-diogenite class of meteorites(1,2,3). Processes active in the space environment produce 'space weathering' products that substantially weaken or mask such diagnostic absorption on airless bodies observed elsewhere(4,5), and it has long been a mystery why Vesta's absorption bands are so strong. Analyses of soil samples from both the Moon(6) and the asteroid Itokawa(7) determined that nanophase metallic particles (commonly nanophase iron) accumulate on the rims of regolith grains with time, accounting for an observed optical degradation. These nanophase particles, believed to be related to solar wind and micrometeoroid bombardment processes, leave unique spectroscopic signatures that can be measured remotely(8-10) but require sufficient spatial resolution to discern the geologic context and history of the surface, which has not been achieved for Vesta until now. Here we report that Vesta shows its own form of space weathering, which is quite different from that of other airless bodies visited. No evidence is detected on Vesta for accumulation of lunar-like nanophase iron on regolith particles, even though distinct material exposed at several fresh craters becomes gradually masked and fades into the background as the craters age. Instead, spectroscopic data reveal that on Vesta a locally homogenized upper regolith is generated with time through small-scale mixing of diverse surface components.
C1 [Pieters, C. M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Ammannito, E.; De Sanctis, M. C.] ARTOV, INAF, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy.
[Blewett, D. T.; Denevi, B. W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Gaffey, M. J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA.
[Le Corre, L.; Nathues, A.; Reddy, V.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Li, J. -Y.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Marchi, S.] NASA, Lunar Sci Inst, Boulder, CO 80302 USA.
[McCord, T. B.] Bear Fight Inst, Winthrop, WA 98862 USA.
[McFadden, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Palmer, E.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
RP Pieters, CM (reprint author), Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
EM carle_pieters@brown.edu
RI Russell, Christopher/E-7745-2012; McFadden, Lucy-Ann/I-4902-2013; De
Sanctis, Maria Cristina/G-5232-2013; Denevi, Brett/I-6502-2012; Blewett,
David/I-4904-2012;
OI Le Corre, Lucille/0000-0003-0349-7932; Russell,
Christopher/0000-0003-1639-8298; McFadden, Lucy-Ann/0000-0002-0537-9975;
De Sanctis, Maria Cristina/0000-0002-3463-4437; Denevi,
Brett/0000-0001-7837-6663; Blewett, David/0000-0002-9241-6358; Reddy,
Vishnu/0000-0002-7743-3491
FU NASA [NNM05AA86C]; NASA Dawn participating scientist programme
FX We acknowledge the Dawn Instrument, Flight and Operations teams for the
successful development, cruise, orbital insertion and operations of the
Dawn spacecraft at Vesta. US team members are supported by the NASA
Discovery Program through contract NNM05AA86C to the University of
California, Los Angeles and by the NASA Dawn participating scientist
programme.
NR 31
TC 71
Z9 71
U1 4
U2 25
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD NOV 1
PY 2012
VL 491
IS 7422
BP 79
EP 82
DI 10.1038/nature11534
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 028PM
UT WOS:000310434500033
PM 23128227
ER
PT J
AU McCord, TB
Li, JY
Combe, JP
McSween, HY
Jaumann, R
Reddy, V
Tosi, F
Williams, DA
Blewett, DT
Turrini, D
Palomba, E
Pieters, CM
De Sanctis, MC
Ammannito, E
Capria, MT
Le Corre, L
Longobardo, A
Nathues, A
Mittlefehldt, DW
Schroder, SE
Hiesinger, H
Beck, AW
Capaccioni, F
Carsenty, U
Keller, HU
Denevi, BW
Sunshine, JM
Raymond, CA
Russell, CT
AF McCord, T. B.
Li, J. -Y.
Combe, J. -P.
McSween, H. Y.
Jaumann, R.
Reddy, V.
Tosi, F.
Williams, D. A.
Blewett, D. T.
Turrini, D.
Palomba, E.
Pieters, C. M.
De Sanctis, M. C.
Ammannito, E.
Capria, M. T.
Le Corre, L.
Longobardo, A.
Nathues, A.
Mittlefehldt, D. W.
Schroeder, S. E.
Hiesinger, H.
Beck, A. W.
Capaccioni, F.
Carsenty, U.
Keller, H. U.
Denevi, B. W.
Sunshine, J. M.
Raymond, C. A.
Russell, C. T.
TI Dark material on Vesta from the infall of carbonaceous volatile-rich
material
SO NATURE
LA English
DT Article
ID DAWN MISSION; HETEROGENEITY; MINERALOGY; SURFACE; ALBEDO; COLOR; WATER;
MOON
AB Localized dark and bright materials, often with extremely different albedos, were recently found on Vesta's surface(1,2). The range of albedos is among the largest observed on Solar System rocky bodies. These dark materials, often associated with craters, appear in ejecta and crater walls, and their pyroxene absorption strengths are correlated with material brightness. It was tentatively suggested that the dark material on Vesta could be either exogenic, from carbon-rich, low-velocity impactors, or endogenic, from freshly exposed mafic material or impact melt, created or exposed by impacts. Here we report Vesta spectra and images and use them to derive and interpret the properties of the 'pure' dark and bright materials. We argue that the dark material is mainly from infall of hydrated carbonaceous material (like that found in a major class of meteorites and some comet surfaces(3-5)), whereas the bright material is the uncontaminated indigenous Vesta basaltic soil. Dark material from low-albedo impactors is diffused over time through the Vestan regolith by impact mixing, creating broader, diffuse darker regions and finally Vesta's background surface material. This is consistent with howardite-eucrite-diogenite meteorites coming from Vesta.
C1 [McCord, T. B.; Combe, J. -P.] Bear Fight Inst, Winthrop, WA 98862 USA.
[Li, J. -Y.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[McSween, H. Y.] Univ Tennessee, Knoxville, TN 37996 USA.
[Jaumann, R.; Carsenty, U.] Inst Planetary Res, DLR, D-80302 Berlin, Germany.
[Reddy, V.; Le Corre, L.; Nathues, A.; Schroeder, S. E.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg, Germany.
[Reddy, V.] Univ N Dakota, Grand Forks, ND 58202 USA.
[Tosi, F.; Turrini, D.; Palomba, E.; De Sanctis, M. C.; Ammannito, E.; Capria, M. T.; Longobardo, A.; Capaccioni, F.] Ist Nazl Astrofis IASF, I-00133 Rome, Italy.
[Williams, D. A.] Arizona State Univ, Tempe, AZ 85287 USA.
[Blewett, D. T.; Denevi, B. W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Pieters, C. M.] Brown Univ, Providence, RI 02912 USA.
[Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA.
[Hiesinger, H.] Univ Munster, Inst Planetol, D-48149 Munster, Germany.
[Beck, A. W.] Smithsonian Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20024 USA.
[Keller, H. U.] Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany.
[Sunshine, J. M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
RP McCord, TB (reprint author), Bear Fight Inst, 22 Fiddlers Rd,Box 667, Winthrop, WA 98862 USA.
EM tmccord@bearfightinstitute.com;
jean-philippe_combe@bearfightinstitutute.com
RI Russell, Christopher/E-7745-2012; Schroder, Stefan/D-9709-2013; De
Sanctis, Maria Cristina/G-5232-2013; Denevi, Brett/I-6502-2012; Blewett,
David/I-4904-2012; Beck, Andrew/J-7215-2015;
OI Le Corre, Lucille/0000-0003-0349-7932; Palomba,
Ernesto/0000-0002-9101-6774; Tosi, Federico/0000-0003-4002-2434;
Russell, Christopher/0000-0003-1639-8298; Capaccioni,
Fabrizio/0000-0003-1631-4314; Schroder, Stefan/0000-0003-0323-8324; De
Sanctis, Maria Cristina/0000-0002-3463-4437; Denevi,
Brett/0000-0001-7837-6663; Blewett, David/0000-0002-9241-6358; Beck,
Andrew/0000-0003-4455-2299; capria, maria teresa/0000-0002-9814-9588;
Reddy, Vishnu/0000-0002-7743-3491; Turrini, Diego/0000-0002-1923-7740
FU NASA Dawn Project under UCLA; NASA Dawn at Vesta Participating Scientist
program; Italian Space Agency; Max Planck Institute for Solar System
Research; Germany Aerospace Agency (DLR)
FX This research was supported by the NASA Dawn Project under contract from
UCLA, by the NASA Dawn at Vesta Participating Scientist program, the
Italian Space Agency, the Max Planck Institute for Solar System
Research, and the Germany Aerospace Agency (DLR). We acknowledge the
support of the Dawn Science, Instrument and Operations Teams.
NR 23
TC 87
Z9 88
U1 4
U2 37
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD NOV 1
PY 2012
VL 491
IS 7422
BP 83
EP U93
DI 10.1038/nature11561
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 028PM
UT WOS:000310434500034
PM 23128228
ER
PT J
AU Vicroy, DD
Loeser, TD
Schutte, A
AF Vicroy, Dan D.
Loeser, Thomas D.
Schuette, Andreas
TI Static and Forced-Oscillation Tests of a Generic Unmanned Combat Air
Vehicle
SO JOURNAL OF AIRCRAFT
LA English
DT Article
AB A series of three wind-tunnel static and forced-oscillation tests were conducted on a model of a generic unmanned combat air vehicle. These tests are part of an international research effort to assess the state of the art of computational fluid dynamics methods to predict the static and dynamic stability and control characteristics. The experimental data set includes not only force and moment time histories, but also surface pressure and offbody particle image velocimetry measurements. The extent of the data precludes a full examination within the scope of this paper. This paper provides a general description and selected examples of the available static and dynamic data, as well as some of the observed trends.
C1 [Vicroy, Dan D.] NASA, Langley Res Ctr, Flight Dynam Branch, Hampton, VA 23681 USA.
[Loeser, Thomas D.] German Dutch Wind Tunnels, Low Speed Wind Tunnel Brunswick, D-38108 Braunschweig, Germany.
[Schuette, Andreas] German Dutch Wind Tunnels, DLR, Inst Aerodynam & Flow Technol, D-38108 Braunschweig, Germany.
RP Vicroy, DD (reprint author), NASA, Langley Res Ctr, Flight Dynam Branch, Mail Stop 308, Hampton, VA 23681 USA.
FU German Federal Office of Defense Technology and Procurement; NASA
FX The authors wish to thank the German Federal Office of Defense
Technology and Procurement (BWB), which supported the work by funding
the DLR, German Aerospace Center, project "UCAV 2010" and the NASA
Fundamental Aeronautics Program's Subsonic Fixed Wing Project, which
provided funding for the stability and control configuration (SACCON)
model and NASA wind-tunnel testing.
NR 21
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U2 1
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PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD NOV-DEC
PY 2012
VL 49
IS 6
BP 1558
EP 1583
DI 10.2514/1.C031501
PG 26
WC Engineering, Aerospace
SC Engineering
GA 060GH
UT WOS:000312764000003
ER
PT J
AU Frink, NT
Tormalm, M
Schmidt, S
AF Frink, Neal T.
Tormalm, Magnus
Schmidt, Stefan
TI Three Unstructured Computational Fluid Dynamics Studies on Generic
Uninhabited Combat Air Vehicle
SO JOURNAL OF AIRCRAFT
LA English
DT Article
ID TURBULENT FLOWS; MODEL
AB Three independent studies from the United States (NASA), Sweden (Swedish Defense Research Agency), and Australia (Defense Science and Technology Organization) are analyzed to assess the state of current unstructured grid computational fluid dynamic tools and practices for predicting the complex static and dynamic aerodynamic and stability characteristics of a generic 53-deg swept, round-leading-edge uninhabited combat air vehicle configuration, called SACCON (which stands for "stability and control configuration"). NASA exercised the USM3D tetrahedral cell-centered flow solver, while the Swedish Defense Research Agency and the Defense Science and Technology Organization applied the Swedish Defense Research Agency/EDGE general-cell vertex-based solver. The authors primarily employ the Reynolds-averaged Navier-Stokes assumption, with a limited assessment of the EDGE detached eddy simulation extension, to explore sensitivities to grids and turbulence models. Correlations with experimental data are provided for force and moments, surface pressure, and off-body flow measurements. The vortical flowfield over SACCON proved extremely difficult to model adequately. As a general rule, the prospect of obtaining reasonable correlations of SACCON pitching moment characteristics with the Reynolds-averaged Navier-Stokes formulation is not promising, even for static cases. However, dynamic pitch oscillation results seem to produce a promising characterization of shapes for the lift and pitching moment hysteresis curves. Future studies of this configuration should include more investigation with higher-fidelity turbulence models such as detached eddy simulation.
C1 [Frink, Neal T.] NASA, Langley Res Ctr, Configurat Aerodynam Branch, Res Directorate, Hampton, VA 23681 USA.
[Tormalm, Magnus] Swedish Def Res Agcy, Dept Aeronaut & Syst Integrat, S-16490 Stockholm, Sweden.
[Schmidt, Stefan] Def Sci & Technol Org, Air Vehicles Div, Fishermans Bend, Vic 3207, Australia.
RP Frink, NT (reprint author), NASA, Langley Res Ctr, Configurat Aerodynam Branch, Res Directorate, MS 499, Hampton, VA 23681 USA.
EM Neal.T.Frink@nasa.gov; Magnus.Tormalm@foi.se;
Stefan.Schmidt@dsto.defence.gov.au
FU Swedish Armed Forces
FX The first author gratefully acknowledges the generous support for this
work from the NASA Aviation Safety Program, Integrated Resilient
Aircraft Controls project, and the Fundamental Aerodynamics Program,
Subsonic Fixed Wing project, for the opportunity to participate in the
NATO/RTO AVT-161 task group. The second author would like to thank the
Swedish Armed Forces for financing the FOI research in this task group.
The third author would like to thank NATO for allowing DSTO to make
active contributions to research in AVT-161.
NR 24
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PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD NOV-DEC
PY 2012
VL 49
IS 6
BP 1619
EP 1637
DI 10.2514/1.C031383
PG 19
WC Engineering, Aerospace
SC Engineering
GA 060GH
UT WOS:000312764000007
ER
PT J
AU Kaul, UK
Ahmad, J
AF Kaul, Upender K.
Ahmad, Jasim
TI Skin-Friction Predictions on a Hovering Tilt-Rotor Blade
SO JOURNAL OF AIRCRAFT
LA English
DT Article
ID COMPUTATIONAL FLUID-DYNAMICS
AB Skin-friction predictions on hovering XV-15 helicopter blades have been made with the OVERFLOW2 flow solver using the Spalart-Allmaras one-equation turbulence model. The figure of merit for the 10 deg collective pitch is predicted reasonably, and for the 3 deg collective pitch it is underpredicted in comparison with experimental data. The trend in the skin-friction predictions at the 10 deg collective pitch in the fully turbulent region is in good agreement with the experimental data at radial stations away from the hub. For the 3 deg collective pitch, the agreement in the fully turbulent region is not as good as for the 10 deg case. In the transition region, the predictions deviate significantly from the experimental data for both the cases. By modulating the turbulence viscosity a priori in the experimentally known transition zone in various ways, a measurable change was predicted in the behavior of skin friction over the blade. This change was observed to be significant for the 3 deg collective pitch. Skin-friction results corresponding to the fully laminar calculations are in good agreement with experimental skin friction in the laminar region for both of the collective pitch angles.
C1 [Kaul, Upender K.; Ahmad, Jasim] NASA, Ames Res Ctr, Appl Modeling & Simulat Branch, Adv Supercomp Div, Moffett Field, CA 94035 USA.
RP Kaul, UK (reprint author), NASA, Ames Res Ctr, Appl Modeling & Simulat Branch, Adv Supercomp Div, Moffett Field, CA 94035 USA.
FU Subsonic Rotary Wing Project of the NASA Fundamental Aeronautics Program
FX This work was funded by the Subsonic Rotary Wing Project of the NASA
Fundamental Aeronautics Program. The authors would like to acknowledge
helpful information on the experimental results provided by Gloria
Yamauchi throughout the course of this study. The authors would also
like to thank Alan Wadcock for providing reference experimental data and
the image of the 80 by 120 ft wind-tunnel experiment setup. Finally, a
critical review of the paper by Cetin Kiris, Mark Potsdam, and Alan
Wadcock is gratefully acknowledged.
NR 29
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PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD NOV-DEC
PY 2012
VL 49
IS 6
BP 1726
EP 1738
DI 10.2514/1.C031401
PG 13
WC Engineering, Aerospace
SC Engineering
GA 060GH
UT WOS:000312764000015
ER
PT J
AU Morelli, EA
AF Morelli, Eugene A.
TI Flight Test Maneuvers for Efficient Aerodynamic Modeling
SO JOURNAL OF AIRCRAFT
LA English
DT Article
AB Novel flight test maneuvers for efficient aerodynamic modeling were developed and demonstrated in flight. Orthogonal optimized multisine inputs were applied to aircraft control surfaces to excite aircraft dynamic response in all six degrees of freedom simultaneously, while keeping the aircraft close to chosen reference flight conditions. Each maneuver was designed for a specific modeling task that cannot be adequately or efficiently accomplished using conventional flight test maneuvers. The maneuvers are described and explained, then demonstrated on a subscale jet transport aircraft in flight. Real-time and post-flight modeling results from equation-error parameter estimation in the frequency domain were used to show the effectiveness and efficiency of the maneuvers, as well as the quality of the aerodynamic models that can be identified from the resultant flight data.
C1 NASA, Langley Res Ctr, Dynam Syst & Control Branch, Hampton, VA 23681 USA.
RP Morelli, EA (reprint author), NASA, Langley Res Ctr, Dynam Syst & Control Branch, Mail Stop 308, Hampton, VA 23681 USA.
FU NASA Aviation Safety Program, Integrated Resilient Aircraft Control
project; NASA Aviation Safety Program, Vehicle Safety Systems Technology
project
FX Research in dynamic modeling is funded by the NASA Aviation Safety
Program, Integrated Resilient Aircraft Control and Vehicle Safety
Systems Technology projects. The efforts of the Airborne Subscale
Transport Aircraft Research (AirSTAR) flight-test team at NASA Langley
Research Center in building and testing the aircraft and associated
systems, carefully calibrating the instrumentation, and carrying out the
flight operations to collect the high-quality flight data used in this
study, are gratefully acknowledged.
NR 17
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U2 6
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 NOV-DEC
PY 2012
VL 49
IS 6
BP 1857
EP 1867
DI 10.2514/1.C031699
PG 11
WC Engineering, Aerospace
SC Engineering
GA 060GH
UT WOS:000312764000027
ER
PT J
AU Ku, JT
Ottenstein, L
Douglas, D
Hoang, T
AF Ku, Jentung
Ottenstein, Laura
Douglas, Donya
Hoang, Triem
TI Technology Overview of a Multi-Evaporator Miniature Loop Heat Pipe for
Spacecraft Applications
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 48th AIAA Aerospace Sciences Meeting and Exhibit / New Horizons Forum
and Aerospace Exposition
CY JAN 04-08, 2010
CL Orlando, FL
SP AIAA
AB A miniature loop heat pipe with multiple evaporators and multiple condensers was developed for thermal control of small spacecraft and instruments requiring low mass, low power, and compactness. Multiple evaporators afford flexible placement of instruments inside the spacecraft and facilitate heat-load sharing among instruments. Multiple condensers allow the radiators to be placed at various locations on the spacecraft surface and exposed to different thermal environments. Thermoelectric converters are used to provide heating and cooling to the reservoir for loop operating temperature control. A breadboard and a protoflight unit of the miniature loop heat pipe with two evaporators and two condensers were built and tested in a thermal vacuum chamber to demonstrate the thermal performance. In addition, an analytical model was developed to simulate the steady-state and transient behaviors of the miniature loop heat pipe during thermal performance tests.
C1 [Ku, Jentung; Ottenstein, Laura] NASA, Goddard Space Flight Ctr, Thermal Engn Branch, Greenbelt, MD 20771 USA.
[Douglas, Donya] NASA, Goddard Space Flight Ctr, Instrument Syst Branch, Greenbelt, MD 20771 USA.
[Hoang, Triem] TTH Res Inc, Clifton, VA 20124 USA.
RP Ku, JT (reprint author), NASA, Goddard Space Flight Ctr, Thermal Engn Branch, Greenbelt, MD 20771 USA.
NR 30
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U1 2
U2 19
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 NOV-DEC
PY 2012
VL 49
IS 6
BP 999
EP 1007
DI 10.2514/1.51348
PG 9
WC Engineering, Aerospace
SC Engineering
GA 064NS
UT WOS:000313082900005
ER
PT J
AU Ku, JT
Ottenstein, L
Douglas, D
Hoang, T
AF Ku, Jentung
Ottenstein, Laura
Douglas, Donya
Hoang, Triem
TI Validation Design for a Multi-Evaporator Miniature Loop Heat Pipe for
Spacecraft Applications
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 48th AIAA Aerospace Sciences Meeting and Exhibit / New Horizons Forum
and Aerospace Exposition
CY JAN 04-08, 2010
CL Orlando, FL
SP AIAA
AB A miniature loop heat pipe with multiple evaporators and multiple condensers for thermal control of small spacecraft and instruments was successfully developed. The miniature loop heat pipe had a 6.35 mm primary wick and used thermoelectric converters to control its operating temperature. A breadboard and a protoflight unit were built and tested under laboratory and thermal vacuum environments. Both loops demonstrated excellent thermal performance, including 100% startup success, tight temperature control under various heat loads and sink conditions, and heat-load sharing between evaporators. An analytical model designed to simulate steady-state and transient behaviors of the miniature loop heat pipe was also developed, and the model predictions agreed very well with experimental data. The maturity of this technology has been advanced from "proof of concept" to "prototype demonstration in a relevant environment."
C1 [Ku, Jentung; Ottenstein, Laura] NASA, Goddard Space Flight Ctr, Thermal Engn Branch, Greenbelt, MD 20771 USA.
[Douglas, Donya] NASA, Goddard Space Flight Ctr, Syst Engn Serv, Greenbelt, MD 20771 USA.
[Douglas, Donya] NASA, Goddard Space Flight Ctr, Adv Concepts Branch, Greenbelt, MD 20771 USA.
[Hoang, Triem] TTH Res Inc, Clifton, VA 20124 USA.
RP Ku, JT (reprint author), NASA, Goddard Space Flight Ctr, Thermal Engn Branch, Greenbelt, MD 20771 USA.
NR 34
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U2 10
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 NOV-DEC
PY 2012
VL 49
IS 6
BP 1008
EP 1018
DI 10.2514/1.51349
PG 11
WC Engineering, Aerospace
SC Engineering
GA 064NS
UT WOS:000313082900006
ER
PT J
AU Everline, CJ
AF Everline, Chester J.
TI Bayesian Approach to Quantifying Epistemic Uncertainty in a Processor
Availability Model
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID PROBABILISTIC RISK-ASSESSMENT; SYSTEMS; RELIABILITY; COMPONENTS
AB It is often necessary to use a combination of testing and analysis to demonstrate compliance with quantitative performance requirements. Increasingly, the demonstration must establish that requirements are satisfied with a certain level of confidence. As an example, a processor intended for space applications may be required to have a certain reliability or availability (e.g., at least 99.9%) with high confidence (e.g., 95%). This paper examines the application of Bayesian statistics and Monte Carlo simulation to such situations, focusing on quantifying epistemic uncertainty associated with the quantity of available data, the validity of alternative models, probabilistically combining alternative models when appropriate, and estimating epistemic uncertainty associated with certain aspects of model completeness.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Everline, CJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 156-206, Pasadena, CA 91109 USA.
EM Chester.J.Everline@jpl.nasa.gov
FU NASA
FX The research described in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA. I especially thank John F. Stocky and Raphael R.
Some of the Jet Propulsion Laboratory for their support of this effort.
NR 31
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PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD NOV-DEC
PY 2012
VL 49
IS 6
BP 1019
EP 1031
DI 10.2514/1.51352
PG 13
WC Engineering, Aerospace
SC Engineering
GA 064NS
UT WOS:000313082900007
ER
PT J
AU Mishra, K
Trivedi, KS
Some, RR
AF Mishra, Kesari
Trivedi, Kishor S.
Some, Raphael R.
TI Uncertainty Analysis of the Remote Exploration and Experimentation
System
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID APPROXIMATE CONFIDENCE LIMITS; INPUT VARIABLES; COMPLEX-SYSTEMS;
RELIABILITY; SERIES; COMPONENT; RISK
AB This paper discusses a method for computing the uncertainty in output metrics of stochastic models due to epistemic uncertainties in the model-input parameters. The method is illustrated by applying it to compute the distribution and confidence interval of the reliability of the Remote Exploration and Experimentation system. This method makes use of Monte Carlo sampling and propagates the epistemic uncertainty in the model parameters through the system reliability model. It acts as a wrapper to already-existing models as well as their solution tools/techniques and has a wide range of applicability. Although it is a sampling-based method, no simulation is carried out when performing uncertainty propagation through analytic models, but analytic or analytic numeric solution of the underlying stochastic model is performed for each set of input-parameter values, sampled from their distributions. Using the input epistemic uncertainty, in the form of 95% confidence intervals of input parameters of the stochastic model, the two-sided 95% confidence interval of reliability of the Remote Exploration and Experimentation system at a time t = 5 years is computed to be (0.949485, 0.981994).
C1 [Mishra, Kesari; Trivedi, Kishor S.] Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA.
[Some, Raphael R.] CALTECH, Jet Prop Lab, Autonomous Syst Div, Pasadena, CA 91109 USA.
RP Mishra, K (reprint author), Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA.
EM km@ee.duke.edu; kst@ee.duke.edu; Raphael.R.Some@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX Part of the research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 44
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U1 0
U2 1
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD NOV-DEC
PY 2012
VL 49
IS 6
BP 1032
EP 1042
DI 10.2514/1.51380
PG 11
WC Engineering, Aerospace
SC Engineering
GA 064NS
UT WOS:000313082900008
ER
PT J
AU Cruden, BA
Prabhu, D
Martinez, R
AF Cruden, Brett A.
Prabhu, Dinesh
Martinez, Ramon
TI Absolute Radiation Measurement in Venus and Mars Entry Conditions
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 10th AIAA/ASME Joint Thermophysics and Heat Transfer Conference
CY JUN 28-JUL 01, 2010
CL Chicago, IL
SP AIAA, ASME
ID CO2-N-2 PLASMAS
AB Comparisons of experimental characterization and model predictions of entry radiation relevant to Mars and Venus exploration are presented. Characterization is performed in the recently upgraded Electric Arc Shock Tube facility at NASA Ames Research Center. Tests are performed in simulated Mars (96% CO2, 4% N-2) and Venus (96.5% CO2, 3.5% N-2) atmospheres at downstream pressures and incident velocities spanning from 0.1 to 2.0 torr and 3-12 km/s. Velocity and pressure conditions were chosen based on expected flight conditions (direct entry or aerocapture) for Mars and Venus atmospheres. The absolute radiance data are spatially and spectrally resolved and span the vacuum ultraviolet through midinfrared (120-1650 nm, 3-5 mu m). Resolved spectra of the CO fourth positive band in the vacuum ultraviolet are reported for the first time. Measurements of CO2 molecular vibrational radiation are also attempted at low-velocity conditions. Radiation modeled using an equilibrium assumption with the NEQAIR code compares favorably to measured radiation under some, but not all, conditions.
C1 [Cruden, Brett A.; Prabhu, Dinesh; Martinez, Ramon] NASA, ERC Inc, Ames Res Ctr, Aerothermodynam Branch, Moffett Field, CA 94035 USA.
RP Cruden, BA (reprint author), NASA, ERC Inc, Ames Res Ctr, Aerothermodynam Branch, Mail Stop 230-3, Moffett Field, CA 94035 USA.
EM Brett.A.Cruden@nasa.gov
NR 20
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U1 0
U2 3
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD NOV-DEC
PY 2012
VL 49
IS 6
BP 1069
EP 1079
DI 10.2514/1.A32204
PG 11
WC Engineering, Aerospace
SC Engineering
GA 064NS
UT WOS:000313082900011
ER
PT J
AU Yap, KC
Macias, J
Kaouk, M
Gafka, TL
Kerr, JH
AF Yap, Keng C.
Macias, Jesus
Kaouk, Mohamed
Gafka, Tammy L.
Kerr, Justin H.
TI Structural Health Monitoring and Risk Management of a Reusable Launch
Vehicle
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 19th AIAA/ASME/AHS Adaptive Structures Conference
CY APR 04-07, 2011
CL Denver, CO
SP AIAA, ASME, AHS
ID RANK PERTURBATION-THEORY
AB A structural-health-monitoring system can contribute to the risk management of a structure operating under hazardous conditions. An example is the wing leading-edge impact-detection system that monitors the debris hazards to the Space Shuttle Orbiter's reinforced carbon carbon panels. Since return to flight after the Columbia accident, the system was developed and subsequently deployed on board the orbiter to detect ascent and on-orbit debris impacts, so as to support the assessment of wing leading edge structural integrity before orbiter reentry. As structural health monitoring is inherently an inverse problem, the analyses involved, including those performed for this system, tend to be associated with significant uncertainty. The use of probabilistic approaches to handle the uncertainty has resulted in the successful implementation of many development and application milestones.
C1 [Yap, Keng C.] Boeing Space Explorat, Loads & Dynam, Boeing Def Space & Secur, Houston, TX 77059 USA.
[Macias, Jesus] United Space Alliance, Vehicle & Syst Anal, USA Orbiter Element, Houston, TX 77058 USA.
[Kaouk, Mohamed] NASA, Struct & Dynam ES6, NASA JSC, Houston, TX 77058 USA.
[Kerr, Justin H.] NASA, Space Shuttle Orbiter Project Off MV6, NASA JSC, Houston, TX 77058 USA.
RP Yap, KC (reprint author), Boeing Space Explorat, Loads & Dynam, Boeing Def Space & Secur, Houston, TX 77059 USA.
EM Keng.C.Yap@Boeing.com; Jesus.Macias@USA-SpaceOps.com;
Mohamed.Kaouk@NASA.com; Tammy.L.Gafka@NASA.com; Justin.H.Kerr@NASA.gov
NR 40
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U2 9
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD NOV-DEC
PY 2012
VL 49
IS 6
BP 1099
EP 1108
DI 10.2514/1.A32156
PG 10
WC Engineering, Aerospace
SC Engineering
GA 064NS
UT WOS:000313082900014
ER
PT J
AU Schuerger, AC
Golden, DC
Ming, DW
AF Schuerger, Andrew C.
Golden, D. C.
Ming, Doug W.
TI Biotoxicity of Mars soils: 1. Dry deposition of analog soils on
microbial colonies and survival under Martian conditions
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Biotoxic soils; Mars geochemistry; Biocidal soils; Regolith; Exobiology
ID PHOENIX LANDING SITE; X-RAY SPECTROMETER; SPACECRAFT SURFACES; GUSEV
CRATER; MOSSBAUER SPECTROMETER; CHEMICAL-COMPOSITION; TERRESTRIAL
ANALOGS; BACILLUS-SUBTILIS; PATHFINDER SITE; SPIRIT ROVER
AB Six Mars analog soils were created to simulate a range of potentially biotoxic geochemistries relevant to the survival of terrestrial microorganisms on Mars, and included basalt-only (non-toxic control), salt, acidic, alkaline, aeolian, and perchlorate rich geochemistries. Experiments were designed to simulate the dry-deposition of Mars soils onto spacecraft surfaces during an active descent landing scenario with propellant engines. Six eubacteria were initially tested for tolerance to desiccation, and the spore-former Bacillus subtilis HA101 and non-spore former Enterococcus faecalis ATCC 29212 were identified to be strongly resistant (HA101) and moderately resistant (29212) to desiccation at 24 degrees C. Furthermore, tests with B. subtilis and E. faecalis demonstrated that at least 1 mm of Mars analog soil was required to fully attenuate the biocidal effects of a simulated Mars-normal equatorial UV flux. Biotoxicity experiments were conducted under simulated Martian conditions of 6.9 mbar, - 10 degrees C, CO2-enriched anoxic atmosphere, and a simulated equatorial solar spectrum (200-1100 nm) with an optical depth of 0.1. For B. subtilis, the six analog soils were found, in general, to be of low biotoxicity with only the high salt and acidic soils exhibiting the capacity to inactivate a moderate number of spores ( < 1 log reductions) exposed 7 days to the soils under simulated Martian conditions. In contrast, the overall response of E. faecalis to the analog soils was more dramatic with between two and three orders of magnitude reductions in viable cells for most soils, and between six and seven orders of magnitude reductions observed for the high-salt soil. Results suggest that Mars soils are likely not to be overtly biotoxic to terrestrial microorganisms, and suggest that the soil geochemistries on Mars will not preclude the habitability of the Martian surface. (C) 2012 Elsevier Ltd. All rights reserved,
C1 [Schuerger, Andrew C.] Univ Florida, Dept Plant Pathol, Space Life Sci Lab, Kennedy Space Ctr, FL 32899 USA.
[Golden, D. C.] ESCG, Houston, TX 77058 USA.
[Ming, Doug W.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Off, Mail Code 7X, Houston, TX 77058 USA.
RP Schuerger, AC (reprint author), Univ Florida, Dept Plant Pathol, Space Life Sci Lab, Bldg M6-1025, Kennedy Space Ctr, FL 32899 USA.
EM schuerg@ufl.edu; d.c.golden@nasa.gov; douglas.w.ming@nasa.gov
FU Planetary Protection grant [NNX08AQ81A]
FX The research was supported by a Planetary Protection grant (NNX08AQ81A).
NR 60
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U1 2
U2 28
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 NOV
PY 2012
VL 72
IS 1
SI SI
BP 91
EP 101
DI 10.1016/j.pss.2012.07.026
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 058DZ
UT WOS:000312615600010
ER
PT J
AU Ciufolini, I
Paolozzi, A
Pavlis, E
Ries, J
Gurzadyan, V
Koenig, R
Matzner, R
Penrose, R
Sindoni, G
AF Ciufolini, Ignazio
Paolozzi, Antonio
Pavlis, Erricos
Ries, John
Gurzadyan, Vahe
Koenig, Rolf
Matzner, Richard
Penrose, Roger
Sindoni, Giampiero
TI Testing General Relativity and gravitational physics using the LARES
satellite
SO EUROPEAN PHYSICAL JOURNAL PLUS
LA English
DT Article
ID ACCELERATING UNIVERSE; DARK ENERGY; SUPERNOVAE; LAGEOS; ORBIT;
CONFIRMATION; GRAVITY; MOTION; SPACE; DRAG
AB The discovery of the accelerating expansion of the Universe, thought to be driven by a mysterious form of "dark energy" constituting most of the Universe, has further revived the interest in testing Einstein's theory of General Relativity. At the very foundation of Einstein's theory is the geodesic motion of a small, structureless test-particle. Depending on the physical context, a star, planet or satellite can behave very nearly like a test-particle, so geodesic motion is used to calculate the advance of the perihelion of a planet's orbit, the dynamics of a binary pulsar system and of an Earth-orbiting satellite. Verifying geodesic motion is then a test of paramount importance to General Relativity and other theories of fundamental physics. On the basis of the first few months of observations of the recently launched satellite LARES, its orbit shows the best agreement of any satellite with the test-particle motion predicted by General Relativity. That is, after modelling its known non-gravitational perturbations, the LARES orbit shows the smallest deviations from geodesic motion of any artificial satellite: its residual mean acceleration away from geodesic motion is less than 0.5 x 10(-12) m/s(2). LARES-type satellites can thus be used for accurate measurements and for tests of gravitational and fundamental physics. Already with only a few months of observation, LARES provides smaller scatter in the determination of several low-degree geopotential coefficients (Earth gravitational deviations from sphericity) than available from observations of any other satellite or combination of satellites.
C1 [Ciufolini, Ignazio] Univ Salento, Dipartimento Ingn Innovaz, Lecce, Italy.
[Ciufolini, Ignazio] Ist Nazl Fis Nucl, I-73100 Lecce, Italy.
[Paolozzi, Antonio; Sindoni, Giampiero] Univ Roma La Sapienza, Scuola Ingn Aerosp, Rome, Italy.
[Paolozzi, Antonio; Sindoni, Giampiero] Univ Roma La Sapienza, DIAEE, Rome, Italy.
[Pavlis, Erricos] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Ries, John] Univ Texas Austin, Ctr Space Res, Austin, TX 78712 USA.
[Gurzadyan, Vahe] Alikhanian Natl Lab, Ctr Cosmol & Astrophys, Yerevan, Armenia.
[Koenig, Rolf] GFZ German Res Ctr Geosci, Helmholtz Ctr Potsdam, Potsdam, Germany.
[Matzner, Richard] Univ Texas Austin, Ctr Relat, Austin, TX 78712 USA.
[Penrose, Roger] Univ Oxford, Math Inst, Oxford OX1 2JD, England.
RP Ciufolini, I (reprint author), Univ Salento, Dipartimento Ingn Innovaz, Lecce, Italy.
EM ignazio.ciufolini@gmail.com
FU Italian Space Agency [I/043/08/0, I/043/08/1]; NASA [NNG06DA07C,
NNX09AU86G]
FX The authors gratefully acknowledge the International Laser Ranging
Service for providing high-quality laser ranging tracking of the LARES
satellites. I. Ciufolini and A. Paolozzi gratefully acknowledge the
support of the Italian Space Agency, Grants I/043/08/0 and I/043/08/1,
J.C. Ries the support of NASA Contract NNG06DA07C, and E. C. Pavlis and
R. A. Matzner the support of NASA Grant NNX09AU86G.
NR 34
TC 38
Z9 38
U1 0
U2 6
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 2190-5444
J9 EUR PHYS J PLUS
JI Eur. Phys. J. Plus
PD NOV
PY 2012
VL 127
IS 11
AR 133
DI 10.1140/epjp/i2012-12133-8
PG 7
WC Physics, Multidisciplinary
SC Physics
GA 056ZU
UT WOS:000312532100002
ER
PT J
AU Reddy, V
Le Corre, L
O'Brien, DP
Nathues, A
Cloutis, EA
Durda, DD
Bottke, WF
Bhatt, MU
Nesvorny, D
Buczkowski, D
Scully, JEC
Palmer, EM
Sierks, H
Mann, PJ
Becker, KJ
Beck, AW
Mittlefehldt, D
Li, JY
Gaskell, R
Russell, CT
Gaffey, MJ
McSween, HY
McCord, TB
Combe, JP
Blewett, D
AF Reddy, Vishnu
Le Corre, Lucille
O'Brien, David P.
Nathues, Andreas
Cloutis, Edward A.
Durda, Daniel D.
Bottke, William F.
Bhatt, Megha U.
Nesvorny, David
Buczkowski, Debra
Scully, Jennifer E. C.
Palmer, Elizabeth M.
Sierks, Holger
Mann, Paul J.
Becker, Kris J.
Beck, Andrew W.
Mittlefehldt, David
Li, Jian-Yang
Gaskell, Robert
Russell, Christopher T.
Gaffey, Michael J.
McSween, Harry Y.
McCord, Thomas B.
Combe, Jean-Philippe
Blewett, David
TI Delivery of dark material to Vesta via carbonaceous chondritic impacts
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Asteroids, Composition; Mineralogy; Spectroscopy
ID ASTEROID 4 VESTA; SOLAR-SYSTEM; EXPLOSIVE ERUPTIONS; PARENT BODY;
ORIGIN; SURFACE; HETEROGENEITY; MINERALOGY; 4-VESTA; CLASTS
AB NASA's Dawn spacecraft observations of Asteroid (4) Vesta reveal a surface with the highest albedo and color variation of any asteroid we have observed so far. Terrains rich in low albedo dark material (DM) have been identified using Dawn Framing Camera (FC) 0.75 mu m filter images in several geologic settings: associated with impact craters (in the ejecta blanket material and/or on the crater walls and rims); as flow-like deposits or rays commonly associated with topographic highs; and as dark spots (likely secondary impacts) nearby impact craters. This DM could be a relic of ancient volcanic activity or exogenic in origin. We report that the majority of the spectra of DM are similar to carbonaceous chondrite meteorites mixed with materials indigenous to Vesta. Using high-resolution seven color images we compared DM color properties (albedo, band depth) with laboratory measurements of possible analog materials. Band depth and albedo of DM are identical to those of carbonaceous chondrite xenolith-rich howardite Mt. Pratt (PRA) 04401: Laboratory mixtures of Murchison CM2 carbonaceous chondrite and basaltic eucrite Millbillillie also show band depth and albedo affinity to DM. Modeling of carbonaceous chondrite abundance in DM (1-6 vol.%) is consistent with howardite meteorites. We find no evidence for large-scale volcanism (exposed dikes/pyroclastic falls) as the source of DM. Our modeling efforts using impact crater scaling laws and numerical models of ejecta reaccretion suggest the delivery and emplacement of this DM on Vesta during the formation of the similar to 400 km Veneneia basin by a low-velocity (<2 km/s) carbonaceous impactor. This discovery is important because it strengthens the long-held idea that primitive bodies are the source of carbon and probably volatiles in the early Solar System. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Reddy, Vishnu; Le Corre, Lucille; Nathues, Andreas; Bhatt, Megha U.; Sierks, Holger] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Reddy, Vishnu; Gaffey, Michael J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58201 USA.
[O'Brien, David P.; Gaskell, Robert] Planetary Sci Inst, Tucson, AZ USA.
[Cloutis, Edward A.; Mann, Paul J.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada.
[Durda, Daniel D.; Bottke, William F.; Nesvorny, David] SW Res Inst, Boulder, CO USA.
[Buczkowski, Debra; Blewett, David] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Scully, Jennifer E. C.; Palmer, Elizabeth M.; Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Becker, Kris J.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Beck, Andrew W.] Smithsonian Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC USA.
[Mittlefehldt, David] NASA Johnson Space Ctr, Astromat Res Off, Houston, TX USA.
[Li, Jian-Yang] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[McSween, Harry Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN USA.
[McCord, Thomas B.; Combe, Jean-Philippe] Bear Fight Inst, Winthrop, WA USA.
RP Reddy, V (reprint author), Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
EM reddy@mps.mpg.de
RI Blewett, David/I-4904-2012; Beck, Andrew/J-7215-2015;
OI Le Corre, Lucille/0000-0003-0349-7932; Blewett,
David/0000-0002-9241-6358; Beck, Andrew/0000-0003-4455-2299; Reddy,
Vishnu/0000-0002-7743-3491
FU Max Planck Society; German Space Agency, DLR; Dawn at Vesta
Participating Scientist Program [NNX10AR22G]; CFI; MRIF; CSA; University
of Winnipeg
FX We thank the Dawn team for the development, cruise, orbital insertion,
and operations of the Dawn spacecraft at Vesta. The Framing Camera
project is financially supported by the Max Planck Society and the
German Space Agency, DLR. We also thank the Dawn at Vesta Participating
Scientist Program (NNX10AR22G) for funding the research. Dawn data is
archived with the NASA Planetary Data System. EAC thanks CFI, MRIF, CSA,
and the University of Winnipeg for support of this project and the
necessary infrastructure. We thank Paul Buchanan (Kilgore College) and
Tom Burbine (Mt Holyoke College) for their helpful reviews to improve
the manuscript. VR would like to thank Richard Binzel (MIT), Rhiannon
Mayne (TCU), and Guneshwar Thangjam (MPS) for their helpful suggestions
to improve the manuscript.
NR 61
TC 89
Z9 90
U1 2
U2 23
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 NOV-DEC
PY 2012
VL 221
IS 2
BP 544
EP 559
DI 10.1016/j.icarus.2012.08.011
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 055RL
UT WOS:000312434300007
ER
PT J
AU Fletcher, LN
Hesman, BE
Achterberg, RK
Irwin, PGJ
Bjoraker, G
Gorius, N
Hurley, J
Sinclair, J
Orton, GS
Legarreta, J
Garcia-Melendo, E
Sanchez-Lavega, A
Read, PL
Simon-Miller, AA
Flasar, FM
AF Fletcher, Leigh N.
Hesman, B. E.
Achterberg, R. K.
Irwin, P. G. J.
Bjoraker, G.
Gorius, N.
Hurley, J.
Sinclair, J.
Orton, G. S.
Legarreta, J.
Garcia-Melendo, E.
Sanchez-Lavega, A.
Read, P. L.
Simon-Miller, A. A.
Flasar, F. M.
TI The origin and evolution of Saturn's 2011-2012 stratospheric vortex
SO ICARUS
LA English
DT Article
DE Saturn; Atmospheres, Composition; Atmospheres, Structure
ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; GREAT WHITE SPOT; INFRARED
MEASUREMENTS; UPPER TROPOSPHERE; THERMAL STRUCTURE; MOIST CONVECTION;
LINE PARAMETERS; OUTER PLANETS; ATMOSPHERE; TEMPERATURES
AB The planet-encircling springtime storm in Saturn's troposphere (December 2010-July 2011, Fletcher, L.N. et al. [2011]. Science 332, 1413-1414; Sanchez-Lavega, A. et al. [2011]. Nature 475, 71-74; Fischer, G. et al. [2011]. Nature 475, 75-77) produced dramatic perturbations to stratospheric temperatures, winds and composition at mbar pressures that persisted long after the tropospheric disturbance had abated. Thermal infrared (IR) spectroscopy from the Cassini Composite Infrared Spectrometer (CIRS), supported by ground-based IR imaging from the VISIR instrument on the Very Large Telescope and the MIRSI instrument on NASA's IRTF, is used to track the evolution of a large, hot stratospheric anticyclone between January 2011 and March 2012. The evolutionary sequence can be divided into three phases: (I) the formation and intensification of two distinct warm airmasses near 0.5 mbar between 25 and 35 degrees N (B1 and B2) between January-April 2011, moving westward with different zonal velocities, B1 residing directly above the convective tropospheric storm head; (II) the merging of the warm airmasses to form the large single 'stratospheric beacon' near 40 degrees N (BO) between April and June 2011, disassociated from the storm head and at a higher pressure (2 mbar) than the original beacons, a downward shift of 1.4 scale heights (approximately 85 km) post-merger; and (III) the mature phase characterised by slow cooling (0.11 +/- 0.01 K/day) and longitudinal shrinkage of the anticyclone since July 2011. Peak temperatures of 221.6 +/- 1.4 K at 2 mbar were measured on May 5th 2011 immediately after the merger, some 80 K warmer than the quiescent surroundings. From July 2011 to the time of writing, BO remained as a long-lived stable stratospheric phenomenon at 2 mbar, moving west with a near-constant velocity of 2.70 +/- 0.04 deg/day (-24.5 +/- 0.4 m/s at 40 degrees N relative to System III longitudes). No perturbations to visible clouds and hazes were detected during this period.
With no direct tracers of motion in the stratosphere, we use thermal windshear calculations to estimate clockwise peripheral velocities of 200-400 m/s at 2 mbar around BO. The peripheral velocities of the two original airmasses were smaller (70-140 m/s). In August 2011, the size of the vortex as defined by the peripheral collar was 65 degrees longitude (50,000 km in diameter) and 25 degrees latitude. Stratospheric acetylene (C2H2) was uniformly enhanced by a factor of three within the vortex, whereas ethane (C2H6) remained unaffected. The passage of BO generated a new band of warm stratospheric emission at 0.5 mbar at its northern edge, and there are hints of warm stratospheric structures associated with the beacons at higher altitudes (p < 0.1 mbar) than can be reliably observed by CIRS nadir spectroscopy. Analysis of the zonal windshear suggests that Rossby wave perturbations from the convective storm could have propagated vertically into the stratosphere at this point in Saturn's seasonal cycle, one possible source of energy for the formation of these stratospheric anticyclones. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Fletcher, Leigh N.; Irwin, P. G. J.; Hurley, J.; Sinclair, J.; Read, P. L.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England.
[Hesman, B. E.; Achterberg, R. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Bjoraker, G.; Simon-Miller, A. A.; Flasar, F. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gorius, N.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Legarreta, J.] Univ Pas Vasco UPV EHU, Dept Ingn Sistemas & Automt, EUITI, Bilbao, Spain.
[Garcia-Melendo, E.] Esteve Duran Observ Fdn, Seva 08553, Spain.
[Garcia-Melendo, E.] Inst Cincies Espai CSIC IEEC, Fac Cincies, E-08193 Bellaterra, Spain.
[Sanchez-Lavega, A.] Univ Pas Vasco, ETS Ingn, Dept Fs Aplicada, Bilbao 48013, Spain.
RP Fletcher, LN (reprint author), Univ Oxford, Dept Phys, Clarendon Lab, Parks Rd, Oxford OX1 3PU, England.
EM fletcher@atm.ox.ac.uk
RI Flasar, F Michael/C-8509-2012; Fletcher, Leigh/D-6093-2011; Simon,
Amy/C-8020-2012;
OI Fletcher, Leigh/0000-0001-5834-9588; Irwin, Patrick/0000-0002-6772-384X;
Simon, Amy/0000-0003-4641-6186; LEGARRETA ETXAGIBEL, JON
JOSU/0000-0001-6501-2705; Sanchez-Lavega, Agustin/0000-0001-7355-1522
FU Glasstone Science Fellowship at the University of Oxford; NASA/Infrared
Telescope Facility [NCC 5-538]; Science and Technology Facilities
Council (STFC); NASA Cassini Data Analysis Participating Scientists
(CDAPS) Program [NNX12AC24G]; NASA; Spanish MICIIN [AYA2009-10701];
FEDER; Grupos Gobierno Vasco [IT-464-07]; Universidad Pas Vasco UPV/EHU
[UFI11/55]; [386.C-0096(A)]
FX Fletcher was supported by a Glasstone Science Fellowship at the
University of Oxford. We thank the members of the Cassini/CIRS
investigation team who have assisted in the design of the imaging
sequences, instrument commands and other vital operational tasks, and
the Ground Systems Operations for the Cassini Project. We wish to thank
the directors and staff of the ESO Very Large Telescope and the NASA
Infrared Telescope Facility for their assistance with the execution of
these observations. This investigation was partially based on
observations acquired at the Paranal UT3/Melipal Observatory under ID
386.C-0096 and 287.C-5032. Program 386.C-0096(A) had been awarded time
to study Saturn's slow seasonal evolution in April 2011, but we are
grateful to ESO for granting our request to obtain these images of
Saturn's storm as soon as the planet became available after solar
conjunction (which occurred in October 2010).; We are grateful to the
operators at the NASA/Infrared Telescope Facility (operated by the
University of Hawaii under Cooperative Agreement No. NCC 5-538 with the
National Aeronautics and Space Administration, Science Mission
Directorate, Planetary Astronomy Program). The UK authors acknowledge
the support of the Science and Technology Facilities Council (STFC).
B.E.H., G.L.B., and R.K.A. were supported by the NASA Cassini Data
Analysis Participating Scientists (CDAPS) Program Grant No. NNX12AC24G.
GSO is supported by Grants from NASA to the Jet Propulsion Laboratory,
California Institute of Technology. J.L., E.G.M. and A.S.L. were
supported by the Spanish MICIIN Project AYA2009-10701 with FEDER funds,
by Grupos Gobierno Vasco IT-464-07 and by Universidad Pas Vasco UPV/EHU
through program UFI11/55. We thank T. Greathouse and J. Moses for
helpful discussions of the beacon results.
NR 70
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U1 0
U2 23
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 NOV-DEC
PY 2012
VL 221
IS 2
BP 560
EP 586
DI 10.1016/j.icarus.2012.08.024
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 055RL
UT WOS:000312434300008
ER
PT J
AU Reddy, V
Le Corre, L
Hicks, M
Lawrence, K
Buratti, BJ
Abell, PA
Gaffey, MJ
Hardersen, PS
AF Reddy, Vishnu
Le Corre, Lucille
Hicks, Michael
Lawrence, Kenneth
Buratti, Bonnie J.
Abell, Paul A.
Gaffey, Michael J.
Hardersen, Paul S.
TI Composition of near-Earth Asteroid 2008 EV5: Potential target for
robotic and human exploration
SO ICARUS
LA English
DT Article
DE Asteroids, Surfaces; Spectroscopy; Asteroids, Composition; Radar
observations
ID SPECTROGRAPH; POPULATION; RESOLUTION; TELESCOPE; CHONDRITE; ALBEDO;
METAL; SPEX
AB We observed Potentially Hazardous Asteroid (PHA) 2008 EV5 in the visible (0.30-0.92 mu m) and near-IR (0.75-2.5 mu m) wavelengths to determine its surface composition. This asteroid is especially interesting because it is a potential target for two sample return mission proposals (Marco Polo-R and Hayabusa-2) and human exploration due to its low delta-v for rendezvous. The spectrum of 2008 EV5 is essentially featureless with exception of a weak 0.48-mu m spin-forbidden Fe3+ absorption band. The spectrum also has an overall blue slope. The albedo of 2008 EV5 remains uncertain with a lower limit at 0.05 and a higher end at 0.20 based on thermal modeling. The Busch et al. (Busch et al. [2011]. Icarus 212, 649-660) albedo estimate of 0.12 +/- 0.04 is consistent with our thermal modeling results. The albedo and composition of 2008 EV5 are also consistent with a C-type taxonomic classification (Somers, J.M., Hicks, M.D., Lawrence, K.J. [2008]. Bull. Am. Astron. Soc. 40, 440). The best spectral match is with CI carbonaceous chondrites similar to Orgueil, which also have a weak 0.48-mu m feature and an overall blue slope. This 0.48-mu m feature is also seen in the spectrum of magnetite. The albedo of Cl chondrites is at the lower limit of our estimated range for the albedo of 2008 EV5. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Reddy, Vishnu; Le Corre, Lucille] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany.
[Reddy, Vishnu; Gaffey, Michael J.; Hardersen, Paul S.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA.
[Hicks, Michael; Lawrence, Kenneth; Buratti, Bonnie J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Abell, Paul A.] NASA Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA.
RP Reddy, V (reprint author), Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany.
EM reddy@mps.mpg.de
RI Hardersen, Paul/N-9343-2014;
OI Hardersen, Paul/0000-0002-0440-9095; Reddy, Vishnu/0000-0002-7743-3491;
Le Corre, Lucille/0000-0003-0349-7932
FU NASA NEOO Program Grant [NNX07AL29G]; NASA Planetary Geology and
Geophysics Grant [NNX07AP73G]; IRTF TAC
FX This research was supported by NASA NEOO Program Grant NNX07AL29G, and
NASA Planetary Geology and Geophysics Grant NNX07AP73G. V.R. would like
to thank Javier Licandro for his helpful comments. We thank the IRTF TAC
for awarding time to this project, and to the IRTF TOs and MKSS staff
for their support.
NR 26
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U1 0
U2 11
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD NOV-DEC
PY 2012
VL 221
IS 2
BP 678
EP 681
DI 10.1016/j.icarus.2012.08.035
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 055RL
UT WOS:000312434300018
ER
PT J
AU Ore, CMD
Cruikshank, DP
Clark, RN
AF Ore, Cristina Morea Dalle
Cruikshank, Dale P.
Clark, Roger N.
TI Infrared spectroscopic characterization of the low-albedo materials on
Iapetus
SO ICARUS
LA English
DT Article
DE Iapetus; Satellites, Composition; Satellites, Surfaces; Saturn,
Satellites; Spectroscopy
ID SATURNS MOON PHOEBE; MAPPING SPECTROMETER; IRREGULAR SATELLITES;
SURFACE-COMPOSITION; DARK MATERIAL; SOLAR-SYSTEM; CASSINI VIMS; MU-M;
HYPERION; SPECTRA
AB Iapetus, one of the large satellites of Saturn, has been studied over the centuries for its signature brightness contrast, light on one side and dark on the opposite. It has recently been suggested that the dark material is a combination of native and exogenous materials with distinct histories. We present an analysis of parts of the Cassini Regio, the darkest region on the leading hemisphere of Iapetus, focusing on the hydrocarbon signature with a view to detect and investigate differences in the material(s). We find variations in the hydrocarbon bands with geographic location, one type predominantly located on the leading hemisphere. A comparison with the equivalent spectral features on Phoebe and -Iyperion reveals a predictable resemblance between the leading hemisphere material and Phoebe and an unexpected likeness between Hyperion's darkest material and Iapetus trailing hemisphere surface. An analysis of the slope in the visible part of the spectrum is strongly affected by a rise in the continuum (similar to 0.35-0.65 mu m) attributed to Rayleigh scattering from nano-size particles on the surface. The continuum rise varies in strength with the albedo and H2O ice content, and when it is properly accounted for, the overall slope in all the identified spectral units is the same over the interval 0.35-2.3 mu m, independent of albedo or ice abundance. The interpretation of current and previous results offers two different scenarios illustrated by the presence of one vs. two dark materials distributed over the Iapetus surface. We describe the scenarios and their implications. The appearance of the aromatic and aliphatic absorption bands together in their measured relative strengths makes this spectral signature unique, and thus enables the comparison among the three satellites. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Ore, Cristina Morea Dalle; Cruikshank, Dale P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ore, Cristina Morea Dalle] SETI Inst, Mountain View, CA 94043 USA.
[Clark, Roger N.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA.
RP Ore, CMD (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA.
EM Cristina.M.DalleOre@nasa.gov
FU Cassini Science Team funding; NASA [NNX11AN90G]
FX We thank Drs. J.A. Mosher and Bonnie J. Buratti for making available the
Phoebe mosaic. D.P.C. acknowledges support from Cassini Science Team
funding.; C.D.O. acknowledges support from NASA Grant NNX11AN90G.
NR 36
TC 5
Z9 5
U1 2
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 NOV-DEC
PY 2012
VL 221
IS 2
BP 735
EP 743
DI 10.1016/j.icarus.2012.09.010
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 055RL
UT WOS:000312434300023
ER
PT J
AU Sotin, C
Lawrence, KJ
Reinhardt, B
Barnes, JW
Brown, RH
Hayes, AG
Le Mouelic, S
Rodriguez, S
Soderblom, JM
Soderblom, LA
Baines, KH
Buratti, BJ
Clark, RN
Jaumann, R
Nicholson, PD
Stephan, K
AF Sotin, C.
Lawrence, K. J.
Reinhardt, B.
Barnes, J. W.
Brown, R. H.
Hayes, A. G.
Le Mouelic, S.
Rodriguez, S.
Soderblom, J. M.
Soderblom, L. A.
Baines, K. H.
Buratti, B. J.
Clark, R. N.
Jaumann, R.
Nicholson, P. D.
Stephan, K.
TI Observations of Titan's Northern lakes at 5 mu m: Implications for the
organic cycle and geology
SO ICARUS
LA English
DT Article
DE Titan; Titan hydrology; Titan atmosphere; Organic chemistry; Exobiology
ID HUYGENS LANDING SITE; HYDROCARBON LAKES; METHANE CYCLE; CASSINI VIMS;
ATMOSPHERE; SURFACE; RADAR; ETHANE; MODEL; HAZE
AB Since Titan entered Northern spring in August 2009, the North Pole has been illuminated allowing observations at optical wavelengths. On June 5, 2010 the Visual and Infrared Mapping Spectrometer (VIMS) onboard the Cassini spacecraft observed the Northern Pole area with a pixel size from 3 to 7 km. Since, as we demonstrate, little of the solar flux at 5 pm is scattered by the atmosphere, these observations were obtained at relatively large incidence angles and allowed us to build a mosaic covering an area of more than 500,000 km(2) that overlaps and complements observations made by the Synthetic Aperture Radar (SAR) in 2007. We find that there is an excellent correlation between the shape of the radar dark area, known as Ligeia Mare and the VIMS 5-mu m dark unit. Matching most of the radar shoreline, the 2010 VIMS observations suggest that the 125,000-km(2) surface area of Ligeia Mare measured by RADAR in 2007 has not significantly changed. The VIMS observations complement the radar observations to the west of Ligeia Mare and suggest that Ligeia Mare is connected to Kraken Mare by either a diffuse network similar to a swamp area, or by well-defined, sub-pixel rivers. Considering the results of recent evaporation models of methane, our preferred interpretation of the relative constancy in surface area of Ligeia is that it is principally composed of ethane although we cannot rule out the possibility that methane evaporation is balanced with replenishment by either precipitation or underground seepage. There is also strong correlation between the location of the small radar lakes and the small VIMS 5-mu m dark patches. The geographic location of the small lakes are within a VIMS pixel of the SAR location, suggesting that the non-synchronous component of Titan's spin rate, if it exists, was less than 2.3 x 10(-4) deg/day between 2007 and 2010 in agreement with the recent T64 radar observations. These observations question the existence of non-synchronous rotation. Two radar-bright features appear dark at 5-mu m. The simplest interpretation is that these are very shallow lakes, less than one meter deep. Three new small lakes, named Freeman, Cardiel, and Towada by the IAU, are found outside of the area mapped with the SAR. A single-scattering model describing reflection of sunlight at 5-mu m suggests that the lake surface is mirror-like and that the albedo of the solid surfaces surrounding the lakes is about 8%. These observations together with information of the haze aerosols allow us to show that Titan's lakes, atmospheric ethane and aerosol haze are smaller carbon reservoirs than Titan's sand dunes and atmospheric methane. A simple model involving an outburst of methane a few hundreds of Myr ago followed by the dissociation of methane in the atmosphere leading to the formation of the haze particles that constitute the dune fields would be consistent with both the present observations and recent measurements of isotopic ratios in atmospheric methane (Mandt, K.E. et al. [2012]. Astrophys. J. 749(160), 14). (C) 2012 Elsevier Inc. All rights reserved.
C1 [Sotin, C.; Lawrence, K. J.; Reinhardt, B.; Hayes, A. G.; Baines, K. H.; Buratti, B. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Barnes, J. W.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA.
[Brown, R. H.; Soderblom, J. M.] Univ Arizona, Lunar & Planetary Lab, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Le Mouelic, S.] Univ Nantes, CNRS, Lab Planetol & Geodynam, UMR 6112, F-44322 Nantes, France.
[Rodriguez, S.] Univ Paris 07, CNRS, CEA Saclay, DSM,IRFU,SAp,Lab AIM, F-75221 Paris 05, France.
[Soderblom, L. A.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Clark, R. N.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA.
[Jaumann, R.; Stephan, K.] Inst Planetary Res, DLR, D-12489 Berlin, Germany.
[Nicholson, P. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
RP Sotin, C (reprint author), CALTECH, Jet Prop Lab, M-S 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Christophe.sotin@jpl.nasa.gov
RI Barnes, Jason/B-1284-2009; Hayes, Alexander/P-2024-2014; Rodriguez,
Sebastien/H-5902-2016
OI Barnes, Jason/0000-0002-7755-3530; Hayes, Alexander/0000-0001-6397-2630;
Rodriguez, Sebastien/0000-0003-1219-0641
FU NASA Astrobiology Institute; JPL RTD program; NASA
FX We thank the VIMS Operations and Science Teams for their dedication in
implementing the observations. Reviews by Ellen Stofan and an anonymous
reviewer are acknowledged. CS acknowledges support by the NASA
Astrobiology Institute and the JPL R&TD program. This work has been
performed at the Jet Propulsion Laboratory, California Institute of
Technology under contract with NASA.
NR 64
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U1 1
U2 36
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 NOV-DEC
PY 2012
VL 221
IS 2
BP 768
EP 786
DI 10.1016/j.icarus.2012.08.017
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 055RL
UT WOS:000312434300026
ER
PT J
AU Johnson, PV
Hodyss, R
Chernow, VF
Lipscomb, DM
Goguen, JD
AF Johnson, Paul V.
Hodyss, Robert
Chernow, Victoria F.
Lipscomb, Dawn M.
Goguen, Jay D.
TI Ultraviolet photolysis of amino acids on the surface of icy Solar System
bodies
SO ICARUS
LA English
DT Article
DE Ices; Ices, IR spectroscopy; Photochemistry; Exobiology; Satellites,
Surfaces
ID MONOCARBOXYLIC ACIDS; PHOTOCHEMISTRY; EUROPA; SPACE; ICES
AB The icy worlds of the outer Solar System are of significant astrobiological interests due, in large part, to the evidence of liquid water beneath the surfaces of a number of jovian and saturnian satellites. Many of these surfaces are subject to various levels of particle and photon radiation. If molecular compounds of biological origin are present in the surface ice layer (originating either in situ or delivered from a subsurface aqueous environment), can they be detected as evidence of biological activity, or do they decompose too rapidly in the surface radiation environment? We present a wavelength resolved study of the ultraviolet photolysis of glycine and phenylalanine to address this question. Studying these reactions at multiple discreet wavelengths distinguishes the present work from previous matrix isolation studies using hydrogen flow lamps and continuum sources by resolving the important contribution of photons with energies much lower than Lyman-alpha (121.6 nm). We find that although the half-lives of glycine and phenylalanine are essentially identical at 147 nm, they diverge at 206 nm and diverge significantly at 254 nm with glycine having longer half-lives at these longer wavelengths. Scaling the results to account for the wavelength dependent variation in solar irradiance shows that despite the reduction of photon energies in the 200-250 nm range, versus 147 nm, it is the longer wavelengths that will dominate the destruction of amino acids in icy surfaces. It seems unlikely that organics can survive long enough on the surface of an icy planetary body to be detected without being frequently replenished from a shielded source such as a subsurface ocean. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Johnson, Paul V.; Hodyss, Robert; Chernow, Victoria F.; Lipscomb, Dawn M.; Goguen, Jay D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Johnson, PV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 183-601, Pasadena, CA 91109 USA.
EM Paul.V.Johnson@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA); NASA's
Astrobiology: Exobiology and Evolutionary Biology program; NASA
Astrobiology Institute (Icy Worlds); NASA Undergraduate Research Program
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 (NASA). Funding from NASA's
Astrobiology: Exobiology and Evolutionary Biology program and the NASA
Astrobiology Institute (Icy Worlds) is gratefully acknowledged. VFC and
DML participated in this work as undergraduate interns sponsored by the
NASA Undergraduate Research Program. We would like to thank Dr. Arthur
L. Lane for his insights into the importance of monochromatic ice
photolysis studies. Finally, we thank two anonymous reviewers for their
constructive comments.
NR 28
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U1 4
U2 30
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 NOV-DEC
PY 2012
VL 221
IS 2
BP 800
EP 805
DI 10.1016/j.icarus.2012.09.005
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 055RL
UT WOS:000312434300028
ER
PT J
AU Morishima, R
Edgington, SG
Spilker, L
AF Morishima, Ryuji
Edgington, Scott G.
Spilker, Linda
TI Regolith grain sizes of Saturn's rings inferred from Cassini-CIRS
far-infrared spectra
SO ICARUS
LA English
DT Article
DE Saturn, Rings; Infrared observations; Radiative transfer; Regoliths
ID SELF-GRAVITY WAKES; MU-M; THERMAL OBSERVATIONS; REFLECTANCE SPECTRA;
MULTILAYER MODEL; MAIN RINGS; IN-SITU; SNOW; EMISSION; PHASE
AB We analyze far-infrared (10-650 cm(-1)) emissivity spectra of Saturn's main rings obtained by the Cassini Composite Infrared Spectrometer (CIRS). In modeling of the spectra, the single scattering albedos of regolith grains are calculated using the Mie theory, diffraction is removed with the delta-Eddington approximation, and the hemispherical emissivities of macroscopic free-floating ring particles are calculated using the Hapke's isotropic scattering model. Only pure crystalline water ice is considered and the size distribution of regolith grains is estimated. We find that good fits are obtained if the size distribution is broad ranging from 1 mu m to 1-10 cm with a power law index of similar to 3. This means that the largest regolith grains are comparable to the smallest free-floating particles in size and that the power law indices for both free-floating particles and regolith grains are similar to each other. The apparent relative abundance of small grains increases with decreasing solar phase angle (or increasing mean temperature). This trend is particularly strong for the C ring and is probably caused by eclipse cooling in Saturn's shadow, which relatively suppresses warming up of grains larger than the thermal skin depth (similar to 1 mm) under subsequent solar illumination. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Morishima, Ryuji; Edgington, Scott G.; 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.
RP Morishima, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Ryuji.Morishima@jpl.nasa.gov
FU NASA; NASA's Cassini Data Analysis Program
FX We are grateful to Bruce Hapke and an anonymous reviewer for their
thorough reviews. We thank Jeffrey Cuzzi, Matthew Hedman, John Spenser,
Deau Estelle, and Donald Jennings for fruitful discussions and helpful
comments on this work, and Stu Pilorz, Shawn Brooks, and Mark Showalter
for designing of CIRS observations. This research was carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under
contract with NASA. Government sponsorship acknowledged. This work was
also supported in part by NASA's Cassini Data Analysis Program.
NR 56
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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
EI 1090-2643
J9 ICARUS
JI Icarus
PD NOV-DEC
PY 2012
VL 221
IS 2
BP 888
EP 899
DI 10.1016/j.icarus.2012.09.012
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 055RL
UT WOS:000312434300036
ER
PT J
AU Cloutis, EA
Hudon, P
Hiroi, T
Gaffey, MJ
AF Cloutis, E. A.
Hudon, P.
Hiroi, T.
Gaffey, M. J.
TI Spectral reflectance properties of carbonaceous chondrites: 7. CK
chondrites
SO ICARUS
LA English
DT Article
DE Asteroids, Surfaces; Asteroids, Composition; Meteorites; Spectroscopy
ID THERMAL METAMORPHISM; ELEMENT ABUNDANCES; CV-CHONDRITES; METEORITE;
ASTEROIDS; OLIVINE; CLASSIFICATION; PLAGIOCLASE; INCLUSIONS; MINERALOGY
AB The reflectance spectra of 15 CK chondrites have been measured as part of an ongoing study of carbonaceous chondrite reflectance spectra. The available sample suite includes multiple grain sizes and samples with petrologic grades varying from CK4 to CK6. CK reflectance spectra are all characterized by an olivine-associated absorption band in the 1.05 mu m region. Compared to pure olivine, CK spectra are darker, have a more subdued olivine absorption band, and are often more blue-sloped. Reflectance at 0.56 mu m varies from 9.6% to 22.5%, and olivine band depth varies from 6.7% to 31.0%, for powder; that include the finest fraction. With increasing grain size, and exclusion of the finest fraction, CK spectra become darker and more blue sloped, while the olivine absorption band initially becomes deeper and then shallower. The presence of calcium-aluminum inclusions (CAIs), whose abundance varies widely in CKs, does not normally lead to the appearance of a well-defined absorption band in the 2.1 mu m region, although the overall blue slope of many CKs is likely attributable to Fe-bearing spinel in CK CAIs. The only consistent spectral feature that relates to metamorphic grade is that CK6 spectra have uniformly deeper olivine absorption band than CK4-5.5 spectra. This could be related to various factors such as loss/aggregation of opaques that may accompany metamorphism. Comparison of CV and thermally metamorphosed carbonaceous chondrite to CK spectra suggests that metamorphism to between similar to 1000 and 1200 degrees C is required for CV spectra to match CK spectra; CV spectra are uniformly darker and have shallower olivine absorption bands than CK spectra. (C) 2012 Elsevier :nc. All rights reserved.
C1 [Cloutis, E. A.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada.
[Hudon, P.] NASA Johnson Space Ctr, Astromat Res & Explorat Sci Off, Mail Code KR, Houston, TX 77058 USA.
[Hiroi, T.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Gaffey, M. J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA.
RP Cloutis, EA (reprint author), Univ Winnipeg, Dept Geog, 515 Portage Ave, Winnipeg, MB R3B 2E9, Canada.
EM e.cloutis@uwinnipeg.ca; pierre.hudon@mcgill.ca;
takahiro_hiroi@brown.edu; gaffey@space.edu
FU NASA [NNG06GJ31G]; NSERC
FX We wish to thank the invaluable and generous assistance provided by many
individuals which made this study possible. In particular we thank the
US and Japanese Antarctic meteorite programs for recovering the majority
of the samples included in this study. The RELAB facility at Brown
University is a multi-user facility operated with support from NASA
Planetary Geology and Geophysics Grant NNG06GJ31G, whose support is
gratefully acknowledged. This study was supported by an NSERC Discovery
grant to EAC. We also wish to thank Alan Rubin and Beth Clark for their
cogent and valuable comments which improved the accuracy and readability
of this manuscript.
NR 92
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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 NOV-DEC
PY 2012
VL 221
IS 2
BP 911
EP 924
DI 10.1016/j.icarus.2012.09.017
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 055RL
UT WOS:000312434300038
ER
PT J
AU Heggy, E
Palmer, EM
Kofman, W
Clifford, SM
Righter, K
Herique, A
AF Heggy, Essam
Palmer, Elizabeth M.
Kofman, Wlodek
Clifford, Stephen M.
Righter, Kevin
Herique, Alain
TI Radar properties of comets: Parametric dielectric modeling of Comet
67P/Churyumov-Gerasimenko
SO ICARUS
LA English
DT Article
DE Comets, Composition; Comets, Dust; Ices; Radar observations;
Experimental techniques
ID SPACE-TELESCOPE OBSERVATIONS; NUCLEUS SOUNDING EXPERIMENT; DEEP IMPACT;
RADIOWAVE TRANSMISSION; INNER COMA; CONSERT; MARS; COMET-9P/TEMPEL-1;
PERMITTIVITY; FREQUENCIES
AB In 2014, the European Space Agency's Rosetta mission is scheduled to rendezvous with Comet 67P/Churyumov-Gerasimenko (Comet 67P). Rosetta's CONSERT experiment aims to explore the cometary nucleus' geophysical properties using radar tomography. The expected scientific return and inversion algorithms are mainly dependent on our understanding of the dielectric properties of the comet nucleus and how they vary with the spatial distribution of geophysical parameters. Using observations of Comets 9P/Tempel 1 and 81P/Wild 2 in combination with dielectric laboratory measurements of temperature, porosity, and dust-to-ice mass ratio dependencies for cometary analog material, we have constructed two hypothetical three-dimensional parametric dielectric models of Comet 67P's nucleus to assess different dielectric scenarios of the inner structure. Our models suggest that dust-to-ice mass ratios and porosity variations generate the most significant measurable dielectric contrast inside the comet nucleus, making it possible to explore the structural and compositional hypotheses of cometary nuclei. Surface dielectric variations, resulting from temperature changes induced by solar illumination of the comet's faces, have also been modeled and suggest that the real part of the dielectric constant varies from 1.9 to 3.0, hence changing the surface radar reflectivity. For CONSERT, this variation could be significant at low incidence angles, when the signal propagates through a length of dust mantle comparable to the wavelength. The overall modeled dielectric permittivity spatial and temporal variations are therefore consistent with the expected deep penetration of CONSERT's transmitted wave through the nucleus. It is also clear that changes in the physical properties of the nucleus induce sufficient variation in the dielectric properties of cometary material to allow their inversion from radar tomography. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Heggy, Essam] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
[Palmer, Elizabeth M.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
[Kofman, Wlodek; Herique, Alain] UJF Grenoble 1 CNRS INSU, Inst Planetol & Astrophys Grenoble IPAG UMR 5274, F-38041 Grenoble, France.
[Kofman, Wlodek] Polish Acad Sci, Space Res Ctr, PL-01237 Warsaw, Poland.
[Clifford, Stephen M.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Righter, Kevin] NASA Johnson Space Ctr, Mail Code KT, Houston, TX 77058 USA.
RP Heggy, E (reprint author), CALTECH, NASA Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 300-227, Pasadena, CA 91109 USA.
EM essam.heggy@jpl.nasa.gov; empalmer@ucla.edu;
wlodek.kofman@obs.ujf-grenoble.fr; clifford@lpi.usra.e-du;
kevin.righter-1@nasa.gov; alain.herique@obs.ujf-grenoble.fr
RI Heggy, Essam/E-8250-2013; Kofman, Wlodek/C-4556-2008; Herique,
Alain/E-7210-2017
OI Heggy, Essam/0000-0001-7476-2735; Herique, Alain/0000-0003-3699-883X
FU NASA Planetary Geology and Geophysics Program [NNXZ08AKA2G, NNG05GL11G];
French Space Agency (CNES); National Aeronautics and Space
Administration
FX The authors would like to thank Drs. Claudia Alexander and Artur
Chmielewski from the Jet Propulsion Laboratory and Prof. Christopher
Russell from UCLA for their helpful comments and discussions. We also
thank the Meteorite Working Group and NASA Johnson Space Center Curation
office for providing samples from the U.S. Antarctic Meteorite
Collection. This work was supported in part by NASA Planetary Geology
and Geophysics Program under Grants NNXZ08AKA2G and NNG05GL11G. The
authors would like to acknowledge the French Space Agency (CNES) for its
support to the part of this study performed in the Institut de
Planetologie et d'Astrophysique de Grenoble. This research was carried
out at the Jet Propulsion Laboratory, California institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 50
TC 24
Z9 24
U1 2
U2 10
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD NOV-DEC
PY 2012
VL 221
IS 2
BP 925
EP 939
DI 10.1016/j.icarus.2012.09.023
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 055RL
UT WOS:000312434300039
ER
PT J
AU Feofilov, AG
Kutepov, AA
Rezac, L
Smith, MD
AF Feofilov, A. G.
Kutepov, A. A.
Rezac, L.
Smith, M. D.
TI Extending MGS-TES temperature retrievals in the martian atmosphere up to
90 km: Retrieval approach and results
SO ICARUS
LA English
DT Article
DE Mars, Atmosphere; Atmospheres, Structure; Infrared observations;
Radiative transfer
ID THERMAL EMISSION SPECTROMETER; ACCELERATED LAMBDA ITERATION; MIDDLE
ATMOSPHERE; PLANETARY-ATMOSPHERES; LOWER THERMOSPHERE; ATOMIC OXYGEN;
RATE-CONSTANT; WATER-VAPOR; MARS; VARIABILITY
AB This paper describes a methodology for performing temperature retrievals in the martian atmosphere in the 60-90 km altitude range using spectrally integrated 15 mu m CO2 limb emissions measured by the Thermal Emission Spectrometer (TES), the infrared spectrometer on-board the Mars Global Surveyor (MGS). We show that a limited number of limb-geometry sequences observed by this instrument are characterized by a high enough signal-to-noise ratio (SNR) to extend the upper limit of the retrievals to 90 km. Using the methodology described in the paper, we have retrieved similar to 200 individual temperature profiles from the MGS TES limb observations in the altitude range between 30 and 90 km. The set of retrieved temperature profiles is available for download in supplemental materials of this paper. The temperature retrieval uncertainties are mainly caused by noise in the observed radiance, and are estimated to be about +/- 2 K at 60 km, +/- 3 K at 70 km, 5 +/- K at 80 km, and +/- 13 K at 90 km. We compare the retrieved profiles to the martian Year 24 (MY 24) dataset of the Mars Climate Database (MCD) and SPI-CAM measured temperature profiles for MY 27 and find good qualitative agreement. Quantitatively, our retrieved profiles are in general warmer and demonstrate strong profile-to-profile variability. The warm bias is partially explained by the selection of high SNR limb scans and can be estimated and taken into account. Overall, the average difference between the TES-retrieved temperatures corrected for warm bias and the MCD MY 24 dataset is 4 K at 60 km, 4 K at 70 km, -2 K at 80 km, and 2 K at 90 km. The root-mean-square of the temperature variability caused by gravity waves estimated in this work is 7 K at 60 km, 11 K at 70 km, 18 K at 80 km, and 25 K at 90 km. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Feofilov, A. G.; Kutepov, A. A.] Catholic Univ Amer, Washington, DC 20064 USA.
[Feofilov, A. G.; Kutepov, A. A.; Smith, M. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rezac, L.] Hampton Univ, Hampton, VA 23668 USA.
RP Feofilov, AG (reprint author), Ecole Polytech, Lab Dynam Meteorol, Palaiseau, France.
EM artem-feofilov@cua-nasa-gsfc.info
RI Feofilov, Artem/A-2271-2015
OI Feofilov, Artem/0000-0001-9924-4846
FU NASA [NNX08AL12G]
FX The work of A. Feofilov and A. Kutepov was supported by NASA Grant
NNX08AL12G. The authors are grateful to two anonymous reviewers for
their thorough analysis of the manuscript and their helpful comments and
recommendations. We also thank Dr. Francois Forget for providing the
SPICAM data and consultations regarding usage of the MCD data.
NR 47
TC 3
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U1 0
U2 3
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD NOV-DEC
PY 2012
VL 221
IS 2
BP 949
EP 959
DI 10.1016/j.icarus.2012.09.033
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 055RL
UT WOS:000312434300041
ER
PT J
AU Cloutis, EA
Hudon, P
Hiroi, T
Gaffey, MJ
Mann, P
AF Cloutis, E. A.
Hudon, P.
Hiroi, T.
Gaffey, M. J.
Mann, P.
TI Spectral reflectance properties of carbonaceous chondrites: 8. "Other"
carbonaceous chondrites: CH, ungrouped, polymict, xenolithic inclusions,
and R chondrites
SO ICARUS
LA English
DT Article
DE Asteroids, Surfaces; Meteorites; Spectroscopy
ID TAGISH LAKE METEORITE; EARLY SOLAR-SYSTEM; X-RAY-DIFFRACTION;
ORGANIC-MATTER; MOSSBAUER-SPECTROSCOPY; ISOTOPIC COMPOSITIONS; MINERAL
CHEMISTRY; CV-CHONDRITES; CM CHONDRITES; EARTH
AB We have analyzed reflectance spectra (0.3-2.5 mu m) of a number of ungrouped or tentatively grouped carbonaceous chondrites (CCs), possible CC-type xenoliths in an aubrite (Cumberland Falls) and a howardite (PRA 04401), a CH chondrite (PCA 91467), a CC polymict breccia (Kaidun), and some R chondrites. The best approach to analysis relies largely on characterizing spectrally active phases - i.e., those phases that contribute diagnostic absorption features, involving absorption band wavelength position, band depth, shape of absorption features, combined with albedo and spectral slope. Mafic silicate (hydrous and/or anhydrous) absorption features are ubiquitous in the CCs and R chondrites we have examined. Combining information on these features along with albedo and spectral slopes allows reasonable inferences to be made concerning their uniqueness. Reflectance spectra of Coolidge show contributions from both olivine and Fe oxyhydroxides (from terrestrial weathering), and its high reflectance and mafic silicate band depths are consistent with a petrologic grade >3 and inconsistent with CVs. The CC nature of the Cumberland Falls inclusions from spectral analysis is inconclusive, but they do exhibit spectral features consistent with their overall mineralogy. DaG 430, which has petrologic characteristics of both CV and CK chondrites, has a spectrum that is not fully consistent with either group. The spectrum of EET 96029 is consistent with some, but not all CM2 chondrites. GRO 95566, a meteorite with some affinities to CM2s, most resembles the Renazzo CR2 chondrite, consistent with their similar mineralogies, and its spectral properties can be related to its major mineralogic characteristics. Spectra of Kaidun are most consistent with CR chondrites, which form the bulk of this meteorite. The reflectance spectrum of MCY 92005 is consistent with its recent classification as a CM2 chondrite. The R3 chondrite MET 01149 shares many characteristics with CKs, but differs in terms of its slightly red slope and 2 mu m region absorption feature. The combination of high reflectance, deep 1 mu m band and, to a lesser extent, slightly red slope and weak 2 mu m region absorption band, distinguishes PRE 95404 from CV3s, to which it was initially assigned. The LAP 04840 R6 spectrum is dominated by olivine, consistent with a petrologic grade >3. Its reflectance is somewhat lower than for the R3 chondrites, and falls within the range of many CCs. Its most characteristic feature is the metal-OH absorption bands in the 2.3 mu m region. Analysis and assignment of PCA 91467 (CH3) is complicated by the presence of terrestrial weathering products. Its red spectral slope is consistent with its high metal content. Reflectance spectra of the howardite PRA 04401, which contains similar to 40% CM2-like inclusions, is dominated by the howardite's pyroxene absorption bands, and expected CM2-type absorption bands near 0.7 and 1.1 mu m are not seen. The CC xenoliths do reduce overall reflectance and pyroxene absorption band depths significantly, and probably add an overall red slope, when compared to inclusion-free howardites. QUE 99038, which has been linked to CM2, CO, or CR chondrites is not spectrally consistent with any of these groups. The 2 mu m band, high overall reflectance, and dominant olivine absorption band are all generally inconsistent with CM2 and CR2-3 chondrites. It resembles the CO3 chondrite ALH 77003 in the 1 mu m region, but differs in the 2 mu m region.
The red-sloped, nearly featureless spectrum of Tagish Lake is unique among carbonaceous chondrites. It probably arises from the highly aromatic nature of the organic component and its intimate association with the phyllosilicate-rich matrix, which makes up a high proportion of this meteorite. Our results suggest that the meteorites included in this study can usually be determined to be either unique or to be placed with a reasonable degree of confidence into established CC groups. Our analysis has also provided insights into the degree to which spectral analysis can be used for characterization, the spectral features that can be used for characterization, and their limitations. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Cloutis, E. A.; Mann, P.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada.
[Hudon, P.] NASA Johnson Space Ctr, Astromat Res & Explorat Sci Off, Mail Code KR, Houston, TX 77058 USA.
[Hiroi, T.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Gaffey, M. J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA.
RP Cloutis, EA (reprint author), Univ Winnipeg, Dept Geog, 515 Portage Ave, Winnipeg, MB R3B 2E9, Canada.
EM e.cloutis@uwinnipeg.ca; pierre.hudon@mcgill.ca;
takahiro_hiroi@brown.edu; gaffey@space.edu
FU NASA [NNG06GJ31G]; NSERC
FX We wish to thank the invaluable and generous assistance provided by many
individuals which made this study possible. In particular we thank the
US and Japanese Antarctic meteorite programs for recovering many of the
samples included in this study. We also wish to thank Dr. Andreas
Nathues from the Max Planck Institute for providing samples of PRA 04401
and a number of other howardites, Mike Zolensky and Andrei Ivanov for
the sample of Kaidun, and Katsuhito Ohtsuka for DaG 430. The RELAB
facility at Brown University is a multi-user facility operated with
support from NASA Planetary Geology and Geophysics Grant NNG06GJ31G,
whose support is gratefully acknowledged. This study was supported by an
NSERC Discovery grant to EAC. We also wish to thank Josep
Trigo-Rodriguez and an anonymous reviewer for their valuable and
thoughtful comments and suggestions.
NR 127
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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 NOV-DEC
PY 2012
VL 221
IS 2
BP 984
EP 1001
DI 10.1016/j.icarus.2012.10.008
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 055RL
UT WOS:000312434300044
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:
Occultations from the Prime and Equinox missions
SO ICARUS
LA English
DT Article
DE Titan; Atmospheres, Structure; Occultations
ID SURFACE TEMPERATURES; STRATOSPHERIC COMPOSITION; PLANETARY-ATMOSPHERES;
INFRARED-SPECTRA; DYNAMICS; MODEL; EQUILIBRIA; PROFILES; METHANE; CLOUDS
AB We present the results of six soundings of the atmosphere of Titan by the radio occultation technique using the Cassini spacecraft currently in orbit around Saturn. These occultations occurred during four separate targeted Titan encounters in both the Prime and Equinox missions of Cassini over 3 years. They cover a wide range of latitude from 75 degrees S to 79 degrees N, split so that three soundings are in the northern hemisphere and three are in the southern hemisphere. Techniques and error analysis are similar to Schinder et al. (2011). The six temperature-altitude profiles presented here are compared to those earlier results. Of special interest is the sudden cooling observed at altitudes of similar to 80-100 km in the two high northern (winter) soundings at 74 degrees N and 80 degrees N, where the temperature drops by about 10 K over the course of 20 km. The northern profiles also exhibit a transition between the troposphere and stratosphere that is much more abrupt than in the south, and the northern tropopause temperatures are much cooler. (C) 2012 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 95192 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@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.na-sa.gov
RI Flasar, F Michael/C-8509-2012;
OI Schinder, Paul/0000-0002-4571-7895
NR 43
TC 20
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U1 0
U2 17
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 NOV-DEC
PY 2012
VL 221
IS 2
BP 1020
EP 1031
DI 10.1016/j.icarus.2012.10.021
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 055RL
UT WOS:000312434300046
ER
PT J
AU White, DW
Mastrapa, RME
Sandford, SA
AF White, Douglas W.
Mastrapa, Rachel M. E.
Sandford, Scott A.
TI Laboratory spectra of CO2 vibrational modes in planetary ice analogs
SO ICARUS
LA English
DT Article
DE Ices, IR spectroscopy; Experimental techniques; Organic chemistry;
Satellites, Surfaces
ID NEAR-INFRARED SPECTROSCOPY; AMORPHOUS SOLID WATER; CARBON-DIOXIDE;
OPTICAL-CONSTANTS; SOLAR-SYSTEM; MOLECULAR-COMPLEXES; GLASS-TRANSITION;
GRAIN MANTLES; MU-M; INTERSTELLAR
AB Laboratory spectra have shown that CO2 is a powerful diagnostic tool for analyzing infrared data from remote observations, as it has been detected on icy moons in the outer Solar System as well as dust grain surfaces in the interstellar medium (ISM). IR absorption band profiles of CO2 within ice mixtures containing H2O and CH3OH change with respect to temperature and mixture ratios. In this particular study, the nu(3) CO2 asymmetric stretch mode near 4.3 mu m (2350 cm(-1)), overtone mode near 1.97 mu m (5080 cm(-1)), and the combination bands near 2.7 mu m (3700 cm(-1)), 2.8 mu m (3600 cm(-1)), and 2.02 mu m (4960 cm(-1)), are systematically observed in different mixtures with H2O and CH3OH in temperature ranges from 15 K to 150 K. Additionally, some high-temperature deposits (T > 50 K) of H2O, CH3OH, and CO2 ice mixtures were performed and it was discovered that CO2 may deposit out at higher temperatures than previously recorded. These data may then be used to interpret infrared observational data obtained from icy surfaces in the outer Solar System and beyond. (C) 2012 Elsevier Inc. All rights reserved.
C1 [White, Douglas W.; Sandford, Scott A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Mastrapa, Rachel M. E.] SETI Inst, Mountain View, CA 94035 USA.
RP White, DW (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM douglas.white@nasa.gov
FU NASA; Oak Ridge Associated Universities; NASA's Origins of Solar Systems
and Planetary Geology and Geophysics Programs
FX The authors thank NASA and Oak Ridge Associated Universities for
sponsoring the NASA Postdoctoral Program (NPP) and NASA's Origins of
Solar Systems and Planetary Geology and Geophysics Programs for support.
We also thank Perry Gerakines and the University of Alabama at
Birmingham (UAB) for use of some of the data in this study.
NR 72
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U1 0
U2 17
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 NOV-DEC
PY 2012
VL 221
IS 2
BP 1032
EP 1042
DI 10.1016/j.icarus.2012.10.024
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 055RL
UT WOS:000312434300047
ER
PT J
AU Perez-Hoyos, S
Sanz-Requena, JF
Sanchez-Lavega, A
Wong, MH
Hammel, HB
Orton, GS
de Pater, I
Simon-Miller, AA
Clarke, JT
Noll, K
AF Perez-Hoyos, S.
Sanz-Requena, J. F.
Sanchez-Lavega, A.
Wong, M. H.
Hammel, H. B.
Orton, G. S.
de Pater, I.
Simon-Miller, A. A.
Clarke, J. T.
Noll, K.
TI Vertical cloud structure of the 2009 Jupiter impact based on HST/WFC3
observations
SO ICARUS
LA English
DT Article
DE Jupiter; Atmospheres, Structure; Jupiter, Atmosphere; Impact processes
ID LEVY 9 H; COMET SHOEMAKER-LEVY-9; PLANETARY ATMOSPHERES; TEMPORAL
EVOLUTION; AEROSOL DEBRIS; CALAR-ALTO; HST; ULTRAVIOLET; EQUATORIAL;
TELESCOPE
AB The impact of a body of unknown origin with Jupiter in July 2009 produced ar intense perturbation of the planet's atmosphere at the visible cloud levels. The vertical cloud structure was deeply affected by the presence of a strongly absorbing dense aerosol layer that was expanded steadily by advection in the local winds. We observed this phenomenon at high spatial resolution with the Hubble Space Telescope in July, August, September and November 2009 using the Wide Field Camera 3. In this work, we present radiative transfer modeling of the observed reflectivity in the wavelength range from the near UV (200 nm) to near IR (950 nm) range. The geometric and spectral variations of reflectivity give information on the main particle properties (optical thickness, size, and imaginary refractive index). The observations can be fitted by introducing small particles into the stratosphere with an optical thickness, at a wavelength of 400 nm, ranging from 0.5 +/- 0.2 (center of the Impact Cloud) to 0.17 +/- 0.03 (impact periphery). Similar effects are detected in the troposphere: the disturbance increases the particle density at all detectable atmospheric levels, with a total aerosol column density of 5 +/- 2 x 10(9) cm(-2). The imaginary refractive indices of the aerosol were also substantially altered, with values of m(i) similar to 0.015 at UV wavelengths, resembling the absorption spectrum of absorber candidates previously proposed for SL9. We find a typical e-folding temporal scale of 10 +/- 3 days in the most rapidly evolving region of the Impact Cloud. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Perez-Hoyos, S.; Sanchez-Lavega, A.] Univ Basque Country, Escuela T Super Ingn, Dept Fis Aplicada 1, Bilbao 48013, Spain.
[Sanz-Requena, J. F.] Univ Europea Miguel de Cervantes, Valladolid, Spain.
[Wong, M. H.; de Pater, I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Hammel, H. B.] AURA Inc, Washington, DC 20005 USA.
[Hammel, H. B.] Space Sci Inst, Boulder, CO 80301 USA.
[Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Simon-Miller, A. A.; Noll, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Clarke, J. T.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
RP Perez-Hoyos, S (reprint author), Univ Basque Country, Escuela T Super Ingn, Dept Fis Aplicada 1, Alameda Urquijo S-N, Bilbao 48013, Spain.
EM santiago.perez@ehu.es
RI Clarke, John/C-8644-2013; Noll, Keith/C-8447-2012; Perez-Hoyos,
Santiago/L-7543-2014; Simon, Amy/C-8020-2012;
OI Perez-Hoyos, Santiago/0000-0002-2587-4682; Simon,
Amy/0000-0003-4641-6186; Sanchez-Lavega, Agustin/0000-0001-7355-1522
FU Spanish MICIIN [AYA2009-10701]; FEDER funds; Grupos Gobierno Vasco
[IT-464-07]; Universidad Pais Vasco UPV/EHU [UFI11/55]; HST Programs
[GO/DD-12045, GO/DD-12003, GO-11559]; NASA through Space Telescope
Science Institute; NASA [NAS 5-26555]
FX This work was supported by the Spanish MICIIN Project AYA2009-10701 with
FEDER funds and Grupos Gobierno Vasco IT-464-07, and by Universidad Pais
Vasco UPV/EHU through Program UFI11/55. The observations were supported
by HST Programs GO/DD-12045, GO/DD-12003 and GO-11559, with support
provided by NASA through a grant from the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA Contract NAS 5-26555.
NR 49
TC 3
Z9 3
U1 0
U2 9
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD NOV-DEC
PY 2012
VL 221
IS 2
BP 1061
EP 1078
DI 10.1016/j.icarus.2012.10.012
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 055RL
UT WOS:000312434300049
ER
PT J
AU Howett, CJA
Spencer, JR
Hurford, T
Verbiscer, A
Segura, M
AF Howett, C. J. A.
Spencer, J. R.
Hurford, T.
Verbiscer, A.
Segura, M.
TI PacMan returns: An electron-generated thermal anomaly on Tethys
SO ICARUS
LA English
DT Article
DE Saturn, Satellites; Satellites, Surfaces; Satellites, Composition
ID SYSTEM
AB New Cassini observations show that Saturn's moon Tethys, like Mimas, has a region of anomalously high thermal inertia at low latitudes centered on its leading hemisphere. Derivation of the thermophysical properties of the surface across three representative regions indicate that the bolometric Bond albedo across Tethys' leading hemisphere remains constant, within error, whilst the thermal inertia increases from 5 +/- 1 J s(-1) m(-1) K-1 outside of the anomalous region to 25 +/- 3 J s(-1) m(-1) K-1 inside. The thermally anomalous region is spatially correlated with a decrease in the IR/UV surface coloration. The discovery greatly strengthens the hypothesis that high-energy electrons, which preferentially bombard the leading hemispheres on both satellites, produce dramatic alterations in surface texture. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Howett, C. J. A.; Spencer, J. R.] SW Res Inst, Boulder, CO 80403 USA.
[Hurford, T.; Segura, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Verbiscer, A.] Univ Virginia, Charlottesville, VA 22904 USA.
RP Howett, CJA (reprint author), 1050 Walnut St,Suite 300, Boulder, CO 80302 USA.
EM howett@boulder.swri.edu
RI Hurford, Terry/F-2625-2012
FU Cassini Project; Cassini Data Analysis Program [NNX12AC23G]
FX The authors would like to thank the Cassini Project and the Cassini Data
Analysis Program (NNX12AC23G) for funding this work. Thanks are also
extended to Chris Paranicas, who supplied data on the energy flux
bombarding Tethys, and Paul Schenk, who provided the IR/UV color ratio
maps of Tethys.
NR 11
TC 17
Z9 17
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 NOV-DEC
PY 2012
VL 221
IS 2
BP 1084
EP 1088
DI 10.1016/j.icarus.2012.10.013
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 055RL
UT WOS:000312434300051
ER
PT J
AU Marchis, F
Enriquez, JE
Emery, JP
Mueller, M
Baek, M
Pollock, J
Assafin, M
Martins, RV
Berthier, J
Vachier, F
Cruikshank, DP
Lim, LF
Reichart, DE
Ivarsen, KM
Haislip, JB
LaCluyze, AP
AF Marchis, F.
Enriquez, J. E.
Emery, J. P.
Mueller, M.
Baek, M.
Pollock, J.
Assafin, M.
Vieira Martins, R.
Berthier, J.
Vachier, F.
Cruikshank, D. P.
Lim, L. F.
Reichart, D. E.
Ivarsen, K. M.
Haislip, J. B.
LaCluyze, A. P.
TI Multiple asteroid systems: Dimensions and thermal properties from
Spitzer Space Telescope and ground-based observations
SO ICARUS
LA English
DT Article
DE Asteroids; Satellites of asteroids; Asteroids, Composition; Infrared
observations
ID NEAR-EARTH ASTEROIDS; MAIN-BELT ASTEROIDS; BINARY MINOR PLANETS; 33342
1998 WT24; INFRARED OBSERVATIONS; 21 LUTETIA; ROTATIONAL PROPERTIES;
SPECTROSCOPIC SURVEY; SURFACE-COMPOSITION; ANGULAR-MOMENTUM
AB We collected mid-IR spectra from 5.2 to 38 mu m using the Spitzer Space Telescope Infrared Spectrograph of 28 asteroids representative of all established types of binary groups. Photometric lightcurves were also obtained for 14 of them during the Spitzer observations to provide the context of the observations and reliable estimates of their absolute magnitudes. The extracted mid-IR spectra were analyzed using a modified standard thermal model (STM) and a thermophysical model (TPM) that takes into account the shape and geometry of the large primary at the time of the Spitzer observation. We derived a reliable estimate of the size, albedo, and beaming factor for each of these asteroids, representing three main taxonomic groups: C, S. and X. For large (volume-equivalent system diameter D-eq > 130 km) binary asteroids, the TPM analysis indicates a low thermal inertia (Gamma <= similar to 100 J s(-1/2) K-1 m(-2)) and their emissivity spectra display strong mineral features, implying that they are covered with a thick layer of thermally insulating regolith. The smaller (surface-equivalent system diameter D-eff < 17 km) asteroids also show some emission lines of minerals, but they are significantly weaker, consistent with regoliths with coarser grains, than those of the large binary asteroids. The average bulk densities of these multiple asteroids vary from 0.7-1.7 g/cm(3) (P-, C-type) to similar to 2 g/cm(3) (S-type). The highest density is estimated for the M-type (22) Kalliope (3.2 +/- 0.9 g/cm(3)). The spectral energy distributions (SEDs) and emissivity spectra, made available as a supplement document, could help to constrain the surface compositions of these asteroids. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Marchis, F.; Enriquez, J. E.; Baek, M.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[Emery, J. P.] Univ Tennessee, Knoxville, TN 37996 USA.
[Mueller, M.] Univ Groningen, SRON, Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands.
[Pollock, J.] Appalachian State Univ, Dept Phys & Astron, Boone, NC 28608 USA.
[Assafin, M.] Univ Fed Rio de Janeiro, Observ Valongo, Rio de Janeiro, Brazil.
[Vieira Martins, R.] MCT, Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Marchis, F.; Berthier, J.; Vachier, F.] Observ Paris, Inst Mecan Celeste & Calcul Ephemerides, F-75014 Paris, France.
[Cruikshank, D. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Lim, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Reichart, D. E.; Ivarsen, K. M.; Haislip, J. B.; LaCluyze, A. P.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27514 USA.
RP Marchis, F (reprint author), SETI Inst, Carl Sagan Ctr, 189 Bernardo Ave, Mountain View, CA 94043 USA.
EM fmarchis@seti.org
RI Assafin, Marcelo/C-3188-2013; Tecnologias espaciai, Inct/I-2415-2013;
Lim, Lucy/C-9557-2012; Baek, Minjin/L-4425-2016;
OI Lim, Lucy/0000-0002-9696-9654; Baek, Minjin/0000-0002-9698-2525;
Mueller, Michael/0000-0003-3217-5385
FU California Institute of Technology; NASA through JPL/Caltech; National
Science Foundation [AAG-0807468]; NAS
FX The authors would like to thank Prof. Alan Harris from DLR and an
anonymous referee for their valuable comments which improved
significantly the quality of this article. This work is based in part on
observations made with the Spitzer Space Telescope, which is operated by
the Jet Propulsion Laboratory. California Institute of Technology under
a Contract with NASA. Support for this work was provided by NASA through
an award issued by JPL/Caltech. FMA, JEN & MBA were supported by the
National Science Foundation under Award Number AAG-0807468.
NR 121
TC 16
Z9 16
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 NOV-DEC
PY 2012
VL 221
IS 2
BP 1130
EP 1161
DI 10.1016/j.icarus.2012.09.013
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 055RL
UT WOS:000312434300055
ER
PT J
AU Reddy, V
Sanchez, JA
Gaffey, MJ
Abell, PA
Le Corre, L
Hardersen, PS
AF Reddy, Vishnu
Sanchez, Juan A.
Gaffey, Michael J.
Abell, Paul A.
Le Corre, Lucille
Hardersen, Paul S.
TI Composition of near-Earth Asteroid (4179) Toutatis
SO ICARUS
LA English
DT Article
DE Asteroids; Asteroids, Composition; Spectroscopy; Meteorites; Infrared
observations
ID SPECTROSCOPIC SURVEY; REFLECTANCE SPECTRA; ORDINARY CHONDRITES; COMPLEX
ROTATION; PHASE-II; METEORITES; BELT; 4179-TOUTATIS; SPECTROGRAPH;
LIGHTCURVE
AB Surface composition of near-Earth Asteroid (4179) Toutatis is consistent with an undiffeientiated L-chondrite composition. This is inconsistent with early observations that suggested high pyroxene iron content and a differentiated body. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Reddy, Vishnu; Gaffey, Michael J.; Hardersen, Paul S.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA.
[Reddy, Vishnu; Le Corre, Lucille] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Sanchez, Juan A.] Univ Munster, Inst Planetol, D-48149 Munster, Germany.
[Abell, Paul A.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA.
RP Reddy, V (reprint author), Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA.
EM reddy@space.edu
RI Hardersen, Paul/N-9343-2014;
OI Hardersen, Paul/0000-0002-0440-9095; Reddy, Vishnu/0000-0002-7743-3491;
Le Corre, Lucille/0000-0003-0349-7932
FU NASA NEOO Program [NNX12AG12G]; NASA Planetary Geology and Geophysics
[NNX11AN84G]
FX This research was supported by NASA NEOO Program Grant NNX12AG12G, and
NASA Planetary Geology and Geophysics Grant NNX11AN84G. We thank the
IRTF TAC for awarding time to this project, and to the IRTF TOs and MKSS
staff for their support. The authors would like to thank Tasha Dunn and
an anonymous reviewer for their helpful reviews to improve the
manuscript.
NR 29
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U1 1
U2 16
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 NOV-DEC
PY 2012
VL 221
IS 2
BP 1177
EP 1179
DI 10.1016/j.icarus.2012.10.005
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 055RL
UT WOS:000312434300058
ER
PT J
AU Hurwitz, FI
Guo, HQ
Rogers, RB
Sheets, EJ
Miller, DR
Newlin, KN
Shave, MK
Palczer, AR
Cox, MT
AF Hurwitz, Frances I.
Guo, Haiquan
Rogers, Richard B.
Sheets, Erik J.
Miller, Derek R.
Newlin, Katy N.
Shave, Molly K.
Palczer, Anna R.
Cox, Michael T.
TI Influence of Ti addition on boehmite-derived aluminum silicate aerogels:
structure and properties
SO JOURNAL OF SOL-GEL SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Aerogel; Boehmite; Aluminum silicate; Titanium isopropoxide; Al2TiO5;
Mullite
ID SOL-GEL PROCESS; SYSTEMS; OXIDES; ROUTE; PHASE
AB Aluminosilicate aerogels offer potential for extremely low thermal conductivities at temperatures greater than 900 A degrees C, beyond where silica aerogels reach their upper temperature use limits. Aerogels have been synthesized at two Al:Si ratios, a 3Al:1Si mullite composition, and an 8Al:1Si alumina rich composition. Boehmite (AlOOH) is used as the Al source, and tetraethoxysilane as the Si precursor. The influence of Ti as a ternary constituent, introduced through the addition of titanium isopropoxide in the sol-gel synthesis, on aerogel morphology and thermal properties is evaluated. Four different boehmite precursor powders are evaluated. Morphology, surface area and pore size, and thermal transformation vary with the crystallite size of the starting boehmite powder, as does incorporation of titanium and evolution of Ti-containing crystalline phases. The addition of Ti influences sol viscosity, gelation time, surface area and pore size distribution, as well as phase formation on heat treatment.
C1 [Hurwitz, Frances I.; Rogers, Richard B.; Palczer, Anna R.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Guo, Haiquan] Ohio Aerosp Inst, Cleveland, OH USA.
[Sheets, Erik J.] Purdue Univ, W Lafayette, IN 47907 USA.
[Miller, Derek R.] Michigan State Univ, E Lansing, MI 48824 USA.
[Newlin, Katy N.] Univ Louisville, Louisville, KY 40292 USA.
[Shave, Molly K.] Colorado Sch Mines, Golden, CO 80401 USA.
[Cox, Michael T.] Arctic Slope Reg Corp, Cleveland, OH USA.
RP Hurwitz, FI (reprint author), NASA, Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA.
EM frances.hurwitz@nasa.gov
NR 20
TC 3
Z9 3
U1 2
U2 28
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0928-0707
EI 1573-4846
J9 J SOL-GEL SCI TECHN
JI J. Sol-Gel Sci. Technol.
PD NOV
PY 2012
VL 64
IS 2
BP 367
EP 374
DI 10.1007/s10971-012-2866-8
PG 8
WC Materials Science, Ceramics
SC Materials Science
GA 057SN
UT WOS:000312584400014
ER
PT J
AU Lopez, J
Boyd, D
Ylitalo, GM
Littnan, C
Pearce, R
AF Lopez, Jessica
Boyd, Daryle
Ylitalo, Gina M.
Littnan, Charles
Pearce, Ronald
TI Persistent organic pollutants in the endangered Hawaiian monk seal
(Monachus schauinslandi) from the main Hawaiian Islands
SO MARINE POLLUTION BULLETIN
LA English
DT Article
DE Hawaiian monk seal; Monachus schauinslandi; Persistent organic
pollutants; Endangered species; Hawaii; Contaminants
ID LIONS ZALOPHUS-CALIFORNIANUS; ORGANOCHLORINE PESTICIDES; HARBOR SEALS;
POLYCHLORINATED-BIPHENYLS; CALLORHINUS-URSINUS; GLOBAL TRANSPORT; FLAME
RETARDANTS; PHOCA-VITULINA; ELEPHANT SEALS; GREY SEALS
AB Little is known about levels or effects of persistent organic pollutants (POPs) in Hawaiian monk seals (HMS) from the main Hawaiian Islands (MHI) subpopulation. This study examined concentrations of a large suite of POPs in blubber and serum of juvenile and adult HMS from the MHI. Adult females have the lowest blubber levels of most POPs, whereas adult males have highest levels. POPs in serum were significantly different in adult males compared with adult females for chlordanes and summed dichlorodiphenyltrichloroethanes (DDTs). Lipid-normalized concentrations of chlordanes, DDTs, polychlorinated biphenyls, and mirex in paired blubber and serum samples were significantly correlated. Contaminant levels from the MHI were at similar or lower levels than those from remote Northwestern Hawaiian Island populations. Determining initial ranges of POPs is an important step towards assessing one of the many potential health threats to this critically endangered species. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Lopez, Jessica] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI 96814 USA.
[Lopez, Jessica] Hawaii Pacific Univ, Kaneohe, HI 96744 USA.
[Boyd, Daryle; Ylitalo, Gina M.; Pearce, Ronald] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98112 USA.
[Littnan, Charles] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96814 USA.
RP Lopez, J (reprint author), Univ Hawaii, Joint Inst Marine & Atmospher Res, JBPHH, 1025 Quincy Ave,Ste 5010, Manoa, HI 96860 USA.
EM Jessica.Lopez@noaa.gov; Daryle.Boyd@noaa.gov; Gina.Ylitalo@noaa.gov;
Charles.Litnnan@noaa.gov; Ronald.W.Pearce@noaa.gov
FU NOAA's PIFSC; NOAA's Nancy Foster Scholarship program
FX The NOAA Pacific Islands Fisheries Science Center (PIFSC) Hawaiian Monk
Seal Research Program staff provided samples and life history
information. We especially thank Lizabeth Kashinsky and Angie Kaufman
for assistance with samples; Tracy Wurth, and Thea Johanos for
individual seal information; Chad Yoshinaga, Kenady Wilson, and Jason
Baker, for field assistance. Thanks to Bernadita Anulacion, Jennie
Bolton, Catherine Sloan, Karen Tilbury and their colleagues at the
Northwest Fisheries Science Center Environmental Assessment program for
sample analysis and guidance. A special thank you to David Hyrenbach,
Jason Baker, and Brenda Jensen for helping with manuscript edits.
Funding was provided by NOAA's PIFSC and NOAA's Nancy Foster Scholarship
program. All sample collection and research was conducted under the
Marine Mammal Protection Act Scientific Research Permit Numbers
848-1335, 848-1695 and 10137 and safe handling and capture protocols of
NOAA Fisheries.
NR 67
TC 10
Z9 10
U1 3
U2 76
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0025-326X
EI 1879-3363
J9 MAR POLLUT BULL
JI Mar. Pollut. Bull.
PD NOV
PY 2012
VL 64
IS 11
BP 2588
EP 2598
DI 10.1016/j.marpolbul.2012.07.012
PG 11
WC Environmental Sciences; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 055LP
UT WOS:000312418100052
PM 22884537
ER
PT J
AU Scott, P
Savage, C
Edsjo, J
Collaboration, I
Abbasi, R
Abdou, Y
Ackermann, M
Adams, J
Aguilar, JA
Ahlers, M
Altmann, D
Andeen, K
Enberg, JAF
Bai, X
Baker, M
Barwick, SW
Baum, V
Bay, R
Beattie, K
Beatty, JJ
Bechet, S
Tjus, JB
Becker, KH
Bell, M
Benabderrahmane, ML
BenZvi, S
Berdermann, J
Berghaus, P
Berley, D
Bernardini, E
Bertrand, D
Besson, DZ
Bindig, D
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohm, C
Bose, D
Boser, S
Botner, O
Brayeur, L
Brown, AM
Bruijn, R
Brunner, J
Buitink, S
Caballero-Mora, KS
Carson, M
Casey, J
Casier, M
Chirkin, D
Christy, B
Clevermann, F
Cohen, S
Cowen, DF
Silva, AHC
Danninger, M
Daughhetee, J
Davis, JC
De Clercq, C
Descamps, F
Desiati, P
de Vries-Uiterweerd, G
DeYoung, T
Diaz-Velez, JC
Dreyer, J
Dumm, JP
Dunkman, M
Eagan, 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
Flis, S
Franckowiak, A
Franke, R
Frantzen, K
Fuchs, T
Gaisser, TK
Gallagher, J
Gerhardt, L
Gladstone, L
Glusenkamp, T
Goldschmidt, A
Goodman, JA
Gora, D
Grant, D
Gross, A
Grullon, S
Gurtner, M
Ha, C
Ismail, AH
Hallgren, A
Halzen, F
Hanson, K
Heereman, D
Heimann, P
Heinen, D
Helbing, K
Hellauer, R
Hickford, S
Hill, GC
Hoffman, KD
Hoffmann, R
Homeier, A
Hoshina, K
Huelsnitz, W
Hulth, PO
Hultqvist, K
Hussain, S
Ishihara, A
Jacobi, E
Jacobsen, J
Japaridze, GS
Jlelati, O
Johansson, H
Kappes, A
Karg, T
Karle, A
Kiryluk, J
Kislat, F
Klas, J
Klein, SR
Kohne, JH
Kohnen, G
Kolanoski, H
Kopke, L
Kopper, C
Kopper, S
Koskinen, DJ
Kowalski, M
Krasberg, M
Kroll, G
Kunnen, J
Kurahashi, N
Kuwabara, T
Labare, M
Laihem, K
Landsman, H
Larson, MJ
Lauer, R
Lesiak-Bzdak, M
Lunemann, J
Madsen, J
Maruyama, R
Mase, K
Matis, HS
McNally, F
Meagher, K
Merck, M
Meszaros, P
Meures, T
Miarecki, S
Middell, E
Milke, N
Miller, J
Mohrmann, L
Montaruli, T
Morse, R
Movit, SM
Nahnhauer, R
Naumann, U
Nowicki, SC
Nygren, DR
Obertacke, A
Odrowski, S
Olivas, A
Olivo, M
O'Murchadha, A
Panknin, S
Paul, L
Pepper, JA
de los Heros, CP
Pieloth, D
Pirk, N
Posselt, J
Price, PB
Przybylski, GT
Raedel, L
Rawlins, K
Redl, P
Resconi, E
Rhode, W
Ribordy, M
Richman, M
Riedel, B
Rodrigues, JP
Rothmaier, F
Rott, C
Ruhe, T
Rutledge, D
Ruzybayev, B
Ryckbosch, D
Saba, SM
Salameh, T
Sander, HG
Santander, M
Sarkar, S
Schatto, K
Scheel, M
Scheriau, F
Schmidt, T
Schmitz, M
Schoenen, S
Schoneberg, S
Schonherr, L
Schonwald, A
Schukraft, A
Schulte, L
Schulz, O
Seckel, D
Seo, SH
Sestayo, Y
Seunarine, S
Smith, MWE
Soiron, M
Soldin, D
Spiczak, GM
Spiering, C
Stamatikos, M
Stanev, T
Stasik, A
Stezelberger, T
Stokstad, RG
Stoessl, A
Strahler, EA
Strom, R
Sullivan, GW
Taavola, H
Taboada, I
Tamburro, A
Ter-Antonyan, S
Tilav, S
Toale, PA
Toscano, S
Usner, M
van Eijndhoven, N
van der Drift, D
Van Overloop, A
van Santen, J
Vehring, M
Voge, M
Walck, C
Waldenmaier, T
Wallraff, M
Walter, M
Wasserman, R
Weaver, C
Wendt, C
Westerhoff, S
Whitehorn, N
Wiebe, K
Wiebusch, CH
Williams, DR
Wissing, H
Wolf, M
Wood, TR
Woschnagg, K
Xu, C
Xu, DL
Xu, XW
Yanez, JP
Yodh, G
Yoshida, S
Zarzhitsky, P
Ziemann, J
Zilles, A
Zoll, M
AF Scott, P.
Savage, C.
Edsjo, J.
Collaboration, IceCube
Abbasi, R.
Abdou, Y.
Ackermann, M.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Altmann, D.
Andeen, K.
Enberg, J. Au Ff
Bai, X.
Baker, M.
Barwick, S. W.
Baum, V.
Bay, R.
Beattie, K.
Beatty, J. J.
Bechet, S.
Tjus, J. Becker
Becker, K. -H.
Bell, M.
Benabderrahmane, M. L.
BenZvi, S.
Berdermann, J.
Berghaus, P.
Berley, D.
Bernardini, E.
Bertrand, D.
Besson, D. Z.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohm, C.
Bose, D.
Boeser, S.
Botner, O.
Brayeur, L.
Brown, A. M.
Bruijn, R.
Brunner, J.
Buitink, S.
Caballero-Mora, K. S.
Carson, M.
Casey, J.
Casier, M.
Chirkin, D.
Christy, B.
Clevermann, F.
Cohen, S.
Cowen, D. F.
Silva, A. H. Cruz
Danninger, M.
Daughhetee, J.
Davis, J. C.
De Clercq, C.
Descamps, F.
Desiati, P.
de Vries-Uiterweerd, G.
DeYoung, T.
Diaz-Velez, J. C.
Dreyer, J.
Dumm, J. P.
Dunkman, M.
Eagan, 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.
Flis, S.
Franckowiak, A.
Franke, R.
Frantzen, K.
Fuchs, T.
Gaisser, T. K.
Gallagher, J.
Gerhardt, L.
Gladstone, L.
Gluesenkamp, T.
Goldschmidt, A.
Goodman, J. A.
Gora, D.
Grant, D.
Gross, A.
Grullon, S.
Gurtner, M.
Ha, C.
Ismail, A. Haj
Hallgren, A.
Halzen, F.
Hanson, K.
Heereman, D.
Heimann, P.
Heinen, D.
Helbing, K.
Hellauer, R.
Hickford, S.
Hill, G. C.
Hoffman, K. D.
Hoffmann, R.
Homeier, A.
Hoshina, K.
Huelsnitz, W.
Hulth, P. O.
Hultqvist, K.
Hussain, S.
Ishihara, A.
Jacobi, E.
Jacobsen, J.
Japaridze, G. S.
Jlelati, O.
Johansson, H.
Kappes, A.
Karg, T.
Karle, A.
Kiryluk, J.
Kislat, F.
Klaes, J.
Klein, S. R.
Koehne, J. -H.
Kohnen, G.
Kolanoski, H.
Koepke, L.
Kopper, C.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Krasberg, M.
Kroll, G.
Kunnen, J.
Kurahashi, N.
Kuwabara, T.
Labare, M.
Laihem, K.
Landsman, H.
Larson, M. J.
Lauer, R.
Lesiak-Bzdak, M.
Luenemann, J.
Madsen, J.
Maruyama, R.
Mase, K.
Matis, H. S.
McNally, F.
Meagher, K.
Merck, M.
Meszaros, P.
Meures, T.
Miarecki, S.
Middell, E.
Milke, N.
Miller, J.
Mohrmann, L.
Montaruli, T.
Morse, R.
Movit, S. M.
Nahnhauer, R.
Naumann, U.
Nowicki, S. C.
Nygren, D. R.
Obertacke, A.
Odrowski, S.
Olivas, A.
Olivo, M.
O'Murchadha, A.
Panknin, S.
Paul, L.
Pepper, J. A.
de los Heros, C. Perez
Pieloth, D.
Pirk, N.
Posselt, J.
Price, P. B.
Przybylski, G. T.
Raedel, L.
Rawlins, K.
Redl, P.
Resconi, E.
Rhode, W.
Ribordy, M.
Richman, M.
Riedel, B.
Rodrigues, J. P.
Rothmaier, F.
Rott, C.
Ruhe, T.
Rutledge, D.
Ruzybayev, B.
Ryckbosch, D.
Saba, S. M.
Salameh, T.
Sander, H. -G.
Santander, M.
Sarkar, S.
Schatto, K.
Scheel, M.
Scheriau, F.
Schmidt, T.
Schmitz, M.
Schoenen, S.
Schoeneberg, S.
Schoenherr, L.
Schoenwald, A.
Schukraft, A.
Schulte, L.
Schulz, O.
Seckel, D.
Seo, S. H.
Sestayo, Y.
Seunarine, S.
Smith, M. W. E.
Soiron, M.
Soldin, D.
Spiczak, G. M.
Spiering, C.
Stamatikos, M.
Stanev, T.
Stasik, A.
Stezelberger, T.
Stokstad, R. G.
Stoessl, A.
Strahler, E. A.
Strom, R.
Sullivan, G. W.
Taavola, H.
Taboada, I.
Tamburro, A.
Ter-Antonyan, S.
Tilav, S.
Toale, P. A.
Toscano, S.
Usner, M.
van Eijndhoven, N.
van der Drift, D.
Van Overloop, A.
van Santen, J.
Vehring, M.
Voge, M.
Walck, C.
Waldenmaier, T.
Wallraff, M.
Walter, M.
Wasserman, R.
Weaver, Ch.
Wendt, C.
Westerhoff, S.
Whitehorn, N.
Wiebe, K.
Wiebusch, C. H.
Williams, D. R.
Wissing, H.
Wolf, M.
Wood, T. R.
Woschnagg, K.
Xu, C.
Xu, D. L.
Xu, X. W.
Yanez, J. P.
Yodh, G.
Yoshida, S.
Zarzhitsky, P.
Ziemann, J.
Zilles, A.
Zoll, M.
TI Use of event-level neutrino telescope data in global fits for theories
of new physics
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE dark matter theory; neutrino astronomy; dark matter experiments;
cosmology of theories beyond the SM
ID DARK-MATTER CANDIDATES; OBSERVATIONS COSMOLOGICAL INTERPRETATION;
CONSTRAINTS; SUPERSYMMETRY; LIMITS; LHC; CAPTURE; SEARCH; LIGHT
AB We present a fast likelihood method for including event-level neutrino telescope data in parameter explorations of theories for new physics, and announce its public release as part of DarkSUSY 5.0.6. Our construction includes both angular and spectral information about neutrino events, as well as their total number. We also present a corresponding measure for simple model exclusion, which can be used for single models without reference to the rest of a parameter space. We perform a number of supersymmetric parameter scans with IceCube data to illustrate the utility of the method: example global fits and a signal recovery in the constrained minimal supersymmetric standard model (CMSSM), and a model exclusion exercise in a 7-parameter phenomenological version of the MSSM. The final IceCube detector con figuration will probe almost the entire focus-point region of the CMSSM, as well as a number of MSSM-7 models that will not otherwise be accessible to e. g. direct detection. Our method accurately recovers the mock signal, and provides tight constraints on model parameters and derived quantities. We show that the inclusion of spectral information significantly improves the accuracy of the recovery, providing motivation for its use in future IceCube analyses.
C1 [Scott, P.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Savage, C.; Edsjo, J.; Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Savage, C.; Edsjo, J.; Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Abbasi, R.; Ahlers, M.; Andeen, K.; Enberg, J. Au Ff; Baker, M.; BenZvi, S.; Chirkin, D.; Descamps, F.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Karle, A.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Abbasi, R.; Ahlers, M.; Andeen, K.; Enberg, J. Au Ff; Baker, M.; BenZvi, S.; Chirkin, D.; Descamps, F.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Karle, A.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA.
[Abdou, Y.; Carson, M.; de Vries-Uiterweerd, G.; Feusels, T.; Ismail, A. Haj; Jlelati, O.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium.
[Ackermann, M.; Benabderrahmane, M. L.; Berdermann, J.; Berghaus, P.; Bernardini, E.; Brunner, J.; Silva, A. H. Cruz; Franke, R.; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Karg, T.; Kislat, F.; Lauer, R.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Pirk, N.; Schoenwald, A.; Spiering, C.; Stoessl, A.; Walter, M.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany.
[Adams, J.; Brown, A. M.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Aguilar, J. A.; Montaruli, T.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland.
[Altmann, D.; Kappes, A.; Kolanoski, H.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Bai, X.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bai, X.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Bai, X.] S Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA.
[Barwick, S. W.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Baum, V.; Koepke, L.; Kroll, G.; Luenemann, J.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[Bay, R.; Filimonov, K.; Gerhardt, L.; Ha, C.; Klein, S. R.; Miarecki, S.; Price, P. B.; Rothmaier, F.; van der Drift, D.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Beattie, K.; Gerhardt, L.; Goldschmidt, A.; Ha, C.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.; van der Drift, D.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Beatty, J. J.; Davis, J. C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Bechet, S.; Bertrand, D.; Hanson, K.; Heereman, D.; Meures, T.; O'Murchadha, A.] Univ Libre Bruxelles, Fac Sci, B-1050 Brussels, Belgium.
[Tjus, J. Becker; Dreyer, J.; Fedynitch, A.; Olivo, M.; Saba, S. M.; Schoeneberg, S.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Hoffmann, R.; Klaes, J.; Kopper, S.; Naumann, U.; Obertacke, A.; Posselt, J.; Soldin, D.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Bell, M.; Caballero-Mora, K. S.; Cowen, D. F.; DeYoung, T.; Dunkman, M.; Eagan, R.; Koskinen, D. J.; Meszaros, P.; Rutledge, D.; Salameh, T.; Smith, M. W. E.; Wasserman, R.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Berley, D.; Blaufuss, E.; Christy, B.; Ellsworth, R. W.; Goodman, J. A.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Richman, M.; Schmidt, T.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Heimann, P.; Heinen, D.; Laihem, K.; Paul, L.; Raedel, L.; Scheel, M.; Schoenen, S.; Schoenherr, L.; Schukraft, A.; Soiron, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.; Zilles, A.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
[Bose, D.; Brayeur, L.; Buitink, S.; Casier, M.; De Clercq, C.; Kunnen, J.; Labare, M.; Miller, J.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Boeser, S.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.; Schulte, L.; Stasik, A.; Usner, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
[Botner, O.; Engdegard, O.; Hallgren, A.; de los Heros, C. Perez; Strom, R.; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Bruijn, R.; Cohen, S.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland.
[Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Clevermann, F.; Frantzen, K.; Fuchs, T.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.; Scheriau, F.; Schmitz, M.; Ziemann, J.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Grant, D.; Nowicki, S. C.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
[Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.] Tech Univ Munich, D-85748 Garching, Germany.
[Hill, G. C.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia.
[Huelsnitz, W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Ishihara, A.; Mase, K.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Kiryluk, J.; Lesiak-Bzdak, M.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Larson, M. J.; Pepper, J. A.; Toale, P. A.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Madsen, J.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Montaruli, T.] Univ Bari, Dipartmento Fis, Sez INFN, I-70126 Bari, Italy.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Scott, P (reprint author), McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H3A 2T8, Canada.
EM patscott@physics.mcgill.ca; savage@fysik.su.se; danning@fysik.su.se
RI Wiebusch, Christopher/G-6490-2012; Koskinen, David/G-3236-2014; Brunner,
Juergen/G-3540-2015; Maruyama, Reina/A-1064-2013; Sarkar,
Subir/G-5978-2011; Beatty, James/D-9310-2011; Tamburro,
Alessio/A-5703-2013; Botner, Olga/A-9110-2013; Hallgren,
Allan/A-8963-2013; Tjus, Julia/G-8145-2012
OI Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Wiebusch,
Christopher/0000-0002-6418-3008; Koskinen, David/0000-0002-0514-5917;
Brunner, Juergen/0000-0002-5052-7236; Maruyama,
Reina/0000-0003-2794-512X; Sarkar, Subir/0000-0002-3542-858X; Beatty,
James/0000-0003-0481-4952; Rott, Carsten/0000-0002-6958-6033;
Ter-Antonyan, Samvel/0000-0002-5788-1369; Schukraft,
Anne/0000-0002-9112-5479;
FU Lorne Trottier Chair in Astrophysics; Canadian Institute for Particle
Physics Theory Fellowship; Swedish Research Council [621-2010-3705,
621-2010-3301]; 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); 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 to
encourage scientific and technological research in industry (IWT);
Belgian Federal Science Policy - Office (Belspo); University of Oxford,
United Kingdom; Marsden Fund, New Zealand; Australian Research Council;
Japan Society for Promotion of Science (JSPS); Swiss National Science
Foundation (SNSF), Switzerland
FX We are grateful to Hamish Silverwood for helpful comments and
discussions. P. S. is supported by the Lorne Trottier Chair in
Astrophysics and a Canadian Institute for Particle Physics Theory
Fellowship. M. D. and K. H. acknowledge support from the Swedish
Research Council (Contract No. 621-2010-3705), as does J.E. (Contract
No. 621-2010-3301).; 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; Australian Research Council;
Japan Society for Promotion of Science (JSPS); the Swiss National
Science Foundation (SNSF), Switzerland.
NR 102
TC 18
Z9 18
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD NOV
PY 2012
IS 11
AR 057
DI 10.1088/1475-7516/2012/11/057
PG 33
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 053IA
UT WOS:000312263500040
ER
PT J
AU Klenzing, J
Rowland, D
AF Klenzing, J.
Rowland, D.
TI The fixed-bias Langmuir probe on the Communication/Navigation Outage
Forecast System satellite: Calibration and validation
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
ID FLOWING PLASMA; ION COLLECTION; SPHERE
AB A fixed-bias spherical Langmuir probe is included as part of the Vector Electric Field Instrument (VEFI) suite on the Communication/Navigation Outage Forecast System (C/NOFS) satellite. C/NOFS gathers data in the equatorial ionosphere between 400 and 860 km, where the primary constituent ions are H+ and O+. The ion current collected by the probe surface per unit plasma density is found to be a strong function of ion composition. The calibration of the collected current to an absolute density is discussed, and the performance of the spherical probe is compared to other in situ instruments on board the C/NOFS satellite. The application of the calibration is discussed with respect to future fixed-bias probes; in particular, it is demonstrated that some density fluctuations will be suppressed in the collected current if the plasma composition rapidly changes along with density. This is illustrated in the observation of plasma density enhancements on C/NOFS. [http://dx.doi.org/10.1063/1.4766333]
C1 [Klenzing, J.; Rowland, D.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
RP Klenzing, J (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Code 674, Greenbelt, MD 20771 USA.
EM jeffrey.klenzing@nasa.gov
RI Klenzing, Jeff/E-2406-2011; Rowland, Douglas/F-5589-2012
OI Klenzing, Jeff/0000-0001-8321-6074; Rowland, Douglas/0000-0003-0948-6257
FU USAF Space Test Program
FX The Communication/Navigation Outage Forecast System (C/NOFS) mission,
conceived and developed by the Air Force Research Laboratory (AFRL), is
sponsored and executed by the USAF Space Test Program. Thanks to F.
Simoes for useful comments on this manuscript and P. A. Roddy of AFRL
and R. A. Heelis of UT Dallas for providing data for the calibration
procedure.
NR 23
TC 0
Z9 0
U1 0
U2 3
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0034-6748
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD NOV
PY 2012
VL 83
IS 11
AR 114501
DI 10.1063/1.4766333
PG 5
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA 050DY
UT WOS:000312034400034
PM 23206077
ER
PT J
AU Sanjuan, J
Korytov, D
Mueller, G
Spannagel, R
Braxmaier, C
Preston, A
Livas, J
AF Sanjuan, J.
Korytov, D.
Mueller, G.
Spannagel, R.
Braxmaier, C.
Preston, A.
Livas, J.
TI Note: Silicon carbide telescope dimensional stability for space-based
gravitational wave detectors
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
AB Space-based gravitational wave detectors are conceived to detect gravitational waves in the low frequency range by measuring the distance between proof masses in spacecraft separated by millions of kilometers. One of the key elements is the telescope which has to have a dimensional stability better than 1 pm Hz(-1/2) at 3 mHz. In addition, the telescope structure must be light, strong, and stiff. For this reason a potential telescope structure consisting of a silicon carbide quadpod has been designed, constructed, and tested. We present dimensional stability results meeting the requirements at room temperature. Results at -60 degrees C are also shown although the requirements are not met due to temperature fluctuations in the setup. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4767247]
C1 [Sanjuan, J.; Korytov, D.; Mueller, G.] Univ Florida, Gainesville, FL 32611 USA.
[Spannagel, R.; Braxmaier, C.] Univ Appl Sci Konstanz HTWG, D-78462 Constance, Germany.
[Preston, A.; Livas, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sanjuan, J (reprint author), Univ Florida, Corner Gale Lemerand Dr & Museum Rd, Gainesville, FL 32611 USA.
FU NASA [NNX10AJ38G, NNX11AO26G]
FX The authors would like to thank J. I. Thorpe for fruitful discussions
and I. Pucher, A. Cordes, and A. Spector for helping on the experimental
setup. This work is supported by NASA Grant Nos. NNX10AJ38G and
NNX11AO26G.
NR 12
TC 7
Z9 7
U1 1
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 0034-6748
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD NOV
PY 2012
VL 83
IS 11
AR 116107
DI 10.1063/1.4767247
PG 3
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA 050DY
UT WOS:000312034400071
PM 23206114
ER
PT J
AU Feofilov, AG
Kutepov, AA
AF Feofilov, Artem G.
Kutepov, Alexander A.
TI Infrared Radiation in the Mesosphere and Lower Thermosphere: Energetic
Effects and Remote Sensing
SO SURVEYS IN GEOPHYSICS
LA English
DT Review
DE Infrared energy; Radiative transfer; Mesosphere lower thermosphere
ID ACCELERATED LAMBDA ITERATION; NONLOCAL THERMODYNAMIC-EQUILIBRIUM;
SCHUMANN-RUNGE CONTINUUM; SPACELAB 3 OBSERVATIONS; CO2 15-MU-M EMISSION;
HOT LUMINOUS STARS; NON-LTE PROBLEM; MIDDLE ATMOSPHERE; MU-M;
WATER-VAPOR
AB This paper discusses the formation mechanisms of infrared radiation in the mesosphere and lower thermosphere (MLT), the energetic effects of the radiative absorption/emission processes, and the retrieval of atmospheric parameters from infrared radiation measurements. In the MLT and above, the vibrational levels of the molecules involved in radiative transitions are not in local thermodynamic equilibrium (LTE) with the surrounding medium, and this then requires specific theoretical treatment. The non-LTE models for CO2, O-3, and H2O molecules are presented, and the radiative cooling/heating rates estimated for five typical atmospheric scenarios, from polar winter to polar summer, are shown. An optimization strategy for calculating the cooling/heating rates in general circulation models is proposed, and its accuracy is estimated for CO2. The sensitivity of the atmospheric quantities retrieved from infrared observations made from satellites to the non-LTE model parameters is shown.
C1 [Feofilov, Artem G.] Ecole Polytech, Meteorol Dynam Lab, Palaiseau, France.
[Kutepov, Alexander A.] Catholic Univ Amer, Washington, DC 20064 USA.
[Kutepov, Alexander A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Feofilov, AG (reprint author), Ecole Polytech, Meteorol Dynam Lab, Palaiseau, France.
EM artem.feofilov@lmd.polytechnique.fr
RI Feofilov, Artem/A-2271-2015
OI Feofilov, Artem/0000-0001-9924-4846
NR 148
TC 9
Z9 10
U1 2
U2 18
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 NOV
PY 2012
VL 33
IS 6
SI SI
BP 1231
EP 1280
DI 10.1007/s10712-012-9204-0
PG 50
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 054SU
UT WOS:000312364400003
ER
PT J
AU Bachelet, E
Fouque, P
Han, C
Gould, A
Albrow, MD
Beaulieu, JP
Bertin, E
Bond, IA
Christie, GW
Heyrovsky, D
Horne, K
Jorgensen, UG
Maoz, D
Mathiasen, M
Matsunaga, N
McCormick, J
Menzies, J
Nataf, D
Natusch, T
Oi, N
Renon, N
Tsapras, Y
Udalski, A
Yee, JC
Batista, V
Bennett, DP
Brillant, S
Caldwell, JAR
Cassan, A
Cole, A
Cook, KH
Coutures, C
Dieters, S
Dominik, M
Prester, DD
Donatowicz, J
Greenhill, J
Kains, N
Kane, SR
Marquette, JB
Martin, R
Pollard, KR
Sahu, KC
Street, RA
Wambsganss, J
Williams, A
Zub, M
Bos, M
Dong, SB
Drummond, J
Gaudi, BS
Graff, D
Janczak, J
Kaspi, S
Kozlowski, S
Lee, CU
Monard, LAG
Munoz, JA
Park, BG
Pogge, RW
Polishook, D
Shporer, A
Abe, F
Botzler, CS
Fukui, A
Furusawa, K
Hearnshaw, JB
Itow, Y
Korpela, AV
Ling, CH
Masuda, K
Matsubara, Y
Miyake, N
Muraki, Y
Ohnishi, K
Rattenbury, NJ
Saito, T
Sullivan, D
Sumi, T
Suzuki, D
Sweatman, WL
Tristram, PJ
Wada, K
Allan, A
Bode, MF
Bramich, DM
Clay, N
Fraser, SN
Hawkins, E
Kerins, E
Lister, TA
Mottram, CJ
Saunders, ES
Snodgrass, C
Steele, IA
Wheatley, PJ
Bozza, V
Browne, P
Burgdorf, MJ
Novati, SC
Dreizler, S
Finet, F
Glitrup, M
Grundahl, F
Harpsoe, K
Hessman, FV
Hinse, TC
Hundertmark, M
Liebig, C
Maier, G
Mancini, L
Rahvar, S
Ricci, D
Scarpetta, G
Skottfelt, J
Southworth, J
Surdej, J
Zimmer, F
AF Bachelet, E.
Fouque, P.
Han, C.
Gould, A.
Albrow, M. D.
Beaulieu, J. -P.
Bertin, E.
Bond, I. A.
Christie, G. W.
Heyrovsky, D.
Horne, K.
Jorgensen, U. G.
Maoz, D.
Mathiasen, M.
Matsunaga, N.
McCormick, J.
Menzies, J.
Nataf, D.
Natusch, T.
Oi, N.
Renon, N.
Tsapras, Y.
Udalski, A.
Yee, J. C.
Batista, V.
Bennett, D. P.
Brillant, S.
Caldwell, J. A. R.
Cassan, A.
Cole, A.
Cook, K. H.
Coutures, C.
Dieters, S.
Dominik, M.
Prester, D. Dominis
Donatowicz, J.
Greenhill, J.
Kains, N.
Kane, S. R.
Marquette, J. -B.
Martin, R.
Pollard, K. R.
Sahu, K. C.
Street, R. A.
Wambsganss, J.
Williams, A.
Zub, M.
Bos, M.
Dong, Subo
Drummond, J.
Gaudi, B. S.
Graff, D.
Janczak, J.
Kaspi, S.
Kozlowski, S.
Lee, C. -U.
Monard, L. A. G.
Munoz, J. A.
Park, B. -G.
Pogge, R. W.
Polishook, D.
Shporer, A.
Abe, F.
Botzler, C. S.
Fukui, A.
Furusawa, K.
Hearnshaw, J. B.
Itow, Y.
Korpela, A. V.
Ling, C. H.
Masuda, K.
Matsubara, Y.
Miyake, N.
Muraki, Y.
Ohnishi, K.
Rattenbury, N. J.
Saito, To.
Sullivan, D.
Sumi, T.
Suzuki, D.
Sweatman, W. L.
Tristram, P. J.
Wada, K.
Allan, A.
Bode, M. F.
Bramich, D. M.
Clay, N.
Fraser, S. N.
Hawkins, E.
Kerins, E.
Lister, T. A.
Mottram, C. J.
Saunders, E. S.
Snodgrass, C.
Steele, I. A.
Wheatley, P. J.
Bozza, V.
Browne, P.
Burgdorf, M. J.
Novati, S. Calchi
Dreizler, S.
Finet, F.
Glitrup, M.
Grundahl, F.
Harpsoe, K.
Hessman, F. V.
Hinse, T. C.
Hundertmark, M.
Liebig, C.
Maier, G.
Mancini, L.
Rahvar, S.
Ricci, D.
Scarpetta, G.
Skottfelt, J.
Southworth, J.
Surdej, J.
Zimmer, F.
CA PLANET Collaboration
FUN Collaboration
MOA Collaboration
RoboNet-II Collaboration
MiNDSTEp Consortium
TI A brown dwarf orbiting an M-dwarf: MOA 2009-BLG-411L
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE binaries: general; gravitational lensing: micro; stars: individual: MOA
2009-BLG-411L
ID MAGNIFICATION MICROLENSING EVENTS; SURFACE BRIGHTNESS RELATIONS;
DIFFERENCE IMAGE-ANALYSIS; CLUMP ABSOLUTE MAGNITUDE; GALACTIC BULGE
FIELDS; INTERSTELLAR EXTINCTION; BINARY INTERPRETATIONS; CENTRAL
PERTURBATIONS; PLANETARY SYSTEMS; MASS PLANET
AB Context. Caustic crossing is the clearest signature of binary lenses in microlensing. In the present context, this signature is diluted by the large source star but a detailed analysis has allowed the companion signal to be extracted.
Aims. MOA 2009-BLG-411 was detected on August 5, 2009 by the MOA-Collaboration. Alerted as a high-magnification event, it was sensitive to planets. Suspected anomalies in the light curve were not confirmed by a real-time model, but further analysis revealed small deviations from a single lens extended source fit.
Methods. Thanks to observations by all the collaborations, this event was well monitored. We first decided to characterize the source star properties by using a more refined method than the classical one: we measure the interstellar absorption along the line of sight in five different passbands (VIJHK). Secondly, we model the lightcurve by using the standard technique: make (s, q, alpha) grids to look for local minima and refine the results by using a downhill method (Markov chain Monte Carlo). Finally, we use a Galactic model to estimate the physical properties of the lens components.
Results. We find that the source star is a giant G star with radius 9 R-circle dot. The grid search gives two local minima, which correspond to the theoretical degeneracy s = s(-1). We find that the lens is composed of a brown dwarf secondary of mass M-S = 0.05 M-circle dot orbiting a primary M-star of mass M-P = 0.18 M-circle dot. We also reveal a new mass-ratio degeneracy for the central caustics of close binaries.
Conclusions. As far as we are aware, this is the first detection using the microlensing technique of a binary system in our Galaxy composed of an M-star and a brown dwarf.
C1 [Gould, A.; Nataf, D.; Yee, J. C.; Gaudi, B. S.; Janczak, J.; Kozlowski, S.; Pogge, R. W.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Albrow, M. D.; Pollard, K. R.; Hearnshaw, J. B.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand.
[Brillant, S.; Snodgrass, C.] European So Observ, Santiago 19, Chile.
[Kains, N.; Bramich, D. M.] European So Observ, D-85748 Garching, Germany.
[Beaulieu, J. -P.; Bertin, E.; Batista, V.; Cassan, A.; Coutures, C.; Dieters, S.; Marquette, J. -B.] Univ Paris 06, Inst Astrophys Paris, CNRS, F-75014 Paris, France.
[Wambsganss, J.; Zub, M.; Liebig, C.; Maier, G.; Zimmer, F.] Heidelberg Univ, ARI, Zentrum Astron, D-69120 Heidelberg, Germany.
[Horne, K.; Dominik, M.; Kains, N.; Browne, P.; Liebig, C.] Univ St Andrews, Sch Phys & Astron, Scottish Univ Phys Alliance, St Andrews KY16 9SS, Fife, Scotland.
Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Bennett, D. P.; Caldwell, J. A. R.] Univ Texas, McDonald Observ, Ft Davis, TX 79734 USA.
[Cook, K. H.] Lawrence Livermore Natl Lab, IGPP, Livermore, CA 94551 USA.
[Prester, D. Dominis] Univ Rijeka, Fac Arts & Sci, Dept Phys, Rijeka 51000, Croatia.
[Donatowicz, J.] Vienna Univ Technol, Dept Comp, A-1060 Vienna, Austria.
[Cole, A.; Greenhill, J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
[Kane, S. R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Martin, R.; Williams, A.] Perth Observ, Perth, WA 6076, Australia.
[Menzies, J.] S African Astron Observ, ZA-7925 Observatory, South Africa.
[Sahu, K. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Han, C.] Chonnam Natl Univ, Inst Basic Sci Res, Dept Phys, Chonju 361763, South Korea.
[Lee, C. -U.; Park, B. -G.; Hinse, T. C.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Monard, L. A. G.] Bronberg Observ, Pretoria, South Africa.
[Udalski, A.; Kozlowski, S.] Univ Warsaw Observ, Warsaw, Poland.
Univ Concepcion, Dept Fis, Astron Grp, Concepcion, Chile.
[Tristram, P. J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Bond, I. A.; Ling, C. H.; Sweatman, W. L.] Massey Univ, Inst Informat & Math Sci, N Shore Mail Ctr, Auckland, New Zealand.
[Abe, F.; Furusawa, K.; Itow, Y.; Masuda, K.; Matsubara, Y.; Miyake, N.; Sumi, T.; Suzuki, D.; Wada, K.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan.
[Kerins, E.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Muraki, Y.] Konan Univ, Dept Phys, Kobe, Hyogo 6588501, Japan.
[Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan.
[Botzler, C. S.; Rattenbury, N. J.] Univ Auckland, Dept Phys, Auckland 1142, New Zealand.
[Saito, To.] Tokyo Metropolitan Coll Ind Technol, Tokyo 1160003, Japan.
Nagoya Univ, Fac Sci, Dept Phys & Astrophys, Nagoya, Aichi 4648602, Japan.
[Korpela, A. V.; Sullivan, D.] Mt John Observ, Lake Tekapo, New Zealand.
[Tsapras, Y.; Street, R. A.; Hawkins, E.; Lister, T. A.; Saunders, E. S.] Las Cumbres Observ, Goleta, CA 93117 USA.
[Bode, M. F.; Clay, N.; Fraser, S. N.; Mottram, C. J.; Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Allan, A.; Saunders, E. S.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Wheatley, P. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Street, R. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Bachelet, E.; Fouque, P.] Univ Toulouse, IRAP, CNRS, F-31400 Toulouse, France.
[Jorgensen, U. G.; Mathiasen, M.; Harpsoe, K.; Hinse, T. C.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Jorgensen, U. G.; Mathiasen, M.; Harpsoe, K.; Hinse, T. C.; Skottfelt, J.] Univ Copenhagen, Ctr Star & Planet Format, DK-2100 Copenhagen, Denmark.
Univ Observ Munich, D-81679 Munich, Germany.
[Mancini, L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Heyrovsky, D.] Charles Univ Prague, Inst Theoret Phys, CR-18000 Prague, Czech Republic.
Bellatrix Observ, I-03023 Ceccano, Italy.
[Bozza, V.; Novati, S. Calchi; Scarpetta, G.] IIASS, Sez Napoli, INFN, Vietri Sur Mare, Italy.
[Botzler, C. S.; Bozza, V.; Novati, S. Calchi; Scarpetta, G.] Univ Salerno, Dipartimento Fis, Fisciano, Italy.
[Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran, Iran.
[Dreizler, S.; Hessman, F. V.; Hundertmark, M.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Finet, F.; Ricci, D.; Surdej, J.] Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Southworth, J.] Univ Keele, Astrophys Grp, Newcastle Under Lyme ST5 5BG, England.
Osserv Astron Brera, INAF, I-23846 Merate, LC, Italy.
[Burgdorf, M. J.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany.
[Burgdorf, M. J.] NASA, SOFIA Sci Ctr, Ames Res Ctr, Moffett Field, CA 94035 USA.
Kyoto Univ, Dept Astron, Kyoto 6068502, Japan.
[Tsapras, Y.] Queen Mary Univ London, Sch Math Sci, London E1 4NS, England.
[Drummond, J.] Possum Observ, Patutahi, Gisbourne, New Zealand.
[Maoz, D.; Kaspi, S.; Polishook, D.; Shporer, A.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Maoz, D.; Kaspi, S.; Polishook, D.; Shporer, A.] Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel.
[Christie, G. W.; Natusch, T.] Auckland Observ, Auckland, New Zealand.
[McCormick, J.] Ctr Backyard Astrophys, Farm Cove Observ, Auckland, New Zealand.
[Matsunaga, N.] Univ Tokyo, Inst Astron, Kiso Observ, Nagano 3970101, Japan.
[Oi, N.] Grad Univ Adv Studies Sokendai, Mitaka, Tokyo 1818588, Japan.
[Renon, N.] Univ Toulouse, DTSI Univ Paul Sabatier, CALMIP, F-31062 Toulouse, France.
[Rahvar, S.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
[Mancini, L.] Int Inst Adv Sci Studies, I-84019 Vietri Sul Mare, SA, Italy.
[Mancini, L.] Univ Salerno, Dept Phys, I-84084 Fisciano, SA, Italy.
[Glitrup, M.; Grundahl, F.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Bos, M.] Molehill Astron Observ, Auckland, New Zealand.
[Munoz, J. A.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain.
Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
[Dong, Subo] Inst Adv Study, Princeton, NJ 08540 USA.
[Natusch, T.] AUT Univ, Auckland, New Zealand.
[Fukui, A.] Natl Inst Nat Sci, Natl Astron Observ Japan, Okayama Astrophys Observ, Kamogatacho, Okayama 7190232, Japan.
EM gwchristie@christie.org.nz; farmcoveobs@xtra.co.nz;
john_drummond@xtra.co.nz; shai@wise.tau.ac.il; shporer@wise.tau.ac.il
RI Kane, Stephen/B-4798-2013; Greenhill, John/C-8367-2013; Kozlowski,
Szymon/G-4799-2013; Williams, Andrew/K-2931-2013; Zimmer,
Fabian/M-4765-2014; Heyrovsky, David/A-2031-2015; Hundertmark,
Markus/C-6190-2015; Rahvar, Sohrab/A-9350-2008;
OI Ricci, Davide/0000-0002-9790-0552; Snodgrass, Colin/0000-0001-9328-2905;
Wheatley, Peter/0000-0003-1452-2240; Kozlowski,
Szymon/0000-0003-4084-880X; Williams, Andrew/0000-0001-9080-0105;
Heyrovsky, David/0000-0002-5198-5343; Hundertmark,
Markus/0000-0003-0961-5231; Rahvar, Sohrab/0000-0002-7084-5725; Dominik,
Martin/0000-0002-3202-0343; Cole, Andrew/0000-0003-0303-3855
FU French Agence Nationale de la Recherche; Czech Science Foundation [GACR
205/07/0824]; Czech Ministry of Education [MSM0021620860]; National
Research Foundation of Korea [2009-0081561]; Department for Culture,
Arts and Leisure, Northern Ireland, UK; Korea Research Council for
Fundamental Science and Technology (KRCF); Communaute francaise de
Belgique - Actions de recherche concertees - Academie universitaire
Wallonie-Europe; European Community [229517]; NSF [AST-1103471,
2009068160]; NASA [NNG04GL51G]; Qatar Foundation through QNRF
[NPRP-09-476-1-78]; Korea Astronomy and Space Science Institute (KASI)
[2012-1-410-02]; [JSPS18253002]; [JSPS20340052]; [JSPS20740104]
FX We are very grateful to the observatories that support our science
(Bronberg, Canopus, CTIO, ESO, IRSF, LCOGT, Liverpool, LOAO, MOA, OGLE,
Perth, SAAO, Skinakas) via the generous allocation of time that makes
this work possible. The operation of Canopus Observatory is in part
supported by a financial contribution from David Warren. Allocation of
the Holmes grant from the French Agence Nationale de la Recherche has
been indispensable to finance observing trips and travel costs for
meetings, and is gratefully acknowledged here. D. H. was supported by
Czech Science Foundation grant GACR 205/07/0824 and by the Czech
Ministry of Education project MSM0021620860. C. H. was supported by the
grant 2009-0081561 of National Research Foundation of Korea. T. C. H.
was financed for his astronomical research at the Armagh Observatory by
the Department for Culture, Arts and Leisure, Northern Ireland, UK and
is now supported by the Korea Research Council for Fundamental Science
and Technology (KRCF) via the Young Scientist Research Fellowship
Program. MOA project was funded by JSPS18253002 and JSPS20340052. T. S.
was funded by JSPS20740104. D. R. and J.S. acknowledge support from the
Communaute francaise de Belgique - Actions de recherche concertees -
Academie universitaire Wallonie-Europe. P. F. wishes to thank Noriyuki
Matsunaga for discussions about the interplay between adopted distance
and derived extinction. The research leading to these results has
received funding from the European Community's Seventh Framework
Programme (/FP7/2007-2013/) under grant agreement No 229517. A. Gould
acknowledges support from NSF AST-1103471. B. S. Gaudi, A. Gould, and R.
W. Pogge acknowledge support from NASA grant NNG04GL51G. Work by J. C.
Yee is supported by a National Science Foundation Graduate Research
Fellowship under Grant No. 2009068160. Work by S. Dong was performed
under contract with the California Institute of Technology (Caltech)
funded by NASA through the Sagan Fellowship Program. The RoboNet team is
supported by the Qatar Foundation through QNRF grant NPRP-09-476-1-78.
CUL acknowledges support by Korea Astronomy and Space Science Institute
(KASI) grant 2012-1-410-02. This publication makes use of data products
from the 2MASS project, as well as the SIMBAD database, Aladin and
Vizier catalogue operation tools (CDS Strasbourg, France). The Two
Micron All Sky Survey 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. This work was
granted access to the HPC resources of CALMIP under the allocation
2012-[1131].
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EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD NOV
PY 2012
VL 547
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PG 12
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SC Astronomy & Astrophysics
GA 036MZ
UT WOS:000311031700055
ER
PT J
AU Furst, F
Pottschmidt, K
Kreykenbohm, I
Muller, S
Kuhnel, M
Wilms, J
Rothschild, RE
AF Fuerst, F.
Pottschmidt, K.
Kreykenbohm, I.
Mueller, S.
Kuehnel, M.
Wilms, J.
Rothschild, R. E.
TI Staring at 4U 1909+07 with Suzaku
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE accretion, accretion disks; X-rays: binaries; stars: neutron
ID X-RAY PULSARS; SPECTROSCOPY; X1908+075; ACCRETION; EMISSION; BINARY;
PERIOD; LINES
AB We present an analysis of the neutron star high mass X-ray binary (HMXB) 4U 1909+07 mainly based on Suzaku data. We extend the pulse period evolution, which behaves in a random-walk like manner, indicative of direct wind accretion. Studying the spectral properties of 4U 1909+07 between 0.5 to 90 keV we find that a power-law with an exponential cutoff can describe the data well, when additionally allowing for a blackbody or a partially covering absorber at low energies.
We find no evidence for a cyclotron resonant scattering feature (CRSF), a feature seen in many other neutron star HMXBs sources. By performing pulse phase resolved spectroscopy we investigate the origin of the strong energy dependence of the pulse profile, which evolves from a broad two-peak profile at low energies to a profile with a single, narrow peak at energies above 20 keV. Our data show that it is very likely that a higher folding energy in the high energy peak is responsible for this behavior. This in turn leads to the assumption that we observe the two magnetic poles and their respective accretion columns at different phases, and that these accretion columns have slightly different physical conditions.
C1 [Fuerst, F.; Kreykenbohm, I.; Mueller, S.; Kuehnel, M.; Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany.
[Fuerst, F.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
[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.
[Rothschild, R. E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Fuerst, F.; Kreykenbohm, I.; Mueller, S.; Kuehnel, M.; Wilms, J.] Univ Erlangen Nurnberg, ECAP, D-96049 Bamberg, Germany.
RP Furst, F (reprint author), Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte, Sternwartstr 7, D-96049 Bamberg, Germany.
EM felix.fuerst@sternwarte.uni-erlangen.de
RI Wilms, Joern/C-8116-2013; Kreykenbohm, Ingo/H-9659-2013; XRAY,
SUZAKU/A-1808-2009
OI Wilms, Joern/0000-0003-2065-5410; Kreykenbohm, Ingo/0000-0001-7335-1803;
FU Bundesministerium fur Wirtschaft und Technologie through DLR [50 OR
0808, 50 OR 0905, 50 OR 1113]; ESA member states
FX This work was supported by the Bundesministerium fur Wirtschaft und
Technologie through DLR grants 50 OR 0808, 50 OR 0905, and 50 OR 1113.
F. F. thanks GSFC for the hospitality. This research has made use of
data obtained from the Suzaku satellite, a collaborative mission between
the space agencies of Japan (JAXA) and the USA (NASA). This work is
furthermore based on observations with INTEGRAL, an ESA project with
instruments and science data centre funded by ESA member states
(especially the PI countries: Denmark, France, Germany, Italy,
Switzerland, Spain), Czech Republic and Poland, and with the
participation of Russia and the USA. We have made use of NASA's
Astrophysics Data System. We like to thank J. E. Davis for the slxfig
module which was used to create all plots throughout this paper.
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JI Astron. Astrophys.
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PY 2012
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SC Astronomy & Astrophysics
GA 036MZ
UT WOS:000311031700002
ER
PT J
AU Lebzelter, T
Heiter, U
Abia, C
Eriksson, K
Ireland, M
Neilson, H
Nowotny, W
Maldonado, J
Merle, T
Peterson, R
Plez, B
Short, CI
Wahlgren, GM
Worley, C
Aringer, B
Bladh, S
de Laverny, P
Goswami, A
Mora, A
Norris, RP
Recio-Blanco, A
Scholz, M
Thevenin, F
Tsuji, T
Kordopatis, G
Montesinos, B
Wing, RF
AF Lebzelter, T.
Heiter, U.
Abia, C.
Eriksson, K.
Ireland, M.
Neilson, H.
Nowotny, W.
Maldonado, J.
Merle, T.
Peterson, R.
Plez, B.
Short, C. I.
Wahlgren, G. M.
Worley, C.
Aringer, B.
Bladh, S.
de Laverny, P.
Goswami, A.
Mora, A.
Norris, R. P.
Recio-Blanco, A.
Scholz, M.
Thevenin, F.
Tsuji, T.
Kordopatis, G.
Montesinos, B.
Wing, R. F.
TI Comparative modelling of the spectra of cool giants
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: atmospheres; stars: late-type; stars: abundances; stars:
fundamental parameters
ID HIGH-RESOLUTION SPECTROSCOPY; EFFECTIVE TEMPERATURE SCALE; SOLAR
CHEMICAL-COMPOSITION; NEUTRAL HYDROGEN-ATOMS; METAL-POOR STARS;
LINE-DATA-BASE; OPTICAL INTERFEROMETRY; ANGULAR DIAMETERS;
INFRARED-SPECTRA; RICH GIANTS
AB Context. Our ability to extract information from the spectra of stars depends on reliable models of stellar atmospheres and appropriate techniques for spectral synthesis. Various model codes and strategies for the analysis of stellar spectra are available today.
Aims. We aim to compare the results of deriving stellar parameters using different atmosphere models and different analysis strategies. The focus is set on high-resolution spectroscopy of cool giant stars.
Methods. Spectra representing four cool giant stars were made available to various groups and individuals working in the area of spectral synthesis, asking them to derive stellar parameters from the data provided. The results were discussed at a workshop in Vienna in 2010. Most of the major codes currently used in the astronomical community for analyses of stellar spectra were included in this experiment.
Results. We present the results from the different groups, as well as an additional experiment comparing the synthetic spectra produced by various codes for a given set of stellar parameters. Similarities and differences of the results are discussed.
Conclusions. Several valid approaches to analyze a given spectrum of a star result in quite a wide range of solutions. The main causes for the differences in parameters derived by different groups seem to lie in the physical input data and in the details of the analysis method. This clearly shows how far from a definitive abundance analysis we still are.
C1 [Lebzelter, T.; Nowotny, W.] Univ Vienna, A-1180 Vienna, Austria.
[Heiter, U.; Eriksson, K.; Bladh, S.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Abia, C.] Univ Granada, Depto Fis Teor & Cosmos, E-18071 Granada, Spain.
[Ireland, M.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia.
[Neilson, H.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Maldonado, J.] Univ Autonoma Madrid, Dpto Fis Teor, Fac Ciencias, E-28049 Madrid, Spain.
[Merle, T.; Worley, C.; de Laverny, P.; Recio-Blanco, A.; Thevenin, F.; Kordopatis, G.] Univ Nice Sophia Antipolis, CNRS, UMR 6202, Observ Cote Azur, F-06304 Nice 04, France.
[Peterson, R.] Astrophys Adv UCOLick, Palo Alto, CA 94301 USA.
[Plez, B.] Univ Montpellier 2, CNRS, Lab Universe & Particules Montpellier, F-34095 Montpellier, France.
[Short, C. I.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Wahlgren, G. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Aringer, B.] INAF OAPD, I-35122 Padua, Italy.
[Goswami, A.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
[Mora, A.] ESA ESAC Gaia SOC, Madrid 28691, Spain.
[Norris, R. P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Scholz, M.] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[Tsuji, T.] Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan.
[Montesinos, B.] ESAC, Ctr Astrobiol INTA CSIC, Madrid 28691, Spain.
[Wing, R. F.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Ireland, M.] Australian Astron Observ, Epping, NSW 1710, Australia.
[Scholz, M.] Univ Sydney, Sch Phys, SIfA, Sydney, NSW 2006, Australia.
RP Lebzelter, T (reprint author), Univ Vienna, Turkenschanzstr 17, A-1180 Vienna, Austria.
EM lebzelter@univie.ac.at
RI Plez, Bertrand/G-6697-2011; Montesinos, Benjamin/C-3493-2017
OI Plez, Bertrand/0000-0002-0398-4434; Montesinos,
Benjamin/0000-0002-7982-2095
FU ESF within the GREAT network initiative; ESF through the GREAT
initiative; Robert F. Wing Support Fund at Ohio State University;
Department of Astronomy at the University of Vienna; Austrian Science
Fund FWF [P20046, P21988, P23737, P23006]; Swedish National Space Board;
Spanish grant [AYA2008-08013-C03-03]; Alexander von Humboldt foundation;
Swedish Research Council; CNES; OCA; ESO; CNRS
FX Kindly funded by the ESF within the GREAT network initiative.; The
workshop on which this paper is based was kindly supported by the ESF
through the GREAT initiative, by the Robert F. Wing Support Fund at Ohio
State University, and the Department of Astronomy at the University of
Vienna. The work of T. L. was funded by the Austrian Science Fund FWF
projects P20046, P21988, and P23737. U. H. acknowledges support from the
Swedish National Space Board. C. A. acknowledges partial support by the
Spanish grant AYA2008-08013-C03-03. H.N. acknowledges financial support
from the Alexander von Humboldt foundation. K. E. gratefully
acknowledges support from The Swedish Research Council. C. W.
acknowledges the financial support of CNES, OCA and ESO. G. K.
acknowledges the financial support of CNES and CNRS. U. H., K. E., T.
M., and F. T. acknowledge the role of the SAM collaboration
(http://www.anst.uu.se/ulhei450/GaiaSAM/) in stimulating this research
through regular workshops. B. A. thanks for support by the Austrian
Science Fund FWF under project number P23006. We thank all participants
in the workshop for contributing to the fruitful discussions there. We
thank B. Edvardsson and B. Gustafsson for comments on a draft version of
the paper. Based on data obtained within the Gaia DPAC (Data Processing
and Analysis Consortium) and coordinated by the GBOG (Ground-Based
Observations for Gaia) working group.
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JI Astron. Astrophys.
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PY 2012
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SC Astronomy & Astrophysics
GA 036MZ
UT WOS:000311031700108
ER
PT J
AU Melandri, A
Pian, E
Ferrero, P
D'Elia, V
Walker, ES
Ghirlanda, G
Covino, S
Amati, L
D'Avanzo, P
Mazzali, PA
Della Valle, M
Guidorzi, C
Antonelli, LA
Bernardini, MG
Bersier, D
Bufano, F
Campana, S
Castro-Tirado, AJ
Chincarini, G
Deng, J
Filippenko, AV
Fugazza, D
Ghisellini, G
Kouveliotou, C
Maeda, K
Marconi, G
Masetti, N
Nomoto, K
Palazzi, E
Patat, F
Piranomonte, S
Salvaterra, R
Saviane, I
Starling, RLC
Tagliaferri, G
Tanaka, M
Vergani, SD
AF Melandri, A.
Pian, E.
Ferrero, P.
D'Elia, V.
Walker, E. S.
Ghirlanda, G.
Covino, S.
Amati, L.
D'Avanzo, P.
Mazzali, P. A.
Della Valle, M.
Guidorzi, C.
Antonelli, L. A.
Bernardini, M. G.
Bersier, D.
Bufano, F.
Campana, S.
Castro-Tirado, A. J.
Chincarini, G.
Deng, J.
Filippenko, A. V.
Fugazza, D.
Ghisellini, G.
Kouveliotou, C.
Maeda, K.
Marconi, G.
Masetti, N.
Nomoto, K.
Palazzi, E.
Patat, F.
Piranomonte, S.
Salvaterra, R.
Saviane, I.
Starling, R. L. C.
Tagliaferri, G.
Tanaka, M.
Vergani, S. D.
TI The optical SN2012bz associated with the long GRB120422A
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gamma-ray burst: general; supernovae: individual: SN2012bz
ID GAMMA-RAY BURST; 25 APRIL 1998; LIGHT-CURVE; SUPERNOVA CONNECTION;
SPECTRAL MODELS; GRB 100316D; AFTERGLOW; GRB-030329; GRB-031203;
GRB-980425
AB Aims. The association of Type Ic supernovae (SNe) with long-duration gamma-ray bursts (GRBs) is well established. We endeavor, through accurate ground-based observational campaigns, to characterize these SNe at increasingly high redshifts.
Methods. We obtained a series of optical photometric and spectroscopic observations of the Type Ic SN2012bz associated with the Swift long-duration GRB120422A (redshift z = 0.283) using the 3.6-m TNG and the 8.2-m VLT telescopes during the time interval between 4 and 36 days after the burst.
Results. The peak times of the light curves of SN2012bz in various optical filters differ, with the B-band and i'-band light curves reaching maximum at 9 +/- 4 and 23 +/- 3 rest-frame days, respectively. The bolometric light curve has been derived from individual bands photometric measurements, but no correction for the unknown contribution in the near-infrared (probably around 10-15%) has been applied. Therefore, the present light curve should be considered as a lower limit to the actual UV-optical-IR bolometric light curve. This pseudo-bolometric curve reaches its maximum (M-bol = -18.56 +/- 0.06) at 13 +/- 1 rest-frame days; it is similar in shape and luminosity to the bolometric light curves of the SNe associated with z < 0.2 GRBs and more luminous than those of SNe associated with X-ray flashes (XRFs). A comparison with the model generated for the bolometric light curve of SN2003dh suggests that SN2012bz produced only about 15% less Ni-56 than SN2003dh, about 0.35 M-circle dot. Similarly the VLT spectra of SN2012bz, after correction for Galactic extinction and for the contribution of the host galaxy, suggest comparable explosion parameters with those observed in SN2003dh (E-K similar to 3.5 x 10(52) erg, M-ej similar to 7 M-circle dot) and a similar progenitor mass (similar to 25-40 M-circle dot). GRB120422A is consistent with the E-peak -E-iso and the E-X,E-iso -E-gamma,E-iso -E-peak relations. GRB120422A / SN2012bz shows the GRB-SN connection at the highest redshift so far accurately monitored both photometrically and spectroscopically.
C1 [Melandri, A.; Ghirlanda, G.; Covino, S.; D'Avanzo, P.; Bernardini, M. G.; Campana, S.; Chincarini, G.; Fugazza, D.; Ghisellini, G.; Tagliaferri, G.; Vergani, S. D.] INAF Brera Astron Observ, I-23807 Merate, LC, Italy.
[Pian, E.; Walker, E. S.] Scuola Normale Super Pisa, I-56126 Pisa, Italy.
[Pian, E.] INAF Trieste Astron Observ, I-34143 Trieste, Italy.
[Pian, E.] INFN, Sez Pisa, I-56127 Pisa, Italy.
[Ferrero, P.] Inst Astrofis Canarias, Tenerife 38200, Spain.
[Ferrero, P.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[D'Elia, V.] ASI, Sci Data Ctr, I-00044 Frascati, Italy.
[D'Elia, V.; Antonelli, L. A.; Piranomonte, S.] INAF Roma Astron Observ, I-00040 Monte Porzio Catone, Italy.
[Amati, L.; Masetti, N.; Palazzi, E.] IASF Bologna, INAF, I-40129 Bologna, Italy.
[Mazzali, P. A.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Mazzali, P. A.] INAF Padova Astron Observ, I-35122 Padua, Italy.
[Della Valle, M.] INAF Capodimonte Astron Observ, I-80131 Naples, Italy.
[Della Valle, M.] ICRANET, I-65122 Pescara, Italy.
[Guidorzi, C.] Univ Ferrara, Dept Phys, I-44122 Ferrara, Italy.
[Bersier, D.] Liverpool John Moores Univ, ARI, Birkenhead CH41 1LD, Merseyside, England.
[Bufano, F.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile.
[Castro-Tirado, A. J.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain.
[Deng, J.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Kouveliotou, C.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Maeda, K.; Nomoto, K.; Saviane, I.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan.
[Marconi, G.] European So Observ, Santiago 19, Chile.
[Patat, F.] European So Observ, D-85748 Garching, Germany.
[Salvaterra, R.] IASF Milano, INAF, I-20133 Milan, Italy.
[Starling, R. L. C.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Tanaka, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Vergani, S. D.] Univ Paris Diderot, CNRS, Observ Paris, GEPI, F-92190 Meudon, France.
RP Melandri, A (reprint author), INAF Brera Astron Observ, Via E Bianchi 46, I-23807 Merate, LC, Italy.
EM andrea.melandri@brera.inaf.it
RI Nomoto, Ken'ichi/A-4393-2011; Palazzi, Eliana/N-4746-2015; Amati,
Lorenzo/N-5586-2015;
OI Ghisellini, Gabriele/0000-0002-0037-1974; Della Valle,
Massimo/0000-0003-3142-5020; Patat, Ferdinando/0000-0002-0537-3573;
Salvaterra, Ruben/0000-0002-9393-8078; Covino,
Stefano/0000-0001-9078-5507; Masetti, Nicola/0000-0001-9487-7740;
Tagliaferri, Gianpiero/0000-0003-0121-0723; Pian,
Elena/0000-0001-8646-4858; Ghirlanda, Giancarlo/0000-0001-5876-9259;
Castro-Tirado, A. J./0000-0003-2999-3563; Amati,
Lorenzo/0000-0001-5355-7388; Palazzi, Eliana/0000-0002-8691-7666;
Campana, Sergio/0000-0001-6278-1576; D'Elia, Valerio/0000-0002-7320-5862
FU VLT observation planning; PRIN INAF; PRIN-MIUR [2009ERC3HT]; ASI INAF
[I/088/06/0, I/011/07/0]; FONDECYT [3120227]; Royal Society; US NSF
[AST-0908886, AST-1211916]; TABASGO Foundation; Christopher R. Redlich
Fund
FX We thank the anonymous referee for valuable comments and suggestions
that improved the paper. We thank the TNG staff, in particular W.
Boschin, M. Cecconi, L. di Fabrizio, F. Ghinassi, A. Harutyunyan, and M.
Pedani, for their valuable support with TNG observations, and the
Paranal Science Operations Team, in particular H. Boffin, S. Brillant,
D. Gadotti, D. Jones, M. Rodrigues, L. Schmidtobreick, and J. Smoker. We
are grateful to D. Malesani, J. Fynbo, N. Tanvir, and K. Wiersema for
their support with VLT observation planning. We acknowledge support from
PRIN INAF 2009 and 2011, PRIN-MIUR grant 2009ERC3HT and from grants ASI
INAF I/088/06/0 and I/011/07/0. E. Pian is grateful for hospitality at
the ESO Headquarters in Santiago, where part of this work was developed.
F.B. acknowledges support from FONDECYT through Postdoctoral grant
3120227. J.D. is supported by the 973 Program of China (Grant No.
2009CB824800). R.L.C.S. is supported by a Royal Society Fellowship. A.
V. F. is grateful for the support of US NSF grants AST-0908886 and
AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich
Fund.
NR 92
TC 26
Z9 26
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 NOV
PY 2012
VL 547
AR A82
DI 10.1051/0004-6361/201219879
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 036MZ
UT WOS:000311031700082
ER
PT J
AU Valcarce, AAR
Catelan, M
Sweigart, AV
AF Valcarce, A. A. R.
Catelan, M.
Sweigart, A. V.
TI Effects of helium enrichment in globular clusters I. Theoretical plane
with PGPUC stellar evolution code
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: evolution; stars: general; stars: horizontal-branch; globular
clusters: general
ID HORIZONTAL-BRANCH STARS; RED GIANT BRANCH; POPULATION-II STARS;
METAL-POOR STARS; THERMONUCLEAR REACTION-RATES; COLOR-MAGNITUDE DIAGRAM;
DOUBLE SUBGIANT BRANCH; 2ND PARAMETER PROBLEM; MAIN-SEQUENCE STARS;
RELATIVE AGES
AB Aims. Recently, the study of globular cluster (GC) color-magnitude diagrams (CMDs) has shown that some of them harbor multiple populations with different chemical compositions and/or ages. In the first case, the most common candidate is a spread in the initial helium abundance, but this quantity is difficult to determine spectroscopically due to the fact that helium absorption lines are not present in cooler stars, whereas for hotter GC stars gravitational settling of helium becomes important. As a consequence, indirect methods to determine the initial helium abundance among populations are necessary. For that reason, in this series of papers, we investigate the effects of a helium enrichment in populations covering the range of GC metallicities.
Methods. In this first paper, we present the theoretical evolutionary tracks, isochrones, and zero-age horizontal branch (ZAHB) loci calculated with the Princeton-Goddard-PUC (PGPUC) stellar evolutionary code, which has been updated with the most recent input physics and compared with other theoretical databases. The chemical composition grid covers 9 metallicities ranging from Z = 1.60 x 10(-4) to 1.57 x 10(-2) (-2.25 less than or similar to [Fe/H] less than or similar to -0.25), 7 helium abundances from Y = 0.230 to 0.370, and an alpha-element enhancement of [alpha/Fe] = 0.3.
Results. The effects of different helium abundances that can be observed in isochrones are: splits in the main sequence (MS), differences in the luminosity (L) and effective temperature (T-eff) of the turn off point, splits in the sub giant branch being more prominent for lower ages or higher metallicities, splits in the lower red giant branch (RGB) being more prominent for higher ages or higher metallicities, differences in L of the RGB bump (with small changes in T-eff), and differences in L at the RGB tip. At the ZAHB, when Y is increased there is an increase of L for low T-eff, which is affected in different degrees depending on the age of the GC being studied. Finally, the ZAHB morphology distribution depending on the age explains how for higher GC metallicities a population with higher helium abundance could be hidden at the red ZAHB locus.
C1 [Valcarce, A. A. R.; Catelan, M.] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 7820436, Chile.
[Valcarce, A. A. R.] Univ Fed Rio Grande do Norte, Dept Fis, BR-59072970 Natal, RN, Brazil.
[Valcarce, A. A. R.; Catelan, M.] Milky Way Millennium Nucleus, Santiago 7820436, Chile.
[Valcarce, A. A. R.; Catelan, M.] Pontificia Univ Catolica Chile, Ctr Astroingn, Santiago 7820436, Chile.
[Sweigart, A. V.] NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA.
RP Valcarce, AAR (reprint author), Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Av Vicuna Mackena 4860, Santiago 7820436, Chile.
EM avalcarc@astro.puc.cl; mcatelan@astro.puc.cl; allen.v.sweigart@nasa.gov
FU Ministry for the Economy, Development, and Tourism's Programa Iniciativa
Cientifica Milenio [P07-021-F]; Proyecto Basal [PFB-06/2007]; FONDAP
Centro de Astrofisica [15010003]; Proyecto FONDECYT Regular [1110326];
Proyecto Anillo de Investigacion en Ciencia y Tecnologia PIA CONICYT-ACT
[86]; CNPq; CAPES; Proyecto ALMA-Conicyt [31090002]; MECESUP2; SOCHIAS
FX We thank the anonymous referee for her/his comments, which have helped
improve the presentation of our results. A. A. R. V. thanks Santi
Casissi for his useful comments during A.A.R.V.'s Ph.D. Thesis on this
topic. Support for A. A. R. V. and M. C. is provided by the Ministry for
the Economy, Development, and Tourism's Programa Iniciativa Cientifica
Milenio through grant P07-021-F, awarded to The Milky Way Millennium
Nucleus; by Proyecto Basal PFB-06/2007; by FONDAP Centro de Astrofisica
15010003; by Proyecto FONDECYT Regular #1110326; and by Proyecto Anillo
de Investigacion en Ciencia y Tecnologia PIA CONICYT-ACT 86. A. A. R. V.
acknowledges additional support from CNPq, CAPES, from Proyecto
ALMA-Conicyt 31090002, MECESUP2, and SOCHIAS.
NR 168
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U1 1
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 NOV
PY 2012
VL 547
AR A5
DI 10.1051/0004-6361/201219510
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 036MZ
UT WOS:000311031700005
ER
PT J
AU Lohn, AJ
Cormia, RD
Fryauf, DM
Zhang, JC
Norris, KJ
Kobayashi, NP
AF Lohn, Andrew J.
Cormia, Robert D.
Fryauf, David M.
Zhang, Junce
Norris, Kate J.
Kobayashi, Nobuhiko P.
TI Morphological Effect of Doping Environment on Silicon Nanowires Grown by
Plasma-Assisted Chemical Vapor Deposition
SO JAPANESE JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID SURFACE; PERFORMANCE; OXIDATION; MODEL; BORON; GOLD
AB Physical properties of semiconductor nanowires are tied intimately to their specific morphologies such as length and diameter. We studied the growth of silicon nanowires and found their lengths and diameters to vary over orders of magnitude in different doping environments. In all cases we examined, doping resulted in increased diameters. In addition, boron doping was found to accelerate volume growth rate while arsenic and antimony both appeared to slow it down. We further studied the formation of the native oxides that cover the nanowires. X-ray photoelectron spectroscopy indicated that properties of the native oxides are also dependent on doping environment and correlated to doping-dependent shifts in apparent binding energy of the Si 2p(3/2) peak illustrating that the electronic contribution is the dominant mechanism for the oxide growth. (C) 2012 The Japan Society of Applied Physics
C1 [Lohn, Andrew J.; Fryauf, David M.; Zhang, Junce; Norris, Kate J.; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA.
[Lohn, Andrew J.; Fryauf, David M.; Zhang, Junce; Norris, Kate J.; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Nanostruct Energy Convers Technol & Res NECTAR, Adv Studies Labs, NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
[Cormia, Robert D.] Foothill Coll, Los Altos Hills, CA 94022 USA.
RP Lohn, AJ (reprint author), Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA.
RI Kobayashi, Nobuhiko/E-3834-2012
FU NASA [SBIR NNX11CE14P]; NSF [0903316, DGE-0809125-006]
FX The authors would like to thank Elane Coleman and Gary S. Tompa at
Structured Materials Industries, Inc for nanowire growth and Vince Crist
at NanoLab Technologies and XPS International LLC for XPS measurements.
The authors would also like to acknowledge the following funding
sources: NASA SBIR NNX11CE14P, NSF grant number 0903316, and NSF grant
number DGE-0809125-006.
NR 32
TC 1
Z9 1
U1 0
U2 11
PU JAPAN SOC APPLIED PHYSICS
PI TOKYO
PA KUDAN-KITA BUILDING 5TH FLOOR, 1-12-3 KUDAN-KITA, CHIYODA-KU, TOKYO,
102-0073, JAPAN
SN 0021-4922
J9 JPN J APPL PHYS
JI Jpn. J. Appl. Phys.
PD NOV
PY 2012
VL 51
IS 11
SI SI
AR 11PE04
DI 10.1143/JJAP.51.11PE04
PN 2
PG 6
WC Physics, Applied
SC Physics
GA 049RP
UT WOS:000312001400019
ER
PT J
AU Meador, MAB
Wright, S
Sandberg, A
Nguyen, BN
Van Keuls, FW
Mueller, CH
Rodriguez-Solis, R
Miranda, FA
AF Meador, Mary Ann B.
Wright, Sarah
Sandberg, Anna
Nguyen, Baochau N.
Van Keuls, Frederick W.
Mueller, Carl H.
Rodriguez-Solis, Rafael
Miranda, Felix A.
TI Low Dielectric Polyimide Aerogels As Substrates for Lightweight Patch
Antennas
SO ACS APPLIED MATERIALS & INTERFACES
LA English
DT Article
DE aerogels; polyimides; low dielectric; antennas; mesoporous
ID POROUS POLYIMIDE; FILMS
AB The dielectric properties and loss tangents of low-density polyimide aerogels have been characterized at various frequencies. Relative dielectric constants as low as 1.16 were measured for polyimide aerogels made from 2,2'-dimethylbenzidine (DMBZ) and biphenyl 3,3',4,4'-tetracarbozylic dianhydride (BPDA) cross-linked with 1,3,5-triamino-phenoxybenzene (TAB). This formulation was used as the substrate to fabricate and test prototype microstrip patch antennas and benchmark against state of practice commercial antenna substrates. The polyimide aerogel antennas exhibited broader bandwidth, higher gain, and lower mass than the antennas made using commercial substrates. These are very encouraging results, which support the potential advantages of the polyimide aerogel-based antennas for aerospace applications.
C1 [Meador, Mary Ann B.; Wright, Sarah; Sandberg, Anna; Miranda, Felix A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Nguyen, Baochau N.] Ohio Aerosp Inst, Cleveland, OH 44135 USA.
[Van Keuls, Frederick W.] Vantage Partners LLC, Brookpark, OH 44142 USA.
[Mueller, Carl H.] Qinetiq N Amer, Brookpark, OH 44142 USA.
[Rodriguez-Solis, Rafael] Univ Puerto Rico, Mayaguez, PR USA.
RP Meador, MAB (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM maryann.meador@nasa.gov
OI Meador, Mary Ann/0000-0003-2513-7372; Rodriguez Solis,
Rafael/0000-0001-5700-2021
FU NASA
FX We thank the NASA Aeronautics Mission Directorate Seedling Fund for
support of this work. We thank our NASA GRC colleagues Mr. Nicholas
Varaljay and Ms. Elizabeth McQuaid for their support in the fabrication
of the antennas, as well as Dr. Kevin Lambert for his support in antenna
metrology.
NR 19
TC 34
Z9 39
U1 18
U2 119
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1944-8244
J9 ACS APPL MATER INTER
JI ACS Appl. Mater. Interfaces
PD NOV
PY 2012
VL 4
IS 11
BP 6346
EP 6353
DI 10.1021/am301985s
PG 8
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary
SC Science & Technology - Other Topics; Materials Science
GA 043DA
UT WOS:000311521900084
PM 23134844
ER
PT J
AU Ponchak, GE
AF Ponchak, George E.
TI Special Issue on Biomedical Applications of RF/Microwave Technologies
SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES
LA English
DT Editorial Material
C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Ponchak, GE (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
NR 0
TC 0
Z9 0
U1 0
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9480
J9 IEEE T MICROW THEORY
JI IEEE Trans. Microw. Theory Tech.
PD NOV
PY 2012
VL 60
IS 11
BP 3345
EP 3345
DI 10.1109/TMTT.2012.2216811
PG 1
WC Engineering, Electrical & Electronic
SC Engineering
GA 035SO
UT WOS:000310969100001
ER
PT J
AU Patterson, CE
Khan, WT
Ponchak, GE
May, GS
Papapolymerou, J
AF Patterson, Chad E.
Khan, Wasif Tanveer
Ponchak, George E.
May, Gary S.
Papapolymerou, John
TI A 60-GHz Active Receiving Switched-Beam Antenna Array With Integrated
Butler Matrix and GaAs Amplifiers
SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES
LA English
DT Article
DE Butler matrix; integrated circuit (IC) packaging; iquid crystal polymer
(LCP); phased arrays; receiving antennas
ID NETWORK; GAIN; BAND; GHZ; G/T
AB This paper presents for the first time a 60-GHz receiving switched-beam antenna on organic liquid crystal polymer (LCP) platform. A 4 x 1 quasi-Yagi array is incorporated with a 4 x 4 Butler matrix beamforming network and GaAs low-noise amplifiers on an LCP substrate. The active beam is controlled by GaAs single-pole-double-throw switches to access the four output states of the Butler matrix. The entire 4 x 1 active array is 1.4 cm x 1.75 cm and consumes 1.1 W of dc power. Successful comparisons of the measured and simulated results verify a working phased array with a return loss better than 10 dB across the frequency band of 56.7-63.7 GHz. A comparison of radiation patterns demonstrate beam steering of +/- 40 degrees with a peak active gain of 27.5 dB. The combined antenna and receiver noise performance at 60 GHz exhibits an estimated merit G/T of -18.6 dB/K and noise figure of 5.4 dB.
C1 [Patterson, Chad E.; Khan, Wasif Tanveer; May, Gary S.; Papapolymerou, John] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA.
[Ponchak, George E.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Patterson, CE (reprint author), Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA.
EM cpatterson@gatech.edu; george.ponchak@sbcglobal.net;
john.papa-polymerou@ece.gatech.edu
NR 23
TC 23
Z9 23
U1 0
U2 9
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9480
J9 IEEE T MICROW THEORY
JI IEEE Trans. Microw. Theory Tech.
PD NOV
PY 2012
VL 60
IS 11
BP 3599
EP 3607
DI 10.1109/TMTT.2012.2213834
PG 9
WC Engineering, Electrical & Electronic
SC Engineering
GA 035SO
UT WOS:000310969100028
ER
PT J
AU Zaretsky, E
AF Zaretsky, Erwin
TI Correspondence regarding the role of white etching cracks and related
features in the failure processes of bearing steels, with responses from
the authors response
SO MATERIALS SCIENCE AND TECHNOLOGY
LA English
DT Letter
C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Zaretsky, E (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM ezaretsky@sbcglobal.net
NR 0
TC 0
Z9 0
U1 1
U2 2
PU MANEY PUBLISHING
PI LEEDS
PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND
SN 0267-0836
J9 MATER SCI TECH-LOND
JI Mater. Sci. Technol.
PD NOV
PY 2012
VL 28
IS 11
BP 1360
EP 1364
PG 5
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA 044LE
UT WOS:000311619900023
ER
PT J
AU Hashmi, AJ
Eftekhar, A
Adibi, A
Amoozegar, F
AF Hashmi, Ali Javed
Eftekhar, Ali
Adibi, Ali
Amoozegar, Farid
TI A Kalman filter based synchronization scheme for telescope array
receivers in deep-space optical communication links
SO OPTICS COMMUNICATIONS
LA English
DT Article
DE Deep-space optical communication; Kalman filter; Telescope array
receiver; Clock synchronization
ID SYSTEM
AB In this paper, the impact of random synchronization errors on the performance of ground-based telescope array receivers for an inter-planetary optical deep-space communication (ODSC) link is investigated. An adaptive method based on Kalman filters is developed for the synchronization and combination of different telescope signals in the array. An end-to-end simulation platform for ODSC link between Earth and planet Mars is implemented that incorporates pulse-position modulation (PPM), direct-detection array receivers, and photon-counting detectors. The effects of atmospheric turbulence and background noise are also modeled. The performance of array receivers is evaluated in terms of probability of symbol error and achievable data rates. The simulation results show that the Kalman filter-based synchronization scheme keeps the synchronization induced power losses to less than 1 dB. The analysis also shows that in the worst-case operational scenario and presence of random synchronization errors, an array consisting of hundred, 1 m telescopes performs almost similar to a single 10 m telescope. Hence, the degradation in the combined signal due to synchronization errors places a minor limitation on the number of telescopes in a telescope array receiver consisting of up to 100 telescope elements. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Hashmi, Ali Javed] Natl Univ Sci & Technol, Islamabad, Pakistan.
[Eftekhar, Ali; Adibi, Ali] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA.
[Amoozegar, Farid] CALTECH, Jet Prop Lab NASA, Pasadena, CA 91109 USA.
RP Hashmi, AJ (reprint author), Natl Univ Sci & Technol, H-12, Islamabad, Pakistan.
EM hashmi@gatech.edu
NR 20
TC 5
Z9 6
U1 0
U2 8
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0030-4018
J9 OPT COMMUN
JI Opt. Commun.
PD NOV 1
PY 2012
VL 285
IS 24
BP 5037
EP 5043
DI 10.1016/j.optcom.2012.08.025
PG 7
WC Optics
SC Optics
GA 038TH
UT WOS:000311196500052
ER
PT J
AU Maneesha, K
Murty, VSN
Ravichandran, M
Lee, T
Yu, WD
McPhaden, MJ
AF Maneesha, K.
Murty, V. S. N.
Ravichandran, M.
Lee, T.
Yu, Weidong
McPhaden, M. J.
TI Upper ocean variability in the Bay of Bengal during the tropical
cyclones Nargis and Laila
SO PROGRESS IN OCEANOGRAPHY
LA English
DT Review
ID INDIAN-OCEAN; HURRICANE; INTENSITY; MONSOON; EDDY
AB Upper ocean variability at different stages in the evolution of the tropical cyclones Nargis and Laila is evaluated over the Bay of Bengal (BoB) during May 2008 and May 2010 respectively. Nargis initially developed on 24 April 2008; intensified twice on 27-28 April and 1 May, and eventually made landfall at Myanmar on 2 May 2008. Laila developed over the western BoB in May 2010 and moved westward towards the east coast of India. Data from the Argo Profiling floats, the Research Moored Array for African-Asian-Australian Monsoon Analysis and prediction (RAMA), and various satellite products are analyzed to evaluate upper ocean variability due to Nargis and Laila. The analysis reveals pre-conditioning of the central BoB prior to Nargis with warm (>30 degrees C) Sea Surface Temperature (SST), low (<33 psu) Sea Surface Salinity (SSS) and shallow (<30 m) mixed layer depths during March-April 2008. Enhanced ocean response to the right of the storm track due to Nargis includes a large SST drop by similar to 1.76 degrees C, SSS increase up to 0.74 psu, mixed layer deepening of 32 m, shoaling of the 26 degrees C isotherm by 36 m and high net heat loss at the sea surface. During Nargis, strong inertial currents (up to 0.9 ms(-1)) were generated to the right of storm track as measured at a RAMA buoy located at 15 degrees N, 90 degrees E, producing strong turbulent mixing that lead to the deepening of mixed layer. This mixing facilitated entrainment of cold waters from as deep as 75 m and, together with net heat loss at sea surface and cyclone-induced subsurface upwelling, contributed to the observed SST cooling in the wake of the storm. A similar upper ocean response occurs during Laila. though it was a significantly weaker storm than Nargis. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Maneesha, K.; Murty, V. S. N.] CSIR, Natl Inst Oceanog, Reg Ctr, Visakhapatnam 530017, Andhra Pradesh, India.
[Ravichandran, M.] Indian Natl Ctr Ocean Informat Serv, Hyderabad, Andhra Pradesh, India.
[Lee, T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Yu, Weidong] SOA, Inst Oceanog 1, Lab Ocean Atmosphere Interact & Climate Change, Qingdao, Peoples R China.
[McPhaden, M. J.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA.
RP Maneesha, K (reprint author), CSIR, Natl Inst Oceanog, Reg Ctr, 176 Lawsons Bay Colony, Visakhapatnam 530017, Andhra Pradesh, India.
EM kkpalli_manisha@yahoo.com
RI McPhaden, Michael/D-9799-2016
OI Ravichandran, Muthalagu/0000-0002-4602-0731;
FU Council of Scientific & Industrial Research (CSIR); NASA Physical
Oceanography Program
FX The authors are thankful to the Director, NIO for his encouragement in
the collaborative research with INCOIS, Hyderabad, PMEL, USA, JPL, USA
and FIO, China through IOGOOS partnership. The lead author is thankful
to the Council of Scientific & Industrial Research (CSIR) for funding
support with Senior Research Fellowship. These data were collected and
made freely available by the International Argo Program and the national
programs that contribute to it (http://www.argo.ucsd.edu,
http://argo.jcommops.org). The Argo Program is part of the Global Ocean
Observing System. ODV software has been used to construct Argo
temperature and salinity sections.; This has the NIO contribution No.
5200, INCOIS contribution No. 119 and the PMEL contribution No. 3622.
The research is partially supported by NASA Physical Oceanography
Program.
NR 32
TC 9
Z9 11
U1 2
U2 21
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0079-6611
J9 PROG OCEANOGR
JI Prog. Oceanogr.
PD NOV
PY 2012
VL 106
BP 49
EP 61
DI 10.1016/j.pocean.2012.06.006
PG 13
WC Oceanography
SC Oceanography
GA 044ZO
UT WOS:000311663900004
ER
PT J
AU Little, MP
Azizova, TV
Bazyka, D
Bouffler, SD
Cardis, E
Chekin, S
Chumak, VV
Cucinotta, FA
de Vathaire, F
Hall, P
Harrison, JD
Hildebrandt, G
Ivanov, V
Kashcheev, VV
Klymenko, SV
Kreuzer, M
Laurent, O
Ozasa, K
Schneider, T
Tapio, S
Taylor, AM
Tzoulaki, I
Vandoolaeghe, WL
Wakeford, R
Zablotska, LB
Zhang, W
Lipshultz, SE
AF Little, Mark P.
Azizova, Tamara V.
Bazyka, Dimitry
Bouffler, Simon D.
Cardis, Elisabeth
Chekin, Sergey
Chumak, Vadim V.
Cucinotta, Francis A.
de Vathaire, Florent
Hall, Per
Harrison, John D.
Hildebrandt, Guido
Ivanov, Victor
Kashcheev, Valeriy V.
Klymenko, Sergiy V.
Kreuzer, Michaela
Laurent, Olivier
Ozasa, Kotaro
Schneider, Thierry
Tapio, Soile
Taylor, Andrew M.
Tzoulaki, Ioanna
Vandoolaeghe, Wendy L.
Wakeford, Richard
Zablotska, Lydia B.
Zhang, Wei
Lipshultz, Steven E.
TI Systematic Review and Meta-analysis of Circulatory Disease from Exposure
to Low-Level Ionizing Radiation and Estimates of Potential Population
Mortality Risks
SO ENVIRONMENTAL HEALTH PERSPECTIVES
LA English
DT Review
DE cancer; circulatory disease; heart disease; radiation; stroke
ID ATOMIC-BOMB SURVIVORS; CORONARY-HEART-DISEASE; POWER INDUSTRY WORKERS;
NUCLEAR-FUELS PLC; LOW-DOSE EXPOSURE; CARDIOVASCULAR-DISEASE;
EPIDEMIOLOGIC EVIDENCE; MAYAK PA; CANCER; COHORT
AB BACKGROUND: Although high doses of ionizing radiation have long been linked to circulatory disease, evidence for an association at lower exposures remains controversial. However, recent analyses suggest excess relative risks at occupational exposure levels.
OBJECTIVES: We performed a systematic review and meta-analysis to summarize information on circulatory disease risks associated with moderate- and low-level whole-body ionizing radiation exposures.
METHODS: We conducted PubMed/ISI Thomson searches of peer-reviewed papers published since 1990 using the terms "radiation" AND "heart" AND "disease," OR "radiation" AND "stroke," OR "radiation" AND "circulatory" AND "disease." Radiation exposures had to be whole-body, with a cumulative mean dose of < 0.5 Sv, or at a low dose rate (< 10 mSv/day). We estimated population risks of circulatory disease from low-level radiation exposure using excess relative risk estimates from this meta-analysis and current mortality rates for nine major developed countries.
RESULTS: Estimated excess population risks for all circulatory diseases combined ranged from 2.5%/Sv [95% confidence interval (Cl): 0.8, 4.2] for France to 8.5%/Sv (95% CI: 4.0, 13.0) for Russia.
CONCLUSIONS: Our review supports an association between circulatory disease mortality and low and moderate doses of ionizing radiation. Our analysis was limited by heterogeneity among studies (particularly for noncardiac end points), the possibility of uncontrolled confounding in some occupational groups by lifestyle factors, and higher dose groups (> 0.5 Sv) generally driving the observed trends. If confirmed, our findings suggest that overall radiation-related mortality is about twice that currently estimated based on estimates for cancer end points alone (which range from 4.2% to 5.6%/Sv for these populations).
C1 [Little, Mark P.] NCI, Radiat Epidemiol Branch, NIH, Dept Hlth & Human Serv, Rockville, MD 20852 USA.
[Azizova, Tamara V.] So Urals Biophys Inst, Ozyorsk, Russia.
[Bazyka, Dimitry; Chumak, Vadim V.] Res Ctr Radiat Med, Kiev, Ukraine.
[Bouffler, Simon D.; Harrison, John D.; Zhang, Wei] Hlth Protect Agcy, Ctr Radiat Chem & Environm Hazards, Chilton, England.
[Cardis, Elisabeth] Ctr Res Environm Epidemiol CREAL, Barcelona, Spain.
[Chekin, Sergey; Ivanov, Victor; Kashcheev, Valeriy V.] Russian Acad Med Sci, Med Radiol Res Ctr, Obninsk, Russia.
[Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Space Radiat Program, Houston, TX 77058 USA.
[de Vathaire, Florent] Inst Gustave Roussy, INSERM, Radiat Epidemiol Grp, Unite U1018, F-94805 Villejuif, France.
[Hall, Per] Karolinska Inst, Dept Med Epidemiol & Biostat, Stockholm, Sweden.
[Hildebrandt, Guido] Univ Leipzig, Dept Radiotherapy & Radiat Oncol, Leipzig, Germany.
[Hildebrandt, Guido] Univ Rostock, Dept Radiotherapy & Radiat Oncol, Rostock, Germany.
[Kreuzer, Michaela] Fed Off Radiat Protect, Dept Radiat Protect & Hlth, Oberschleissheim, Germany.
[Laurent, Olivier] Inst Radioprotect & Surete Nucl, Lab Epidemiol, Fontenay Aux Roses, France.
[Ozasa, Kotaro] Radiat Effects Res Fdn, Dept Epidemiol, Hiroshima, Japan.
[Schneider, Thierry] CEPN Nucl Evaluat Protect Ctr, Fontenay Aux Roses, France.
[Tapio, Soile] Helmholtz Zentrum Munchen, German Res Ctr Environm Hlth, Inst Radiat Biol ISB, Oberschleissheim, Germany.
[Taylor, Andrew M.] UCL, Inst Cardiovasc Sci, London, England.
[Taylor, Andrew M.] Great Ormond St Hosp Sick Children, London WC1N 3JH, England.
[Tzoulaki, Ioanna; Vandoolaeghe, Wendy L.] Univ London Imperial Coll Sci Technol & Med, Fac Med, Dept Epidemiol & Biostat, London, England.
[Wakeford, Richard] Univ Manchester, Dalton Nucl Inst, Manchester, Lancs, England.
[Zablotska, Lydia B.] Univ Calif San Francisco, Sch Med, Dept Epidemiol & Biostat, San Francisco, CA USA.
[Lipshultz, Steven E.] Univ Miami, Dept Pediat, Leonard M Miller Sch Med, Miami, FL 33152 USA.
RP Little, MP (reprint author), NCI, Radiat Epidemiol Branch, NIH, Dept Hlth & Human Serv, Execut Plaza S,6120 Execut Blvd,MSC 7238, Rockville, MD 20852 USA.
EM mark.little@nih.gov
RI Taylor, Andrew/C-4311-2008; Tapio, Soile/M-7358-2014; Kashcheev,
Valeriy/L-7794-2015; Chumak, Vadim/N-6960-2015; de Vathaire,
Florent/L-2983-2016; Ivanov, Victor/R-9385-2016; Cardis,
Elisabeth/C-3904-2017;
OI Little, Mark/0000-0003-0980-7567; Klymenko, Sergiy/0000-0002-9758-7316;
Tapio, Soile/0000-0001-9860-3683; Kashcheev,
Valeriy/0000-0003-4108-9761; Chumak, Vadim/0000-0001-6045-9356; Ivanov,
Victor/0000-0003-1372-0018; Bazyka, Dimitry/0000-0001-9982-5990;
Wakeford, Richard/0000-0002-2934-0987
FU European Commission (EC) [FP6-036465]; Intramural Research Program of
the National Institutes of Health (NIH); National Cancer Institute;
Japanese Ministry of Health, Labour and Welfare; U.S. Department of
Energy through the National Academy of Sciences
FX This work was funded partially by the European Commission (EC) under
contract FP6-036465 [NOn-Targeted Effects of ionising radiation (NOTE)
integrated project]. This research was also supported by the Intramural
Research Program of the National Institutes of Health (NIH) and the
National Cancer Institute. This report makes use of data obtained from
the Radiation Effects Research Foundation (RERF), Hiroshima and
Nagasaki, Japan. RERF is a private, nonprofit foundation funded by the
Japanese Ministry of Health, Labour and Welfare and the U.S. Department
of Energy, the latter through the National Academy of Sciences.
NR 59
TC 83
Z9 93
U1 3
U2 27
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
J9 ENVIRON HEALTH PERSP
JI Environ. Health Perspect.
PD NOV
PY 2012
VL 120
IS 11
BP 1503
EP 1511
DI 10.1289/ehp.1204982
PG 9
WC Environmental Sciences; Public, Environmental & Occupational Health;
Toxicology
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Toxicology
GA 036ZE
UT WOS:000311070000017
PM 22728254
ER
PT J
AU Morgan, JLL
Zwart, SR
Heer, M
Ploutz-Snyder, R
Ericson, K
Smith, SM
AF Morgan, Jennifer L. L.
Zwart, Sara R.
Heer, Martina
Ploutz-Snyder, Robert
Ericson, Karen
Smith, Scott M.
TI Bone metabolism and nutritional status during 30-day head-down-tilt bed
rest
SO JOURNAL OF APPLIED PHYSIOLOGY
LA English
DT Article
DE bed rest; bone metabolism; nutritional status; oxalate; parathyroid
hormone
ID BODY NEGATIVE-PRESSURE; DURATION SPACE-FLIGHT; RED-BLOOD-CELL; TREADMILL
EXERCISE; RESISTANCE EXERCISE; ARTIFICIAL GRAVITY; CALCIUM-METABOLISM;
IDENTICAL-TWINS; SPACEFLIGHT; COUNTERMEASURE
AB Morgan JL, Zwart SR, Heer M, Ploutz-Snyder R, Ericson K, Smith SM. Bone metabolism and nutritional status during 30-day head-down-tilt bed rest. J Appl Physiol 113: 1519-1529, 2012. First published September 20, 2012; doi:10.1152/japplphysiol.01064.2012.-Bed rest studies provide an important tool for modeling physiological changes that occur during spaceflight. Markers of bone metabolism and nutritional status were evaluated in 12 subjects (8 men, 4 women; ages 25-49 yr) who participated in a 30-day -6 degrees head-down-tilt diet-controlled bed rest study. Blood and urine samples were collected twice before, once a week during, and twice after bed rest. Data were analyzed using a mixed-effects linear regression with a priori contrasts comparing all days to the second week of the pre-bed rest acclimation period. During bed rest, all urinary markers of bone resorption increased similar to 20% (P < 0.001), and serum parathyroid hormone decreased similar to 25% (P < 0.001). Unlike longer (>60 days) bed rest studies, neither markers of oxidative damage nor iron status indexes changed over the 30 days of bed rest. Urinary oxalate excretion decreased similar to 20% during bed rest (P < 0.001) and correlated inversely with urinary calcium (R = -0.18, P < 0.02). These data provide a broad overview of the biochemistry associated with short-duration bed rest studies and provide an impetus for using shorter studies to save time and costs wherever possible. For some effects related to bone biochemistry, short-duration bed rest will fulfill the scientific requirements to simulate spaceflight, but other effects (antioxidants/oxidative damage, iron status) do not manifest until subjects are in bed longer, in which case longer studies or other analogs may be needed. Regardless, maximizing research funding and opportunities will be critical to enable the next steps in space exploration.
C1 [Morgan, Jennifer L. L.; Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Oak Ridge Assoc Univ NASA, Houston, TX 77058 USA.
[Zwart, Sara R.; Ploutz-Snyder, Robert] NASA, Lyndon B Johnson Space Ctr, Univ Space Res Assoc & NASA, Houston, TX 77058 USA.
[Heer, Martina] Univ Bonn, Dept Nutr & Food Sci, Bonn, Germany.
[Heer, Martina] Profil Inst Metab Res, Neuss, Germany.
[Ericson, Karen] Indiana Univ Purdue Univ, Dept Chem, Ft Wayne, IN 46805 USA.
RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Oak Ridge Assoc Univ NASA, Attn Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA.
EM scott.m.smith@nasa.gov
FU NASA Flight Analogs Project of NASA's Human Research Program; National
Center for Advancing Translational Sciences, National Institutes of
Health [1UL1RR029876-01]
FX This study was funded in part by the NASA Flight Analogs Project of
NASA's Human Research Program, and in part by grant 1UL1RR029876-01 from
the National Center for Advancing Translational Sciences, National
Institutes of Health.
NR 42
TC 15
Z9 16
U1 0
U2 12
PU AMER PHYSIOLOGICAL SOC
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 8750-7587
J9 J APPL PHYSIOL
JI J. Appl. Physiol.
PD NOV
PY 2012
VL 113
IS 10
BP 1519
EP 1529
DI 10.1152/japplphysiol.01064.2012
PG 11
WC Physiology; Sport Sciences
SC Physiology; Sport Sciences
GA 038XZ
UT WOS:000311208700003
PM 22995395
ER
PT J
AU Yeh, SW
Ham, YG
Lee, JY
AF Yeh, Sang-Wook
Ham, Yoo-Geun
Lee, June-Yi
TI Changes in the Tropical Pacific SST Trend from CMIP3 to CMIP5 and Its
Implication of ENSO
SO JOURNAL OF CLIMATE
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; EL-NINO-LIKE; CLIMATE-CHANGE; DECADAL
VARIABILITY; OSCILLATION; AMPLITUDE; OCEAN; MODULATIONS; MODEL; ICE
AB This study assesses the changes in the tropical Pacific Ocean sea surface temperature (SST) trend and ENSO amplitude by comparing a historical run of the World Climate Research Programme Coupled Model Intercomparison Project (CMIP) phase-5 multimodel ensemble dataset (CMIP5) and the CMIP phase-3 dataset (CMIP3). The results indicate that the magnitude of the SST trend in the tropical Pacific basin has been significantly reduced from CMIP3 to CMIP5, which may be associated with the overestimation of the response to natural forcing and aerosols by including Earth system models in CMIP5. Moreover, the patterns of tropical warming over the second half of the twentieth century have changed from a La Nina-like structure in CMIP3 to an El Nino-like structure in CMIP5. Further analysis indicates that such changes in the background state of the tropical Pacific and an increase in the sensitivity of the atmospheric response to the SST changes in the eastern tropical Pacific have influenced the ENSO properties. In particular, the ratio of the SST anomaly variance in the eastern and western tropical Pacific increased from CMIP3 to CMIP5, indicating that a center of action associated with the ENSO amplitude has shifted to the east.
C1 [Ham, Yoo-Geun] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Ham, Yoo-Geun] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Studies & Investi, Columbia, MD USA.
[Yeh, Sang-Wook] Hanyang Univ, Dept Environm Marine Sci, Ansan, South Korea.
[Lee, June-Yi] Univ Hawaii Manoa, Dept Meteorol, Honolulu, HI 96822 USA.
[Lee, June-Yi] Univ Hawaii Manoa, Int Pacific Res Ctr, Honolulu, HI 96822 USA.
RP Ham, YG (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Mail Code 610-1, Greenbelt, MD 20771 USA.
EM yoo-geun.ham@nasa.gov
RI Lee, June-Yi/D-5752-2012; Yeh, Sang-Wook/G-3007-2014
OI Yeh, Sang-Wook/0000-0003-4549-1686
FU Korea Meteorological Administration Research and Development Program
[CATER 2012-3041]; International Pacific Research Center (IPRC);
JAMSTEC; NOAA; NASA
FX We acknowledge the WCRP's Working Group on Coupled Modeling, which is
responsible for CMIP, and we thank the climate modeling groups (listed
in Table 2) for producing and making available their model output. For
CMIP, the U.S. Department of Energy's Program for Climate Model
Diagnosis and Intercomparison provides coordinating support and led
development of software infrastructure in partnership with the Global
Organization for Earth System Science Portals. S.-W. Yeh was funded by
the Korea Meteorological Administration Research and Development Program
under Grant CATER 2012-3041. J.-Y. Lee acknowledges support from the
International Pacific Research Center (IPRC) which is funded jointly by
JAMSTEC, NOAA, and NASA.
NR 33
TC 44
Z9 46
U1 5
U2 51
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 NOV 1
PY 2012
VL 25
IS 21
BP 7764
EP 7771
DI 10.1175/JCLI-D-12-00304.1
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 036BZ
UT WOS:000311002700026
ER
PT J
AU Miller, RL
AF Miller, R. L.
TI Adjustment to Radiative Forcing in a Simple Coupled Ocean-Atmosphere
Model
SO JOURNAL OF CLIMATE
LA English
DT Article
ID SAHARAN AIR LAYER; TROPICAL NORTH-ATLANTIC; SOIL DUST AEROSOLS; CLIMATE
RESPONSE; TEMPERATURE; IMPACTS; AFRICA; ENSO
AB This study calculates the adjustment to radiative forcing in a simple model of a mixed layer ocean coupled to the overlying atmosphere. One application of the model is to calculate how dust aerosols perturb the temperature of the atmosphere and ocean, which in turn influence tropical cyclone development. Forcing at the top of the atmosphere (TOA) is the primary control upon both the atmospheric and ocean temperature anomalies, both at equilibrium and during most of the adjustment to the forcing. Ocean temperature is directly influenced by forcing only at the surface, but is indirectly related to forcing at TOA due to heat exchange with the atmosphere. Within a few days of the forcing onset, the atmospheric temperature adjusts to heating within the aerosol layer, reducing the net transfer of heat from the ocean to the atmosphere. For realistic levels of aerosol radiative forcing, the perturbed net surface heating strongly opposes forcing at the surface. This means that surface forcing dominates the ocean response only within the first few days following a dust outbreak, before the atmosphere has responded. This suggests that, to calculate the effect of dust upon the ocean temperature, the atmospheric adjustment must be taken into account explicitly and forcing at TOA must be considered in addition to the surface forcing. The importance of TOA forcing should be investigated in a model where vertical and lateral mixing of heat are calculated with fewer assumptions than in the simple model presented here. Nonetheless, the fundamental influence of TOA forcing appears to be only weakly sensitive to the model assumptions.
C1 [Miller, R. L.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Miller, R. L.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
RP Miller, RL (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM ron.l.miller@nasa.gov
RI Miller, Ron/E-1902-2012
FU National Science Foundation [ATM-06-20066]
FX I am grateful for the thoughtful comments of two anonymous reviewers and
Amato Evan (who suggested representing dynamical transport as linear
relaxation). I also benefited from discussions with Peter Knippertz,
Natalie Mahowald, Carlos Perez, Adam Sobel, and Charlie Zender. Thanks
also to Lilly Del Valle for drafting Fig. 1. This work was supported by
the Climate Dynamics Program of the National Science Foundation under
ATM-06-20066.
NR 41
TC 3
Z9 3
U1 0
U2 2
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 NOV
PY 2012
VL 25
IS 22
BP 7802
EP 7821
DI 10.1175/JCLI-D-11-00119.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 036NO
UT WOS:000311034300002
ER
PT J
AU Englander, JA
Conway, BA
Williams, T
AF Englander, Jacob A.
Conway, Bruce A.
Williams, Trevor
TI Automated Mission Planning via Evolutionary Algorithms
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article; Proceedings Paper
CT 21st AAS/AIAA Space Flight Mechanics Meeting
CY FEB 13-17, 2011
CL New Orleans, LA
SP AAS, AIAA
ID ASSIST TRAJECTORIES OPTIMIZATION; DIFFERENTIAL EVOLUTION; GLOBAL
OPTIMIZATION; GENETIC ALGORITHM; DESIGN
AB Many space mission planning problems may be formulated as hybrid optimal control problems, that is, problems that include both real-valued variables and categorical variables. In orbital mechanics problems, the categorical variables will typically specify the sequence of events that qualitatively describe the trajectory or mission, and the real-valued variables will represent the launch date, flight times between planets, magnitudes and directions of rocket burns, flyby altitudes, etc. A current practice is to preprune the categorical state space to limit the number of possible missions to a number whose cost may reasonably be evaluated. Of course, this risks pruning away the optimal solution. The method to be developed here avoids the need for prepruning by incorporating a new solution approach. The new approach uses nested loops: an outer-loop problem solver that handles the finite dynamics and finds a solution sequence in terms of the categorical variables, and an inner-loop problem solver that finds the optimal trajectory for a given sequence A binary genetic algorithm is used to solve the outer-loop problem, and a cooperative algorithm based on particle swarm optimization and differential evolution is used to solve the inner-loop problem. The hybrid optimal control solver is successfully demonstrated here by reproducing the Galileo and Cassini missions.
C1 [Englander, Jacob A.; Conway, Bruce A.] Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA.
[Williams, Trevor] NASA, Goddard Space Flight Ctr, Nav & Mission Design Branch, Greenbelt, MD 20770 USA.
RP Englander, JA (reprint author), Univ Illinois, Dept Aerosp Engn, 104 S Wright St,Mail Code 236, Urbana, IL 61801 USA.
NR 22
TC 26
Z9 26
U1 1
U2 20
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
EI 1533-3884
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD NOV-DEC
PY 2012
VL 35
IS 6
BP 1878
EP 1887
DI 10.2514/1.54101
PG 10
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 037TM
UT WOS:000311129400017
ER
PT J
AU Zanetti, R
D'Souza, C
AF Zanetti, Renato
D'Souza, Chris
TI Dual Accelerometer Usage Strategy for Onboard Space Navigation
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article; Proceedings Paper
CT 22nd AAS/AIAA Space Flight Mechanics Meeting
CY JAN 29-FEB 02, 2012
CL Charleston, SC
SP AAS, Space Flight Mech Comm, AIAA, Astrodynam Techn Comm
C1 [Zanetti, Renato] Charles Stark Draper Lab Inc, Houston, TX 77058 USA.
[D'Souza, Chris] NASA, Lyndon B Johnson Space Ctr, Aerosci & Flight Mech Div, Houston, TX 77058 USA.
RP Zanetti, R (reprint author), Charles Stark Draper Lab Inc, Houston, TX 77058 USA.
EM rzanetti@draper.com; chris.dsouza@nasa.gov
NR 6
TC 0
Z9 0
U1 1
U2 5
PU AMER INST AERONAUTICS ASTRONAUTICS
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 NOV-DEC
PY 2012
VL 35
IS 6
BP 1899
EP 1902
DI 10.2514/1.58154
PG 4
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 037TM
UT WOS:000311129400019
ER
PT J
AU Zaretsky, EV
Litt, JS
Hendricks, RC
Soditus, SM
AF Zaretsky, Erwin V.
Litt, Jonathan S.
Hendricks, Robert C.
Soditus, Sherry M.
TI Determination of Turbine Blade Life from Engine Field Data
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article; Proceedings Paper
CT AIAA/ASME/ASCE/AHS/ASC 49th Structures, Structural Dynamics, and
Materials Conference
CY APR 07-10, 2008
CL Schaumburg, IL
SP Amer Inst Aeronaut & Astronaut (AIAA), ASME, ASCE, AHS, ASC
ID WEIBULL STATISTICS
AB It is probable that no two engine companies determine the life of their engines or their components in the same way or apply the same experience and safety factors to their designs. Available data regarding failure mode for aircraft engine blades, although favoring low-cycle thermal-mechanical fatigue as the controlling mode of failure, are not definitive. Sixteen high-pressure turbine T-1 blade sets were removed from commercial aircraft engines that had been commercially flown by a single airline and inspected for damage. Each set contained 82 blades. The damage was cataloged into three categories related to their mode of failure: 1) Thermal-mechanical fatigue, 2) Oxidation/Erosion, and 3) Other. From these field data the turbine blade life was determined as well as the lives related to individual blade failure modes. A simplified formula for calculating turbine blade life and reliability was formulated. The L-10 blade life was calculated to be 2427 cycles (11,077 h). The resulting blade life attributed to oxidation/erosion equaled that attributed to thermal-mechanical fatigue. The category that contributed most to blade failure was Other. If there were there no blade failures attributed to oxidation/erosion and thermal-mechanical fatigue, the overall blade L-10 life would increase approximately 11 to 17%.
C1 [Zaretsky, Erwin V.; Litt, Jonathan S.; Hendricks, Robert C.] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA.
[Soditus, Sherry M.] United Airlines Maintenance, San Francisco, CA 94128 USA.
NR 27
TC 1
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U1 1
U2 5
PU AMER INST AERONAUTICS ASTRONAUTICS
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 NOV-DEC
PY 2012
VL 28
IS 6
BP 1156
EP 1167
DI 10.2514/1.B34375
PG 12
WC Engineering, Aerospace
SC Engineering
GA 037UQ
UT WOS:000311132400002
ER
PT J
AU Heymans, C
Van Waerbeke, L
Miller, L
Erben, T
Hildebrandt, H
Hoekstra, H
Kitching, TD
Mellier, Y
Simon, P
Bonnett, C
Coupon, J
Fu, LP
Harnois-Deraps, J
Hudson, MJ
Kilbinger, M
Kuijken, K
Rowe, B
Schrabback, T
Semboloni, E
van Uitert, E
Vafaei, S
Velander, M
AF Heymans, Catherine
Van Waerbeke, Ludovic
Miller, Lance
Erben, Thomas
Hildebrandt, Hendrik
Hoekstra, Henk
Kitching, Thomas D.
Mellier, Yannick
Simon, Patrick
Bonnett, Christopher
Coupon, Jean
Fu, Liping
Harnois-Deraps, Joachim
Hudson, Michael J.
Kilbinger, Martin
Kuijken, Koenraad
Rowe, Barnaby
Schrabback, Tim
Semboloni, Elisabetta
van Uitert, Edo
Vafaei, Sanaz
Velander, Malin
TI CFHTLenS: the Canada-France-Hawaii Telescope Lensing Survey
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: weak; cosmology: observations
ID SHEAR CORRELATION-FUNCTIONS; WEAK GRAVITATIONAL SHEAR; GALAXY SHAPE
MEASUREMENT; POINT-SPREAD FUNCTION; COSMIC SHEAR; DARK-MATTER;
PHOTOMETRIC REDSHIFTS; IMAGE-ANALYSIS; LEGACY SURVEY; LARGE SCALES
AB We present the CanadaFranceHawaii Telescope Lensing Survey (CFHTLenS) that accurately determines a weak gravitational lensing signal from the full 154 deg(2) of deep multicolour data obtained by the CFHT Legacy Survey. Weak gravitational lensing by large-scale structure is widely recognized as one of the most powerful but technically challenging probes of cosmology. We outline the CFHTLenS analysis pipeline, describing how and why every step of the chain from the raw pixel data to the lensing shear and photometric redshift measurement has been revised and improved compared to previous analyses of a subset of the same data. We present a novel method to identify data which contributes a non-negligible contamination to our sample and quantify the required level of calibration for the survey. Through a series of cosmology-insensitive tests we demonstrate the robustness of the resulting cosmic shear signal, presenting a science-ready shear and photometric redshift catalogue for future exploitation.
C1 [Heymans, Catherine] Univ Edinburgh, Scottish Univ Phys Alliance, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Van Waerbeke, Ludovic; Hildebrandt, Hendrik; Vafaei, Sanaz] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Miller, Lance; Velander, Malin] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Erben, Thomas; Hildebrandt, Hendrik; Schrabback, Tim; van Uitert, Edo] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Hoekstra, Henk; Kuijken, Koenraad; Schrabback, Tim; Semboloni, Elisabetta; van Uitert, Edo; Velander, Malin] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands.
[Hoekstra, Henk] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada.
[Mellier, Yannick] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France.
[Bonnett, Christopher] CSIC IEEC, Inst Ciencies Espai, Barcelona 08193, Spain.
[Coupon, Jean] Acad Sinica, Ins Astron & Astrophys, Taipei 10617, Taiwan.
[Fu, Liping] Shanghai Normal Univ, Key Lab Astrophys, Shanghai 200234, Peoples R China.
[Harnois-Deraps, Joachim] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Harnois-Deraps, Joachim] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Hudson, Michael J.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Hudson, Michael J.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 1Y5, Canada.
[Kilbinger, Martin] CEA Saclay, Serv Astrophys SAp, F-91191 Gif Sur Yvette, France.
[Kilbinger, Martin] Excellence Cluster Univ, D-85748 Garching, Germany.
[Kilbinger, Martin] Univ Munich, Univ Sternwarte, D-81679 Munich, Germany.
[Rowe, Barnaby] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Rowe, Barnaby] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Rowe, Barnaby] CALTECH, Pasadena, CA 91125 USA.
[Schrabback, Tim] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
RP Heymans, C (reprint author), Univ Edinburgh, Scottish Univ Phys Alliance, Inst Astron, Royal Observ, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland.
EM heymans@roe.ac.uk
RI Hudson, Michael/H-3238-2012;
OI Hudson, Michael/0000-0002-1437-3786; Kilbinger,
Martin/0000-0001-9513-7138; Rowe, Barnaby/0000-0002-7042-9174; Hoekstra,
Henk/0000-0002-0641-3231
FU Canadian Space Agency; NSERC Research Tools and Instruments grant
programme; Canada Foundation for Innovation under Compute Canada;
Government of Ontario; Ontario Research Fund - Research Excellence;
University of Toronto; European Commissions Marie Curie Research
Training Network DUEL [MRTN-CT-2006-036133]; European Research Council
under the EC [240185, 279396, 240672]; Natural Sciences and Engineering
Research Council of Canada; Canadian Institute for Advanced Research;
Deutsche Forschungsgemeinschaft [ER 327/3-1]; Transregional
Collaborative Research Centre [TR 33]; Marie Curie IOF [252760]; CITA;
Marie Curie IRG grant [230924]; Netherlands Organisation for Scientific
Research [639.042.814]; Royal Society; CNRS/INSU (Institut National des
Sciences de l'Univers); Programme National Galaxies et Cosmologie
(PNCG); NSFC [11103012, 10878003]; Innovation Program [12ZZ134]; Chen
Guang project; SMEC [10CG46]; STCSM [11290706600]; NSF
[AST-0444059-001]; SAO [GO0-11147A]; NWO; Beecroft Institute for
Particle Astrophysics and Cosmology; Spanish Science Ministry
[AYA2009-13936, CSD2007-00060]; Generalitat de Catalunya [2009SGR1398];
European Commissions Marie Curie Initial Training Network CosmoComp
[PITN-GA-2009-238356]
FX This work is based on observations obtained with MegaPrime/MegaCam, a
joint project of CFHT and CEA/DAPNIA, at the CFHT which is operated by
the National Research Council (NRC) of Canada, the Institut National des
Sciences de l'Univers of the Centre National de la Recherche
Scientifique (CNRS) of France, and the University of Hawaii. This
research used the facilities of the Canadian Astronomy Data Centre
operated by the National Research Council of Canada with the support of
the Canadian Space Agency. We thank the CFHT staff for successfully
conducting the CFHTLS observations and in particular Jean-Charles
Cuillandre and Eugene Magnier for the continuous improvement of the
instrument calibration and the ELIXIR detrended data that we used. We
also thank TERAPIX for the quality assessment and validation of
individual exposures during the CFHTLS data acquisition period, and
Emmanuel Bertin for developing some of the software used in this study.
CFHTLenS data processing was made possible thanks to significant
computing support from the NSERC Research Tools and Instruments grant
programme, and to HPC specialist Ovidiu Toader. The N-body simulations
used in this analysis were performed on the TCS supercomputer at the
SciNet HPC Consortium. SciNet is funded by: the Canada Foundation for
Innovation under the auspices of Compute Canada; the Government of
Ontario; the Ontario Research Fund - Research Excellence; and the
University of Toronto. The early stages of the CFHTLenS project were
made possible thanks to the support of the European Commissions Marie
Curie Research Training Network DUEL (MRTN-CT-2006-036133) which
directly supported six members of the CFHTLenS team (LF, HHi, PS, BR,
CB, MV) between 2007 and 2011 in addition to providing travel support
and expenses for team meetings.; CH, HHo and BR acknowledge support from
the European Research Council under the EC FP7 grant numbers 240185
(CH), 279396 (HHo) and 240672 (BR). LVW acknowledges support from the
Natural Sciences and Engineering Research Council of Canada and the
Canadian Institute for Advanced Research (Cosmology and Gravity
programme). TE is supported by the Deutsche Forschungsgemeinschaft
through project ER 327/3-1 and, with PS, is supported by the
Transregional Collaborative Research Centre TR 33 - 'The Dark Universe'.
HHi is supported by the Marie Curie IOF 252760 and by a CITA National
Fellowship. HHo also acknowledges support from Marie Curie IRG grant
230924 and the Netherlands Organisation for Scientific Research grant
number 639.042.814. TDK acknowledges support from a Royal Society
University Research Fellowship. YM acknowledges support from CNRS/INSU
(Institut National des Sciences de l'Univers) and the Programme National
Galaxies et Cosmologie (PNCG). LF acknowledges support from NSFC grants
11103012 and 10878003, Innovation Program 12ZZ134 and Chen Guang project
10CG46 of SMEC, and STCSM grant 11290706600. MJH acknowledges support
from the Natural Sciences and Engineering Research Council of Canada. TS
acknowledges support from NSF through grant AST-0444059-001, SAO through
grant GO0-11147A, and NWO.; MV acknowledges support from the Netherlands
Organisation for Scientific Research (NWO) and from the Beecroft
Institute for Particle Astrophysics and Cosmology. CB is supported by
the Spanish Science Ministry AYA2009-13936 Consolider-Ingenio
CSD2007-00060, project 2009SGR1398 from Generalitat de Catalunya and by
the European Commissions Marie Curie Initial Training Network CosmoComp
(PITN-GA-2009-238356). Part of BR's work was done at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA.
NR 77
TC 227
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U1 1
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 NOV
PY 2012
VL 427
IS 1
BP 146
EP 166
DI 10.1111/j.1365-2966.2012.21952.x
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 031XH
UT WOS:000310675400013
ER
PT J
AU Cappelluti, N
Ranalli, P
Roncarelli, M
Arevalo, P
Zamorani, G
Comastri, A
Gilli, R
Rovilos, E
Vignali, C
Allevato, V
Finoguenov, A
Miyaji, T
Nicastro, F
Georgantopoulos, I
Kashlinsky, A
AF Cappelluti, N.
Ranalli, P.
Roncarelli, M.
Arevalo, P.
Zamorani, G.
Comastri, A.
Gilli, R.
Rovilos, E.
Vignali, C.
Allevato, V.
Finoguenov, A.
Miyaji, T.
Nicastro, F.
Georgantopoulos, I.
Kashlinsky, A.
TI The nature of the unresolved extragalactic cosmic soft X-ray background
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; dark matter; diffuse radiation; large-scale structure
of Universe; X-rays: galaxies
ID HOT INTERGALACTIC MEDIUM; ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; MS
SOURCE CATALOGS; STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES;
DARK-MATTER HALOES; XMM-NEWTON; NUMBER COUNTS; MISSING BARYONS
AB In this paper we investigate the power spectrum of the unresolved 0.5-2 keV cosmic X-ray background (CXB) with deep Chandra 4-Msec (Ms) observations in the Chandra Deep Field South (CDFS). We measured a signal that, on scales >30 arcsec, is significantly higher than the shot noise and is increasing with angular scale. We interpreted this signal as the joint contribution of clustered undetected sources like active galactic nuclei (AGN), galaxies and the intergalactic medium (IGM). The power of unresolved cosmic source fluctuations accounts for similar to 12 per cent of the 0.5-2 keV extragalactic CXB. Overall, our modelling predicts that similar to 20 per cent of the unresolved CXB flux is produced by low-luminosity AGN, similar to 25 per cent by galaxies and similar to 55 per cent by the IGM. We do not find any direct evidence of the so-called 'warm hot intergalactic medium' (i.e. matter with 10(5) < T < 10(7) K and density contrast delta < 1000), but we estimated that it could produce about 1/7 of the unresolved CXB. We placed an upper limit on the space density of postulated X-ray-emitting early black holes at z > 7.5 and compared it with supermassive black hole evolution models.
C1 [Cappelluti, N.; Ranalli, P.; Zamorani, G.; Comastri, A.; Gilli, R.; Rovilos, E.; Vignali, C.; Georgantopoulos, I.] INAF, Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Cappelluti, N.; Finoguenov, A.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Ranalli, P.; Georgantopoulos, I.] Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece.
[Ranalli, P.; Roncarelli, M.; Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Arevalo, P.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile.
[Allevato, V.] Max Planck Inst Plasmaphys & Excellence Cluster U, D-85748 Garching, Germany.
[Finoguenov, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Miyaji, T.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Baja California, Mexico.
[Nicastro, F.] INAF, Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Kashlinsky, A.] SSAI, Lanham, MD 20706 USA.
[Kashlinsky, A.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
RP Cappelluti, N (reprint author), INAF, Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy.
EM nico.cappelluti@oabo.inaf.it
RI Vignali, Cristian/J-4974-2012; Ranalli, Piero/K-6363-2013;
Georgantopoulos, Ioannis/L-3687-2013; Comastri, Andrea/O-9543-2015;
Gilli, Roberto/P-1110-2015;
OI Cappelluti, Nico/0000-0002-1697-186X; Zamorani,
Giovanni/0000-0002-2318-301X; Vignali, Cristian/0000-0002-8853-9611;
Ranalli, Piero/0000-0003-3956-755X; Comastri,
Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177;
Nicastro, Fabrizio/0000-0002-6896-1364
FU INAF-Fellowship program; Fondecyt [11100449]; ASI-INAF [1/009/10/0]; NAS
XMM [NNX08AX51G, NNX09AQ05G]; ASI [ASI-ADAE]; Greek General Secretariat
of Research and Technology
FX NC acknowledges the INAF-Fellowship program for support. PA acknowledges
support from Fondecyt 11100449. We acknowledge financial contribution
from the agreement ASI-INAF 1/009/10/0. FN acknowledges support from NAS
XMM Grant NNX08AX51G, XMM Grant NNX09AQ05G and ASI Grant ASI-ADAE. PR
acknowledges a grant from the Greek General Secretariat of Research and
Technology in the framework of the programme Support of Postdoctoral
Researchers. NC thanks the anonymous referee for the suggested
improvements.
NR 74
TC 21
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U1 0
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2012
VL 427
IS 1
BP 651
EP 663
DI 10.1111/j.1365-2966.2012.21867.x
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 031XH
UT WOS:000310675400050
ER
PT J
AU Livermore, RC
Jones, T
Richard, J
Bower, RG
Ellis, RS
Swinbank, AM
Rigby, JR
Smail, I
Arribas, S
Rodriguez-Zaurin, J
Colina, L
Ebeling, H
Crain, RA
AF Livermore, R. C.
Jones, T.
Richard, J.
Bower, R. G.
Ellis, R. S.
Swinbank, A. M.
Rigby, J. R.
Smail, Ian
Arribas, S.
Rodriguez-Zaurin, J.
Colina, L.
Ebeling, H.
Crain, R. A.
TI Hubble Space Telescope H alpha imaging of star-forming galaxies at z
similar or equal to 1-1.5: evolution in the size and luminosity of giant
H II regions
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: strong; galaxies: high-redshift; galaxies: star
formation
ID INTEGRAL FIELD SPECTROSCOPY; ULTRA DEEP FIELD; HIGH-REDSHIFT; MOLECULAR
CLOUDS; INTERSTELLAR-MEDIUM; RESOLVED SPECTROSCOPY; COMPACT SPHEROIDS;
SCALING RELATIONS; SURFACE-DENSITY; BILLION YEARS
AB We present Hubble Space Telescope/Wide Field Camera 3 narrow-band imaging of the H alpha emission in a sample of eight gravitationally lensed galaxies at z = 1-1.5. The magnification caused by the foreground clusters enables us to obtain a median source plane spatial resolution of 360 pc, as well as providing magnifications in flux ranging from similar to 10x to similar to 50x. This enables us to identify resolved star-forming H II regions at this epoch and therefore study their H alpha luminosity distributions for comparisons with equivalent samples at z similar to 2 and in the local Universe. We find evolution in the both luminosity and surface brightness of H II regions with redshift. The distribution of clump properties can be quantified with an H II region luminosity function, which can be fit by a power law with an exponential break at some cut-off, and we find that the cut-off evolves with redshift. We therefore conclude that clumpy galaxies are seen at high redshift because of the evolution of the cut-off mass; the galaxies themselves follow similar scaling relations to those at z = 0, but their H II regions are larger and brighter and thus appear as clumps which dominate the morphology of the galaxy. A simple theoretical argument based on gas collapsing on scales of the Jeans mass in a marginally unstable disc shows that the clumpy morphologies of high-z galaxies are driven by the competing effects of higher gas fractions causing perturbations on larger scales, partially compensated by higher epicyclic frequencies which stabilize the disc.
C1 [Livermore, R. C.; Richard, J.; Bower, R. G.; Swinbank, A. M.; Smail, Ian] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England.
[Jones, T.; Ellis, R. S.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Richard, J.] Observ Lyon, CRAL, F-69561 St Genis Laval, France.
[Rigby, J. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Arribas, S.; Colina, L.] CSIC INTA, Ctr Astrobiol, Dept Astrofis, Madrid 28850, Spain.
[Rodriguez-Zaurin, J.] IAC, E-38205 Tenerife, Spain.
[Ebeling, H.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Crain, R. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Livermore, RC (reprint author), Univ Durham, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England.
EM r.c.livermore@durham.ac.uk
RI Smail, Ian/M-5161-2013; Rigby, Jane/D-4588-2012; Arribas,
Santiago/F-9277-2015
OI Smail, Ian/0000-0003-3037-257X; Rigby, Jane/0000-0002-7627-6551;
Arribas, Santiago/0000-0001-7997-1640
FU STFC; Marie Curie Career Integration Grant [294074]; STScI [GO-09722,
GO-10491, GO-10875, GO-12166]; NASA [NAS5-26555]; NASA through Space
Telescope Science Institute [12197, 11678]
FX The authors would like to thank Karl Glazebrook, Emily Wisnioski, Lisa
Kewley and Norm Murray for useful discussions and Andrew Newman for
providing an updated strong lensing model of the cluster Abell 611. RCL
acknowledges a studentship from STFC, RGB and IS are supported by STFC
and IS further acknowledges a Leverhulme Senior Fellowship. AMS
acknowledges an STFC Advanced Fellowship, and JR is supported by the
Marie Curie Career Integration Grant 294074. HE gratefully acknowledges
financial support from STScI grants GO-09722, GO-10491, GO-10875 and
GO-12166. 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, Inc., under NASA contract NAS5-26555. Support for Program
number 12197 and Program number 11678 was provided by NASA through a
grant from the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS5-26555.
NR 64
TC 34
Z9 34
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 NOV
PY 2012
VL 427
IS 1
BP 688
EP 702
DI 10.1111/j.1365-2966.2012.21900.x
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 031XH
UT WOS:000310675400053
ER
PT J
AU Smith, DJB
Dunne, L
da Cunha, E
Rowlands, K
Maddox, SJ
Gomez, HL
Bonfield, DG
Charlot, S
Driver, SP
Popescu, CC
Tuffs, RJ
Dunlop, JS
Jarvis, MJ
Seymour, N
Symeonidis, M
Baes, M
Bourne, N
Clements, DL
Cooray, A
De Zotti, G
Dye, S
Eales, S
Scott, D
Verma, A
van der Werf, P
Andrae, E
Auld, R
Buttiglione, S
Cava, A
Dariush, A
Fritz, J
Hopwood, R
Ibar, E
Ivison, RJ
Kelvin, L
Madore, BF
Pohlen, M
Rigby, EE
Robotham, A
Seibert, M
Temi, P
AF Smith, D. J. B.
Dunne, L.
da Cunha, E.
Rowlands, K.
Maddox, S. J.
Gomez, H. L.
Bonfield, D. G.
Charlot, S.
Driver, S. P.
Popescu, C. C.
Tuffs, R. J.
Dunlop, J. S.
Jarvis, M. J.
Seymour, N.
Symeonidis, M.
Baes, M.
Bourne, N.
Clements, D. L.
Cooray, A.
De Zotti, G.
Dye, S.
Eales, S.
Scott, D.
Verma, A.
van der Werf, P.
Andrae, E.
Auld, R.
Buttiglione, S.
Cava, A.
Dariush, A.
Fritz, J.
Hopwood, R.
Ibar, E.
Ivison, R. J.
Kelvin, L.
Madore, B. F.
Pohlen, M.
Rigby, E. E.
Robotham, A.
Seibert, M.
Temi, P.
TI Herschel-ATLAS: multi-wavelength SEDs and physical properties of 250 mu
m selected galaxies at z < 0.5
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Review
DE Galaxies: starburst
ID SPECTRAL ENERGY-DISTRIBUTION; SCIENCE DEMONSTRATION PHASE; STAR-FORMING
GALAXIES; DEEP FIELD-SOUTH; STELLAR POPULATIONS; COLD DUST; NEARBY
GALAXIES; SKY SURVEY; SUBMILLIMETER WAVELENGTHS; PHOTOMETRIC REDSHIFTS
AB We present a pan-chromatic analysis of an unprecedented sample of 1402 250 mu m selected galaxies at z < 0.5 (<(z)over bar> = 0.24) from the Herschel-ATLAS survey. We complement our Herschel 100-500 mu m data with UV-K-band photometry from the Galaxy And Mass Assembly (GAMA) survey and apply the magphys energy-balance technique to produce pan-chromatic spectral energy distributions (SEDs) for a representative sample of 250 mu m selected galaxies spanning the most recent 5 Gyr of cosmic history. We derive estimates of physical parameters, including star formation rates, stellar masses, dust masses and infrared (IR) luminosities. The typical H-ATLAS galaxy at z < 0.5 has a far-infrared luminosity in the range 10(10)-10(12) L-circle dot (SFR: 1-50 M-circle dot yr(-1)) and thus is broadly representative of normal star-forming galaxies over this redshift range. We show that 250 mu m selected galaxies contain a larger mass of dust at a given IR luminosity or star formation rate than previous samples selected at 60 mu m from the IRAS. We derive typical SEDs for H-ATLAS galaxies, and show that the emergent SED shape is most sensitive to specific star formation rate. The optical-UV SEDs also become more reddened due to dust at higher redshifts. Our template SEDs are significantly cooler than existing IR templates. They may therefore be most appropriate for inferring total IR luminosities from moderate redshift sub-millimetre selected samples and for inclusion in models of the lower redshift sub-millimetre galaxy populations.
C1 [Smith, D. J. B.; Dunne, L.; Rowlands, K.; Maddox, S. J.; Bourne, N.; Dye, S.; Rigby, E. E.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Smith, D. J. B.; Bonfield, D. G.; Jarvis, M. J.] Univ Hertfordshire, Ctr Astrophys, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England.
[Dunne, L.; Maddox, S. J.] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand.
[da Cunha, E.; Eales, S.] Max Planck Inst Astron, D-60115 Heidelberg, Germany.
[Gomez, H. L.; Auld, R.; Dariush, A.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Charlot, S.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Driver, S. P.; Kelvin, L.; Robotham, A.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Driver, S. P.; Kelvin, L.; Robotham, A.] Univ Western Australia, Int Ctr Radio Astron Res, Perth, WA 6009, Australia.
[Popescu, C. C.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Tuffs, R. J.; Andrae, E.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Dunlop, J. S.; Ivison, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Seymour, N.; Symeonidis, M.] Univ Coll London, Mullard Space Sci Lab, Dept Space & Climate Phys, Dorking RH5 6NT, Surrey, England.
[Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[De Zotti, G.; Buttiglione, S.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[De Zotti, G.] SISSA, I-34136 Trieste, Italy.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Verma, A.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain.
[Dariush, A.; Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England.
[Ibar, E.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Madore, B. F.; Seibert, M.] Observ Carnegie Inst, Pasadena, CA 91101 USA.
[Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA.
[Jarvis, M. J.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa.
RP Smith, DJB (reprint author), Univ Nottingham, Sch Phys & Astron, Univ Pk, Nottingham NG7 2RD, England.
EM daniel.j.b.smith@gmail.com
RI 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 Seymour, Nicholas/0000-0003-3506-5536; 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; Scott,
Douglas/0000-0002-6878-9840
FU STFC (UK); ARC (Australia); AAO; Alfred P. Sloan Foundation; National
Science Foundation; U.S. Department of Energy; National Aeronautics and
Space Administration; Japanese Monbukagakusho; Max Planck Society;
Higher Education Funding Council for England; ASI/INAF [I/009/10/0]
FX The authors wish to thank the anonymous referee for his/her tireless
work and insightful comments, which have substantially improved this
paper. The Herschel-ATLAS is a project with Herschel, which is an ESA
space observatory with science instruments provided by European-led
Principal Investigator consortia and with important participation from
NASA. The H-ATLAS website is http://www.hatlas.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 Sloan Digital Sky Survey and the UKIRT Infrared
Deep Sky Survey. Complementary imaging of the GAMA regions is being
obtained by a number of independent survey programmes including GALEX
MIS, VST KIDS, VISTA VIKING, WISE, GMRT and ASKAP providing UV to radio
coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO,
and the participating institutions. The GAMA website is
http://www.gama-survey.org/. 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 U.S. 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/INAF
agreement no. I/009/10/0.
NR 106
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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 NOV
PY 2012
VL 427
IS 1
BP 703
EP 727
DI 10.1111/j.1365-2966.2012.21930.x
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 031XH
UT WOS:000310675400054
ER
PT J
AU D'Ammando, F
Rau, A
Schady, P
Finke, J
Orienti, M
Greiner, J
Kann, DA
Ojha, R
Foley, AR
Stevens, J
Blanchard, JM
Edwards, PG
Kadler, M
Lovell, JEJ
AF D'Ammando, F.
Rau, A.
Schady, P.
Finke, J.
Orienti, M.
Greiner, J.
Kann, D. A.
Ojha, R.
Foley, A. R.
Stevens, J.
Blanchard, J. M.
Edwards, P. G.
Kadler, M.
Lovell, J. E. J.
TI PKS 2123-463: a confirmed gamma-ray blazar at high redshift
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; galaxies: nuclei; quasars: general; quasars:
individual: PKS 2123-463; gamma rays: general
ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; ALL-SKY SURVEY; BL
LACERTAE OBJECTS; PHOTOMETRIC REDSHIFT; RADIO-SOURCES; COMPTON ANALYSIS;
SOURCE CATALOG; BLACK-HOLES; MISSION
AB The flat spectrum radio quasar (FSRQ) PKS 2123-463 was associated in the first Fermi-Large Area Telescope (LAT) source catalogue with the gamma-ray source 1FGL J2126.1-4603, but when considering the full first two years of Fermi observations, no gamma-ray source at a position consistent with this FSRQ was detected, and thus PKS 2123-463 was not reported in the second Fermi-LAT source catalogue. On 2011 December 14 a gamma-ray source positionally consistent with PKS 2123-463 was detected in flaring activity by Fermi-LAT. This activity triggered radio-to-X-ray observations by the Swift, Gamma-ray Optical/Near-Infrared Detector (GROND), Australia Telescope Compact Array (ATCA), Ceduna and Seven Dishes Karoo Array Telescope (KAT-7) observatories. Results of the localization of the gamma-ray source over 41 months of Fermi-LAT operation are reported here in conjunction with the results of the analysis of radio, optical, ultraviolet (UV) and X-ray data collected soon after the gamma-ray flare. The strict spatial association with the lower energy counterpart together with a simultaneous increase of the activity in optical, UV, X-ray and gamma-ray bands led to a firm identification of the gamma-ray source with PKS 2123-463. A new photometric redshift has been estimated as z = 1.46 +/- 0.05 using GROND and Swift Ultraviolet/Optical Telescope (UVOT) observations, in rough agreement with the disputed spectroscopic redshift of z = 1.67. We fit the broad-band spectral energy distribution with a synchrotron/external Compton model. We find that a thermal disc component is necessary to explain the optical/UV emission detected by Swift/UVOT. This disc has a luminosity of similar to 1.8 x 10(46) erg s(-1), and a fit to the disc emission assuming a Schwarzschild (i.e. non-rotating) black hole gives a mass of similar to 2 x 10(9) M-circle dot. This is the first black hole mass estimate for this source.
C1 [D'Ammando, F.] Univ Perugia, Dip Fis, I-06123 Perugia, Italy.
[D'Ammando, F.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[D'Ammando, F.; Orienti, M.] INAF, Ist Radioastron, I-40129 Bologna, Italy.
[Rau, A.; Schady, P.; Greiner, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Finke, J.] USN, Res Lab, Washington, DC 20375 USA.
[Orienti, M.] Univ Bologna, Dip Astron, I-40127 Bologna, Italy.
[Kann, D. A.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany.
[Ojha, R.] Catholic Univ Amer, Dept Phys, IACS, Washington, DC 20064 USA.
[Foley, A. R.] SKA SA, Cape Town, South Africa.
[Stevens, J.] ATNF, CSIRO Astron & Space Sci, Narrabri, NSW 2390, Australia.
[Blanchard, J. M.; Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
[Edwards, P. G.] ATNF, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Kadler, M.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
[Kadler, M.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
RP D'Ammando, F (reprint author), Univ Perugia, Dip Fis, Via A Pascoli, I-06123 Perugia, Italy.
EM filippo.dammando@fisica.unipg.it
FU DFG [HA 1850/28-1, Kl 766/16-1]; MPE; Commonwealth of Australia; NASA
[NNH09ZDA001N, 31263]
FX Part of the funding for GROND (both hardware and personnel) was
generously granted from the Leibniz-Prize to Professor G. Hasinger (DFG
grant HA 1850/28-1). We thank the Swift team for making these
observations possible, the duty scientists and science planners. DAK
acknowledges support by DFG grant Kl 766/16-1, and is grateful for
travel funding support through MPE. The Australia Telescope Compact
Array is part of the Australia Telescope National Facility which is
funded by the Commonwealth of Australia for operation as a National
Facility managed by CSIRO. This research was funded in part by NASA
through Fermi Guest Investigator grant NNH09ZDA001N (proposal number
31263). This research was supported by an appointment to the NASA
Postdoctoral Program at the Goddard Space Flight Center, administered by
Oak Ridge Associated Universities through a contract with NASA. We thank
Silvia Raino and the anonymous referee for useful comments and
suggestions.
NR 58
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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 NOV
PY 2012
VL 427
IS 1
BP 893
EP 900
DI 10.1111/j.1365-2966.2012.22041.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 031XH
UT WOS:000310675400069
ER
PT J
AU Burgess, D
Drake, J
Marsch, E
Velli, M
von Steiger, R
Zurbuchen, TH
AF Burgess, David
Drake, James
Marsch, Eckart
Velli, Marco
von Steiger, Rudolf
Zurbuchen, Thomas H.
TI Multi-Scale Physics in Coronal Heating and Solar Wind Acceleration
Foreword
SO SPACE SCIENCE REVIEWS
LA English
DT Editorial Material
C1 [von Steiger, Rudolf] Int Space Sci Inst, CH-3012 Bern, Switzerland.
[Burgess, David] Univ London, Sch Phys & Astron, London E1 4NS, England.
[Drake, James] Univ Maryland, Dept Phys, Inst Phys Sci & Technol, College Pk, MD 20742 USA.
[Marsch, Eckart] Univ Kiel, IEAP, D-24118 Kiel, Germany.
[Velli, Marco] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RP von Steiger, R (reprint author), Int Space Sci Inst, Hallerstr 6, CH-3012 Bern, Switzerland.
EM d.burgess@qmul.ac.uk; drake@plasma.umd.edu; marsch@physik.uni-kiel.de;
mvelli@mail.jpl.nasa.gov; vsteiger@issibern.ch; thomasz@umich.edu
RI Von Steiger, Rudolf/F-6822-2011
OI Von Steiger, Rudolf/0000-0002-3350-0023
NR 0
TC 0
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U1 0
U2 6
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD NOV
PY 2012
VL 172
IS 1-4
BP 1
EP 3
DI 10.1007/s11214-012-9939-4
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034MJ
UT WOS:000310877300001
ER
PT J
AU Hansteen, VH
Velli, M
AF Hansteen, Viggo H.
Velli, Marco
TI Solar Wind Models from the Chromosphere to 1 AU
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Solar wind acceleration; Energy conservation; Thermal force; Scaling
laws; Solar wind origins
ID ALFVEN WAVES; TRANSPORT-EQUATIONS; CORONAL HOLES; ACCELERATION;
TURBULENCE; ATMOSPHERE; HELIUM; ENERGY; RECONNECTION; ANISOTROPY
AB Recent models of the fast solar wind are characterized by low coronal electron temperatures while proton, alpha-particle, and minor ion temperatures are expected to be quite high and generally anisotropic, including large temperatures perpendicular to the magnetic field and parallel beams. This entails that the electric field should be relatively unimportant and that solar wind outflows with both high asymptotic flow speeds but maintaining a low mass flux should be a natural outcome of plasma expansion along open polar magnetic field lines. In this chapter we will explain why such changes with respect to the classical, electron thermally driven solar wind have come about and outline the most important remaining concerning the astrophysics of coronal winds.
The progress we have seen in the last decade is largely due observations made with instruments onboard Ulysses (McComas et al. in Space Sci. Rev. 72:93, 1995) and SOHO (Fleck et al. in The SOHO Mission, Kluwer, Dordrecht, 1995). These observations have spawned a new understanding of solar wind energetics, and the consideration of the chromosphere, corona, and solar wind as a unified system.
We will begin by giving our own, highly biased, "pocket history" of solar wind theory highlighting the problems that had to be resolved in order to make the original Parker formulation of thermally driven winds conform with observational results. Central to this discussion are questions of how the wind's asymptotic flow speed and mass flux are set, but we will also touch upon higher order moments such as the ion and electron temperatures and heat fluxes as well as the possible role of Alfv,n waves and particle effects in driving the solar wind outflow. Solar wind scaling laws will be discussed in the context of the origin of slow and fast wind streams.
C1 [Hansteen, Viggo H.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway.
[Velli, Marco] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Hansteen, VH (reprint author), Univ Oslo, Inst Theoret Astrophys, Oslo, Norway.
EM viggoh@astro.uio.no; mvelli@jpl.nasa.gov
NR 75
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PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD NOV
PY 2012
VL 172
IS 1-4
BP 89
EP 121
DI 10.1007/s11214-012-9887-z
PG 33
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034MJ
UT WOS:000310877300007
ER
PT J
AU Antiochos, SK
Linker, JA
Lionello, R
Mikic, Z
Titov, V
Zurbuchen, TH
AF Antiochos, Spiro K.
Linker, Jon A.
Lionello, Roberto
Mikic, Zoran
Titov, Viacheslav
Zurbuchen, Thomas H.
TI The Structure and Dynamics of the Corona-Heliosphere Connection
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Sun: corona; Sun: solar wind
ID SLOW SOLAR-WIND; WHOLE SUN MONTH; MAGNETIC-FIELD; MASS EJECTIONS;
RECONNECTION; STREAMERS; MODELS; FLUX; FLOW; DISCONNECTION
AB Determining how the heliospheric magnetic field and plasma connect to the Sun's corona and photosphere is, perhaps, the central problem in solar and heliospheric physics. For much of the heliosphere, this connection appears to be well understood. It is now generally accepted that so-called coronal holes, which appear dark in X-rays and are predominantly unipolar at the photosphere, are the sources of quasi-steady wind that is generally fast, > 500 km/s, but can sometimes be slow. However, the connection to the Sun of the slow, non-steady wind is far from understood and remains a major mystery. We review the existing theories for the sources of the non-steady wind and demonstrate that they have difficulty accounting for both the observed composition of the wind and its large angular extent. A new theory is described in which this wind originates from the continuous opening and closing of narrow open field corridors in the corona, which give rise to a web of separatrices (the S-Web) in the heliosphere. Note that in this theory the corona-heliosphere connection is intrinsically dynamic, at least for this type of wind. Support for the S-Web model is derived from MHD solutions for the corona and wind during the time of the August 1, 2008 eclipse. Additionally, we perform fully dynamic numerical simulations of the corona and heliosphere in order to test the S-Web model as well as the interchange model proposed by Fisk and co-workers. We discuss the implications of our simulations for the competing theories and for understanding the corona-heliosphere connection, in general.
C1 [Antiochos, Spiro K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Linker, Jon A.; Lionello, Roberto; Mikic, Zoran; Titov, Viacheslav] Predict Sci Inc, San Diego, CA 92121 USA.
[Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Coll Engn, Ann Arbor, MI 48109 USA.
RP Antiochos, SK (reprint author), NASA, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA.
EM spiro.antiochos@nasa.gov
RI Antiochos, Spiro/D-4668-2012
OI Antiochos, Spiro/0000-0003-0176-4312
FU NASA HTP Program; NASA GI Program; NASA SRT Program; NASA TRT Program;
CISM (an NSF Science and Technology Center); Strategic Capabilities;
NASA; NSF; AFOSR; ISSI
FX This work originated from numerous discussions in a LWS Focus Team on
open flux in the heliosphere. The work was funded, in part, by the NASA
HTP, GI, SR&T, and TR&T Programs, by CISM (an NSF Science and Technology
Center), and by Strategic Capabilities (jointly funded by NASA, NSF, and
AFOSR). THZ acknowledges the support of ISSI where much of his work on
this paper was performed. Computational resources were provided by the
NSF supported Texas Advanced Computing Center (TACC) in Austin and the
NASA Advanced Supercomputing Division (NAS) at Ames Research Center.
NR 67
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PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD NOV
PY 2012
VL 172
IS 1-4
BP 169
EP 185
DI 10.1007/s11214-011-9795-7
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034MJ
UT WOS:000310877300011
ER
PT J
AU Edmondson, JK
AF Edmondson, J. K.
TI On the Role of Interchange Reconnection in the Generation of the Slow
Solar Wind
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Solar corona; Solar wind; MHD; Reconnection
ID CORONAL-HOLE BOUNDARIES; OPEN MAGNETIC-FIELD; MASS EJECTIONS; STELLAR
WINDS; EVOLUTION; DYNAMICS; MODELS; SUN; ROTATION; STABILITY
AB The heating of the solar corona and therefore the generation of the solar wind, remain an active area of solar and heliophysics research. Several decades of in situ solar wind plasma observations have revealed a rich bimodal solar wind structure, well correlated with coronal magnetic field activity. Therefore, the reconnection processes associated with the large-scale dynamics of the corona likely play a major role in the generation of the slow solar wind flow regime. In order to elucidate the relationship between reconnection-driven coronal magnetic field structure and dynamics and the generation of the slow solar wind, this paper reviews the observations and phenomenology of the solar wind and coronal magnetic field structure. The geometry and topology of nested flux systems, and the (interchange) reconnection process, in the context of coronal physics is then explained. Once these foundations are laid out, the paper summarizes several fully dynamic, 3D MHD calculations of the global coronal system. Finally, the results of these calculations justify a number of important implications and conclusions on the role of reconnection in the structural dynamics of the coronal magnetic field and the generation of the solar wind.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Edmondson, JK (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 169-506, Pasadena, CA 91109 USA.
EM justin.k.edmondson@jpl.nasa.gov
FU ISSI
FX I would like to gratefully acknowledge S. K. Antiochos, C. R. DeVore,
B.J. Lynch, and T. H. Zurbuchen for their involvement in the
calculations (Edmondson et al. 2009, 2010a, 2010b) and subsequent
discussions. In addition, I want to thank M. Velli, S. Lepri, and the
two reviewers for their valuable insights and discussions regarding this
paper. This review was supported in part by the ISSI workshop on the
"Multi-scale physics in coronal heating and solar wind acceleration-from
the Sun into the inner heliosphere", 25-29 January, 2010, as well as by
an appointment to the NASA Postdoctoral Program at the Jet Propulsion
Laboratory, California Institute of Technology, administered by Oak
Ridge Associated Universities under a contract with the National
Aeronautics and Space Administration. Copyright 2010 California
Institute of Technology. Government sponsorship acknowledged.
NR 61
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PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD NOV
PY 2012
VL 172
IS 1-4
BP 209
EP 225
DI 10.1007/s11214-011-9767-y
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034MJ
UT WOS:000310877300014
ER
PT J
AU Matteini, L
Hellinger, P
Landi, S
Travnicek, PM
Velli, M
AF Matteini, Lorenzo
Hellinger, Petr
Landi, Simone
Travnicek, Pavel M.
Velli, Marco
TI Ion Kinetics in the Solar Wind: Coupling Global Expansion to Local
Microphysics
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Solar wind; Ion kinetics; Numerical simulations
ID POLARIZED ALFVEN WAVES; ELECTROMAGNETIC PROTON/PROTON INSTABILITIES;
PROTON TEMPERATURE ANISOTROPY; HYBRID SIMULATIONS; COULOMB COLLISIONS;
VELOCITY DISTRIBUTIONS; PARAMETRIC DECAY; RADIAL EVOLUTION; CORONAL
HOLES; FIRE HOSE
AB We discuss selected ion kinetic processes relevant in the context of the expanding solar wind. We focus on the role of wave-wave and wave-particle interactions, plasma instabilities and Coulomb collisions on the overall kinetic evolution of ions. We review recent results from the hybrid expanding box model, which enables the coupling of the large scale effects of the solar wind expansion to the microscale kinetics of ions. We discuss how different plasma processes develop and influence each other during the expansion, as well their role in the shaping of ion distribution functions, and we compare the simulation results with the observed trends in the solar wind.
C1 [Matteini, Lorenzo; Landi, Simone; Velli, Marco] Univ Florence, Dipartimento Fis & Astron, I-50125 Florence, Italy.
[Hellinger, Petr; Travnicek, Pavel M.] AS CR, Astron Inst, Prague 14131, Czech Republic.
[Hellinger, Petr; Travnicek, Pavel M.] AS CR, Inst Atmospher Phys, Prague 14131, Czech Republic.
[Travnicek, Pavel M.] Univ Calif Berkeley, SSL, Berkeley, CA 94720 USA.
[Velli, Marco] CALTECH, JPL, Pasadena, CA 91109 USA.
RP Matteini, L (reprint author), Univ Florence, Dipartimento Fis & Astron, Largo Enrico Fermi 2, I-50125 Florence, Italy.
EM matteini@arcetri.astro.it
RI Hellinger, Petr/F-5267-2014; Travnicek, Pavel/G-8608-2014; Landi,
Simone/G-7282-2015
OI Hellinger, Petr/0000-0002-5608-0834; Landi, Simone/0000-0002-1322-8712
FU Italian Space Agency [I/015/07/0]; PECS from European Space Agency
[98068]; ISSI; Czech grant [GAAV IAA300420702]
FX The research described in this paper was supported by the Italian Space
Agency contract ASI No. I/015/07/0 "Solar System Exploration". It was
also carried out in part at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. P. H. and P. M. T. acknowledge the Czech grant
GAAV IAA300420702 and PECS contract No. 98068 from the European Space
Agency. L. M., P. H. and S. L. thanks the ISSI staff for their kind
hospitality and acknowledge ISSI financial support during the ISSI
workshop on Coronal Heating and Solar Wind Acceleration.
NR 97
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD NOV
PY 2012
VL 172
IS 1-4
BP 373
EP 396
DI 10.1007/s11214-011-9774-z
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034MJ
UT WOS:000310877300025
ER
PT J
AU Voytek, MA
AF Voytek, Mary A.
TI Where Will Curiosity Take Us?
SO ASTROBIOLOGY
LA English
DT Editorial Material
C1 NASA Headquarters, Washington, DC 20546 USA.
RP Voytek, MA (reprint author), NASA Headquarters, Room 3Y56, Washington, DC 20546 USA.
EM mary.voytek-1@nasa.gov
NR 0
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PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD NOV
PY 2012
VL 12
IS 11
BP 1093
EP 1094
DI 10.1089/ast.2012.1022
PG 2
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 031NT
UT WOS:000310649600009
PM 23121016
ER
PT J
AU Breger, M
Fossati, L
Balona, L
Kurtz, DW
Robertson, P
Bohlender, D
Lenz, P
Mueller, I
Lueftinger, T
Clarke, BD
Hall, JR
Ibrahim, KA
AF Breger, M.
Fossati, L.
Balona, L.
Kurtz, D. W.
Robertson, P.
Bohlender, D.
Lenz, P.
Mueller, I.
Lueftinger, Th.
Clarke, Bruce D.
Hall, Jennifer R.
Ibrahim, Khadeejah A.
TI RELATIONSHIP BETWEEN LOW AND HIGH FREQUENCIES IN delta SCUTI STARS:
PHOTOMETRIC KEPLER AND SPECTROSCOPIC ANALYSES OF THE RAPID ROTATOR KIC
8054146
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: abundances; stars: individual (KIC 8054146); stars: oscillations;
stars: rotation; stars: variables: delta Scuti
ID LINE-DATA-BASE; A-TYPE STARS; PRAESEPE CLUSTER; TURBULENT CONVECTION;
MODEL; ATMOSPHERES; ABUNDANCES
AB Two years of Kepler data of KIC 8054146 (delta Sct/gamma Dor hybrid) revealed 349 statistically significant frequencies between 0.54 and 191.36 cycles day(-1) (6.3 mu Hz to 2.21 mHz). The 117 low frequencies cluster in specific frequency bands, but do not show the equidistant period spacings predicted for gravity modes of successive radial order, n, and reported for at least one other hybrid pulsator. The four dominant low frequencies in the 2.8-3.0 cycles day(-1) (32-35 mu Hz) range show strong amplitude variability with timescales of months and years. These four low frequencies also determine the spacing of the higher frequencies in and beyond the delta Sct pressure-mode frequency domain. In fact, most of the higher frequencies belong to one of three families with spacings linked to a specific dominant low frequency. In the Fourier spectrum, these family regularities show up as triplets, high-frequency sequences with absolutely equidistant frequency spacings, side lobes (amplitude modulations), and other regularities in frequency spacings. Furthermore, within two families the amplitude variations between the low and high frequencies are related. We conclude that the low frequencies (gravity modes, rotation) and observed high frequencies (mostly pressure modes) are physically connected. This unusual behavior may be related to the very rapid rotation of the star: from a combination of high-and low-resolution spectroscopy we determined that KIC 8054146 is a very fast rotator (upsilon sin i = 300 +/- 20 km s(-1)) with an effective temperature of 7600 +/- 200 K and a surface gravity log g of 3.9 +/- 0.3. Several astrophysical ideas explaining the origin of the relationship between the low and high frequencies are explored.
C1 [Breger, M.; Robertson, P.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Breger, M.; Mueller, I.; Lueftinger, Th.] Univ Vienna, Inst Astronphys, A-1180 Vienna, Austria.
[Fossati, L.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[Balona, L.] S African Astron Observ, ZA-7935 Cape Town, South Africa.
[Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Bohlender, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Lenz, P.] Polish Acad Sci, N Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Clarke, Bruce D.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Hall, Jennifer R.; Ibrahim, Khadeejah A.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Breger, M (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA.
FU Austrian Fonds zur Forderung der wissenschaftlichen Forschung [P
21830-N16]; NASA's Science Mission Directorate
FX M.B. is grateful to E. L. Robinson, K. Zwintz, and M. Montgomery for
helpful discussions. This investigation has been supported by the
Austrian Fonds zur Forderung der wissenschaftlichen Forschung through
project P 21830-N16. The authors wish to thank the Kepler team for their
generosity in allowing the data to be released to the Kepler
Asteroseismic Science Consortium (KASC) ahead of public release and for
their outstanding efforts which have made these results possible.
Funding for the Kepler mission is provided by NASA's Science Mission
Directorate.
NR 26
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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 NOV 1
PY 2012
VL 759
IS 1
AR 62
DI 10.1088/0004-637X/759/1/62
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030JL
UT WOS:000310566900062
ER
PT J
AU Debes, JH
Hoard, DW
Farihi, J
Wachter, S
Leisawitz, DT
Cohen, M
AF Debes, John H.
Hoard, D. W.
Farihi, Jay
Wachter, Stefanie
Leisawitz, David T.
Cohen, Martin
TI THE WIRED SURVEY. III. AN INFRARED EXCESS AROUND THE ECLIPSING
POST-COMMON ENVELOPE BINARY SDSS J030308.35+005443.7
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; circumstellar matter; white dwarfs
ID DIGITAL-SKY-SURVEY; SPITZER-SPACE-TELESCOPE; MAIN-SEQUENCE BINARIES;
WHITE-DWARF CATALOG; PLANETARY SYSTEMS; DUST; CALIBRATION; ACCRETION;
STARS; I.
AB We present the discovery with WISE of a significant infrared excess associated with the eclipsing post-common envelope binary SDSS J030308.35+005443.7, the first excess discovered around a non-interacting white dwarf+main-sequence M dwarf binary. The spectral energy distribution of the white dwarf+M dwarf companion shows significant excess longward of 3 mu m. A T-eff of 8940 K for the white dwarf is consistent with a cooling age >2 Gyr, implying that the excess may be due to a recently formed circumbinary dust disk of material that extends from the tidal truncation radius of the binary at 1.96 R-circle dot out to <0.8 AU, with a total mass of similar to 10(20) g. We also construct WISE and follow-up ground-based near-infrared light curves of the system and find variability in the K band that appears to be in phase with ellipsoidal variations observed in the visible. The presence of dust might be due to (1) material being generated by the destruction of small rocky bodies that are being perturbed by an unseen planetary system or (2) dust condensing from the companion's wind. The high inclination of this system and the presence of dust make it an attractive target for M dwarf transit surveys and long-term photometric monitoring.
C1 [Debes, John H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Hoard, D. W.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Farihi, Jay] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Wachter, Stefanie] CALTECH, IPAC, Pasadena, CA 91125 USA.
[Leisawitz, David T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cohen, Martin] Monterey Inst Res Astron, Marina, CA 93933 USA.
RP Debes, JH (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
OI Hoard, Donald W./0000-0002-6800-6519; Farihi, Jay/0000-0003-1748-602X
FU National Aeronautics and Space Administration (NASA); NASA; National
Science Foundation; NASA [1000-S-MA756]; UCLA FAU [26311]
FX This work is based on data obtained from: (1) the Wide-field Infrared
Survey Explorer, which is a joint project of the University of
California, Los Angeles, and the Jet Propulsion Laboratory (JPL),
California Institute of Technology (Caltech), funded by the National
Aeronautics and Space Administration (NASA); (2) the Two Micron All Sky
Survey (2MASS), a joint project of the University of Massachusetts and
the Infrared Processing and Analysis Center (IPAC)/Caltech, funded by
NASA and the National Science Foundation; (3) the SIMBAD database,
operated at CDS, Strasbourg, France; and (4) the NASA/IPAC Infrared
Science Archive, which is operated by JPL, Caltech, under a contract
with NASA. M. C. thanks NASA for supporting his participation in this
work through UCLA Sub-Award 1000-S-MA756 with a UCLA FAU 26311 to MIRA.
NR 33
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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 NOV 1
PY 2012
VL 759
IS 1
AR 37
DI 10.1088/0004-637X/759/1/37
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030JL
UT WOS:000310566900037
ER
PT J
AU Dominik, M
Belczynski, K
Fryer, C
Holz, DE
Berti, E
Bulik, T
Mandel, I
O'Shaughnessy, R
AF Dominik, Michal
Belczynski, Krzysztof
Fryer, Christopher
Holz, Daniel E.
Berti, Emanuele
Bulik, Tomasz
Mandel, Ilya
O'Shaughnessy, Richard
TI DOUBLE COMPACT OBJECTS. I. THE SIGNIFICANCE OF THE COMMON ENVELOPE ON
MERGER RATES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; black hole physics; stars: evolution; stars: neutron
ID BLACK-HOLE BINARIES; GAMMA-RAY BURSTS; BINDING-ENERGY PARAMETER; MASSIVE
CLOSE BINARIES; NEUTRON-STAR SYSTEMS; O-TYPE STARS; GLOBULAR-CLUSTERS;
INSPIRALING BINARIES; EXPLOSION MECHANISM; GRAVITATIONAL-WAVES
AB The last decade of observational and theoretical developments in stellar and binary evolution provides an opportunity to incorporate major improvements to the predictions from population synthesis models. We compute the Galactic merger rates for NS-NS, BH-NS, and BH-BH mergers with the StarTrack code. The most important revisions include updated wind mass-loss rates (allowing for stellar-mass black holes up to 80 M-circle dot), a realistic treatment of the common envelope phase (a process that can affect merger rates by 2-3 orders of magnitude), and a qualitatively new neutron star/black hole mass distribution (consistent with the observed "mass gap"). Our findings include the following. (1) The binding energy of the envelope plays a pivotal role in determining whether a binary merges within a Hubble time. (2) Our description of natal kicks from supernovae plays an important role, especially for the formation of BH-BH systems. (3) The masses of BH-BH systems can be substantially increased in the case of low metallicities or weak winds. (4) Certain combinations of parameters underpredict the Galactic NS-NS merger rate and can be ruled out. (5) Models incorporating delayed supernovae do not agree with the observed NS/BH "mass gap," in accordance with our previous work. This is the first in a series of three papers. The second paper will study the merger rates of double compact objects as a function of redshift, star formation rate, and metallicity. In the third paper, we will present the detection rates for gravitational-wave observatories, using up-to-date signal waveforms and sensitivity curves.
C1 [Dominik, Michal; Belczynski, Krzysztof; Bulik, Tomasz] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland.
[Belczynski, Krzysztof] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA.
[Holz, Daniel E.] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA.
[Holz, Daniel E.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Holz, Daniel E.] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA.
[Berti, Emanuele] Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA.
[Berti, Emanuele] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mandel, Ilya] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[O'Shaughnessy, Richard] Univ Wisconsin, Ctr Gravitat & Cosmol, Milwaukee, WI 53211 USA.
RP Dominik, M (reprint author), Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland.
RI Berti, Emanuele/C-9331-2016;
OI Berti, Emanuele/0000-0003-0751-5130; O'Shaughnessy,
Richard/0000-0001-5832-8517; Mandel, Ilya/0000-0002-6134-8946
FU National Nuclear Security Administration of the U.S. Department of
Energy at Los Alamos National Laboratory [DE-AC52-06NA25396]; NSF
[PHY-0900735, PHY-1055103, PHY-0970074]; Bradley Program Fellowship; UWM
Research Growth Initiative; Polish grant [N N203 511238,
DPN/N176/VIRGO/2009, N N203 302835, GR-4071]
FX We thank Francesca Valsecchi for providing detailed calculations of
specific mass transfer scenarios. We also thank the N. Copernicus
Astronomical Centre in Warsaw, Poland, and the University of Texas at
Brownsville, USA, for their courtesy in allowing us to use their
computational resources. Work at LANL was done under the auspices of the
National Nuclear Security Administration of the U.S. Department of
Energy at Los Alamos National Laboratory under Contract No.
DE-AC52-06NA25396. E.B. is supported by NSF grant PHY-0900735 and by NSF
CAREER grant PHY-1055103. R.O.S. is currently supported by NSF award
PHY-0970074, the Bradley Program Fellowship, and the UWM Research Growth
Initiative. T.B. is supported by the Polish grants N N203 511238 and
DPN/N176/VIRGO/2009. K.B. is supported by the Polish grant N N203
302835. M.D. is supported by the Polish grant GR-4071.
NR 82
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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 NOV 1
PY 2012
VL 759
IS 1
AR 52
DI 10.1088/0004-637X/759/1/52
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030JL
UT WOS:000310566900052
ER
PT J
AU Dragomir, D
Matthews, JM
Kuschnig, R
Rowe, JF
Gladman, BJ
Guenther, DB
Moffat, AFJ
Rucinski, SM
Sasselov, D
Weiss, WW
AF Dragomir, Diana
Matthews, Jaymie M.
Kuschnig, Rainer
Rowe, Jason F.
Gladman, Brett J.
Guenther, David B.
Moffat, Anthony F. J.
Rucinski, Slavek M.
Sasselov, Dimitar
Weiss, Werner W.
TI A SEARCH FOR TRANSITS OF GJ 581e AND CHARACTERIZATION OF THE HOST STAR
VARIABILITY USING MOST SPACE TELESCOPE PHOTOMETRY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (GJ 581); techniques: photometric
ID EXTRA-SOLAR PLANETS; M-CIRCLE-PLUS; SUPER-EARTHS; TRANSMISSION SPECTRUM;
HABITABLE ZONE; TAU-BOOTIS; EXOPLANET SYSTEM; MAGNETIC CYCLES; HARPS
SEARCH; LOW-MASS
AB The GJ 581 system has been amply studied since its discovery in 2005: the number of known planets in the system has increased and their orbital parameters are among the most precisely determined for radial-velocity-detected exoplanets. We have acquired MOST space-based photometry during 2007 and 2009, with the aims of measuring the stellar variability and searching for transits of GJ 581e, respectively. We quantify our sensitivity to shallow transit signals using Monte Carlo simulations, and perform a transit search within the 3 sigma transit windows corresponding to both the circular and Keplerian orbit ephemerides. Our analysis rules out transits for a planet with an orbital period of 3.15 days (GJ 581e) having a radius larger than 1.62 R-circle plus (or a density lower than 2.39 g cm(-3) for an orbital inclination of 90 degrees) to 2 sigma confidence. Thus, if the planet transits, we can exclude hydrogen, helium, and water theoretical model compositions. The MOST photometry also allows us to rule out transits of GJ 581b within the Keplerian orbit-derived transit window for impact parameter values smaller than similar to 0.4 and confirm previous results which exclude transits for this planet within the circular orbit-derived transit window, for all plausible interior compositions. We find that the stellar brightness of GJ 581 is stable to within 1%, a characteristic which is favorable to the development of life in the habitable zone of the system. In the 2009 photometry, we detect a stellar signal with a period of 5.586 +/- 0.051 days, which is close to the orbital period of GJ 581b (P = 5.37 days). However, further monitoring of the system is necessary to verify the nature of this variation.
C1 [Dragomir, Diana; Matthews, Jaymie M.; Gladman, Brett J.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Guenther, David B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Moffat, Anthony F. J.] Univ Montreal, Dept Phys & Obs Mt Megant, Montreal, PQ H3C 3J7, Canada.
[Rucinski, Slavek M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Dragomir, D (reprint author), Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
EM diana@phas.ubc.ca
OI Dragomir, Diana/0000-0003-2313-467X
FU University of British Columbia; Natural Sciences and Engineering
Research Council of Canada; FQRNT (Qubec); Austrian Science Fund
[P22691-N16]; Austrian Research Promotion Agency-ALR
FX The authors thank Michael Gillon, Stephen Kane, and Bryce Croll for
useful conversations. We are grateful to Xavier Bonfils and Thierry
Forveille for providing additional information regarding their analysis
of the GJ 581 system parameters. We also thank the anonymous referee for
valuable comments and suggestions which have helped improve and clarify
the manuscript. D.D. is supported by a University of British Columbia
Four Year Fellowship. The Natural Sciences and Engineering Research
Council of Canada supports the research of D.B.G., J.M.M., A.F.J.M., and
S.M.R. Additional support for A.F.J.M. comes from FQRNT (Qubec). R.K.
and W.W.W. were supported by the Austrian Science Fund (P22691-N16) and
by the Austrian Research Promotion Agency-ALR.
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 NOV 1
PY 2012
VL 759
IS 1
AR 2
DI 10.1088/0004-637X/759/1/2
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030JL
UT WOS:000310566900002
ER
PT J
AU Emslie, AG
Dennis, BR
Shih, AY
Chamberlin, PC
Mewaldt, RA
Moore, CS
Share, GH
Vourlidas, A
Welsch, BT
AF Emslie, A. G.
Dennis, B. R.
Shih, A. Y.
Chamberlin, P. C.
Mewaldt, R. A.
Moore, C. S.
Share, G. H.
Vourlidas, A.
Welsch, B. T.
TI GLOBAL ENERGETICS OF THIRTY-EIGHT LARGE SOLAR ERUPTIVE EVENTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: coronal mass ejections (CMEs); Sun: flares; Sun:
particle emission; Sun: X-rays, gamma rays
ID CORONAL MASS EJECTIONS; 20 JANUARY 2005; ADVANCED COMPOSITION EXPLORER;
FREE FIELD EXTRAPOLATIONS; GROUND-LEVEL EVENTS; X-RAY IMAGER;
FORCE-FREE; GAMMA-RAY; MAGNETIC-FIELDS; INTERPLANETARY MEDIUM
AB We have evaluated the energetics of 38 solar eruptive events observed by a variety of spacecraft instruments between 2002 February and 2006 December, as accurately as the observations allow. The measured energetic components include: (1) the radiated energy in the Geostationary Operational Environmental Satellite 1-8 angstrom band, (2) the total energy radiated from the soft X-ray (SXR) emitting plasma, (3) the peak energy in the SXR-emitting plasma, (4) the bolometric radiated energy over the full duration of the event, (5) the energy in flare-accelerated electrons above 20 keV and in flare-accelerated ions above 1MeV, (6) the kinetic and potential energies of the coronal mass ejection (CME), (7) the energy in solar energetic particles (SEPs) observed in interplanetary space, and (8) the amount of free (non-potential) magnetic energy estimated to be available in the pertinent active region. Major conclusions include: (1) the energy radiated by the SXR-emitting plasma exceeds, by about half an order of magnitude, the peak energy content of the thermal plasma that produces this radiation; (2) the energy content in flare-accelerated electrons and ions is sufficient to supply the bolometric energy radiated across all wavelengths throughout the event; (3) the energy contents of flare-accelerated electrons and ions are comparable; (4) the energy in SEPs is typically a few percent of the CME kinetic energy (measured in the rest frame of the solar wind); and (5) the available magnetic energy is sufficient to power the CME, the flare-accelerated particles, and the hot thermal plasma.
C1 [Emslie, A. G.] Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA.
[Dennis, B. R.; Shih, A. Y.; Chamberlin, P. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mewaldt, R. A.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
[Moore, C. S.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Share, G. H.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Vourlidas, A.] USN, Res Lab, Washington, DC 20375 USA.
[Welsch, B. T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Emslie, AG (reprint author), Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA.
EM emslieg@wku.edu; brian.r.dennis@nasa.gov; albert.y.shih@nasa.gov;
phillip.c.chamberlin@nasa.gov; rmewaldt@srl.caltech.edu;
christopher.moore-1@colorado.edu; share@astro.umd.edu;
vourlidas@nrl.navy.mil; welsch@ssl.berkeley.edu
RI Chamberlin, Phillip/C-9531-2012; Vourlidas, Angelos/C-8231-2009
OI Chamberlin, Phillip/0000-0003-4372-7405; Vourlidas,
Angelos/0000-0002-8164-5948
FU NASA [NNX10AT78J, NNX08AI11G, NNX11AO75G]; NASA
FX We thank Gordon Holman, Richard Schwartz, and Kim Tolbert for help with
analyzing the GOES and RHESSI data, and Anil Gopie for doing most of the
GOES data analysis. We also thank the referee for an unusually
comprehensive and thorough review of the originally submitted version of
this manuscript, which resulted in a significantly improved paper.
A.G.E. was supported by NASA Grant NNX10AT78J, R.A.M. by NASA Grants
NNX08AI11G and NNX11AO75G, and A.V. by various NASA grants to the Naval
Research Laboratory. SOHO is a joint ESA and NASA mission. CHIANTI is a
collaborative project involving researchers at NRL (USA), RAL (UK), and
the Universities of Cambridge (UK), George Mason (USA), and Florence
(Italy).
NR 97
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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 NOV 1
PY 2012
VL 759
IS 1
AR 71
DI 10.1088/0004-637X/759/1/71
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030JL
UT WOS:000310566900071
ER
PT J
AU Grav, T
Mainzer, AK
Bauer, JM
Masiero, JR
Nugent, CR
AF Grav, T.
Mainzer, A. K.
Bauer, J. M.
Masiero, J. R.
Nugent, C. R.
TI WISE/NEOWISE OBSERVATIONS OF THE JOVIAN TROJAN POPULATION: TAXONOMY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: planetary systems; minor planets, asteroids: general
ID ASTEROID SPECTROSCOPIC SURVEY; THERMAL-MODEL CALIBRATION;
INFRARED-SURVEY-EXPLORER; MAIN BELT ASTEROIDS; SOLAR-SYSTEM; DYNAMICAL
FAMILIES; PHOTOMETRIC SURVEY; JUPITER TROJANS; MINOR PLANETS; IRREGULAR
SATELLITES
AB We present updated/new thermal model fits for 478 Jovian Trojan asteroids observed with the Wide-field Infrared Survey Explorer (WISE). Using the fact that the two shortest bands used by WISE, centered on 3.4 and 4.6 mu m, are dominated by reflected light, we derive albedos of a significant fraction of these objects in these bands. While the visible albedos of both the C-, P-, and D-type asteroids are strikingly similar, the WISE data reveal that the albedo at 3.4 mu m is different between C-/P- and D-types. The albedo at 3.4 mu m can thus be used to classify the objects, with C-/P-types having values less than 10% and D-types have values larger than 10%. Classifying all objects larger than 50 km shows that the D-type objects dominate both the leading cloud (L-4), with a fraction of 84%, and trailing cloud (L-5), with a fraction of 71%-80%. The two clouds thus have very similar taxonomic distribution for these large objects, but the leading cloud has a larger number of these large objects, L-4/L-5 = 1.34. The taxonomic distribution of the Jovian Trojans is found to be different from that of the large Hildas, which is dominated by C-and P-type objects. At smaller sizes, the fraction of D-type Hildas starts increasing, showing more similarities with the Jovian Trojans. If this similarity is confirmed through deeper surveys, it could hold important clues to the formation and evolution of the two populations. The Jovian Trojans does have similar taxonomic distribution to that of the Jovian irregular satellites, but lacks the ultra red surfaces found among the Saturnian irregular satellites and Centaur population.
C1 [Grav, T.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Mainzer, A. K.; Bauer, J. M.; Masiero, J. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Nugent, C. R.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
RP Grav, T (reprint author), Planetary Sci Inst, Tucson, AZ 85719 USA.
EM tgrav@psi.edu
OI Masiero, Joseph/0000-0003-2638-720X
FU National Aeronautics and Space Administration; Planetary Science
Division of the National Aeronautics and Space Administration
FX This publication makes use of data products from the Wide-field Infrared
Survey Explorer, which is a joint project of the University of
California, Los Angeles, and the Jet Propulsion Laboratory/California
Institute of Technology, funded by the National Aeronautics and Space
Administration. This publication also makes use of data products from
NEOWISE, which is a project of the Jet Propulsion Laboratory/California
Institute of Technology, funded by the Planetary Science Division of the
National Aeronautics and Space Administration. We gratefully acknowledge
the extraordinary services specific to NEOWISE contributed by the
International Astronomical Union's Minor Planet Center, operated by the
Harvard-Smithsonian Center for Astro-physics, and the Central Bureau for
Astronomical Telegrams, operated by Harvard University. We also thank
the worldwide community of dedicated amateur and professional
astronomers devoted to minor planet follow-up observations. This
research has made use the NASA/IPAC Infrared Science Archive, which is
operated by the Jet Propulsion Laboratory/California Institute of
Technology, under contract with the National Aeronautics and Space
Administration.
NR 58
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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 NOV 1
PY 2012
VL 759
IS 1
AR 49
DI 10.1088/0004-637X/759/1/49
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030JL
UT WOS:000310566900049
ER
PT J
AU Jia, JJ
Ptak, A
Heckman, TM
Braito, V
Reeves, J
AF Jia, Jianjun
Ptak, Andrew
Heckman, Timothy M.
Braito, Valentina
Reeves, James
TI A CHANDRA OBSERVATION OF THE ULTRALUMINOUS INFRARED GALAXY IRAS
19254-7245 (THE SUPERANTENNAE): X-RAY EMISSION FROM THE COMPTON-THICK
ACTIVE GALACTIC NUCLEUS AND THE DIFFUSE STARBURST
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (IRAS 19254-7245 (the
Superantennae)); galaxies: starburst; X-rays: galaxies
ID STAR-FORMING GALAXIES; LYMAN BREAK GALAXIES; FAR-ULTRAVIOLET; FEEDBACK;
LINE; LUMINOSITY; MERGERS; SPECTROSCOPY; SUPERWINDS; ANALOG
AB We present a Chandra observation of IRAS 19254-7245, a nearby ultraluminous infrared galaxy also known as the Superantennae. The high spatial resolution of Chandra allows us to disentangle for the first time the diffuse starburst (SB) emission from the embedded Compton-thick active galactic nucleus (AGN) in the southern nucleus. No AGN activity is detected in the northern nucleus. The 2-10 keV spectrum of the AGN emission is fitted by a flat power law (Gamma = 1.3) and an He-like Fe K alpha line with equivalent width similar to 1.5 keV, consistent with previous observations. The Fe K alpha line profile could be resolved as a blend of a neutral 6.4 keV line and an ionized 6.7 keV (He-like) or 6.9 keV (H-like) line. Variability of the neutral line is detected compared with the previous XMM-Newton and Suzaku observations, demonstrating the compact size of the iron line emission. The spectrum of the galaxy-scale extended emission excluding the AGN and other bright point sources is fitted with a thermal component with a best-fit kT of similar to 0.8 keV. The 2-10 keV luminosity of the extended emission is about one order of magnitude lower than that of the AGN. The basic physical and structural properties of the extended emission are fully consistent with a galactic wind being driven by the SB. A candidate ultraluminous X-ray source is detected 8 '' south of the southern nucleus. The 0.3-10 keV luminosity of this off-nuclear point source is similar to 6 x 10(40) erg s(-1) if the emission is isotropic and the source is associated with the Superantennae.
C1 [Jia, Jianjun; Heckman, Timothy M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Ptak, Andrew] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Braito, Valentina] INAF Osservatorio Astron Brera, I-20121 Milan, Italy.
[Reeves, James] Univ Keele, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England.
RP Jia, JJ (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RI XRAY, SUZAKU/A-1808-2009;
OI Braito, Valentina/0000-0002-2629-4989
FU Chandra grant [GO9-0091X]
FX This work was supported by Chandra grant GO9-0091X. The authors thank
the anonymous referee for helpful comments and suggestions.
NR 51
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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 NOV 1
PY 2012
VL 759
IS 1
AR 41
DI 10.1088/0004-637X/759/1/41
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030JL
UT WOS:000310566900041
ER
PT J
AU Kanner, J
Camp, J
Racusin, J
Gehrels, N
White, D
AF Kanner, Jonah
Camp, Jordan
Racusin, Judith
Gehrels, Neil
White, Darren
TI SEEKING COUNTERPARTS TO ADVANCED LIGO/Virgo TRANSIENTS WITH SWIFT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: statistics; gamma-ray burst: general; gravitational waves;
X-rays: general
ID GAMMA-RAY BURSTS; COMPACT OBJECT MERGERS; NEUTRON-STAR BINARIES; ALL-SKY
SURVEY; ELECTROMAGNETIC COUNTERPARTS; LIGHT CURVES; SEARCH; TELESCOPE;
RATES; FERMI
AB Binary neutron star (NS) mergers are among the most promising astrophysical sources of gravitational wave (GW) emission for Advanced LIGO and Advanced Virgo, expected to be operational in 2015. Finding electromagnetic counterparts to these signals will be essential to placing them in an astronomical context. The Swift satellite carries a sensitive X-Ray Telescope (XRT), and can respond to target-of-opportunity requests within one to two hours, and so is uniquely poised to find the X-ray counterparts to LIGO/Virgo triggers. Assuming that NS mergers are the progenitors of short gamma-ray bursts (GRBs), some percentage of LIGO/Virgo triggers will be accompanied by X-ray band afterglows that are brighter than 10(-12) erg s(-1) cm(-2) in the XRT band one day after the trigger time. We find that a soft X-ray transient of this flux is bright enough to be extremely rare, and so could be confidently associated with even a moderately localized GW signal. We examine two possible search strategies with the Swift XRT to find bright transients in LIGO/Virgo error boxes. In the first strategy, XRT could search a volume of space with a similar to 100 Mpc radius by observing similar to 30 galaxies over the course of a day, with sufficient depth to observe the expected X-ray afterglow. For an extended LIGO/Virgo horizon distance, the XRT could employ 100 s exposures to cover an area of similar to 35 deg(2) in about a day and remain sensitive enough to image GW-discovered GRB afterglows. These strategies demonstrate that discovery of X-ray band counterparts to GW triggers will be possible, though challenging, with current facilities.
C1 [Kanner, Jonah; Camp, Jordan; Racusin, Judith; Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[White, Darren] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England.
RP Kanner, J (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 663, Greenbelt, MD 20771 USA.
EM jonah.b.kanner@nasa.gov
RI Racusin, Judith/D-2935-2012;
OI Kanner, Jonah/0000-0001-8115-0577
FU NASA Postdoctoral Program at Goddard Space Flight Center
FX We are grateful for fruitful discussions and feedback from Lindy
Blackburn, David Burrows, Thomas Dent, Brennan Hughey, Susan Kassin,
Takanori Sakamoto, and Peter Shawhan. J.K. is supported by an
appointment to the NASA Postdoctoral Program at Goddard Space Flight
Center, administered by Oak Ridge Associated Universities through a
contract with NASA. This work made use of data supplied by the UK Swift
Science Data Centre at the University of Leicester and data obtained
from the High Energy Astrophysics Science Archive Research Center
(HEASARC), provided by NASA's Goddard Space Flight Center.
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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 NOV 1
PY 2012
VL 759
IS 1
AR 22
DI 10.1088/0004-637X/759/1/22
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030JL
UT WOS:000310566900022
ER
PT J
AU Masiero, JR
Mainzer, AK
Grav, T
Bauer, JM
Jedicke, R
AF Masiero, Joseph R.
Mainzer, A. K.
Grav, T.
Bauer, J. M.
Jedicke, R.
TI REVISING THE AGE FOR THE BAPTISTINA ASTEROID FAMILY USING WISE/NEOWISE
DATA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE minor planets, asteroids: general
ID MAIN-BELT ASTEROIDS; INFRARED-SURVEY-EXPLORER; SOLAR-SYSTEM; K/T
IMPACTOR; YARKOVSKY; FRAGMENTS; EVOLUTION; CHRONOLOGY; PLANETS; NEOWISE
AB We have used numerical routines to model the evolution of a simulated Baptistina family to constrain its age in light of new measurements of the diameters and albedos of family members from the Wide-field Infrared Survey Explorer. We also investigate the effect of varying the assumed physical and orbital parameters on the best-fitting age. We find that the physically allowed range of assumed values for the density and thermal conductivity induces a large uncertainty in the rate of evolution. When realistic uncertainties in the family members' physical parameters are taken into account, we find that the best-fitting age can fall anywhere in the range of 140-320 Myr. Without more information on the physical properties of the family members, it is difficult to place a more firm constraint on Baptistina's age.
C1 [Masiero, Joseph R.; Mainzer, A. K.; Bauer, J. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grav, T.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Bauer, J. M.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Jedicke, R.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP Masiero, JR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 321-520, Pasadena, CA 91109 USA.
EM Joseph.Masiero@jpl.nasa.gov
OI Masiero, Joseph/0000-0003-2638-720X
FU NASA Postdoctoral Program at JPL; JPL Office of the Chief Information
Officer; National Aeronautics and Space Administration; Planetary
Science Division of the National Aeronautics and Space Administration
FX We thank the referee, Bill Bottke, for his helpful and insightful
comments that resulted in a critical reanalysis of the data, greatly
improving our results and the manuscript in general. We also thank Bob
McMillan for his editing of this manuscript. J.R.M. was supported by an
appointment to the NASA Postdoctoral Program at JPL, administered by Oak
Ridge Associated Universities through a contract with NASA. Computer
simulations for this research were carried out on JPL's Zodiac
supercomputer, which is administered by the JPL Supercomputing and
Visualization Facility. The supercomputer used in this investigation was
provided by funding from the JPL Office of the Chief Information
Officer. 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. This research has made
use of the NASA/IPAC Infrared Science Archive, which is operated by the
Jet Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration.
NR 42
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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 NOV 1
PY 2012
VL 759
IS 1
AR 14
DI 10.1088/0004-637X/759/1/14
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030JL
UT WOS:000310566900014
ER
PT J
AU Pereira, TMD
De Pontieu, B
Carlsson, M
AF Pereira, Tiago M. D.
De Pontieu, Bart
Carlsson, Mats
TI QUANTIFYING SPICULES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: atmosphere; Sun: chromosphere; Sun: transition region
ID HIGH-RESOLUTION OBSERVATIONS; SOLAR OPTICAL TELESCOPE; II SPICULES;
MAGNETOACOUSTIC SHOCKS; MAGNETIC CHROMOSPHERE; DYNAMIC FIBRILS; HINODE;
WAVES; SIMULATIONS; DRIVEN
AB Understanding the dynamic solar chromosphere is fundamental in solar physics. Spicules are an important feature of the chromosphere, connecting the photosphere to the corona, potentially mediating the transfer of energy and mass. The aim of this work is to study the properties of spicules over different regions of the Sun. Our goal is to investigate if there is more than one type of spicule, and how spicules behave in the quiet Sun, coronal holes, and active regions. We make use of high cadence and high spatial resolution Ca II H observations taken by Hinode/Solar Optical Telescope. Making use of a semi-automated detection algorithm, we self-consistently track and measure the properties of 519 spicules over different regions. We find clear evidence of two types of spicules. Type I spicules show a rise and fall and have typical lifetimes of 150-400 s and maximum ascending velocities of 15-40 km s(-1), while type II spicules have shorter lifetimes of 50-150 s, faster velocities of 30-110 km s(-1), and are not seen to fall down, but rather fade at around their maximum length. Type II spicules are the most common, seen in the quiet Sun and coronal holes. Type I spicules are seen mostly in active regions. There are regional differences between quiet-Sun and coronal hole spicules, likely attributable to the different field configurations. The properties of type II spicules are consistent with published results of rapid blueshifted events (RBEs), supporting the hypothesis that RBEs are their disk counterparts. For type I spicules we find the relations between their properties to be consistent with a magnetoacoustic shock wave driver, and with dynamic fibrils as their disk counterpart. The driver of type II spicules remains unclear from limb observations.
C1 [Pereira, Tiago M. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Pereira, Tiago M. D.; De Pontieu, Bart] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Carlsson, Mats] Inst Theoret Astrophys, NO-0315 Oslo, Norway.
[Carlsson, Mats] Univ Oslo, Ctr Math Applicat, NO-0316 Oslo, Norway.
RP Pereira, TMD (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM tiago.pereira@nasa.gov
RI Pereira, Tiago/G-4079-2014
OI Pereira, Tiago/0000-0003-4747-4329
FU NASA Postdoctoral Program at Ames Research Center [NNH06CC03B]; NASA
[NNX08AH45G, NNX08BA99G, NNX11AN98G]; Research Council of Norway
FX T.M.D.P.'s research was supported by the NASA Postdoctoral Program at
Ames Research Center through Contract Number NNH06CC03B. B.D.P.
gratefully acknowledges support by NASA grants NNX08AH45G, NNX08BA99G,
and NNX11AN98G. This research was supported by the Research Council of
Norway. Hinode is a Japanese mission developed by ISAS/JAXA, with the
NAOJ as domestic partner and NASA and STFC (UK) as international
partners. It is operated in cooperation with ESA and NSC (Norway). The
authors thank Silje Bjolseth and Anne Fox for help with the data
reduction and Alan Title, Rob Rutten, Luc Rouppe van der Voort, Viggo
Hansteen, Scott McIntosh, and Ted Tarbell for interesting discussions.
We thank the referee, whose comments were very helpful and improved the
manuscript.
NR 42
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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 NOV 1
PY 2012
VL 759
IS 1
AR 18
DI 10.1088/0004-637X/759/1/18
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030JL
UT WOS:000310566900018
ER
PT J
AU Richey, CR
Gerakines, PA
AF Richey, C. R.
Gerakines, P. A.
TI NEAR-INFRARED BAND STRENGTHS OF MOLECULES DILUTED IN N-2 AND H2O ICE
MIXTURES RELEVANT TO INTERSTELLAR AND PLANETARY ICES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; infrared: general; infrared: ISM; techniques:
spectroscopic
ID OUTER SOLAR-SYSTEM; LABORATORY SIMULATIONS; PHYSICAL STATE; WATER-ICE;
CARBON-DIOXIDE; SOLID CH4; SURFACE; SPECTROSCOPY; CLOUDS; TRITON
AB The relative abundances of ices in astrophysical environments rely on accurate laboratory measurements of physical parameters, such as band strengths (or absorption intensities), determined for the molecules of interest in relevant mixtures. In an extension of our previous study on pure-ice samples, here we focus on the near-infrared absorption features of molecules in mixtures with the dominant components of interstellar and planetary ices, H2O and N-2. We present experimentally measured near-infrared spectral information (peak positions, widths, and band strengths) for both H2O- and N-2-dominated mixtures of CO (carbon monoxide), CO2 (carbon dioxide), CH4 (methane), and NH3 (ammonia). Band strengths were determined during sample deposition by correlating the growth of near-infrared features (10,000-4000 cm(-1), 1-2.5 mu m) with better-known mid-infrared features (4000-400 cm(-1), 2.5-25 mu m) at longer wavelengths.
C1 [Richey, C. R.; Gerakines, P. A.] Univ Alabama Birmingham, Astro & Solar Syst Phys Program, Dept Phys, Birmingham, AL 35294 USA.
RP Richey, CR (reprint author), NASA, GSFC, Mail Code 665, Greenbelt, MD 20771 USA.
EM christina.r.richey@nasa.gov; gerak@uab.edu
RI Gerakines, Perry/D-2226-2012
OI Gerakines, Perry/0000-0002-9667-5904
FU National Aeronautics and Space Administration [NNG05GG95G]; U.S. Dept.
of Education [P200A090143]; NASA Alabama Space Grant Consortium
[NNG05GE80H]
FX C.R.R. gratefully acknowledges support for this research from the
National Aeronautics and Space Administration under Grant No. NNG05GG95G
issued through the Outer Planets Research Program and the Graduate
Assistance in Areas of National Need (GAANN) Fellowship (U.S. Dept. of
Education Grant No. P200A090143), as well as in earlier years through
the NASA Alabama Space Grant Consortium Fellowship through Grant No.
NNG05GE80H.
NR 46
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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 NOV 1
PY 2012
VL 759
IS 1
AR 74
DI 10.1088/0004-637X/759/1/74
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030JL
UT WOS:000310566900074
ER
PT J
AU Ackermann, M
Ajello, M
Albert, A
Allafort, A
Atwood, WB
Axelsson, M
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Bissaldi, E
Blandford, RD
Bloom, ED
Bogart, JR
Bonamente, E
Borgland, AW
Bottacini, E
Bouvier, A
Brandt, TJ
Bregeon, J
Brigida, M
Bruel, P
Buehler, R
Burnett, TH
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Casandjian, JM
Cavazzuti, E
Cecchi, C
Celik, O
Charles, E
Chaves, RCG
Chekhtman, A
Cheung, CC
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Corbet, R
Cutini, S
D'Ammando, F
Davis, DS
de Angelis, A
DeKlotz, M
de Palma, F
Dermer, CD
Digel, SW
Silva, EDE
Drell, PS
Drlica-Wagner, A
Dubois, R
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Fortin, P
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Giebels, B
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Grove, JE
Guiriec, S
Hadasch, D
Hayashida, M
Hays, E
Horan, D
Hou, X
Hughes, RE
Jackson, MS
Jogler, T
Johannesson, G
Johnson, RP
Johnson, TJ
Johnson, WN
Kamae, T
Katagiri, H
Kataoka, J
Kerr, M
Knodlseder, J
Kuss, M
Lande, J
Larsson, S
Latronico, L
Lavalley, C
Lemoine-Goumard, M
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Mazziotta, MN
McConville, W
McEnery, JE
Mehault, J
Michelson, PF
Mitthumsiri, W
Mizuno, T
Moiseev, AA
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Naumann-Godo, M
Nemmen, R
Nishino, S
Norris, JP
Nuss, E
Ohno, M
Ohsugi, T
Okumura, A
Omodei, N
Orienti, M
Orlando, E
Ormes, JF
Paneque, D
Panetta, JH
Perkins, JS
Pesce-Rollins, M
Pierbattista, M
Piron, F
Pivato, G
Porter, TA
Racusin, JL
Raino, S
Rando, R
Razzano, M
Razzaque, S
Reimer, A
Reimer, O
Reposeur, T
Reyes, LC
Ritz, S
Rochester, LS
Romoli, C
Roth, M
Sadrozinski, HFW
Sanchez, DA
Parkinson, PMS
Sbarra, C
Scargle, JD
Sgro, C
Siegal-Gaskins, J
Siskind, EJ
Spandre, G
Spinelli, P
Stephens, TE
Suson, DJ
Tajima, H
Takahashi, H
Tanaka, T
Thayer, JG
Thayer, JB
Thompson, DJ
Tibaldo, L
Tinivella, M
Tosti, G
Troja, E
Usher, TL
Vandenbroucke, J
Van Klaveren, B
Vasileiou, V
Vianello, G
Vitale, V
Waite, AP
Wallace, E
Winer, BL
Wood, DL
Wood, KS
Wood, M
Yang, Z
Zimmer, S
AF Ackermann, M.
Ajello, M.
Albert, A.
Allafort, A.
Atwood, W. B.
Axelsson, M.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Bissaldi, E.
Blandford, R. D.
Bloom, E. D.
Bogart, J. R.
Bonamente, E.
Borgland, A. W.
Bottacini, E.
Bouvier, A.
Brandt, T. J.
Bregeon, J.
Brigida, M.
Bruel, P.
Buehler, R.
Burnett, T. H.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Casandjian, J. M.
Cavazzuti, E.
Cecchi, C.
Celik, O.
Charles, E.
Chaves, R. C. G.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Corbet, R.
Cutini, S.
D'Ammando, F.
Davis, D. S.
de Angelis, A.
DeKlotz, M.
de Palma, F.
Dermer, C. D.
Digel, S. W.
do Couto e Silva, E.
Drell, P. S.
Drlica-Wagner, A.
Dubois, R.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Fortin, P.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Giebels, B.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Grove, J. E.
Guiriec, S.
Hadasch, D.
Hayashida, M.
Hays, E.
Horan, D.
Hou, X.
Hughes, R. E.
Jackson, M. S.
Jogler, T.
Johannesson, G.
Johnson, R. P.
Johnson, T. J.
Johnson, W. N.
Kamae, T.
Katagiri, H.
Kataoka, J.
Kerr, M.
Knoedlseder, J.
Kuss, M.
Lande, J.
Larsson, S.
Latronico, L.
Lavalley, C.
Lemoine-Goumard, M.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Mazziotta, M. N.
McConville, W.
McEnery, J. E.
Mehault, J.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Moiseev, A. A.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Naumann-Godo, M.
Nemmen, R.
Nishino, S.
Norris, J. P.
Nuss, E.
Ohno, M.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orienti, M.
Orlando, E.
Ormes, J. F.
Paneque, D.
Panetta, J. H.
Perkins, J. S.
Pesce-Rollins, M.
Pierbattista, M.
Piron, F.
Pivato, G.
Porter, T. A.
Racusin, J. L.
Raino, S.
Rando, R.
Razzano, M.
Razzaque, S.
Reimer, A.
Reimer, O.
Reposeur, T.
Reyes, L. C.
Ritz, S.
Rochester, L. S.
Romoli, C.
Roth, M.
Sadrozinski, H. F. -W.
Sanchez, D. A.
Parkinson, P. M. Saz
Sbarra, C.
Scargle, J. D.
Sgro, C.
Siegal-Gaskins, J.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Stephens, T. E.
Suson, D. J.
Tajima, H.
Takahashi, H.
Tanaka, T.
Thayer, J. G.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Tinivella, M.
Tosti, G.
Troja, E.
Usher, T. L.
Vandenbroucke, J.
Van Klaveren, B.
Vasileiou, V.
Vianello, G.
Vitale, V.
Waite, A. P.
Wallace, E.
Winer, B. L.
Wood, D. L.
Wood, K. S.
Wood, M.
Yang, Z.
Zimmer, S.
TI THE FERMI LARGE AREA TELESCOPE ON ORBIT: EVENT CLASSIFICATION,
INSTRUMENT RESPONSE FUNCTIONS, AND CALIBRATION
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE instrumentation: detectors; instrumentation: miscellaneous; methods:
data analysis; methods: observational; telescopes
ID GAMMA-RAY EMISSION; SPACE-TELESCOPE; LAT OBSERVATIONS; SOURCE CATALOG;
VELA PULSAR; MISSION; TESTS; EGRET
AB The Fermi Large Area Telescope (Fermi-LAT, hereafter LAT), the primary instrument on the Fermi Gamma-ray Space Telescope (Fermi) mission, is an imaging, wide field-of-view, high-energy gamma-ray telescope, covering the energy range from 20 MeV to more than 300 GeV. During the first years of the mission, the LAT team has gained considerable insight into the in-flight performance of the instrument. Accordingly, we have updated the analysis used to reduce LAT data for public release as well as the instrument response functions (IRFs), the description of the instrument performance provided for data analysis. In this paper, we describe the effects that motivated these updates. Furthermore, we discuss how we originally derived IRFs from Monte Carlo simulations and later corrected those IRFs for discrepancies observed between flight and simulated data. We also give details of the validations performed using flight data and quantify the residual uncertainties in the IRFs. Finally, we describe techniques the LAT team has developed to propagate those uncertainties into estimates of the systematic errors on common measurements such as fluxes and spectra of astrophysical sources.
C1 [Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.; Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Jogler, T.; Kamae, T.; Kerr, M.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Usher, T. L.; Vandenbroucke, J.; Van Klaveren, B.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Ajello, M.; Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Jogler, T.; Kamae, T.; Kerr, M.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Usher, T. L.; Vandenbroucke, J.; Van Klaveren, B.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Albert, A.; Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Atwood, W. B.; Bouvier, A.; Johnson, R. P.; Razzano, M.; Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Atwood, W. B.; Bouvier, A.; Johnson, R. P.; Razzano, M.; Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Axelsson, M.; Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Axelsson, M.; Conrad, J.; Jackson, M. S.; Larsson, S.; Yang, Z.; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Axelsson, M.; Jackson, M. S.] AlbaNova, Dept Phys, Royal Inst Technol KTH, SE-10691 Stockholm, Sweden.
[Baldini, L.] Univ Pisa, I-56127 Pisa, Italy.
[Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Casandjian, J. M.; Chaves, R. C. G.; Grenier, I. A.; Naumann-Godo, M.; Pierbattista, M.] Univ Paris Diderot, Lab AIM, CNRS, CEA,IRFU,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.; Sbarra, C.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Pivato, G.; Rando, R.; Romoli, C.; Tibaldo, L.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Bissaldi, E.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Bissaldi, E.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Bonamente, E.; Cecchi, C.; D'Ammando, F.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Ciprini, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brandt, T. J.; Celik, O.; Corbet, R.; Davis, D. S.; Ferrara, E. C.; Gehrels, N.; Guiriec, S.; Hays, E.; McConville, W.; McEnery, J. E.; Moiseev, A. A.; Nemmen, R.; Perkins, J. S.; Racusin, J. L.; Stephens, T. E.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Fortin, P.; Giebels, B.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Burnett, T. H.; Roth, M.; Wallace, E.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Caliandro, G. A.; Hadasch, D.] CSIC, Inst Ciencies Espai IEEE, E-08193 Barcelona, Spain.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Frascati, Roma, Italy.
[Celik, O.; Moiseev, A. A.; Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA.
[Celik, O.; Corbet, R.; Davis, D. S.; Perkins, J. S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Celik, O.; Corbet, R.; Davis, D. S.; Perkins, J. S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Chekhtman, A.; Razzaque, S.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Cheung, C. C.; Johnson, T. J.] Natl Acad Sci, Washington, DC 20001 USA.
[Cohen-Tanugi, J.; Lavalley, C.; Mehault, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, F-34095 Montpellier, France.
[Conrad, J.; Larsson, S.; Yang, Z.; Zimmer, S.] Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden.
[D'Ammando, F.] IASF Palermo, I-90146 Palermo, Italy.
[D'Ammando, F.] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy.
[DeKlotz, M.] Stellar Solut Inc, Palo Alto, CA 94306 USA.
[Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Wood, K. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
[Fukazawa, Y.; Nishino, S.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Hou, X.; Lemoine-Goumard, M.; Lott, B.; Reposeur, T.] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, IN2P3, CNRS, F-33175 Gradignan, France.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Katagiri, H.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, F-31028 Toulouse, France.
[Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[McConville, W.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McConville, W.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA.
[Ohno, M.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Okumura, A.; Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Perkins, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93401 USA.
[Sanchez, D. A.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Scargle, J. D.] NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Siegal-Gaskins, J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Stephens, T. E.] Wyle Labs, El Segundo, CA 90245 USA.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Vianello, G.] CIFS, I-10133 Turin, Italy.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Wood, D. L.] Praxis Inc, Alexandria, VA 22303 USA.
RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
EM luca.baldini@pi.infn.it; echarles@slac.stanford.edu; rando@pd.infn.it
RI Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro,
Carmelo/K-3395-2016; Bissaldi, Elisabetta/K-7911-2016; Orlando,
E/R-5594-2016; Reimer, Olaf/A-3117-2013; Racusin, Judith/D-2935-2012;
Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; giglietto,
nicola/I-8951-2012; Tosti, Gino/E-9976-2013; Saz Parkinson, Pablo
Miguel/I-7980-2013; Rando, Riccardo/M-7179-2013; Hays,
Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Nemmen,
Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015; Johannesson,
Gudlaugur/O-8741-2015;
OI Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario
/0000-0001-9325-4672; Bissaldi, Elisabetta/0000-0001-9935-8106; De
Angelis, Alessandro/0000-0002-3288-2517; Caraveo,
Patrizia/0000-0003-2478-8018; Stephens, Thomas/0000-0003-3065-6871;
Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864;
Rando, Riccardo/0000-0001-6992-818X; Zimmer,
Stephan/0000-0002-5735-0082; Bastieri, Denis/0000-0002-6954-8862;
Omodei, Nicola/0000-0002-5448-7577; Reimer, Olaf/0000-0001-6953-1385;
Loparco, Francesco/0000-0002-1173-5673; Gargano,
Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Funk,
Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036;
Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti,
monica/0000-0003-4470-7094; Axelsson, Magnus/0000-0003-4378-8785;
Giroletti, Marcello/0000-0002-8657-8852; Cutini,
Sara/0000-0002-1271-2924; Gasparrini, Dario/0000-0002-5064-9495;
Baldini, Luca/0000-0002-9785-7726
FU K. A. Wallenberg Foundation; European Community [ERC-StG-259391];
Commonwealth Government
FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant
from the K. A. Wallenberg Foundation.; Funded by contract ERC-StG-259391
from the European Community.; The Parkes radio telescope is part of the
Australia Telescope, which is funded by the Commonwealth Government for
operation as a National Facility managed by CSIRO. We thank our
colleagues for their assistance with the radio timing observations.
NR 52
TC 215
Z9 215
U1 5
U2 23
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 NOV
PY 2012
VL 203
IS 1
AR 4
DI 10.1088/0067-0049/203/1/4
PG 70
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034YH
UT WOS:000310908300004
ER
PT J
AU Donato, D
Angelini, L
Padgett, CA
Reichard, T
Gehrels, N
Marshall, FE
Sakamoto, T
AF Donato, D.
Angelini, L.
Padgett, C. A.
Reichard, T.
Gehrels, N.
Marshall, F. E.
Sakamoto, T.
TI THE HEASARC Swift GAMMA-RAY BURST ARCHIVE: THE PIPELINE AND THE CATALOG
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; methods: data analysis; X-rays: bursts
ID ULTRAVIOLET/OPTICAL TELESCOPE; AFTERGLOW; CALIBRATION; MISSION; BAT
AB Since its launch in late 2004, the Swift satellite triggered or observed an average of one gamma-ray burst (GRB) every 3 days, for a total of 771 GRBs by 2012 January. Here, we report the development of a pipeline that semiautomatically performs the data-reduction and data-analysis processes for the three instruments on board Swift (BAT, XRT, UVOT). The pipeline is written in Perl, and it uses only HEAsoft tools and can be used to perform the analysis of a majority of the point-like objects (e.g., GRBs, active galactic nuclei, pulsars) observed by Swift. We run the pipeline on the GRBs, and we present a database containing the screened data, the output products, and the results of our ongoing analysis. Furthermore, we created a catalog summarizing some GRB information, collected either by running the pipeline or from the literature. The Perl script, the database, and the catalog are available for downloading and querying at the HEASARC Web site.
C1 [Donato, D.; Sakamoto, T.] CRESST, Greenbelt, MD 20771 USA.
[Donato, D.; Angelini, L.; Gehrels, N.; Marshall, F. E.; Sakamoto, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Donato, D.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Donato, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Padgett, C. A.] RS Informat Syst Inc, Mclean, VA 22102 USA.
[Reichard, T.] ADNET Syst Inc, Rockville, MD 20852 USA.
[Sakamoto, T.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
RP Donato, D (reprint author), CRESST, Greenbelt, MD 20771 USA.
EM davide.donato-1@nasa.gov
NR 22
TC 4
Z9 4
U1 0
U2 2
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 NOV
PY 2012
VL 203
IS 1
AR 2
DI 10.1088/0067-0049/203/1/2
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034YH
UT WOS:000310908300002
ER
PT J
AU Goldsmith, PF
Langer, WD
Pineda, JL
Velusamy, T
AF Goldsmith, Paul F.
Langer, William D.
Pineda, Jorge L.
Velusamy, T.
TI COLLISIONAL EXCITATION OF THE [C II] FINE STRUCTURE TRANSITION IN
INTERSTELLAR CLOUDS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE atomic processes; photon-dominated region (PDR); submillimeter: ISM
ID 158 MU-M; FAR-INFRARED SPECTROSCOPY; STAR-FORMATION; MOLECULAR CLOUDS;
IONIZED CARBON; GROUND-STATE; HETERODYNE INSTRUMENT; CII EMISSION; LINE
SURVEY; HERSCHEL
AB We analyze the collisional excitation of the 158 mu m (1900.5 GHz) fine structure transition of ionized carbon in terms of line intensities produced by simple cloud models. The single C+ fine structure transition is a very important coolant of the atomic interstellar medium (ISM) and of photon-dominated regions in which carbon is partially or completely in ionized form. The [C II] line is widely used as a tracer of star formation in the Milky Way and other galaxies. Excitation of the [C II] fine structure transition can be via collisions with hydrogen molecules, atoms, and electrons. Analysis of [C II] observations is complicated by the fact that it is difficult to determine the optical depth of the line. We discuss the excitation of the [C II] line, deriving analytic results for several limiting cases and carry out numerical solutions using a large velocity gradient model for a more inclusive analysis. For antenna temperatures up to 1/3 of the brightness temperature of the gas kinetic temperature, the antenna temperature is linearly proportional to the column density of C+ irrespective of the optical depth of the transition. This is appropriately referred to as the effectively optically thin approximation. We review the critical densities for excitation of the [C II] line by various collision partners, briefly analyze C+ absorption, and conclude with a discussion of C+ cooling and how the considerations for line intensities affect the behavior of this important coolant of the ISM.
C1 [Goldsmith, Paul F.; Langer, William D.; Pineda, Jorge L.; Velusamy, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Goldsmith, PF (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Paul.F.Goldsmith@jpl.nasa.gov
RI Goldsmith, Paul/H-3159-2016
FU National Aeronautics and Space Administration
FX This work was largely carried out at the Jet Propulsion Laboratory,
which is operated by the California Institute of Technology under
contract with the National Aeronautics and Space Administration. It was
supported by a Senior Research Scientist leave from JPL in conjunction
with a stay as Professeur Invite at the Ecole Normale Superieure, Paris,
both of which are gratefully acknowledged. We thank Maryvonne Gerin for
allowing us to use PRISMAS data prior to publication and for extensive
discussions about [C II] absorption, and Edith Falgarone for interesting
discussions about the ISM and the role of ionized carbon. We greatly
appreciate a critical reading of the manuscript by David Neufeld that
led to clearing up a significant problem with an earlier version of
Figure 1.
NR 50
TC 38
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U1 1
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD NOV
PY 2012
VL 203
IS 1
AR 13
DI 10.1088/0067-0049/203/1/13
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034YH
UT WOS:000310908300013
ER
PT J
AU Contreras, CS
Sahai, R
AF Sanchez Contreras, C.
Sahai, R.
TI OPACOS: OVRO POST-AGB CO (1-0) EMISSION SURVEY. I. DATA AND DERIVED
NEBULAR PARAMETERS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE circumstellar matter; ISM: jets and outflows; planetary nebulae:
general; stars: AGB and post-AGB; stars: mass-loss
ID ASYMPTOTIC GIANT BRANCH; MASS-LOSS RATES; RICH CIRCUMSTELLAR ENVELOPES;
YOUNG PLANETARY-NEBULAE; MORPHOLOGICAL CLASSIFICATION-SYSTEM; TELESCOPE
SNAPSHOT SURVEY; EXTREME CARBON STARS; POINT-SOURCE CATALOG;
PROTOPLANETARY NEBULA; OH/IR STARS
AB We have performed interferometric observations of the (CO)-C-12 (J = 1-0) emission in a sample of 27 objects spanning different evolutionary stages from the late asymptotic giant branch (late-AGB), through the post-AGB (pAGB) phase, and to the planetary nebula (PN) stage, but dominated by pAGB objects and young PNs (>= 81%). In this paper (the first in a series) we present our maps and main nebular properties derived for the whole sample. Observations were performed with the Caltech Millimeter Array at the Owens Valley Radio Observatory. The angular resolution obtained in our survey ranges between 2 ''.3 and 10 ''.7. The (CO)-C-13 and (CO)-O-18 (J = 1-0) transitions as well as the 2.6 mm continuum emission have also been observed in several objects. The detection statistics in the (CO)-C-12, (CO)-C-13, (CO)-O-18 transitions and 2.6 mm continuum are 89%, 83%, 0%, and 37%, respectively. We report first detections of (CO)-C-12 (J = 1-0) emission in 13 targets and confirm emission from several previous marginal detections. The molecular envelope probed by (CO)-C-12 (J = 1-0) emission is extended for 18 (out of 24) sources; envelope asymmetries and/or velocity gradients are found in most extended objects. Our data have been used to derive accurate target coordinates and systemic velocities and to characterize the envelope size, morphology, and kinematics. We also provide an estimate of the total molecular mass and the fraction of it contained in fast flows, lower limits to the linear momentum and to the isotopic C-12/C-13 ratio, as well as the AGB mass-loss rate and timescale for sources with extended CO emission.
C1 [Sanchez Contreras, C.] INTA CSIC, Ctr Astrobiol, E-28691 Madrid, Spain.
[Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Contreras, CS (reprint author), ESAC, POB 78, E-28691 Madrid, Spain.
RI Sanchez-Contreras, Carmen/N-3718-2015
OI Sanchez-Contreras, Carmen/0000-0002-6341-592X
FU Spanish MICINN [AYA2009-07304]; Spanish MICINN through CONSOLIDER
INGENIO for the team "Molecular Astrophysics: The Herschel and Alma Era
- ASTROMOL" [CSD2009-00038]; Spanish MEC [PIE 200750I028]; National
Science Foundation [AST 08-38260]; NASA [NMO710651/399-20-40-06,
399-20-40-08]; HST/GO awards from the Space Telescope Science Institute
[GO-09463.01, 09801.01, 10185.01, 10851.01]; Association of Universities
for Research in Astronomy, under NASA [NAS5-26555]
FX We thank the anonymous referees for their helpful comments and
suggestions. This work has been partially performed at the Astrophysics
Department of the Astrobiology Center (CAB, CSIC/INTA) and the
California Institute of Technology and has been partially supported by
the Spanish MICINN through grants AYA2009-07304 and CONSOLIDER INGENIO
2010 for the team "Molecular Astrophysics: The Herschel and Alma Era -
ASTROMOL" (ref.: CSD2009-00038), and by the Spanish MEC under project
PIE 200750I028. Ongoing development and operations for OVRO and CARMA
are supported by the National Science Foundation under a cooperative
agreement (grant AST 08-38260). R.S.'s contribution to the research
described here was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contact with NASA. R.S.
thanks NASA for partially funding this work by NASA LTSA and ADP awards
(nos. NMO710651/399-20-40-06 and 399-20-40-08); R.S. also received
partial support for this work from HST/GO awards (nos. GO-09463.01,
09801.01, 10185.01, and 10851.01) from the Space Telescope Science
Institute (operated by the Association of Universities for Research in
Astronomy, under NASA contract NAS5-26555). This research has made use
of the SIMBAD database, operated at CDS, Strasbourg, France, the NASA's
Astrophysics Data System, and Aladin. This research has made use of
observations with AKARI, a JAXA project with the participation of ESA.
NR 166
TC 7
Z9 7
U1 3
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD NOV
PY 2012
VL 203
IS 1
AR 16
DI 10.1088/0067-0049/203/1/16
PG 33
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034YH
UT WOS:000310908300016
ER
PT J
AU Vivian, U
Sanders, DB
Mazzarella, JM
Evans, AS
Howell, JH
Surace, JA
Armus, L
Iwasawa, K
Kim, DC
Casey, CM
Vavilkin, T
Dufault, M
Larson, KL
Barnes, JE
Chan, BHP
Frayer, DT
Haan, S
Inami, H
Ishida, CM
Kartaltepe, JS
Melbourne, JL
Petric, AO
AF Vivian, U.
Sanders, D. B.
Mazzarella, J. M.
Evans, A. S.
Howell, J. H.
Surace, J. A.
Armus, L.
Iwasawa, K.
Kim, D. -C.
Casey, C. M.
Vavilkin, T.
Dufault, M.
Larson, K. L.
Barnes, J. E.
Chan, B. H. P.
Frayer, D. T.
Haan, S.
Inami, H.
Ishida, C. M.
Kartaltepe, J. S.
Melbourne, J. L.
Petric, A. O.
TI SPECTRAL ENERGY DISTRIBUTIONS OF LOCAL LUMINOUS AND ULTRALUMINOUS
INFRARED GALAXIES
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE galaxies: active; galaxies: interactions; galaxies: photometry;
infrared: galaxies
ID ACTIVE GALACTIC NUCLEI; SKY LIRG SURVEY; STAR-FORMATION; STARBURST
GALAXIES; GHZ ATLAS; DUST; SAMPLE; STELLAR; ULTRAVIOLET; RESOLUTION
AB Luminous (LIRGs; log (L-IR/L-circle dot) = 11.00-11.99) and ultraluminous infrared galaxies (ULIRGs; log (L-IR/L-circle dot) = 12.00-12.99) are the most extreme star-forming galaxies in the universe. The local (U)LIRGs provide a unique opportunity to study their multi-wavelength properties in detail for comparison with their more numerous counterparts at high redshifts. We present common large aperture photometry at radio through X-ray wavelengths and spectral energy distributions (SEDs) for a sample of 53 nearby (z < 0.083) LIRGs and 11 ULIRGs spanning log (L-IR/L-circle dot) = 11.14-12.57 from the flux-limited (f(60 mu m) > 5.24 Jy) Great Observatories All-sky LIRG Survey. The SEDs for all objects are similar in that they show a broad, thermal stellar peak (similar to 0.3-2 mu m), and a dominant FIR (similar to 40-200 mu m) thermal dust peak, where vL(v) (60 mu m)/vL(v) (V) increases from similar to 2 to 30 with increasing L-IR. When normalized at IRAS 60 mu m, the largest range in the luminosity ratio, R(lambda) = log[vL(v)(lambda)/vL(v) (60 mu m)], observed over the full sample is seen in the hard X-rays (HX = 2-10 keV), where Delta R-HX = 3.73 ((R) over bar (HX) = -3.10). A small range is found in the radio (1.4 GHz), Delta R-1.4 GHz = 1.75, where the mean ratio is largest, ((R) over bar (1.4 GHz) = -5.81). Total infrared luminosities, L-IR(8-1000 mu m), dust temperatures, and dust masses were computed from fitting thermal dust emission modified blackbodies to the mid-infrared (MIR) through submillimeter SEDs. The new results reflect an overall similar to 0.02 dex lower luminosity than the original IRAS values. Total stellar masses were computed by fitting stellar population synthesis models to the observed near-infrared (NIR) through ultraviolet (UV) SEDs. Mean stellar masses are found to be log(M-*/M-circle dot) = 10.79 +/- 0.40. Star formation rates have been determined from the infrared (SFRIR similar to 45M(circle dot) yr(-1)) and from the monochromatic UV luminosities (SFRUV similar to 1.3M(circle dot) yr(-1)), respectively. Multi-wavelength active galactic nucleus (AGN) indicators have be used to select putative AGNs: About 60% of the ULIRGs would have been classified as an AGN by at least one of the selection criteria.
C1 [Vivian, U.; Sanders, D. B.; Casey, C. M.; Larson, K. L.; Barnes, J. E.; Ishida, C. M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Vivian, U.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mazzarella, J. M.; Howell, J. H.; Chan, B. H. P.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Evans, A. S.; Kim, D. -C.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Evans, A. S.; Kim, D. -C.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Howell, J. H.; Surace, J. A.; Armus, L.; Petric, A. O.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Iwasawa, K.] Univ Barcelona IEEC UB, ICREA, E-08028 Barcelona, Spain.
[Iwasawa, K.] Univ Barcelona IEEC UB, Inst Ciencies Cosmos, E-08028 Barcelona, Spain.
[Vavilkin, T.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Dufault, M.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Frayer, D. T.] Natl Radio Astron Observ, Green Bank, WV 24944 USA.
[Haan, S.] CSIRO Astron & Space Sci, Marsfield, NSW 2122, Australia.
[Inami, H.; Kartaltepe, J. S.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Melbourne, J. L.] CALTECH, Caltech Opt Observ, Div Phys Math & Astron, Pasadena, CA 91125 USA.
RP Vivian, U (reprint author), NASA, Washington, DC 20546 USA.
EM vivian@ifa.hawaii.edu
OI Mazzarella, Joseph/0000-0002-8204-8619; Casey,
Caitlin/0000-0002-0930-6466
FU National Aeronautics and Space Administration; National Science
Foundation; NASA; JPL Contract/IRAC GTO Grant [1256790]; Giovanni Fazio
via the Smithsonian Astrophysical Observatory Predoctoral Fellowship
FX V. U. thanks O. Ilbert and S. Arnouts for their help with using the Le
PHARE code, C. J. Ma for his help with UH 2.2 m data acquisition and
reduction, T.-T. Yuan for her help with various scientific and technical
contributions, and C. W. K. Chiang for statistical consult and technical
help with Figures 1 and 3. V. U. also extends appreciation toward the UH
TAC for their generous support of this project in awarding telescope
time on Mauna Kea, as well as Colin Aspin and the UH 2.2 m Telescope
staff for their help and support in the acquisition of the ground-based
optical photometry. This research has made use of the NASA/IPAC
Extragalactic Database (NED) and IPAC Infrared Science Archive, which
are operated by the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. This publication has also made 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. V. U. wishes to acknowledge funding support from the NASA
Harriet G. Jenkins Predoctoral Fellowship Project and Giovanni Fazio via
the Smithsonian Astrophysical Observatory Predoctoral Fellowship and JPL
Contract/IRAC GTO Grant 1256790. This paper is dedicated to the memory
of Michele Dufault, who led the effort to obtain accurate large
aperature photometric optical and near-infrared data for our complete
sample of objects, and whose early work was critical in our decision to
publish this paper.
NR 52
TC 5
Z9 5
U1 0
U2 2
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 NOV
PY 2012
VL 203
IS 1
AR 9
DI 10.1088/0067-0049/203/1/9
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034YH
UT WOS:000310908300009
ER
PT J
AU Zavodsky, BT
Chou, SH
Jedlovec, GJ
AF Zavodsky, Bradley T.
Chou, Shih-Hung
Jedlovec, Gary J.
TI Improved Regional Analyses and Heavy Precipitation Forecasts With
Assimilation of Atmospheric Infrared Sounder Retrieved Thermodynamic
Profiles
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Atmosphere; hyperspectral sensors; meteorology; remote sensing; weather
forecasting
ID ANALYSIS SYSTEM; AIRS/AMSU/HSB; RADIANCES; MISSION; AIRS; AQUA
AB This paper describes a procedure to assimilate Atmospheric Infrared Sounder (AIRS)-retrieved thermodynamic profiles into a regional configuration of the Weather Research and Forecasting (WRF) model and validates subsequent precipitation forecasts over the eastern half of the continental U. S. Quality indicators were used to select the highest quality temperature and moisture profiles for assimilation throughout the entire atmosphere in clear and partly cloudy regions and above cloud top in cloudy regions. Separate error characteristics for land and water profiles were also used in the assimilation process. Assimilation of AIRS profiles produced analyses with a better validation to in situ observations than the short-term WRF forecast first-guess field. The AIRS-enhanced initial conditions improved simulation of a severe weather event over Texas and Louisiana from February 12-13, 2007. For this event, assimilation of AIRS profiles produced a more unstable boundary-layer air mass in the warm sector ahead of an advancing midlatitude cyclone, resulting in enhanced convective available potential energy in the model. The simulated squall line and precipitation totals from a forecast initialized with AIRS-enhanced initial conditions more closely reflected ground-based observations than one initialized with a no-AIRS control forecast. The impact of the improved initial conditions through the assimilation of AIRS profiles was further demonstrated through an evaluation of a 37-day period from the winter of 2007. The unstable environment over the Gulf of Mexico and coastal region with the AIRS-enhanced initial conditions resulted in 20%+ improvements in the 6-h accumulated precipitation forecasts out to 48 h over that period.
C1 [Zavodsky, Bradley T.; Chou, Shih-Hung; Jedlovec, Gary J.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
RP Zavodsky, BT (reprint author), NASA, Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
EM brad.zavodsky@nasa.gov; shih.h.chou@nasa.gov; gary.jedlovec@nasa.gov
NR 29
TC 5
Z9 6
U1 0
U2 11
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD NOV
PY 2012
VL 50
IS 11
BP 4243
EP 4251
DI 10.1109/TGRS.2012.2194158
PN 1
PG 9
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 034QM
UT WOS:000310888000002
ER
PT J
AU Tilton, JC
Tarabalka, Y
Montesano, PM
Gofman, E
AF Tilton, James C.
Tarabalka, Yuliya
Montesano, Paul M.
Gofman, Emanuel
TI Best Merge Region-Growing Segmentation With Integrated Nonadjacent
Region Object Aggregation
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Image analysis; image classification; image region analysis; image
segmentation; object detection
ID IMAGE SEGMENTATION; CLASSIFICATION; SYSTEM
AB Best merge region growing normally produces segmentations with closed connected region objects. Recognizing that spectrally similar objects often appear in spatially separate locations, we present an approach for tightly integrating best merge region growing with nonadjacent region object aggregation, which we call hierarchical segmentation or HSeg. However, the original implementation of nonadjacent region object aggregation in HSeg required excessive computing time even for moderately sized images because of the required intercomparison of each region with all other regions. This problem was previously addressed by a recursive approximation of HSeg, called RHSeg. In this paper, we introduce a refined implementation of nonadjacent region object aggregation in HSeg that reduces the computational requirements of HSeg without resorting to the recursive approximation. In this refinement, HSeg's region intercomparisons among nonadjacent regions are limited to regions of a dynamically determined minimum size. We show that this refined version of HSeg can process moderately sized images in about the same amount of time as RHSeg incorporating the original HSeg. Nonetheless, RHSeg is still required for processing very large images due to its lower computer memory requirements and amenability to parallel processing. We then note a limitation of RHSeg with the original HSeg for high spatial resolution images and show how incorporating the refined HSeg into RHSeg overcomes this limitation. The quality of the image segmentations produced by the refined HSeg is then compared with other available best merge segmentation approaches. Finally, we comment on the unique nature of the hierarchical segmentations produced by HSeg.
C1 [Tilton, James C.; Tarabalka, Yuliya] NASA, Goddard Space Flight Ctr, Computat & Informat Sci & Technol Off, Greenbelt, MD 20771 USA.
[Montesano, Paul M.] Sigma Space Corp, Lanham, MD 20706 USA.
[Montesano, Paul M.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Gofman, Emanuel] IBM Haifa Res Labs, IL-31905 Haifa, Israel.
RP Tilton, JC (reprint author), NASA, Goddard Space Flight Ctr, Computat & Informat Sci & Technol Off, Greenbelt, MD 20771 USA.
EM James.C.Tilton@nasa.gov; yuliya.tarabalka@inria.fr;
Paul.M.Montesano@nasa.gov; gofman@il.ibm.com
FU U.S. National Aeronautics and Space Administration (NASA); Internal
Research and Development program at NASA's Goddard Space Flight Center;
Marie Curie Research Training Network "Hyper-I-Net"
FX This work was supported in part by the Applied Information Systems
Research program of the U.S. National Aeronautics and Space
Administration (NASA), by the Internal Research and Development program
at NASA's Goddard Space Flight Center, and by the Marie Curie Research
Training Network "Hyper-I-Net."
NR 35
TC 46
Z9 51
U1 1
U2 21
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 NOV
PY 2012
VL 50
IS 11
BP 4454
EP 4467
DI 10.1109/TGRS.2012.2190079
PN 1
PG 14
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 034QM
UT WOS:000310888000019
ER
PT J
AU Misra, S
De Roo, RD
Ruf, CS
AF Misra, Sidharth
De Roo, Roger D.
Ruf, Christopher S.
TI An Improved Radio Frequency Interference Model: Reevaluation of the
Kurtosis Detection Algorithm Performance Under Central-Limit Conditions
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Central limit; microwave radiometry; radio frequency interference (RFI)
ID RADIOFREQUENCY INTERFERENCE; L-BAND; MICROWAVE RADIOMETERS; RFI
DETECTION; MITIGATION; OCEAN; LAND
AB Recent airborne field campaigns making passive microwave measurements have observed some radio frequency interference (RFI) that remained undetected by the kurtosis RFI-detection algorithm. The current pulsed-sinusoidal model for RFI does not explain this anomalous behavior of the detection algorithm. In this paper, a new RFI model is developed that takes into account multiple RFI sources within an antenna footprint. The performance of the kurtosis algorithm with the new model is evaluated. The behavior of the kurtosis detection algorithm under central-limit conditions due to multiple sources is experimentally verified. The new RFI model offers a plausible explanation for the lack of detection by the kurtosis algorithm of the RFI otherwise observed.
C1 [Misra, Sidharth] CALTECH, Jet Prop Lab, Microwave Syst Technol Grp, Pasadena, CA 91109 USA.
[De Roo, Roger D.; Ruf, Christopher S.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Ruf, Christopher S.] Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA.
RP Misra, S (reprint author), CALTECH, Jet Prop Lab, Microwave Syst Technol Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM sidharth.misra@jpl.nasa.gov; deroo@umich.edu; cruf@umich.edu
RI De Roo, Roger/J-2208-2012; Ruf, Christopher/I-9463-2012
OI De Roo, Roger/0000-0001-8391-2950;
FU National Aeronautics and Space Administration (NASA) under the NASA
Earth and Space Science Fellowship [NNX08AU76H]
FX This work was supported in part by the National Aeronautics and Space
Administration (NASA) under the NASA Earth and Space Science Fellowship
(NNX08AU76H).
NR 31
TC 1
Z9 1
U1 0
U2 8
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 NOV
PY 2012
VL 50
IS 11
BP 4565
EP 4574
DI 10.1109/TGRS.2012.2191972
PN 2
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 034QS
UT WOS:000310888600002
ER
PT J
AU Brasunas, JC
AF Brasunas, John C.
TI Laser mode behavior of the Cassini CIRS Fourier transform spectrometer
at Saturn
SO INFRARED PHYSICS & TECHNOLOGY
LA English
DT Article
DE Fourier transform spectrometer; Wavelength calibration; Laser mode;
Mylar
ID INFRARED SPECTROMETER; SYSTEM
AB The CIRS Fourier transform spectrometer aboard the NASA/ESA/ASI Cassini orbiter has been acquiring spectra of the Saturnian system since 2004. The CIRS reference interferometer employs a laser diode to trigger the interferogram sampling. Although the control of laser diode drive current and operating temperature are stringent enough to restrict laser wavelength variation to a small fraction of CIRS finest resolution element, the CIRS instrument does need to be restarted every year or two, at which time it may start in a new laser mode. By monitoring the Mylar absorption features in un-calibrated spectra due to the beam splitter Mylar substrate, it can be shown that these jumps are to adjacent modes and that most of the 8-year operation so far is restricted to three adjacent modes. For a given mode, the wavelength stability appears consistent with the stability of the laser diode drive current and operating temperature. Published by Elsevier B.V.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Brasunas, JC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM john.c.brasunas@nasa.gov
RI brasunas, john/I-2798-2013
FU NASA's Cassini mission; Cassini CIRS calibration team
FX The author acknowledges support from NASA's Cassini mission and from the
Cassini CIRS calibration team.
NR 3
TC 1
Z9 1
U1 2
U2 4
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1350-4495
J9 INFRARED PHYS TECHN
JI Infrared Phys. Technol.
PD NOV
PY 2012
VL 55
IS 6
BP 533
EP 537
DI 10.1016/j.infrared.2012.07.003
PG 5
WC Instruments & Instrumentation; Optics; Physics, Applied
SC Instruments & Instrumentation; Optics; Physics
GA 036JZ
UT WOS:000311023500014
ER
PT J
AU Bringi, VN
Huang, GJ
Munchak, SJ
Kummerow, CD
Marks, DA
Wolff, DB
AF Bringi, V. N.
Huang, Gwo-Jong
Munchak, S. Joseph
Kummerow, Christian D.
Marks, David A.
Wolff, David B.
TI Comparison of Drop Size Distribution Parameter (D-0) and Rain Rate from
S-Band Dual-Polarized Ground Radar, TRMM Precipitation Radar (PR), and
Combined PR TMI: Two Events from Kwajalein Atoll
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID PROFILING ALGORITHM; POLARIMETRIC RADAR; SPACEBORNE RADAR; GAUGE DATA;
VALIDATION; SATELLITE; SPECTRA; DISDROMETER; RETRIEVAL; CLOUDS
AB The estimation of the drop size distribution parameter [median volume diameter (D-0)] and rain rate (R) from the Tropical Rainfall Measuring Mission (TRMM) precipitation radar (PR) as well as from combined PR TRMM Microwave Imager (TMI) algorithms are considered in this study for two TRMM satellite overpasses near the Kwajalein Atoll. An operational dual-polarized S-band radar (KPOL) located in Kwajalein is central as the only TRMM ground validation site for measurement of precipitation over the open ocean. The accuracy of the TRMM PR in retrieving D-0 and R is better for precipitation over the ocean based on a more stable surface reference technique for estimating the path-integrated attenuation. Also, combined PR TMI methods are more accurate over the open ocean because of better knowledge of the surface microwave emissivity. Using Z(h) (horizontal polarized radar reflectivity) and Z(dr) (differential reflectivity) data for the two TRMM overpass events over Kwajalein, Do and R from KPOL arc retrieved. Herein, the main objective is to see if the D-0 retrieved from either PR or the combined PR TMI algorithms are in agreement with KPOL-derived values. Also, the variation of D-0 versus R is compared for convective rain pixels from KPOL, PR, and PR-TMI. It is shown that the PR-TMI optimal estimation scheme does indeed adjust the D-0 in the "correct" direction, on average, from the a priori state if the KPOL data are considered to be the ground truth. This correct adjustment may be considered as evidence of the value added by the TMI brightness temperatures in the combined PR-TMI variational scheme, at least for the two overpass events considered herein.
C1 [Bringi, V. N.; Huang, Gwo-Jong] Colorado State Univ, Dept Elect & Comp Engn, Ft Collins, CO 80523 USA.
[Munchak, S. Joseph] Univ Maryland, NASA, GSFC, Greenbelt & Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Kummerow, Christian D.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Marks, David A.; Wolff, David B.] NASA, GSFC, Greenbelt & Sci Syst Applicat Inc, Lanham, MD USA.
RP Bringi, VN (reprint author), Colorado State Univ, Dept Elect & Comp Engn, Ft Collins, CO 80523 USA.
EM bringi@engr.colostate.edu
FU NASA PMM Science Grant [NNX10AG74G]; NASA Headquarters; NASA
[NNG06HX18C]
FX VNB and GJH were supported by the NASA PMM Science Grant NNX10AG74G.
Development and use of the MK algorithm was supported by NASA
Headquarters through the NASA Earth and Space Science Fellowship Program
under Dr. Ming-Ying Wei and the Global Precipitation Science Program
under Dr. Ramesh Kakar. DBW and DAM were supported by Drs. Arthur Hou
and Matt Schwaller (TRMM Ground Validation) under NASA Grant NNG06HX18C.
The Joss disdrometer data were provided by Dr. Ali Tokay of the
University of Maryland, Baltimore County.
NR 50
TC 3
Z9 3
U1 1
U2 11
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 NOV
PY 2012
VL 29
IS 11
BP 1603
EP 1616
DI 10.1175/JTECH-D-11-00153.1
PG 14
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 036WZ
UT WOS:000311064300002
ER
PT J
AU Wu, XB
Yan, XH
Jo, YH
Liu, WT
AF Wu, Xiangbai
Yan, Xiao-Hai
Jo, Young-Heon
Liu, W. Timothy
TI Estimation of Subsurface Temperature Anomaly in the North Atlantic Using
a Self-Organizing Map Neural Network
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID MIXED-LAYER DEPTH; MULTIDECADAL OSCILLATION; MEDITERRANEAN OUTFLOW;
THERMAL STRUCTURE; ANALYTICAL MODEL; SEA; VARIABILITY; WATER; ARGO
AB A self-organizing map (SOM) neural network was developed from Argo gridded datasets in order to estimate a subsurface temperature anomaly (STA) from remote sensing data. The SOM maps were trained using anomalies of sea surface temperature (SST), height (SSH), and salinity (SSS) data from Argo gridded monthly anomaly datasets, labeled with Argo STA data from 2005 through 2010, which were then used to estimate the STAs at different depths in the North Atlantic from the sea surface data. The estimated STA maps and time series were compared with Argo STAs including independent datasets for validation. In the Gulf Stream path areas, the STA estimations from the SOM algorithm show good agreement with in situ measurements taken from the surface down to 700-m depth, with a correlation coefficient larger than 0.8. Sensitivity of the SUM, when including salinity, shows that with SSS anomaly data in the SOM training process reveal the importance of SSS information, which can improve the estimation of STA in the subtropical ocean by up to 30%. In subpolar basins, the monthly climatology SST and SSH can also help to improve the estimation by as much as 40%. The STA time series for 1993-2004 in the midlatitude North Atlantic were estimated from remote sensing SST and altimetry time series using the SOM algorithm. Limitations for the SUM algorithm and possible error sources in the estimation are briefly discussed.
C1 [Yan, Xiao-Hai] Univ Delaware, Coll Earth Ocean & Environm, Ctr Remote Sensing, Newark, DE 19716 USA.
[Wu, Xiangbai; Yan, Xiao-Hai; Jo, Young-Heon] Univ Delaware, Joint Inst Coastal Res & Management, Newark, DE 19716 USA.
[Wu, Xiangbai; Yan, Xiao-Hai] Xiamen Univ, State Key Lab Marine Environm Sci, Xiamen, Peoples R China.
[Liu, W. Timothy] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Yan, XH (reprint author), Univ Delaware, Coll Earth Ocean & Environm, Ctr Remote Sensing, 209 Robinson Hall, Newark, DE 19716 USA.
EM xiaohai@udel.edu
FU NASA Physical Oceanography Program; NASA EPSCoR Program; NASA Space
Grant; NOAA Sea Grant
FX This research was partially supported by the NASA Physical Oceanography
Program, NASA EPSCoR Program, NASA Space Grant, and NOAA Sea Grant. The
authors thank Weiwei Zhang and Feili Li for the help in data analysis.
We also thank Federico Ienna for editorial assistance with the English
language. Argo gridded data used in this study provided by IPRC,
University of Hawaii. NOAA_OI_SST_V2 data provided by the NOAA/OAR/ESRL
PSD, Boulder, Colorado, from their website at
http://www.esrl.noaa.gov/psd/. The altimeter products (MSLA data) were
produced by Ssalto/Duacs and distributed by AVISO with support from
CNES. We thank two anonymous reviewers whose comments have helped
improve the manuscript.
NR 38
TC 6
Z9 6
U1 0
U2 11
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 NOV
PY 2012
VL 29
IS 11
BP 1675
EP 1688
DI 10.1175/JTECH-D-12-00013.1
PG 14
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 036WZ
UT WOS:000311064300008
ER
PT J
AU Hirata, A
Fujishima, K
Yamagami, R
Kawamura, T
Banfield, JF
Kanai, A
Hori, H
AF Hirata, Akira
Fujishima, Kosuke
Yamagami, Ryota
Kawamura, Takuya
Banfield, Jillian F.
Kanai, Akio
Hori, Hiroyuki
TI X-ray structure of the fourth type of archaeal tRNA splicing
endonuclease: insights into the evolution of a novel three-unit
composition and a unique loop involved in broad substrate specificity
SO NUCLEIC ACIDS RESEARCH
LA English
DT Article
ID NANOARCHAEUM-EQUITANS; ORDER THERMOPROTEALES; INTRON; RECOGNITION;
GENES; MOTIFS; SITE; CONSERVATION; ULTRASMALL; SOFTWARE
AB Cleavage of introns from precursor transfer RNAs (tRNAs) by tRNA splicing endonuclease (EndA) is essential for tRNA maturation in Archaea and Eukarya. In the past, archaeal EndAs were classified into three types (alpha'(2), alpha(4) and alpha(2)beta(2)) according to subunit composition. Recently, we have identified a fourth type of archaeal EndA from an uncultivated archaeon Candidatus Micrarchaeum acidiphilum, referred to as ARMAN-2, which is deeply branched within Euryarchaea. The ARMAN-2 EndA forms an epsilon(2) homodimer and has broad substrate specificity like the alpha(2)beta(2) type EndAs found in Crenarchaea and Nanoarchaea. However, the precise architecture of ARMAN-2 EndA was unknown. Here, we report the crystal structure of the epsilon(2) homodimer of ARMAN-2 EndA. The structure reveals that the epsilon protomer is separated into three novel units (alpha(N), alpha and beta(C)) fused by two distinct linkers, although the overall structure of ARMAN-2 EndA is similar to those of the other three types of archaeal EndAs. Structural comparison and mutational analyses reveal that an ARMAN-2 type-specific loop (ASL) is involved in the broad substrate specificity and that K161 in the ASL functions as the RNA recognition site. These findings suggest that the broad substrate specificities of epsilon(2) and alpha(2)beta(2) EndAs were separately acquired through different evolutionary processes.
C1 [Hirata, Akira; Yamagami, Ryota; Kawamura, Takuya; Hori, Hiroyuki] Ehime Univ, Grad Sch Sci & Engn, Dept Mat Sci & Biotechnol, Matsuyama, Ehime 7908577, Japan.
[Fujishima, Kosuke; Kanai, Akio] Keio Univ, Inst Adv Biosci, Tsuruoka, Yamagata 9970017, Japan.
[Fujishima, Kosuke] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Banfield, Jillian F.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94270 USA.
[Hori, Hiroyuki] Ehime Univ, Venture Business Lab, Matsuyama, Ehime 7908577, Japan.
RP Hori, H (reprint author), Ehime Univ, Grad Sch Sci & Engn, Dept Mat Sci & Biotechnol, 3 Bunkyo Cho, Matsuyama, Ehime 7908577, Japan.
EM hori@eng.ehime-u.ac.jp
OI Kanai, Akio/0000-0002-6362-2419; Fujishima, Kosuke/0000-0002-8844-812X
FU Japan Society for the Promotion of Science; [24770125]; [23350081]
FX Funding for open access charge: The Grant-in-Aid for Young Scientists
(B) [No. 24770125 to A. H.]; Grant-in-Aid for Science Research (B) [No.
23350081 to H. H.]; Japan Society for the Promotion of Science.
NR 42
TC 4
Z9 4
U1 0
U2 6
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0305-1048
J9 NUCLEIC ACIDS RES
JI Nucleic Acids Res.
PD NOV
PY 2012
VL 40
IS 20
BP 10554
EP 10566
DI 10.1093/nar/gks826
PG 13
WC Biochemistry & Molecular Biology
SC Biochemistry & Molecular Biology
GA 035TC
UT WOS:000310970700058
PM 22941657
ER
PT J
AU Thompson, DJ
Digel, SW
Racusin, JL
AF Thompson, David J.
Digel, Seth W.
Racusin, Judith L.
TI Exploring the extreme universe with the Fermi Gamma-Ray Space Telescope
SO PHYSICS TODAY
LA English
DT Article
ID LARGE-AREA TELESCOPE
C1 [Thompson, David J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Digel, Seth W.] SLAC, Menlo Pk, CA USA.
RP Thompson, DJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RI Racusin, Judith/D-2935-2012
NR 9
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 NOV
PY 2012
VL 65
IS 11
BP 39
EP 45
PG 7
WC Physics, Multidisciplinary
SC Physics
GA 037UG
UT WOS:000311131400020
ER
PT J
AU Bykov, A
Gehrels, N
Krawczynski, H
Lemoine, M
Pelletier, G
Pohl, M
AF Bykov, Andrei
Gehrels, Neil
Krawczynski, Henric
Lemoine, Martin
Pelletier, Guy
Pohl, Martin
TI Particle Acceleration in Relativistic Outflows
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Cosmic rays; Particle acceleration; Shocks
ID GAMMA-RAY BURSTS; ENERGY COSMIC-RAYS; ACTIVE GALACTIC NUCLEI;
ULTRARELATIVISTIC SHOCK-WAVES; MAGNETIC-FIELD AMPLIFICATION;
VERY-HIGH-ENERGY; 28 FEBRUARY 1997; X-RAY; FERMI ACCELERATION; PROMPT
EMISSION
AB In this review we confront the current theoretical understanding of particle acceleration at relativistic outflows with recent observational results on various source classes thought to involve such outflows, e.g. gamma-ray bursts, active galactic nuclei, and pulsar wind nebulae. We highlight the possible contributions of these sources to ultra-high-energy cosmic rays.
C1 [Pohl, Martin] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Bykov, Andrei] Ioffe Inst Phys & Technol, St Petersburg 194021, Russia.
[Bykov, Andrei] St Petersburg State Politech Univ, St Petersburg 195251, Russia.
[Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Krawczynski, Henric] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Lemoine, Martin] UPMC, CNRS, Inst Astrophys Paris, F-75014 Paris, France.
[Pelletier, Guy] Inst Planetol & Astrophys Grenoble, F-38041 Grenoble 9, France.
[Pohl, Martin] DESY, D-15738 Zeuthen, Germany.
RP Pohl, M (reprint author), Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
EM byk@astro.ioffe.ru; neil.gehrels@nasa.gov; krawcz@wuphys.wustl.edu;
lemoine@iap.fr; Guy.Pelletier@obs.ujf-grenoble.fr;
marpohl@uni-potsdam.de
RI Bykov, Andrei/E-3131-2014;
OI Lemoine, Martin/0000-0002-2395-7812
FU Russian government [11.G34.31.0001]; RAS; RAS Presidium; RFBR
[11-02-12082]; Helmholtz Alliance for Astroparticle Phyics HAP;
Initiative and Networking Fund of Helmholtz Association; PEPS/PTI
program of CNRS-INP
FX A.M.B. was supported in part by the Russian government grant
11.G34.31.0001 to Sankt-Petersburg State Politechnical University, and
also by the RAS and RAS Presidium Programs and by the RFBR grant
11-02-12082. N.G. acknowledges scientific discussions and assistance by
J. Cannizzo. M. P. is supported by the 'Helmholtz Alliance for
Astroparticle Phyics HAP' funded by the Initiative and Networking Fund
of the Helmholtz Association. M. L. and G. P. acknowledge financial
support of the PEPS/PTI program of the CNRS-INP.
NR 166
TC 20
Z9 20
U1 0
U2 6
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 NOV
PY 2012
VL 173
IS 1-4
BP 309
EP 339
DI 10.1007/s11214-012-9896-y
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 034MR
UT WOS:000310878100010
ER
PT J
AU Simon, M
Bobskill, MR
Wilhite, A
AF Simon, M.
Bobskill, M. R.
Wilhite, A.
TI Historical volume estimation and a structured method for calculating
habitable volume for in-space and surface habitats
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Habitable volume; Volume; Pressurized volume; Numerical method;
Spacecraft design; Interior; Habitat; Requirements; Gravity environment;
Mission duration; Habitability; Utility; Boolean test; Collision
detection; Accessibility
AB Habitable volume is an important spacecraft design figure of merit necessary to determine the required size of crewed space vehicles, or habitats. In order to design habitats for future missions and properly compare the habitable volumes of future habitat designs with historical spacecraft, consistent methods of both defining the required amount of habitable volume and estimating the habitable volume for a given layout are required. This paper provides a brief summary of historical habitable volume requirements and describes the appropriate application of requirements to various types of missions, particularly highlighting the appropriate application for various gravity environments. Then the proposed "Marching Grid Method", a structured automatic, numerical method to calculate habitable volume for a given habitat design, is described in detail. This method uses a set of geometric Boolean tests applied to a discrete set of points within the pressurized volume to numerically estimate the functionally usable and accessible space that comprises the habitable volume. The application of this method to zero gravity and nonzero gravity environments is also discussed. This proposed method is then demonstrated by calculating habitable volumes using two conceptual-level layouts of habitat designs, one for each type of gravity environment. These include the US Laboratory Module on ISS and the Scenario 12.0 Pressurized Core Module from the recent NASA Lunar Surface Systems studies. Results of this study include a description of the effectiveness of this method for various resolutions of the investigated grid, and commentary highlighting the use of this method to determine the overall utility of interior configurations for automatically evaluating interior layouts. Published by Elsevier Ltd.
C1 [Simon, M.; Wilhite, A.] Georgia Inst Technol, Hampton, VA USA.
[Bobskill, M. R.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Simon, M (reprint author), Georgia Inst Technol, Hampton, VA USA.
EM msimon@gatech.edu; wilhite@nianet.org
NR 19
TC 0
Z9 0
U1 0
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD NOV-DEC
PY 2012
VL 80
BP 65
EP 81
DI 10.1016/j.actaastro.2012.04.041
PG 17
WC Engineering, Aerospace
SC Engineering
GA 005EN
UT WOS:000308733400009
ER
PT J
AU Johnson, NL
AF Johnson, Nicholas L.
TI A new look at the GEO and near-GEO regimes: Operations, disposals, and
debris
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Geosynchronous; Operations; Debris; Disposal
AB Since 1963 more than 900 spacecraft and more than 200 launch vehicle upper stages have been inserted into the vicinity of the geosynchronous regime. Equally important, more than 300 spacecraft have been maneuvered into disposal orbits at mission termination to alleviate unnecessary congestion in the finite GEO region. However, the number of GEO satellites continues to grow, and evidence exists of a substantial small debris population. In addition, the operational modes of an increasing number of GEO spacecraft differ from those of their predecessors of several decades ago, including more frequent utilization of inclined and eccentric geosynchronous orbits. Consequently, the nature of the GEO regime and its immediate surroundings is evolving from well-known classical characteristics. This paper takes a fresh look at the GEO satellite population and the near- and far-term environmental implications of the region, including the effects of national and international debris mitigation measures. Published by Elsevier Ltd.
C1 NASA, Orbital Debris Program Off, Houston, TX USA.
RP Johnson, NL (reprint author), NASA, Orbital Debris Program Off, Houston, TX USA.
EM Nicholas.L.Johnson@nasa.gov
NR 9
TC 4
Z9 4
U1 0
U2 1
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 NOV-DEC
PY 2012
VL 80
BP 82
EP 88
DI 10.1016/j.actaastro.2012.05.024
PG 7
WC Engineering, Aerospace
SC Engineering
GA 005EN
UT WOS:000308733400010
ER
PT J
AU Schmidt, GR
Landis, GA
Oleson, SR
AF Schmidt, George R.
Landis, Geoffrey A.
Oleson, Steven R.
TI Human Exploration using Real-Time Robotic Operations (HERRO): A space
exploration strategy for the 21st century
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Space exploration; Human spaceflight; Space science; Planetary
exploration; Telerobotics; Communications latency
AB This paper presents an exploration strategy for human missions beyond Low Earth Orbit (LEO) and the Moon that combines the best features of human and robotic spaceflight. This "Human Exploration using Real-time Robotic Operations" (HERRO) strategy refrains from placing humans on the surfaces of the Moon and Mars in the near-term. Rather, it focuses on sending piloted spacecraft and crews into orbit around Mars and other exploration targets of interest, and conducting astronaut exploration of the surfaces using telerobots and remotely-controlled systems. By eliminating the significant communications delay or "latency" with Earth due to the speed of light limit, teleoperation provides scientists real-time control of rovers and other sophisticated instruments. This in effect gives them a "virtual presence" on planetary surfaces, and thus expands the scientific return at these destinations. HERRO mitigates several of the major issues that have hindered the progress of human spaceflight beyond Low Earth Orbit (LEO) by: (1) broadening the range of destinations for near-term human missions; (2) reducing cost and risk through less complexity and fewer man-rated elements; (3) offering benefits of human-equivalent in-situ cognition, decision-making and fieldwork on planetary bodies; (4) providing a simpler approach to returning samples from Mars and planetary surfaces; and (5) facilitating opportunities for international collaboration through contribution of diverse robotic systems. HERRO provides a firm justification for human spaceflight-one that expands the near-term capabilities of scientific exploration while providing the space transportation infrastructure needed for eventual human landings in the future. Published by Elsevier Ltd.
C1 [Schmidt, George R.; Landis, Geoffrey A.; Oleson, Steven R.] NASA Glenn Res Ctr, Cleveland, OH USA.
RP Schmidt, GR (reprint author), NASA Glenn Res Ctr, Cleveland, OH USA.
EM George.Schmidt@nasa.gov; Geoffrey.Landis@nasa.gov;
Steven.R.Oleson@nasa.gov
NR 25
TC 1
Z9 1
U1 2
U2 17
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 NOV-DEC
PY 2012
VL 80
BP 105
EP 113
DI 10.1016/j.actaastro.2012.05.036
PG 9
WC Engineering, Aerospace
SC Engineering
GA 005EN
UT WOS:000308733400012
ER
PT J
AU Lee, BJ
Liou, MS
AF Lee, Byung Joon
Liou, Meng-Sing
TI Unsteady Adjoint Approach for Design Optimization of Flapping Airfoils
SO AIAA JOURNAL
LA English
DT Article
ID PROPULSIVE EFFICIENCY; PERFORMANCE; FOIL
AB This paper describes the work for optimizing the propulsive efficiency of flapping airfoils (i.e., improving the thrust under constraining aerodynamic work during the flapping flights by changing their shape and trajectory of motion with the unsteady discrete adjoint approach). For unsteady problems, it is essential that the time scales of motion under consideration should be properly resolved and must be compatible with the objective sought after. Both the instantaneous and time-averaged (periodic) formulations are included in this study. For the design optimization with shape parameters or motion parameters, the time-averaged objective function is found to be more useful, while the instantaneous one is more suitable for flow control. The instantaneous objective function is operationally straightforward. On the other hand, the time-averaged objective function requires additional steps in the adjoint approach; the adjoint vectors for the whole time domain must be solved in a reverse time manner. In the current study, applying the periodicity condition allows the unsteady discrete adjoint equations to be reformulated and the resulting system of equations for each sub-time-interval is solved iteratively. The design results from shape and trajectory optimizations are compared, and the physical relevance of design variables to the flapping motion at on- and off-design conditions is investigated.
C1 [Lee, Byung Joon; Liou, Meng-Sing] NASA, John H Glenn Res Ctr, Lewis Field, Aeroprop Div, Cleveland, OH 44135 USA.
RP Lee, BJ (reprint author), NASA, John H Glenn Res Ctr, Lewis Field, Aeroprop Div, Cleveland, OH 44135 USA.
EM mdo.bjlee@gmail.com
FU NASA
FX The authors are grateful for the financial supports provided by NASA's
Subsonic Fixed Wing Project.
NR 25
TC 3
Z9 3
U1 1
U2 9
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 NOV
PY 2012
VL 50
IS 11
BP 2460
EP 2475
DI 10.2514/1.J051663
PG 16
WC Engineering, Aerospace
SC Engineering
GA 030GM
UT WOS:000310559000014
ER
PT J
AU Feldman, Y
Colonius, T
Pauken, MT
Hall, JL
Jones, JA
AF Feldman, Yuri
Colonius, Tim
Pauken, Michael T.
Hall, Jeffrey L.
Jones, Jack A.
TI Simulation and Cryogenic Experiments of Natural Convection for the Titan
Montgolfiere
SO AIAA JOURNAL
LA English
DT Article
ID BALLOONS; SPHERES
AB Natural convection in a spherical geometry is considered for prediction of the buoyancy of single- and double-walled balloons in a cryogenic environment such as Titan's atmosphere. The steady-state flow characteristics obtained by solving the Reynolds-averaged Navier-Stokes equations with a standard turbulence model are used to determine the net buoyancy as a function of heat input. Thermal radiation effects are shown to have a minor impact on the buoyancy, as would he expected at cryogenic conditions. The predicted buoyancy and temperature fields compare favorably with experiments preformed on a 1-m-diameter Montgolfiere prototype in a cryogenic facility. In addition, both numerical and experimental results were compared with correlations for the heat transfer coefficients for free convection internal and external to the balloon as well as in the concentric gap of the double-walled balloons. Finally, scaling issues related to inferring the performance of the full-scale Montgolfiere from the model-scale results are examined.
C1 [Feldman, Yuri; Colonius, Tim] CALTECH, Pasadena, CA 91125 USA.
[Pauken, Michael T.; Hall, Jeffrey L.; Jones, Jack A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Feldman, Y (reprint author), CALTECH, Pasadena, CA 91125 USA.
NR 15
TC 5
Z9 5
U1 2
U2 4
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 NOV
PY 2012
VL 50
IS 11
BP 2483
EP 2491
DI 10.2514/1.J051672
PG 9
WC Engineering, Aerospace
SC Engineering
GA 030GM
UT WOS:000310559000016
ER
PT J
AU Yi, J
Kim, C
Lee, BJ
AF Yi, JunSok
Kim, Chongam
Lee, Byung Joon
TI Adjoint-Based Design Optimization of Vortex Generator in an S-Shaped
Subsonic Inlet
SO AIAA JOURNAL
LA English
DT Article
ID NAVIER-STOKES EQUATIONS; TURBULENCE MODELS; FLOW-CONTROL; DISTORTION
AB This paper deals with an adjoint-based design optimization of vortex generators for the performance improvement of an S-shaped subsonic inlet, the Royal Aircraft Establishment intake model 2129. To enhance the flow quality entering the engine face maximally, the vortex generators are independently optimized with five design parameters per each vortex generator (a total of 55 design variables). To increase the design efficiency, the source term model of the vortex generator is employed. The original source term model, which does not reflect a small change in position and thus has difficulties in differentiation for sensitivity analysis, is modified into a differentiable source term model. To deal with a large number of design variables, the gradient-based design optimization method using the discrete adjoint approach is employed to minimize the distortion coefficient while maintaining the baseline total pressure recovery ratio. A total of five design cases are conducted to validate the proposed design approach, to obtain the optimized vortex generators, and to confirm their enhanced performance. Through the proposed design process, the performance of the target inlet is remarkably improved, showing that the distortion coefficient decreases well over 70% while maintaining the total pressure recovery ratio.
C1 [Kim, Chongam] Seoul Natl Univ, Dept Aerosp Engn, Inst Adv Aerosp Technol, Seoul 151744, South Korea.
[Yi, JunSok] Seoul Natl Univ, Dept Aerosp Engn, Flight Vehicle Res Ctr, Seoul 151744, South Korea.
[Lee, Byung Joon] NASA, John H Glenn Res Ctr, Lewis Field, Cleveland, OH 44135 USA.
RP Kim, C (reprint author), Seoul Natl Univ, Dept Aerosp Engn, Inst Adv Aerosp Technol, Seoul 151744, South Korea.
EM chongam@snu.ac.kr
FU National Research Foundation of Korea; Korean government [2011-0027486];
National Space Lab program through the National Research Foundation of
Korea; Ministry of Education, Science and Technology [2011-0029871];
Ministry of Education, Science, and Technology [2011-0020559]
FX This work was supported by the National Research Foundation of Korea
grant funded by the Korean government (no. 2011-0027486) and National
Space Lab program through the National Research Foundation of Korea,
funded by the Ministry of Education, Science and Technology (no.
2011-0029871). This research was also supported by the Ministry of
Education, Science, and Technology, subject to the Education-Research
Integration Through Simulation on the Net project (no. 2011-0020559).
NR 33
TC 2
Z9 2
U1 2
U2 10
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
J9 AIAA J
JI AIAA J.
PD NOV
PY 2012
VL 50
IS 11
BP 2492
EP 2507
DI 10.2514/1.J051687
PG 16
WC Engineering, Aerospace
SC Engineering
GA 030GM
UT WOS:000310559000017
ER
PT J
AU Schultz, MR
Oremont, L
Guzman, JC
McCarville, D
Rose, CA
Hilburger, MW
AF Schultz, Marc R.
Oremont, Leonard
Guzman, J. Carlos
McCarville, Douglas
Rose, Cheryl A.
Hilburger, Mark W.
TI Compression Response of Fluted-Core Composite Panels
SO AIAA JOURNAL
LA English
DT Article
ID SANDWICH; BEHAVIOR
AB In recent years, fiber-reinforced composites have become more accepted for aerospace applications. For example, during NASA's recent efforts to develop new launch vehicles, composite materials were considered and baselined for a number of structures, including dry barrel sections, which are primarily loaded in longitudinal compression. Because of mass and stiffness requirements, sandwich composites are often selected for these applications. However, there are a number of manufacturing and in-service concerns associated with traditional honeycomb-core sandwich composites that in certain instances may be alleviated through the use of other core materials or construction methods. A fluted core, which consists of integral angled web members with structural radius fillers spaced between laminate facesheets, is one such construction alternative. In this paper, two different fluted-core composite designs were considered: a subscale design and a full-scale design sized for a heavy-lift-launch-vehicle interstage. In particular, the longitudinal compression behavior of fluted-core composites was evaluated with experiments and finite-element analyses. Detailed branched-shell finite-element models were developed, and geometrically nonlinear analyses were conducted to predict both buckling and material failures. Good agreement was obtained between test data and analysis predictions for both failure types. Though the local buckling events are not catastrophic, the resulting deformations contribute to material failures. Consequently, neither the local buckling behavior nor the material failure loads and modes can be predicted by either linear analyses or nonlinear smeared-shell analyses. Compression-after-impact performance of fluted-core composites was also investigated experimentally. Nondestructive inspection of the damage zones indicated that the detectable damage was limited to no more than one flute on either side of any given impact. More study is needed, but this may indicate that an inherent damage-arrest capability of fluted core could provide benefits over traditional sandwich designs in certain weight-critical applications.
C1 [Schultz, Marc R.; Rose, Cheryl A.; Hilburger, Mark W.] NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA.
[Oremont, Leonard] Lockheed Martin Corp, Hampton, VA 23681 USA.
[Guzman, J. Carlos; McCarville, Douglas] Boeing Co, Boeing Res & Technol, Seattle, WA 98124 USA.
RP Schultz, MR (reprint author), NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Mail Stop 190, Hampton, VA 23681 USA.
NR 22
TC 2
Z9 2
U1 1
U2 8
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
J9 AIAA J
JI AIAA J.
PD NOV
PY 2012
VL 50
IS 11
BP 2546
EP 2557
DI 10.2514/1.J051728
PG 12
WC Engineering, Aerospace
SC Engineering
GA 030GM
UT WOS:000310559000021
ER
PT J
AU Bhagwat, MJ
Ramasamy, M
AF Bhagwat, Mahendra J.
Ramasamy, Manikandan
TI Effect of tip vortex aperiodicity on measurement uncertainty
SO EXPERIMENTS IN FLUIDS
LA English
DT Article
ID HELICOPTER ROTOR; FLOW; WAKE; VORTICES
AB Vortex aperiodicity introduces random uncertainty in the measured vortex center location. Unless corrected, this may lead to systematic uncertainty in the vortex properties derived from the measured velocity field. For example, the vortex core size derived from averaged or mean flow field appears larger because of aperiodicity. Several methodologies for aperiodicity correction have been developed over the past two decades to alleviate this systematic uncertainty. However, these do not always reduce the accompanying random uncertainty. The current work shows that the analysis methods used to derive the vortex properties from the measured velocity field play an important role in the resultant random uncertainty in these properties; perhaps, even more important role than the aperiodicity correction methodology itself. It is hypothesized that a class of methods called global methods, which use a large extent of measured data, yield a smaller measurement uncertainty compared to local methods. This hypothesis is verified using a newly proposed global method based on a planar least-squares fit. The general applicability of the method is demonstrated using previous particle image velocimetry measurements of rotor tip vortices. The results clearly demonstrate a reduced random uncertainty in the vortex core properties, even in the presence of secondary vortical structures. Furthermore, the results are independent of the choice of aperiodicity correction methodology.
C1 [Bhagwat, Mahendra J.] USA, Aeroflightdynam Directorate AMRDEC, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ramasamy, Manikandan] NASA, UARC AFDD, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Bhagwat, MJ (reprint author), USA, Aeroflightdynam Directorate AMRDEC, Ames Res Ctr, M-S 215-1, Moffett Field, CA 94035 USA.
EM mahendra.bhagwat@us.army.mil
NR 24
TC 8
Z9 8
U1 1
U2 6
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0723-4864
J9 EXP FLUIDS
JI Exp. Fluids
PD NOV
PY 2012
VL 53
IS 5
BP 1191
EP 1202
DI 10.1007/s00348-012-1348-7
PG 12
WC Engineering, Mechanical; Mechanics
SC Engineering; Mechanics
GA 031MA
UT WOS:000310643600002
ER
PT J
AU Rampe, EB
Kraft, MD
Sharp, TG
Golden, DC
Ming, DW
Christensen, PR
AF Rampe, E. B.
Kraft, M. D.
Sharp, T. G.
Golden, D. C.
Ming, D. W.
Christensen, P. R.
TI Allophane detection on Mars with Thermal Emission Spectrometer data and
implications for regional-scale chemical weathering processes
SO GEOLOGY
LA English
DT Article
ID MARTIAN SURFACE; SYNTHETIC ALLOPHANE; MERIDIANI-PLANUM; ICE DEPOSITS;
MINERALOGY; COMPONENT; SPECTRA; BASALT; TES
AB Models of Thermal Emission Spectrometer (TES) data suggest that poorly-crystalline weathering products allophane and aluminosilicate gel occur in several low-albedo regions of Mars. The presence of allophane in TES models indicates that the martian surface experienced low-temperature chemical weathering at low water-to-rock ratios and mildly acidic to neutral pH on regional scales. The allophane and gel may be ancient and preserved by a persistently dry martian climate. Alternatively, evidence for recent ground ice in these regions suggests that pedogenic processes causing the formation of poorly-crystalline aluminosilicates could be late Amazonian in age and may be active today. While previous models have suggested that global-scale acidic weathering has occurred on Mars for the past 3.5 billion years, the presence of allophane indicates that acidic weathering was not occurring in these low-albedo regions and that mildly acidic to neutral weathering has been an important regional-scale weathering process on the martian surface.
C1 [Rampe, E. B.; Ming, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Rampe, E. B.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
[Kraft, M. D.; Sharp, T. G.; Christensen, P. R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Golden, D. C.] Engn & Sci Contract Grp Hamilton Sundstrand, Houston, TX 77058 USA.
RP Rampe, EB (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
EM elizabeth.b.rampe@nasa.gov
FU NASA [NNX07AP11H]
FX We thank A.D. Rogers for her input and insight. We thank J. Quinn for
quantifying allophane compositions. We gratefully acknowledge the use of
facilities within the LeRoy Eyring Center for Solid State Science at
Arizona State University. This manuscript was improved by helpful
reviews by M. McDowell and two anonymous reviewers. This research was
supported by NASA Graduate Student Researchers Program grant NNX07AP11H.
NR 29
TC 13
Z9 13
U1 0
U2 15
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 NOV
PY 2012
VL 40
IS 11
BP 995
EP 998
DI 10.1130/G33215.1
PG 4
WC Geology
SC Geology
GA 028GO
UT WOS:000310411000009
ER
PT J
AU Hui, FK
Yim, J
Spiotta, AM
Hussain, MS
Toth, G
AF Hui, Ferdinand K.
Yim, John
Spiotta, Alejandro M.
Hussain, M. Shazam
Toth, Gabor
TI Intermediate catheter injections in closed segments during acute stroke
intervention: a cautionary note
SO JOURNAL OF NEUROINTERVENTIONAL SURGERY
LA English
DT Article
ID TRIAL
AB Objective and importance In the setting of stroke intervention, there is typically an occlusion that limits angiographic visualization of patent vasculature distal to the embolus. Certain mechanical thrombectomy paradigms include angiography of the vasculature distal to the point of occlusion in preparation for thrombectomy, typically using a microcatheter. Injections using an intermediate catheter allows for higher volume of injection at a faster rate, resulting in radically different pressure gradients.
Clinical presentations Two patients presenting with acute ischemic stroke were treated via mechanical thrombectomy using the Penumbra 054 system. The first was a tandem occlusion with a high grade narrowing and occlusion of the internal carotid artery (ICA) origin and an ICA terminus thrombus. The second was a long segment, high volume thrombus extending from the cavernous segment to the ICA terminus.
Intervention Conventional access techniques were utilized to position the Penumbra 054 catheter in the ICA in both cases. Intraprocedurally, angiography through the 054 catheter within the closed segment resulted in contrast extravasation adjacent to the tentorium, originating from the communicating segment of the ICA, both of which cleared within 48 h. Due to the extravasation, the interventions were both terminated, and the infarcts went on to complete.
Conclusion During an acute stroke, flow within large vessels is abnormal, and rapid changes in volume may result in drastic changes in pressure which may lead to extravasation. The authors recommend never performing a contrast injection through a large lumen catheter when flow may be impeded proximally and distally. Closed segment injections of large volumes at a high rate are probably at high risk for vessel injury.
C1 [Hui, Ferdinand K.] Cleveland Clin, Cerebrovasc Ctr, Cleveland, OH 44195 USA.
[Yim, John] NASA, Glenn Res Ctr, Cleveland, OH USA.
[Spiotta, Alejandro M.] Cleveland Clin, Neurol Inst, Cleveland, OH 44195 USA.
[Hussain, M. Shazam; Toth, Gabor] CCF, Cerebrovasc Ctr, Cleveland, OH USA.
RP Hui, FK (reprint author), Cleveland Clin, Cerebrovasc Ctr, 9500 Euclid Ave S80 55, Cleveland, OH 44195 USA.
EM huif@ccf.org
NR 6
TC 4
Z9 4
U1 0
U2 0
PU BMJ PUBLISHING GROUP
PI LONDON
PA BRITISH MED ASSOC HOUSE, TAVISTOCK SQUARE, LONDON WC1H 9JR, ENGLAND
SN 1759-8478
J9 J NEUROINTERV SURG
JI J. NeuroInterventional Surg.
PD NOV
PY 2012
VL 4
IS 6
AR e39
DI 10.1136/neurintsurg-2011-010163
PG 5
WC Neuroimaging; Surgery
SC Neurosciences & Neurology; Surgery
GA 029MX
UT WOS:000310501000009
PM 22234947
ER
PT J
AU Thompson, DR
Benner, DC
Brown, LR
Crisp, D
Devi, VM
Jiang, YB
Natraj, V
Oyafuso, F
Sung, K
Wunch, D
Castano, R
Miller, CE
AF Thompson, David R.
Benner, D. Chris
Brown, Linda R.
Crisp, David
Devi, V. Malathy
Jiang, Yibo
Natraj, Vijay
Oyafuso, Fabiano
Sung, Keeyoon
Wunch, Debra
Castano, Rebecca
Miller, Charles E.
TI Atmospheric validation of high accuracy CO2 absorption coefficients for
the OCO-2 mission
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Fourier transform spectroscopy; Infrared CO2 spectroscopy; Atmospheric
CO2 retrievals; Line shapes; Line mixing; Speed dependence
ID COLUMN OBSERVING NETWORK; 20 MU-M; SPEED DEPENDENCE; SPECTROSCOPIC
DATABASE; SATELLITE-OBSERVATIONS; INFRARED-SPECTRA; LINE PARAMETERS;
WING REGIONS; A-BAND; RETRIEVALS
AB We describe atmospheric validation of 1.61 mu m and 2.06 mu m CO2 absorption coefficient databases for use by the Orbiting Carbon Observatory (OCO-2). The OCO-2 mission will collect the measurements needed to estimate column-averaged CO2 similar to dry air mole fraction within 1 ppm accuracy without the region- or airmass-dependent biases that would significantly degrade efforts to understand carbon sources and sinks on a global scale. To accomplish this, the forward radiative transfer model used to generate synthetic atmospheric spectra for retrievals must achieve unprecedented spectroscopic fidelity within the short wave infrared CO2 bands sampled by the sensors. The failure of Voigt line shapes and conventional line mixing formulations for such objectives has motivated significant revisions to line shape models used to generate the gas absorption cross sections for the OCO-2 forward model. In this paper, we test line mixing and speed dependent line shapes combined with improved experimental line parameters. We evaluate pre-computed absorption coefficients in the two spectral regions of CO2 absorbtion using high resolution FT-IR laboratory spectra, atmospheric spectra from the Total Carbon Column Observing Network (TCCON), and medium resolution soundings from the space-based Greenhouse Gases Observing Satellite (GOSAT). (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Thompson, David R.; Brown, Linda R.; Crisp, David; Jiang, Yibo; Natraj, Vijay; Oyafuso, Fabiano; Sung, Keeyoon; Castano, Rebecca; Miller, Charles E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Benner, D. Chris; Devi, V. Malathy] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
[Wunch, Debra] CALTECH, Pasadena, CA 91125 USA.
RP Thompson, DR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM david.r.thompson@jpl.nasa.gov
RI Sung, Keeyoon/I-6533-2015
FU U.S. NASA's Terrestrial Ecology Program [NNX11AG01G]; US Government
FX We thank the OCO-2 ACOS Level 2 algorithm team including Annmarie
Eldering, Vivienne Payne and Michael Gunson. We thank the members of the
OCO-2 science team including Eli Mlawer and Iouli Gordon. We have also
benefited from the counsel of Mitchio Okumura, Joseph Hodges, and David
Long. GOSAT TANSO-FTS spectra were provided to the ACOS Team through a
GOSAT Research Announcement (RA) agreement between the California
Institute of Technology and the three parties, JAXA, NIES and the MOE.
The European Centre for Medium-Range Weather Forecasts (ECMWF) provided
meteorological data for initializing the retrievals. The Total Carbon
Column Observing Network (TCCON) Archive, operated by the California
Institute of Technology, supplied upward-looking measurements. U.S.
funding for the Park Falls TCCON station comes from NASA's Terrestrial
Ecology Program, grant number NNX11AG01G. A portion of the research
described was carried out at the Jet Propulsion Laboratory, California
Institute of Technology and The College of William and Mary under
contracts with the National Aeronautics and Space Administration.
Copyright 2012, California Institute of Technology. All Rights Reserved.
US Government support acknowledged.
NR 54
TC 28
Z9 29
U1 0
U2 36
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 NOV
PY 2012
VL 113
IS 17
BP 2265
EP 2276
DI 10.1016/j.jqsrt.2012.05.021
PG 12
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 031RP
UT WOS:000310660300013
ER
PT J
AU Moncada, AM
Chattopadhyay, A
Bednarcyk, BA
Arnold, SM
AF Moncada, Albert M.
Chattopadhyay, Aditi
Bednarcyk, Brett A.
Arnold, Steven M.
TI Micromechanics-based progressive failure analysis of composite laminates
using different constituent failure theories
SO JOURNAL OF REINFORCED PLASTICS AND COMPOSITES
LA English
DT Article
DE Micromechanics; composite material; failure; Worldwide Failure Exercise
ID PERIODIC MULTIPHASE MATERIALS; HIGHER-ORDER THEORY; GLASSY-POLYMERS;
EPOXY-RESIN; GENERALIZED-METHOD; STRAIN; MODEL; DEFORMATION; STRENGTH;
EXERCISE
AB Predicting failure in a composite can be performed using ply level mechanisms and/or micro level mechanisms. This paper uses the generalized method of cells and high-fidelity generalized method of cells micromechanics theories, coupled with classical lamination theory, to study progressive damage in composites. Different failure theories, implemented at the fiber and matrix constituent level within a laminate, are investigated. A comparison is made among maximum stress, maximum strain, Tsai-Hill, and Tsai-Wu failure theories. To verify the failure theories, the Worldwide Failure Exercise experiments are used. The Worldwide Failure Exercise is a comprehensive study that covers a wide range of polymer matrix composite laminates. The objectives of this paper are to evaluate the current predictive capabilities of the generalized method of cells and high-fidelity generalized method of cells micromechanics theories for the progressive failure prediction of polymer matrix composite laminates and to evaluate the influence of four failure criteria applied at the fiber/matrix constituent scale. The numerical results demonstrate overall agreement with the experimental results for most of the composite layups examined, but also point to the need for more accurate resin damage progression models.
C1 [Moncada, Albert M.; Chattopadhyay, Aditi] Arizona State Univ, Dept Mech & Aerosp Engn, Sch Engn Matter Transport & Energy, Tempe, AZ 85287 USA.
[Bednarcyk, Brett A.; Arnold, Steven M.] NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Moncada, AM (reprint author), Arizona State Univ, Dept Mech & Aerosp Engn, Sch Engn Matter Transport & Energy, Tempe, AZ 85287 USA.
EM amoncada@asu.edu
FU NASA [NNX07AD70A]
FX This work was supported by NASA [grant number NNX07AD70A].
NR 37
TC 5
Z9 6
U1 4
U2 23
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0731-6844
J9 J REINF PLAST COMP
JI J. Reinf. Plast. Compos.
PD NOV
PY 2012
VL 31
IS 21
BP 1467
EP 1487
DI 10.1177/0731684412456330
PG 21
WC Materials Science, Composites; Polymer Science
SC Materials Science; Polymer Science
GA 033OR
UT WOS:000310807900006
ER
PT J
AU Grudinin, IS
Yu, N
AF Grudinin, Ivan S.
Yu, Nan
TI Finite-element modeling of coupled optical microdisk resonators for
displacement sensing
SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA B-OPTICAL PHYSICS
LA English
DT Article
ID WHISPERING-GALLERY MODES; SENSITIVITY; MICROCAVITIES; MICROSPHERES;
LASER
AB We analyze normal mode splitting in a pair of vertically coupled microdisk resonators. A full vectorial finite-element model is used to find the eigenfrequencies of the symmetric and antisymmetric composite modes as a function of coupling distance. We find that the coupled microdisks can compete with the best Fabry-Perot resonators in displacement sensing. We also show how we configured FreeFem++ for the sphere eigenvalue problem. (C) 2012 Optical Society of America
C1 [Grudinin, Ivan S.; Yu, Nan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Grudinin, IS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM grudinin@jpl.nasa.gov
FU National Aeronautics and Space Administration; NASA Center Innovation
Fund; Jet Propulsion Laboratory (JPL) Research and Technology
Development Program
FX This work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration, with partial support from the NASA Center
Innovation Fund and Jet Propulsion Laboratory (JPL) Research and
Technology Development Program. We are grateful to K. J. Vahala, M. L.
Gorodetsky, R. Thompson, F. Hecht, and participants of the FreeFem
mailing list for helpful discussions.
NR 34
TC 9
Z9 9
U1 1
U2 27
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 NOV
PY 2012
VL 29
IS 11
BP 3010
EP 3014
PG 5
WC Optics
SC Optics
GA 032IG
UT WOS:000310708700004
ER
PT J
AU Campana, S
Immler, S
AF Campana, Sergio
Immler, Stefan
TI XMM-Newton and Swift observations of the Type IIb supernova 2011dh in
Messier 51
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE supernovae: individual: SN 2011dh; galaxies: ISM; X-rays: individual: SN
2011dh
ID X-RAY-EMISSION; SUPERGIANT PROGENITOR; H-I; GALAXY; M51; EXPLOSION;
EVOLUTION; COMPACT; 1993J
AB The Type IIb supernova (SN) 2011dh exploded in the nearby galaxy M51 (the Whirlpool galaxy) and provides us with one of the best laboratories to study early high-energy emission from SNe. We give here a comprehensive view of the X-ray properties of SN 2011dh from the analyses of two pointed XMMNewton early observations as well as the full Swift X-ray Telescope (XRT) data set (163 ks). Due to the high XMMNewton throughput, we were able to satisfactorily fit the X-ray spectrum with two hot diffuse gas components including an additional absorption component to our Galaxy. A power-law model provided a worse description of the data. In addition, the early Swift XRT light curve hints of a flux excess at early times (less than or similar to 3 d), consistent with the adiabatic cooling of stellars photosphere a few days after the shock breakout.
C1 [Campana, Sergio] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy.
[Immler, Stefan] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Immler, Stefan] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Campana, S (reprint author), INAF Osservatorio Astron Brera, Via Bianchi 46, I-23807 Merate, LC, Italy.
EM sergio.campana@brera.inaf.it
OI Campana, Sergio/0000-0001-6278-1576
FU ASI [I/004/11/0]; PRIN-MIUR grant [2009ERC3HT]
FX SC thanks Norbert Schartel for granting DDT XMM-Newton observations and
Neil Gehrels and the Swift science operations team for approving and
scheduling the Swift observational campaign. We thank the referee for
comments that helped improve the manuscript. This work made use of data
supplied by the UK Swift Science Data Centre at the University of
Leicester. This work has been partially supported by the ASI grant
I/004/11/0 and by the PRIN-MIUR grant 2009ERC3HT.
NR 30
TC 5
Z9 5
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 NOV
PY 2012
VL 427
IS 1
BP L70
EP L74
DI 10.1111/j.1745-3933.2012.01347.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 033MH
UT WOS:000310800300015
ER
PT J
AU Mercury, M
Green, R
Hook, S
Oaida, B
Wu, W
Gunderson, A
Chodas, M
AF Mercury, M.
Green, R.
Hook, S.
Oaida, B.
Wu, W.
Gunderson, A.
Chodas, M.
TI Global cloud cover for assessment of optical satellite observation
opportunities: A HyspIRI case study
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Global clouds; Remote sensing; Viewing opportunities; HyspIRI;
Cloudiness
ID MODIS; MASK
AB The number of cloud-free views by Earth-orbiting optical remote sensing instruments must be characterized to verify that the coverage is sufficient to address a mission's science objectives. This study determines the expected cloud-free coverage for the Hyperspectral Infra-red Imager (HyspIRI) mission concept using the Terra MODIS 5 km daytime cloud mask dataset covering the period 2001-2010. The HyspIRI mission concept has two instruments: a Visible Shortwave Infrared (VSWIR) imaging spectrometer and a Thermal Infrared (TIR) multispectral imager. The VSWIR and TIR instruments have equatorial revisit times of 19 and 5 days, respectively.
Using the MODIS cloud mask data, we determined the percentage of the Earth's land and shallow water regions that would have been viewable with cloud-free acquisitions for each quarter and year in 2001 through 2010. For the VSWIR, the average cloud-free coverage was 83.0% quarterly and 99.6% annually. Average TIR monthly coverage was also evaluated to be 90.7%. The standard deviations for these statistics were all less than 1.2%, and the average coverages exceed HyspIRI's quarterly and annual requirements (listed in Table 6) by over twenty standard deviations. By the central limit theorem, it follows that in a typical year, HyspIRI will meet its coverage requirements (listed in Table 6) with extremely low uncertainty, acquiring a sufficient number of scenes to enable both monthly and quarterly assessments of the vast majority of the Earth's land and shallow water.
This paper includes: yearly global statistics for cloud-free MODIS observations at 5 km resolution between 2001 and 2010; a one year global map representing percent cloud-free observations between 2001 and 2010; global maps representing percent cloud-free observations between 2001 and 2010 for each quarter; maps of the predicted number of views by each HyspIRI instrument quarterly and over the course of a year; and predicted global coverage quarterly and for one year for each HyspIRI instrument, with additional monthly statistics for TIR. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Mercury, M.; Green, R.; Hook, S.; Oaida, B.; Wu, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gunderson, A.] Montana State Univ, Bozeman, MT 59718 USA.
[Chodas, M.] MIT, Cambridge, MA 02139 USA.
RP Mercury, M (reprint author), 4800 Oak Grove Dr,Mail Stop 301-165, Pasadena, CA 91109 USA.
EM michael.b.mercuty@jpl.nasa.gov
FU NASA through the HyspIRI project
FX The authors gratefully acknowledge the insightful contributions of David
H. Atkinson and the anonymous peer reviewers. Figure 4's analyses and
visualizations were produced with the Giovanni online data system,
developed and maintained by the NASA GES DISC. This work was supported
by NASA through the HyspIRI project under contract to JPL/Caltech.
NR 22
TC 10
Z9 10
U1 0
U2 26
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 NOV
PY 2012
VL 126
BP 62
EP 71
DI 10.1016/j.rse.2012.08.007
PG 10
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 027XY
UT WOS:000310388600006
ER
PT J
AU Brown, ME
de Beurs, KM
Marshall, M
AF Brown, M. E.
de Beurs, K. M.
Marshall, M.
TI Global phenological response to climate change in crop areas using
satellite remote sensing of vegetation, humidity and temperature over 26
years
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Phenology; NDVI; Agriculture; Cereal crops; Temperature; Humidity
ID NET PRIMARY PRODUCTION; LAND-SURFACE PHENOLOGY; FOOD SECURITY;
SPOT-VEGETATION; AVHRR; NDVI; VARIABILITY; RAINFALL; SEASON; CHINA
AB The recent increase in food prices has revealed that climate, combined with an expanding population and a widespread change in diet, may result in an end to an era of predictable abundance of global cereal crops. The objective of this paper is to estimate changes of agriculturally-relevant growing season parameters, including the start of the season, length of the growing period and the position of the height or peak of the season, in the primary regions with rainfed agriculture during the past 26 years. Our analysis found that globally, 27% of cereal crop areas have experienced changes in the length of the growing season since 1981, the majority of which had seasons that were at least 2.3 days per year longer on average. We also found both negative and positive trends in the start of season globally, with different effects of changing temperature and humidity being isolated depending on the country and region. We investigated the correlation between the peak timing of the growing season and agricultural production statistics for rain fed agriculture. We found that two thirds of the countries investigated had at least 25% of pixels with crop production that behaved differently than expected from the null hypothesis of no correlation. The results show that variations in the peak of the growing season have a strong effect on global food production in these countries. We show that northern hemisphere countries and states appear to have improved model fit when using phenological models based on humidity while southern hemisphere countries and states have improved model fit by phenological models based on accumulated growing degree days, showing the impact of climate variability during the past two and a half decades. Published by Elsevier Inc.
C1 [Brown, M. E.] NASA, Biospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20171 USA.
[de Beurs, K. M.] Univ Oklahoma, Dept Geog & Environm Sustainabil, Norman, OK 73019 USA.
[Marshall, M.] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
RP Brown, ME (reprint author), NASA, Biospher Sci Branch, Goddard Space Flight Ctr, Code 614-4, Greenbelt, MD 20171 USA.
EM molly.brown@nasa.gov
RI Brown, Molly/M-5146-2013; Brown, Molly/E-2724-2010
OI Brown, Molly/0000-0001-7384-3314; Brown, Molly/0000-0001-7384-3314
NR 46
TC 35
Z9 40
U1 12
U2 119
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 NOV
PY 2012
VL 126
BP 174
EP 183
DI 10.1016/j.rse.2012.08.009
PG 10
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 027XY
UT WOS:000310388600015
ER
PT J
AU Fleck, B
Heber, B
Vourlidas, A
van Driel-Gesztelyi, L
Mandrini, CH
Leibacher, J
AF Fleck, Bernhard
Heber, Bernd
Vourlidas, Angelos
van Driel-Gesztelyi, Lidia
Mandrini, Cristina H.
Leibacher, John
TI The Sun 360 Preface
SO SOLAR PHYSICS
LA English
DT Editorial Material
C1 [Fleck, Bernhard] NASA, Goddard Space Flight Ctr, ESA Sci Operat Dept, Greenbelt, MD 20771 USA.
[Heber, Bernd] Univ Kiel, Inst Expt & Angew Phys, Kiel, Germany.
[Vourlidas, Angelos] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[van Driel-Gesztelyi, Lidia] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[van Driel-Gesztelyi, Lidia] Univ Paris Diderot, Univ Paris 06, Observ Paris, CNRS,LESIA, Meudon, France.
[van Driel-Gesztelyi, Lidia] Hungarian Acad Sci, Konkoly Observ, Budapest, Hungary.
[Mandrini, Cristina H.] Int Space Sci Inst, Bern, Switzerland.
[Mandrini, Cristina H.] Univ Buenos Aires, CONICET, Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina.
[Mandrini, Cristina H.] Univ Buenos Aires, Fac Ciencias Exactas & Nat, Buenos Aires, DF, Argentina.
[Leibacher, John] Natl Opt Astron Observ, Natl Solar Observ, Tucson, AZ 85726 USA.
[Leibacher, John] Inst Astrophys Spatiale, Orsay, France.
RP Fleck, B (reprint author), NASA, Goddard Space Flight Ctr, ESA Sci Operat Dept, Greenbelt, MD 20771 USA.
EM bfleck@esa.nascom.nasa.gov
RI Vourlidas, Angelos/C-8231-2009
OI Vourlidas, Angelos/0000-0002-8164-5948
NR 0
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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 NOV
PY 2012
VL 281
IS 1
BP 1
EP 2
DI 10.1007/s11207-012-0120-8
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 033QB
UT WOS:000310811900001
ER
PT J
AU Liewer, PC
Hernandez, IG
Hall, JR
Thompson, WT
Misrak, A
AF Liewer, P. C.
Hernandez, I. Gonzalez
Hall, J. R.
Thompson, W. T.
Misrak, A.
TI Comparison of Far-Side STEREO Observations of Solar Activity and Active
Region Predictions from GONG
SO SOLAR PHYSICS
LA English
DT Article
DE Corona; Active regions; Helioseismology; Space weather
ID SUNSPOT; SUN
AB On 6 February 2011, the two Solar TErrestrial Relations Observatory (STEREO) spacecraft reached 180A degrees separation and began imaging the entire far-side hemisphere of the Sun in extreme ultraviolet light (EUV). Here, we compare STEREO's observations of far-side solar activity, as evidenced by bright regions in the EUV images, to predictions of far-side active regions from helioseismology using National Solar Observatory Global Oscilla-tion Network Group (GONG) observations. GONG produces seismic Carrington maps of strong magnetic field regions, labeling far-side regions with a probability >= 70%. By visual comparison of these GONG maps with STEREO EUV Carrington maps, we determine whether or not solar activity is observed at the locations of the predicted active regions. For data from February -June 2011, we find that for 139 of 157 comparisons activity is observed in EUV at the predicted site, yielding an 89% success rate. For 18 comparisons, no activity was seen at the predicted region (11% false predictions). We also investigated GONG's success at predicting large active regions before they appear at the east limb as viewed from Earth. Of 15 such east-limb active regions, eight were predicted by GONG at least once in the seven days preceding their Earth-side appearance. STEREO B observations of activity in the days preceding the appearance of the other seven large East-limb active regions indicated that, while three were possibly too small for GONG to make a prediction, four seemed as large and active as other active regions that had been predicted successfully by GONG.
C1 [Liewer, P. C.; Hall, J. R.; Misrak, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hernandez, I. Gonzalez] Natl Solar Observ, Tucson, AZ 85719 USA.
[Thompson, W. T.] Adnet Syst Inc, Lanham, MD 20706 USA.
RP Liewer, PC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Paulett.Liewer@jpl.nasa.gov
FU NASA [NNG06EB68C]; Star Targeted Research and Technology program
FX We would like to thank F. Hill, P. Scherrer and A. Kosovichev for
informative discussions on the use of helioseismology to make far-side
active region predictions. We also thank Eric De Jong, Marco Velli and
Angelos Vourlidas for useful discussions of this research. The work of
P. C. L., J.R.H. and A. M. was conducted at the Jet Propulsion
Laboratory, California Institute of Technology under a contract from
NASA. The work of I. G. H. was supported by the NASA Living with a Star
Targeted Research and Technology program. The work of W. T. T. was
supported by NASA grant NNG06EB68C. The STEREO/SECCHI data used here are
produced by an international consortium of the Naval Research Laboratory
(USA), Lockheed Martin Solar and Astrophysics Lab (USA), NASA Goddard
Space Flight Center (USA) Rutherford Appleton Laboratory (UK),
University of Birmingham (UK), Max-Planck-Institut fur
Sonnensystemforschung (Germany), Centre Spatiale de Liege (Belgium),
Institut d'Optique Theorique et Applique (France), Institut
d'Astrophysique Spatiale (France). This work utilizes data obtained by
the Global Oscillation Network Group (GONG) Program. GONG is managed by
the National Solar Observatory, which is operated by AURA, Inc. under a
cooperative agreement with the NSF. The GONG data were acquired by
instruments operated by the Big Bear Solar Observatory, High Altitude
Observatory, Learmonth Solar Observatory, Udaipur Solar Observatory,
Instituto de Astrofisica de Canarias, and Cerro Tololo Interamerican
Observatory.
NR 15
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PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD NOV
PY 2012
VL 281
IS 1
BP 3
EP 20
DI 10.1007/s11207-012-9932-9
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 033QB
UT WOS:000310811900002
ER
PT J
AU Watanabe, T
Hara, H
Sterling, AC
Harra, LK
AF Watanabe, T.
Hara, H.
Sterling, A. C.
Harra, L. K.
TI Production of High-Temperature Plasmas During the Early Phases of a C9.7
Flare. II. Bi-directional Flows Suggestive of Reconnection in a
Pre-flare Brightening Region
SO SOLAR PHYSICS
LA English
DT Article
DE Flares, dynamics; Flares, spectrum; Heating, in flares
ID ULTRAVIOLET IMAGING SPECTROMETER; LOOP RADIATIVE HYDRODYNAMICS;
SOLAR-FLARES; CHROMOSPHERIC EVAPORATION; MAGNETIC RECONNECTION; FILAMENT
ERUPTION; HINODE; EMISSION; ONSET; DYNAMICS
AB The 6 June 2007 16:55 UT flare was well observed with high time-cadence sparse raster scans by the EUV Imaging Spectrometer (EIS) on board the Hinode spacecraft. The observation covers an active region area of 240 arcsec x 240 arcsec with the 1 arcsec slit in about 160 seconds.
We describe here spectral properties of a "pre-flare brightening" to this flare, which started about nine minutes prior to flare-ribbon onset. This flare brightening looks like two small loops apparently having a cusp-shape structure about 40 -aEuro parts per thousand 50 arcsec west of the main flaring loops, which show dynamic behavior in velocity during the early phases of the flare: The He ii line at 256.32 shows the existence of a bi-directional flow along the Sun-Earth line of sight of about -70 and +100 km s(-1). On the other hand, the Fe xvi line at 262.98 formed at higher coronal temperatures shows only a slight increase in intensity at the location of these loops, and the Fe xxiii line at 263.76 barely appears. Electron density at the site derived from the intensity ratios of the Fe xiv line pair at 264.78 and 274.20 is lower than the average of 10(9.3) cm(-3) in other parts of the active-region outskirts. Combining a time series of STEREO-A/B SECCHI-EUVI 171 images, we conclude that the pre-flare-brightening region may be heated via magnetic reconnection taking place as a result of loop-loop interaction.
C1 [Watanabe, T.; Hara, H.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Watanabe, T.; Hara, H.] Grad Sch Adv Studies, Hayama, Kanagawa 2400193, Japan.
[Sterling, A. C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Sterling, A. C.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Harra, L. K.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
RP Watanabe, T (reprint author), Natl Inst Nat Sci, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
EM watanabe@uvlab.mtk.nao.ac.jp; hara@solar.mtk.nao.ac.jp;
alphonse.sterling@nasa.gov; lkh@mssl.ucl.ac.uk
OI Harra, Louise/0000-0001-9457-6200
FU MEXT, Japan; Sun Microsystems; NAOJ/NINS; NINS inter-institute
collaborative program for Creation of New Research Area; NIFS/NINS under
the project of Formation of International Network for Scientific
Collaborations; NASA's Office of Space Science
FX Hinode is a Japanese mission developed and launched by ISAS/JAXA,
collaborating with NAOJ as domestic partner, NASA and STFC (UK) as
international partners. Scientific operation of the Hinode mission is
conducted by the Hinode science team organized at ISAS/JAXA. This team
mainly consists of scientists from institutes in the partner countries.
Support for the post-launch operation is provided by JAXA and NAOJ
(Japan), STFC (UK), NASA (USA), ESA, and NSC (Norway). This work is
partly carried out at the NAOJ Hinode Science Center, which was
supported by the Grant-in-Aid for Creative Scientific Research: "The
Basic Study of Space Weather Prediction" from MEXT, Japan (Head
Investigator: K. Shibata), generous donations from Sun Microsystems, and
NAOJ/NINS internal funding. It was also supported by NINS
inter-institute collaborative program for Creation of New Research Area
(Head Investigator: T. Watanabe), and by NIFS/NINS under the project of
Formation of International Network for Scientific Collaborations (Head
Investigator: H. Yamada). ACS was supported by funding from NASA's
Office of Space Science through the Living with a Star and the
Supporting Research and Technology programs.
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD NOV
PY 2012
VL 281
IS 1
BP 87
EP 99
DI 10.1007/s11207-012-0079-5
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 033QB
UT WOS:000310811900007
ER
PT J
AU Kliem, B
Torok, T
Thompson, WT
AF Kliem, B.
Toeroek, T.
Thompson, W. T.
TI A Parametric Study of Erupting Flux Rope Rotation Modeling the
"Cartwheel CME" on 9 April 2008
SO SOLAR PHYSICS
LA English
DT Article
DE Corona, active; Prominences, dynamics; Coronal mass ejections,
initiation and propagation; Magnetic fields, corona;
Magnetohydrodynamics
ID CORONAL MASS EJECTIONS; SOLAR ACTIVE REGIONS; KINK INSTABILITY; MAGNETIC
CLOUDS; PROMINENCES; FIELD; FILAMENT; SIGMOIDS; STEREO; LINE
AB The rotation of erupting filaments in the solar corona is addressed through a parametric simulation study of unstable, rotating flux ropes in bipolar force-free initial equilibrium. The Lorentz force due to the external shear-field component and the relaxation of tension in the twisted field are the major contributors to the rotation in this model, while reconnection with the ambient field is of minor importance, due to the field's simple structure. In the low-beta corona, the rotation is not guided by the changing orientation of the vertical field component's polarity inversion line with height. The model yields strong initial rotations which saturate in the corona and differ qualitatively from the profile of rotation vs. height obtained in a recent simulation of an eruption without preexisting flux rope. Both major mechanisms writhe the flux rope axis, converting part of the initial twist helicity, and produce rotation profiles which, to a large part, are very similar within a range of shear-twist combinations. A difference lies in the tendency of twist-driven rotation to saturate at lower heights than shear-driven rotation. For parameters characteristic of the source regions of erupting filaments and coronal mass ejections, the shear field is found to be the dominant origin of rotations in the corona and to be required if the rotation reaches angles of order 90 degrees and higher; it dominates even if the twist exceeds the threshold of the helical kink instability. The contributions by shear and twist to the total rotation can be disentangled in the analysis of observations if the rotation and rise profiles are simultaneously compared with model calculations. The resulting twist estimate allows one to judge whether the helical kink instability occurred. This is demonstrated for the erupting prominence in the "Cartwheel CME" on 9 April 2008, which has shown a rotation of a parts per thousand aEuro parts per thousand 115(a similar to) up to a height of 1.5 R (aS (TM)) above the photosphere. Out of a range of initial equilibria which include strongly kink-unstable (twist I broken vertical bar=5 pi), weakly kink-unstable (I broken vertical bar=3.5 pi), and kink-stable (I broken vertical bar=2.5 pi) configurations, only the evolution of the weakly kink-unstable flux rope matches the observations in their entirety.
C1 [Kliem, B.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Kliem, B.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Kliem, B.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Toeroek, T.] Univ Paris Diderot, UPMC, Observ Paris, CNRS,LESIA, F-92195 Meudon, France.
[Thompson, W. T.] NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Greenbelt, MD 20771 USA.
RP Kliem, B (reprint author), Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany.
EM bkliem@uni-potsdam.de
FU DFG; STFC; NASA [NNX08AG44G, NNG06EB68C]; European Commission through
the SOTERIA Network (EU) [218816]; NASA HTP program; NASA LWS program
FX We acknowledge the careful reading of the manuscript and the
constructive comments by the referee. BK acknowledges support by the
DFG, the STFC, and by NASA through Grant NNX08AG44G. TT's work was
partially supported by the European Commission through the SOTERIA
Network (EU FP7 Space Science Project No. 218816) and by the NASA HTP
and LWS programs. WTT's work was supported by NASA Grant NNG06EB68C.
NR 56
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U2 3
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PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD NOV
PY 2012
VL 281
IS 1
BP 137
EP 166
DI 10.1007/s11207-012-9990-z
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 033QB
UT WOS:000310811900010
ER
PT J
AU Leske, RA
Cohen, CMS
Mewaldt, RA
Christian, ER
Cummings, AC
Labrador, AW
Stone, EC
Wiedenbeck, ME
von Rosenvinge, TT
AF Leske, R. A.
Cohen, C. M. S.
Mewaldt, R. A.
Christian, E. R.
Cummings, A. C.
Labrador, A. W.
Stone, E. C.
Wiedenbeck, M. E.
von Rosenvinge, T. T.
TI Large Proton Anisotropies in the 18 August 2010 Solar Particle Event
SO SOLAR PHYSICS
LA English
DT Article
DE Cosmic rays, solar; Energetic particles, propagation; Magnetic fields,
interplanetary
ID CORONAL MASS EJECTIONS; ENERGETIC PARTICLES; ELECTRON EVENTS; STEREO
MISSION; MAGNETIC CLOUD; TELESCOPE; ONSET; TOPOLOGY; PLASMA; WAVES
AB The solar particle event observed at STEREO Ahead on 18 August 2010 displayed a rich variety of behavior in the particle anisotropies. Sectored rates measured by the Low Energy Telescope (LET) on STEREO showed very large bidirectional anisotropies in 4-6 MeV protons for the first 17 hours of the event while inside a magnetic cloud, with intensities along the field direction several hundred to nearly 1000 times greater than those perpendicular to the field. At the trailing end of the cloud, the protons became isotropic and their spectrum hardened slightly, while the He/H abundance ratio plunged by a factor of approximately four for about four hours. Associated with the arrival of a shock on 20 August was a series of brief (< 10 minute duration) intensity increases (commonly called "shock spikes") with relatively narrow angular distributions (45(a) FWHM), followed by an abrupt decrease in particle intensities at the shock itself and a reversal of the proton flow to a direction toward the Sun and away from the receding shock. We discuss the STEREO/LET observations of this interesting event in the context of other observations reported in the literature.
C1 [Leske, R. A.; Cohen, C. M. S.; Mewaldt, R. A.; Cummings, A. C.; Labrador, A. W.; Stone, E. C.] CALTECH, Pasadena, CA 91125 USA.
[Christian, E. R.; von Rosenvinge, T. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wiedenbeck, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Leske, RA (reprint author), CALTECH, Mail Code 290-17, Pasadena, CA 91125 USA.
EM ral@srl.caltech.edu
RI Christian, Eric/D-4974-2012
OI Christian, Eric/0000-0003-2134-3937
FU National Aeronautics and Space Administration (NASA) at Caltech; JPL
from the University of California at Berkeley under NASA [SA2715-26309,
NAS5-03131]; NASA [NNX08AK87G, NAS5-00132]
FX This work was supported by the National Aeronautics and Space
Administration (NASA) at Caltech and JPL under subcontract SA2715-26309
from the University of California at Berkeley under NASA contract
NAS5-03131, and by NASA award NNX08AK87G. We thank the PLASTIC (NASA
contract NAS5-00132), MAG, and SWEA investigators on STEREO for making
their data publicly available. This work benefited greatly from
discussions at "The Sun-360 Workshop" held at the
Christian-Albrechts-Universitat in Kiel, Germany in July 2011. We thank
B. Dotson for help in analyzing the data and in preparing the figures.
NR 37
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD NOV
PY 2012
VL 281
IS 1
BP 301
EP 318
DI 10.1007/s11207-012-0018-5
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 033QB
UT WOS:000310811900017
ER
PT J
AU Wood, BE
Rouillard, AP
Mostl, C
Battams, K
Savani, NP
Marubashi, K
Howard, RA
Socker, DG
AF Wood, B. E.
Rouillard, A. P.
Moestl, C.
Battams, K.
Savani, N. P.
Marubashi, K.
Howard, R. A.
Socker, D. G.
TI Connecting Coronal Mass Ejections and Magnetic Clouds: A Case Study
Using an Event from 22 June 2009
SO SOLAR PHYSICS
LA English
DT Article
DE Coronal mass ejections, initiation and propagation; Coronal mass
ejections, interplanetary
ID SOLAR-WIND; INNER HELIOSPHERE; WHITE-LIGHT; 1 AU; FLUX; EVOLUTION;
RECONSTRUCTION; SIGNATURES; LASCO; CME
AB On 27 June 2009 the Wind and Advanced Composition Explorer (ACE) spacecraft near Earth detected a magnetic cloud (MC). The MC can be traced back to a slow coronal mass ejection (CME) launched from the Sun on 22 June 2009 but this connection relies entirely on heliospheric imaging of the Sun-Earth line from the two STEREO spacecraft, illustrating the value of such imaging. The STEREO and SOHO/LASCO views of this event collectively suggest strongly that the CME has the shape of a magnetic flux rope. The arrival times of two density peaks at ACE are consistent with the expected arrival times of the front and back of the flux rope observed in the images, and the velocity of the CME seen by ACE is also consistent with the STEREO measurements. However, the complex nature of the MC signature of this event complicates attempts to compare the flux rope orientations inferred from the imaging and in situ data. Various analyses of the in situ data, performed using both force-free and Grad-Shafranov approaches to MC modeling, yield a wide range of flux rope orientations depending on the type of analysis and on the exact time interval used. The best reproduction of the image-inferred orientation occurs when the first third of the MC time interval is ignored.
C1 [Wood, B. E.; Battams, K.; Howard, R. A.; Socker, D. G.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Rouillard, A. P.] George Mason Univ, Fairfax, VA 22030 USA.
[Rouillard, A. P.] IRAP, F-31028 Toulouse 4, France.
[Moestl, C.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Moestl, C.] Graz Univ, Inst Phys, Kanzelhohe Observ IGAM, A-8010 Graz, Austria.
[Moestl, C.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria.
[Savani, N. P.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Savani, N. P.; Marubashi, K.] UCAR, Boulder, CO 80307 USA.
[Savani, N. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Wood, BE (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
EM brian.wood@nrl.navy.mil
RI Savani, Neel/G-4066-2014;
OI Savani, Neel/0000-0002-1916-7877; Moestl, Christian/0000-0001-6868-4152
FU NASA [NNH10AN83I]; NASA; NRL; USAF Space Test Program; ONR; Marie Curie
International Outgoing Fellowship within European Community; Austrian
Science Fund (FWF) [P20145-N16]; European Union [263252]
FX This work has been supported by NASA award NNH10AN83I to the Naval
Research Laboratory. The STEREO/SECCHI data are produced by a consortium
of NRL (US), LMSAL (US), NASA/GSFC (US), RAL (UK), UBHAM (UK), MPS
(Germany), CSL (Belgium), IOTA (France), and IAS (France). In addition
to funding by NASA, NRL also received support from the USAF Space Test
Program and ONR. C. M. was supported by a Marie Curie International
Outgoing Fellowship within the 7th European Community Framework
Programme, by the Austrian Science Fund (FWF): P20145-N16, and by
funding from the European Union Seventh Framework Programme
(FP7/2007-2013) under grant agreement no 263252 [COMESEP].
NR 52
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD NOV
PY 2012
VL 281
IS 1
BP 369
EP 389
DI 10.1007/s11207-012-0036-3
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 033QB
UT WOS:000310811900021
ER
PT J
AU Simunac, KDC
Galvin, AB
Farrugia, CJ
Kistler, LM
Kucharek, H
Lavraud, B
Liu, YCM
Luhmann, JG
Ogilvie, KW
Opitz, A
Popecki, MA
Sauvaud, JA
Wang, S
AF Simunac, K. D. C.
Galvin, A. B.
Farrugia, C. J.
Kistler, L. M.
Kucharek, H.
Lavraud, B.
Liu, Y. C. -M.
Luhmann, J. G.
Ogilvie, K. W.
Opitz, A.
Popecki, M. A.
Sauvaud, J. -A.
Wang, S.
TI The Heliospheric Plasma Sheet Observed in situ by Three Spacecraft over
Four Solar Rotations
SO SOLAR PHYSICS
LA English
DT Article
ID ADVANCED COMPOSITION EXPLORER; CORONAL STREAMERS; MAGNETIC CLOUDS; 1 AU;
WIND; INTERFACES; ORIGIN
AB In this paper we present in situ observations of the heliospheric plasma sheet (HPS) from STEREO-A, Wind, and STEREO-B over four solar rotations in the declining phase of Solar Cycle 23, covering late March through late June 2007. During this time period the three spacecraft were located in the ecliptic plane, and were gradually separating in heliographic longitude from about 3 degrees to 14 degrees. Crossings of the HPS were identified using the following criteria: reversal of the interplanetary magnetic field sector, enhanced proton density, and local minima in both the proton specific entropy argument and in the alpha particle-to-proton number density ratio (N (a)/N (p)). Two interplanetary coronal mass ejections (ICMEs) were observed during the third solar rotation of our study period, which disrupted the HPS from its quasi-stationary state. We find differences in the in situ proton parameters at the HPS between the three spacecraft despite temporal separations of less than one day. We attribute these differences to both small separations in heliographic latitude and radial evolution of the solar wind leading to the development of compression regions associated with stream interaction regions (SIRs). We also observed a modest enhancement in the density of iron ions at the HPS.
C1 [Simunac, K. D. C.; Galvin, A. B.; Farrugia, C. J.; Kistler, L. M.; Kucharek, H.; Liu, Y. C. -M.; Popecki, M. A.; Wang, S.] Univ New Hampshire, Durham, NH 03824 USA.
[Luhmann, J. G.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Ogilvie, K. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lavraud, B.; Opitz, A.; Sauvaud, J. -A.] Univ Toulouse, IRAP CNRS UPS, Toulouse, France.
[Liu, Y. C. -M.] Chinese Acad Sci, Ctr Space Sci & Appl Res, State Key Lab Space Weather, Beijing, Peoples R China.
RP Simunac, KDC (reprint author), Univ New Hampshire, Durham, NH 03824 USA.
EM K.Simunac@unh.edu
RI Galvin, Antoinette/A-6114-2013; Yong, Liu/H-5333-2011
FU NASA [NAS5-00132, NNX10AQ29G]
FX This work was supported at UNH under NASA contract NAS5-00132, and grant
NNX10AQ29G.
NR 42
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD NOV
PY 2012
VL 281
IS 1
BP 423
EP 447
DI 10.1007/s11207-012-0156-9
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 033QB
UT WOS:000310811900024
ER
PT J
AU Farrugia, CJ
Harris, B
Leitner, M
Mostl, C
Galvin, AB
Simunac, KDC
Torbert, RB
Temmer, MB
Veronig, AM
Erkaev, NV
Szabo, A
Ogilvie, KW
Luhmann, JG
Osherovich, VA
AF Farrugia, C. J.
Harris, B.
Leitner, M.
Moestl, C.
Galvin, A. B.
Simunac, K. D. C.
Torbert, R. B.
Temmer, M. B.
Veronig, A. M.
Erkaev, N. V.
Szabo, A.
Ogilvie, K. W.
Luhmann, J. G.
Osherovich, V. A.
TI Deep Solar Activity Minimum 2007-2009: Solar Wind Properties and Major
Effects on the Terrestrial Magnetosphere
SO SOLAR PHYSICS
LA English
DT Article
ID CORONAL MASS EJECTIONS; MAGNETIC-FIELD; QUASI-INVARIANT; BOW SHOCK;
PLASMA INSTRUMENT; MAGNETOPAUSE; SATURATION; INDEX; DEPENDENCE;
EVOLUTION
AB We discuss the temporal variations and frequency distributions of solar wind and interplanetary magnetic field parameters during the solar minimum of 2007-2009 from measurements returned by the IMPACT and PLASTIC instruments on STEREO-A. We find that the density and total field strength were significantly weaker than in the previous minimum. The Alfv,n Mach number was higher than typical. This reflects the weakness of magnetohydrodynamic (MHD) forces, and has a direct effect on the solar wind-magnetosphere interactions. We then discuss two major aspects that this weak solar activity had on the magnetosphere, using data from Wind and ground-based observations: i) the dayside contribution to the cross-polar cap potential (CPCP), and ii) the shapes of the magnetopause and bow shock. For i) we find a low interplanetary electric field of 1.3 +/- 0.9 mV m(-1) and a CPCP of 37.3 +/- 20.2 kV. The auroral activity is closely correlated to the prevalent stream-stream interactions. We suggest that the Alfven wave trains in the fast streams and Kelvin-Helmholtz instability were the predominant agents mediating the transfer of solar wind momentum and energy to the magnetosphere during this three-year period. For ii) we determine 328 magnetopause and 271 bow shock crossings made by Geotail, Cluster 1, and the THEMIS B and C spacecraft during a three-month interval when the daily averages of the magnetic and kinetic energy densities attained their lowest value during the three years under survey. We use the same numerical approach as in Fairfield's (J. Geophys. Res. 76, 7600, 1971) empirical model and compare our findings with three magnetopause models. The stand-off distance of the subsolar magnetopause and bow shock were 11.8 R-E and 14.35 R-E, respectively. When comparing with Fairfield's (1971) classic result, we find that the subsolar magnetosheath is thinner by similar to 1 R-E. This is mainly due to the low dynamic pressure which results in a sunward shift of the magnetopause. The magnetopause is more flared than in Fairfield's model. By contrast the bow shock is less flared, and the latter is the result of weaker MHD forces.
C1 [Farrugia, C. J.; Harris, B.; Leitner, M.; Galvin, A. B.; Simunac, K. D. C.; Torbert, R. B.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Farrugia, C. J.; Harris, B.; Leitner, M.; Galvin, A. B.; Simunac, K. D. C.; Torbert, R. B.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA.
[Leitner, M.] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria.
[Moestl, C.; Temmer, M. B.; Veronig, A. M.] Graz Univ, Inst Phys, Kanzelhohe Observ IGAM, A-8010 Graz, Austria.
[Moestl, C.; Temmer, M. B.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria.
[Erkaev, N. V.] Russian Acad Sci, Inst Computat Modeling, Krasnoyarsk, Russia.
[Erkaev, N. V.] Siberian Fed Univ, Krasnoyarsk, Russia.
[Szabo, A.; Ogilvie, K. W.; Osherovich, V. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Moestl, C.; Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Farrugia, CJ (reprint author), Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
EM charlie.farrugia@unh.edu
RI Galvin, Antoinette/A-6114-2013; Erkaev, Nikolai/M-1608-2013; Veronig,
Astrid/B-8422-2009;
OI Erkaev, Nikolai/0000-0001-8993-6400; Moestl,
Christian/0000-0001-6868-4152; Temmer, Manuela/0000-0003-4867-7558
FU NASA [NNX10AQ29G, NAS5-03131, NNXO9AR80G]; European Commissions
[263253]; Austrian Science Fund (FWF) [FWF V195-N16]; European Community
FX We are grateful to the referee for many helpful suggestions. We thank
Marc Hairston, Jana Safrankova and Zdenek Nemecek for helpful comments.
For the data used in the geomagnetic response section, we thank the
World Data Center for Geomagnetism at the Kyoto web site, Japan; the
OMNI website at Goddard Space Flight Center, USA; and the Defense
Meteorological Satellite Program (DMSP) program, NOAA. Work at UNH was
supported by NASA grants NNX10AQ29G and NAS5-03131. This work has
received funding from the European Commissions's Seventh Framework
Programme (FP7/2007-2013) under the grant agreement No. 263253
[COMESEP]. V.O. was supported by NASA Grant NNXO9AR80G. M.T. greatly
acknowledges the Austrian Science Fund (FWF): FWF V195-N16. This
research was supported by a Marie Curie International Outgoing
Fellowship within the 7th European Community Framework Program.
NR 53
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD NOV
PY 2012
VL 281
IS 1
BP 461
EP 489
DI 10.1007/s11207-012-0119-1
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 033QB
UT WOS:000310811900026
ER
PT J
AU Pesnell, WD
AF Pesnell, W. Dean
TI Solar Cycle Predictions (Invited Review)
SO SOLAR PHYSICS
LA English
DT Article
DE Solar cycle; Predictions
ID SUNSPOT NUMBER; SPECTRAL COMPONENTS; MAXIMUM AMPLITUDE; ACTIVITY
FORECAST; PRECURSOR METHOD; SOUTH ASYMMETRY; AVERAGE METHOD;
SOLAR-CYCLE-24; MINIMUM; MODELS
AB Solar cycle predictions are needed to plan long-term space missions, just as weather predictions are needed to plan the launch. Fleets of satellites circle the Earth collecting many types of science data, protecting astronauts, and relaying information. All of these satellites are sensitive at some level to solar cycle effects. Predictions of drag on low-Earth orbit spacecraft are one of the most important. Launching a satellite with less propellant can mean a higher orbit, but unanticipated solar activity and increased drag can make that a Pyrrhic victory as the reduced propellant load is consumed more rapidly. Energetic events at the Sun can produce crippling radiation storms that endanger all assets in space. Solar cycle predictions also anticipate the shortwave emissions that cause degradation of solar panels. Testing solar dynamo theories by quantitative predictions of what will happen in 5-20 years is the next arena for solar cycle predictions. A summary and analysis of 75 predictions of the amplitude of the upcoming Solar Cycle 24 is presented. The current state of solar cycle predictions and some anticipations of how those predictions could be made more accurate in the future are discussed.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Pesnell, WD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM william.d.pesnell@nasa.gov
RI Pesnell, William/D-1062-2012
OI Pesnell, William/0000-0002-8306-2500
FU NASA's Solar Dynamics Observatory at the Goddard Space Flight Center
FX This work was supported by NASA's Solar Dynamics Observatory at the
Goddard Space Flight Center.
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD NOV
PY 2012
VL 281
IS 1
BP 507
EP 532
DI 10.1007/s11207-012-9997-5
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 033QB
UT WOS:000310811900029
ER
PT J
AU Berta, ZK
Irwin, J
Charbonneau, D
Burke, CJ
Falco, EE
AF Berta, Zachory K.
Irwin, Jonathan
Charbonneau, David
Burke, Christopher J.
Falco, Emilio E.
TI TRANSIT DETECTION IN THE MEarth SURVEY OF NEARBY M DWARFS: BRIDGING THE
CLEAN-FIRST, SEARCH-LATER DIVIDE
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE eclipses; methods: data analysis; planetary systems; stars: low-mass;
techniques: photometric
ID EARTH GJ 1214B; SOLAR-LIKE VARIABILITY; PLANETARY TRANSITS; LIGHT
CURVES; TRANSMISSION SPECTROSCOPY; MONITOR PROJECT; DETECTION
ALGORITHMS; STELLAR VARIABILITY; ECLIPSING BINARIES; EXTRASOLAR PLANETS
AB In the effort to characterize the masses, radii, and atmospheres of potentially habitable exoplanets, there is an urgent need to find examples of such planets transiting nearby M dwarfs. The MEarth Project is an ongoing effort to do so, as a ground-based photometric survey designed to detect exoplanets as small as 2 R-circle plus. transiting mid-to-late M dwarfs within 33 pc of the Sun. Unfortunately, identifying transits of such planets in photometric monitoring is complicated both by the intrinsic stellar variability that is common among these stars and by the nocturnal cadence, atmospheric variations, and instrumental systematics that often plague Earth-bound observatories. Here, we summarize the properties of MEarth data gathered so far, emphasizing the challenges they present for transit detection. We address these challenges with a new framework to detect shallow exoplanet transits in wiggly and irregularly spaced light curves. In contrast to previous methods that clean trends from light curves before searching for transits, this framework assesses the significance of individual transits simultaneously while modeling variability, systematics, and the photometric quality of individual nights. Our Method for Including Starspots and Systematics in the Marginalized Probability of a Lone Eclipse (MISS MarPLE) uses a computationally efficient semi-Bayesian approach to explore the vast probability space spanned by the many parameters of this model, naturally incorporating the uncertainties in these parameters into its evaluation of candidate events. We show how to combine individual transits processed by MISS MarPLE into periodic transiting planet candidates and compare our results to the popular box-fitting least-squares method with simulations. By applying MISS MarPLE to observations from the MEarth Project, we demonstrate the utility of this framework for robustly assessing the false alarm probability of transit signals in real data.
C1 [Berta, Zachory K.; Irwin, Jonathan; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Burke, Christopher J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Burke, Christopher J.] SETI Inst, Mountain View, CA 94043 USA.
[Falco, Emilio E.] Smithsonian Astrophys Observ, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
RP Berta, ZK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM zberta@cfa.harvard.edu
OI Berta-Thompson, Zachory/0000-0002-3321-4924; Charbonneau,
David/0000-0002-9003-484X
FU David and Lucile Packard Fellowship for Science and Engineering;
National Science Foundation (NSF) [AST-0807690]
FX We thank Philip Nutzman for inspirational conversations regarding this
work; John Johnson, Diana Dragomir, Scott Gaudi, and Elisabeth Newton
for discussions regarding the method and the paper; and the referee
whose careful reading improved the manuscript considerably. We
gratefully acknowledge funding for the MEarth Project from the David and
Lucile Packard Fellowship for Science and Engineering and from the
National Science Foundation (NSF) under grant No. AST-0807690. The
MEarth team is greatly indebted to the staff at the Fred Lawrence
Whipple Observatory for their efforts in construction and maintenance of
the facility and would like to thank Wayne Peters, Ted Groner, Karen
Erdman-Myres, Grace Alegria, Rodger Harris, Bob Hutchins, Dave Martina,
Dennis Jankovsky, Tom Welsh, Robert Hyne, Mike Calkins, Perry Berlind,
and Gil Esquerdo for their support. This research has made use of NASA's
Astro-Physics Data System.
NR 98
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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 NOV
PY 2012
VL 144
IS 5
AR 145
DI 10.1088/0004-6256/144/5/145
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 029XI
UT WOS:000310530400021
ER
PT J
AU Griffith, RL
Kirkpatrick, JD
Eisenhardt, PRM
Gelino, CR
Cushing, MC
Benford, D
Blain, A
Bridge, CR
Cohen, M
Cutri, RM
Donoso, E
Jarrett, TH
Lonsdale, C
Mace, G
Mainzer, A
Marsh, K
Padgett, D
Petty, S
Ressler, ME
Skrutskie, MF
Stanford, SA
Stern, D
Tsai, CW
Wright, EL
Wu, JW
Yan, L
AF Griffith, Roger L.
Kirkpatrick, J. Davy
Eisenhardt, Peter R. M.
Gelino, Christopher R.
Cushing, Michael C.
Benford, Dominic
Blain, Andrew
Bridge, Carrie R.
Cohen, Martin
Cutri, Roc M.
Donoso, Emilio
Jarrett, Thomas H.
Lonsdale, Carol
Mace, Gregory
Mainzer, A.
Marsh, Ken
Padgett, Deborah
Petty, Sara
Ressler, Michael E.
Skrutskie, Michael F.
Stanford, Spencer A.
Stern, Daniel
Tsai, Chao-Wei
Wright, Edward L.
Wu, Jingwen
Yan, Lin
TI SPITZER PHOTOMETRY OF WISE-SELECTED BROWN DWARF AND HYPER-LUMINOUS
INFRARED GALAXY CANDIDATES
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE brown dwarfs; galaxies: evolution; galaxies: high-redshift; galaxies:
photometry
ID ARRAY CAMERA IRAC; SKY SURVEY 2MASS; SPECTRAL TYPE-L; SURVEY EXPLORER;
T-DWARFS; LOW-MASS; SPACE DENSITY; FIELD; WIDE; STARS
AB We present Spitzer 3.6 and 4.5 mu m photometry and positions for a sample of 1510 brown dwarf candidates identified by the Wide-field Infrared Survey Explorer (WISE) all-sky survey. Of these, 166 have been spectroscopically classified as objects with spectral types M(1), L(7), T(146), and Y(12). Sixteen other objects are non-(sub) stellar in nature. The remainder are most likely distant L and T dwarfs lacking spectroscopic verification, other Y dwarf candidates still awaiting follow-up, and assorted other objects whose Spitzer photometry reveals them to be background sources. We present a catalog of Spitzer photometry for all astrophysical sources identified in these fields and use this catalog to identify seven fainter (4.5 mu m similar to 17.0 mag) brown dwarf candidates, which are possibly wide-field companions to the original WISE sources. To test this hypothesis, we use a sample of 919 Spitzer observations around WISE-selected high-redshift hyper-luminous infrared galaxy candidates. For this control sample, we find another six brown dwarf candidates, suggesting that the seven companion candidates are not physically associated. In fact, only one of these seven Spitzer brown dwarf candidates has a photometric distance estimate consistent with being a companion to the WISE brown dwarf candidate. Other than this, there is no evidence for any widely separated (>20 AU) ultra-cool binaries. As an adjunct to this paper, we make available a source catalog of similar to 7.33 x 10(5) objects detected in all of these Spitzer follow-up fields for use by the astronomical community. The complete catalog includes the Spitzer 3.6 and 4.5 mu m photometry, along with positionally matched B and R photometry from USNO-B; J, H, and K-s photometry from Two Micron All-Sky Survey; and W1, W2, W3, and W4 photometry from the WISE all-sky catalog.
C1 [Griffith, Roger L.; Kirkpatrick, J. Davy; Gelino, Christopher R.; Cutri, Roc M.; Donoso, Emilio; Jarrett, Thomas H.; Tsai, Chao-Wei; Yan, Lin] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Eisenhardt, Peter R. M.; Mainzer, A.; Ressler, Michael E.; Stern, Daniel; Wu, Jingwen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cushing, Michael C.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
[Benford, Dominic; Padgett, Deborah] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Blain, Andrew] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Bridge, Carrie R.; Cohen, Martin] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA.
Monterey Inst Res Astron, Marina, CA 93933 USA.
[Lonsdale, Carol] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Mace, Gregory; Petty, Sara; Wright, Edward L.] Univ Calif Los Angeles, Dept Astron, Los Angeles, CA USA.
[Marsh, Ken] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Skrutskie, Michael F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Stanford, Spencer A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
RP Griffith, RL (reprint author), CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
RI Benford, Dominic/D-4760-2012
OI Benford, Dominic/0000-0002-9884-4206
FU National Aeronautics and Space Administration (NASA); National Science
Foundation
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 (NASA). This publication also makes use 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. This work is also based in part 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. Some of the spectroscopic classifications presented herein were
obtained at the W. M. Keck Observatory, which is operated as a
scientific partnership among the California Institute of Technology, the
University of California and the National Aeronautics and Space
Administration. This publication also makes use of data products from
2MASS. 2MASS 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. This research has made use of the
NASA/IPAC Infrared Science Archive (IRSA), which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with NASA.
NR 36
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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 NOV
PY 2012
VL 144
IS 5
AR 148
DI 10.1088/0004-6256/144/5/148
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 029XI
UT WOS:000310530400024
ER
PT J
AU Jacobson, R
Brozovic, M
Gladman, B
Alexandersen, M
Nicholson, PD
Veillet, C
AF Jacobson, R.
Brozovic, M.
Gladman, B.
Alexandersen, M.
Nicholson, P. D.
Veillet, C.
TI IRREGULAR SATELLITES OF THE OUTER PLANETS: ORBITAL UNCERTAINTIES AND
ASTROMETRIC RECOVERIES IN 2009-2011
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE planets and satellites: individual (Jupiter, Saturn, Uranus, Neptune)
ID EPHEMERIDES; FACILITY
AB More than 100 small satellites have been identified orbiting the giant planets in distant, inclined, eccentric orbits. Detailed study of these objects requires that their orbits be known well enough to permit routine observations both from the Earth and from spacecraft. Unfortunately, many of the satellites have very poorly known orbits due to a scarcity of astrometric measurements. We have developed a reliable method to estimate the future on-sky position uncertainties of the satellites and have verified that those uncertainties provide a correct measure of the true on-sky positional uncertainty. Based on the uncertainties, we identified a set of satellites that are effectively "lost" and another set that would be lost if additional observations were not obtained in the near future. We attempted recoveries of 26 of the latter group using the Hale 5 m and CFHT 3.6 m telescopes and found 23. This validated our method's predictions and led to significant improvements in our knowledge of the orbits of the recovered moons. There remains a handful of irregular moons which are recoverable and whose orbits will benefit from additional observations during the next decade, while 16 moons of Jupiter and Saturn are essentially lost and will require a re-survey to be located again.
C1 [Jacobson, R.; Brozovic, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gladman, B.; Alexandersen, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Nicholson, P. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Veillet, C.] Canada France Hawaii Telescope Corp, Kameula, HI 96743 USA.
RP Jacobson, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM robert.jacobson@jpl.nasa.gov
OI Alexandersen, Mike/0000-0003-4143-8589
FU National Aeronautics and Space Administration
FX Thanks to Palomar and CFHT staff for assisting us in the acquisition of
the recovery observations. The research described in this publication
was carried out at the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with the National Aeronautics and Space
Administration.
NR 19
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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 NOV
PY 2012
VL 144
IS 5
AR 132
DI 10.1088/0004-6256/144/5/132
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 029XI
UT WOS:000310530400008
ER
PT J
AU Mazzarella, JM
Iwasawa, K
Vavilkin, T
Armus, L
Kim, DC
Bothun, G
Evans, AS
Spoon, HWW
Haan, S
Howell, JH
Lord, S
Marshall, JA
Ishida, CM
Xu, CK
Petric, A
Sanders, DB
Surace, JA
Appleton, P
Chan, BHP
Frayer, DT
Inami, H
Khachikian, EY
Madore, BF
Privon, GC
Sturm, E
Vivian, U
Veilleux, S
AF Mazzarella, J. M.
Iwasawa, K.
Vavilkin, T.
Armus, L.
Kim, D. -C.
Bothun, G.
Evans, A. S.
Spoon, H. W. W.
Haan, S.
Howell, J. H.
Lord, S.
Marshall, J. A.
Ishida, C. M.
Xu, C. K.
Petric, A.
Sanders, D. B.
Surace, J. A.
Appleton, P.
Chan, B. H. P.
Frayer, D. T.
Inami, H.
Khachikian, E. Ye.
Madore, B. F.
Privon, G. C.
Sturm, E.
Vivian, U.
Veilleux, S.
TI INVESTIGATION OF DUAL ACTIVE NUCLEI, OUTFLOWS, SHOCK-HEATED GAS, AND
YOUNG STAR CLUSTERS IN MARKARIAN 266
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: interactions; galaxies: nuclei; galaxies:
Seyfert; galaxies: starburst; galaxies: star clusters: general
ID ULTRALUMINOUS INFRARED GALAXIES; SPITZER-SPACE-TELESCOPE; SUPERMASSIVE
BLACK-HOLES; DARK-MATTER HALOS; SKY LIRG SURVEY; X-RAY; GALACTIC NUCLEI;
SEYFERT-GALAXIES; LUMINOSITY FUNCTION; ANTENNAE GALAXIES
AB Results of observations with the Spitzer, Hubble, GALEX, Chandra, and XMM-Newton space telescopes are presented for the luminous infrared galaxy (LIRG) merger Markarian 266. The SW (Seyfert 2) and NE (LINER) nuclei reside in galaxies with Hubble types SBb (pec) and S0/a (pec), respectively. Both companions are more luminous than L* galaxies and they are inferred to each contain a approximate to 2.5 x 10(8) M-circle dot black hole. Although the nuclei have an observed hard X-ray flux ratio of f(X)(NE)/f(X)(SW) = 6.4, Mrk 266 SW is likely the primary source of a bright Fe K alpha line detected from the system, consistent with the reflection-dominated X-ray spectrum of a heavily obscured active galactic nucleus (AGN). Optical knots embedded in an arc with aligned radio continuum radiation, combined with luminous H-2 line emission, provide evidence for a radiative bow shock in an AGN-driven outflow surrounding the NE nucleus. A soft X-ray emission feature modeled as shock-heated plasma with T similar to 10(7) K is cospatial with radio continuum emission between the galaxies. Mid-infrared diagnostics provide mixed results, but overall suggest a composite system with roughly equal contributions of AGN and starburst radiation powering the bolometric luminosity. Approximately 120 star clusters have been detected, with most having estimated ages less than 50 Myr. Detection of 24 mu m emission aligned with soft X-rays, radio continuum, and ionized gas emission extending similar to 34 '' (20 kpc) north of the galaxies is interpreted as similar to 2 x 10(7) M-circle dot of dust entrained in an outflowing superwind. At optical wavelengths this Northern Loop region is resolved into a fragmented morphology indicative of Rayleigh-Taylor instabilities in an expanding shell of ionized gas. Mrk 266 demonstrates that the dust "blowout" phase can begin in a LIRG well before the galaxies fully coalesce during a subsequent ultraluminous infrared galaxy (ULIRG) phase, and rapid gas consumption in luminous dual AGNs with kiloparsec-scale separations early in the merger process may explain the paucity of detected binary QSOs (with parsec-scale orbital separations) in spectroscopic surveys. An evolutionary sequence is proposed representing a progression from dual to binary AGNs, accompanied by an increase in observed L-x/L-ir ratios by over two orders of magnitude.
C1 [Mazzarella, J. M.; Chan, B. H. P.; Madore, B. F.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Iwasawa, K.] Univ Barcelona IEEC UB, ICREA, E-08028 Barcelona, Spain.
[Iwasawa, K.] Univ Barcelona, IEEC UB, Inst Ciencies Cosmos, E-08028 Barcelona, Spain.
[Vavilkin, T.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Armus, L.; Haan, S.; Howell, J. H.; Marshall, J. A.; Petric, A.; Surace, J. A.; Inami, H.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Kim, D. -C.; Evans, A. S.; Privon, G. C.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Kim, D. -C.; Evans, A. S.; Frayer, D. T.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Bothun, G.] Univ Oregon, Dept Phys, Eugene, OR 97402 USA.
[Spoon, H. W. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Haan, S.] ATNF, CSIRO Astron & Space Sci, Marsfield, NSW 2122, Australia.
[Lord, S.; Xu, C. K.; Appleton, P.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA.
[Marshall, J. A.; Petric, A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Ishida, C. M.] Natl Astron Observ Japan, Hilo, HI 96720 USA.
[Sanders, D. B.; Vivian, U.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Khachikian, E. Ye.] Natl Acad Sci Armenia, Byurakan Astrophys Observ, Byurakan 378433, Aragatsodn Prov, Armenia.
[Madore, B. F.] Carnegie Inst Washington Observ, The Observ, Pasadena, CA 91101 USA.
[Sturm, E.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Mazzarella, JM (reprint author), CALTECH, Ctr Infrared Proc & Anal, MS 100-22, Pasadena, CA 91125 USA.
EM mazz@ipac.caltech.edu; kazushi.iwasawa@icc.ub.edu;
vavilkin@grad.physics.sunysb.edu; lee@ipac.caltech.edu; dkim@nrao.edu;
nuts@bigmoo.uoregon.edu; aevans@virginia.edu;
spoon@isc.astro.cornell.edu; haan@ipac.caltech.edu;
jhhowell@ipac.caltech.edu; lord@ipac.caltech.edu;
jason.mashall@caltech.edu; cmishida@mac.com; cxu@ipac.caltech.edu;
ap@astro.caltech.edu; sanders@ifa.hawaii.edu; jason@ipac.caltech.edu;
apple@ipac.caltech.edu; bchan@ipac.caltech.edu; dfrayer@nrao.edu;
inami@ipac.caltech.edu; khache@bao.sci.am;
barry@obs.carnegiescience.edu; gcp8y@virginia.edu; sturm@mpe.mpg.de;
vivian@ifa.hawaii.edu; veilleux@astro.umd.edu
OI Mazzarella, Joseph/0000-0002-8204-8619; Appleton,
Philip/0000-0002-7607-8766; Privon, George/0000-0003-3474-1125
FU Jet Propulsion Laboratory, California Institute of Technology under a
contract with NASA; NASA/ESA Hubble Space Telescope; Association of
Universities for Research in Astronomy, Inc. under NASA [NAS5-26555];
Chandra X-ray Observatory Center; Smithsonian Astrophysical Observatory
for and on behalf of NASA [NAS8-03060]; Galaxy Evolution Explorer
(GALEX); NASA by the California Institute of Technology under NASA
[NAS5-98034]; JPL/Caltech [Spitzer PID 3672, HST-GO10592.01-A, 11235];
Spanish grant MICINN [AYA2010-21782-C03-01]; NASA
FX This work is based on observations with the following facilities: the
Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA, the NASA/ESA Hubble Space Telescope, which is operated by the
Association of Universities for Research in Astronomy, Inc. under NASA
contract NAS5-26555, the Chandra X-ray Observatory Center, which is
operated by the Smithsonian Astrophysical Observatory for and on behalf
of NASA under contract NAS8-03060, and the Galaxy Evolution Explorer
(GALEX), which is operated for NASA by the California Institute of
Technology under NASA contract NAS5-98034. The Aladin (CDS, Strasbourg)
and SAOImage DS9 tools were used for image analysis. Support for this
work was provided by the following NASA grants: an award issued by
JPL/Caltech (Spitzer PID 3672, PI: J. Mazzarella); HST-GO10592.01-A (ACS
imaging, PI: A. Evans) and program 11235 (NICMOS imaging, PI: J. Surace)
issued by the STScI. K. Iwasawa acknowledges support from Spanish grant
MICINN (AYA2010-21782-C03-01). This research made use of the NASA/IPAC
Extragalactic Database (NED) and the Infrared Science Archive (IRSA),
which are operated by the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA. We thank Masa
Imanishi for providing FITS files for the NobeyamaMillimeter Array
observations and Tsuyoshi Ishigaki for supplying optical emission-line
images. We thank ChrisMihos for helpful discussions regarding merger
timescales. Finally, we thank the anonymous referee for very helpful
comments that led to improvements to the manuscript.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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JI Astron. J.
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SC Astronomy & Astrophysics
GA 029XI
UT WOS:000310530400001
ER
PT J
AU Mizusawa, TF
Rebull, LM
Stauffer, JR
Bryden, G
Meyer, M
Song, I
AF Mizusawa, Trisha F.
Rebull, Luisa M.
Stauffer, John R.
Bryden, Geoffrey
Meyer, Michael
Song, Inseok
TI EXPLORING THE EFFECTS OF STELLAR ROTATION AND WIND CLEARING: DEBRIS
DISKS AROUND F STARS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared: stars
ID SPITZER-SPACE-TELESCOPE; SOLAR-TYPE STARS; GENEVA-COPENHAGEN SURVEY;
LOW-MASS STARS; MULTIBAND IMAGING PHOTOMETER; ANGULAR-MOMENTUM
EVOLUTION; MAIN-SEQUENCE STARS; SUN-LIKE STARS; ALL-SKY SURVEY; T-TAURI
STARS
AB We have conducted a study of debris disks around F stars in order to explore correlations between rotation, stellar winds, and circumstellar disks. We obtained new 24 mu m photometry from the Multiband Imaging Photometer for Spitzer (MIPS) camera for a sample of 188 relatively nearby F dwarfs with various rotation rates and optical colors, and combined it with archival MIPS data for 66 more F stars, as well as Wide-field Infrared Survey Explorer data for the entire sample, plus 9 more F stars. Based on the objects' K-s - [24] and [3.4] - [22] colors, we identify 22 stars in our sample as having 22 and/or 24 mu m excesses above our detection limit, 13 of which are new discoveries. Our overall disk detection rate is 22/263, or 8%, consistent with previous determinations of disk fractions in the solar neighborhood. While fast-rotating stars are expected to have strong winds capable of efficiently removing dust, we find no correlation between rotational velocity and infrared excess. Similarly, we find no significant difference in excess detection rate between late-type F stars, which have convective surfaces, and early-type F stars, which have fully radiative envelopes. However, the essentially unknown range of ages in this sample may be washing out any effects relating rotation, winds, and disks.
C1 [Mizusawa, Trisha F.] Florida Inst Technol, Melbourne, FL 32901 USA.
[Rebull, Luisa M.; Stauffer, John R.] CALTECH, SSC, Pasadena, CA 91125 USA.
[Bryden, Geoffrey] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Meyer, Michael] ETH, Zurich, Switzerland.
[Song, Inseok] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA.
[Mizusawa, Trisha F.; Bryden, Geoffrey] CALTECH, NASA Star & Exoplanet Database NStED, Pasadena, CA 91125 USA.
RP Mizusawa, TF (reprint author), Florida Inst Technol, 150 W Univ Blvd, Melbourne, FL 32901 USA.
EM trisha.mizusawa@gmail.com
OI Rebull, Luisa/0000-0001-6381-515X
FU NASA; National Aeronautics and Space Administration; National Science
Foundation; U.S. Government [NAG W-2166]
FX This work is based in part on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with NASA. Support
for this work was provided by NASA through an award issued by
JPL/Caltech. 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. This research has made use of what was then called the
NASA/IPAC/NExScI Star and Exoplanet Database, which was operated by the
Jet Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration.; This
research has made use of NASA's Astrophysics Data System (ADS) Abstract
Service, and of the SIMBAD database, operated at CDS, Strasbourg,
France. This research has made use of data products from the Two Micron
All Sky Survey (2MASS), which is a joint project of the University of
Massachusetts and the Infrared Processing and Analysis Center, funded by
the National Aeronautics and Space Administration and the National
Science Foundation. 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. The WISE and 2MASS data are served
by 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. This
research has made use of the Digitized Sky Surveys, which were produced
at the Space Telescope Science Institute under U.S. Government grant NAG
W-2166.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
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JI Astron. J.
PD NOV
PY 2012
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SC Astronomy & Astrophysics
GA 029XI
UT WOS:000310530400011
ER
PT J
AU Stevenson, R
Jewitt, D
AF Stevenson, Rachel
Jewitt, David
TI NEAR-NUCLEUS PHOTOMETRY OF OUTBURSTING COMET 17P/HOLMES
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE comets: general; comets: individual (17P/Holmes)
ID FRANCE-HAWAII-TELESCOPE; BAND PHOTOMETRY; OBJECTS; COLORS; GRAINS;
SYSTEM; RATES
AB Comet 17P/Holmes underwent the largest cometary outburst in recorded history on UT 2007 October 23, releasing massive quantities of dust and gas. We used the Canada-France-Hawaii Telescope to obtain wide-field images of 17P/Holmes on 15 dates over a period of three months following the outburst and employ them here to examine the subsequent activity of the nucleus and the nature of the ejecta closest to the nucleus. Through aperture photometry we observed the inner coma (within 2500 km of the nucleus) to fade from an apparent magnitude of 11.7 mag to 17.6 mag, corresponding to absolute magnitudes of 8.1 mag and 12.4 mag, between UT 2007 November 6 and 2008 February 12. A second much smaller outburst occurred on UT 2007 November 12, three weeks after the original outburst, suggesting that the nucleus remained unstable. The surface brightness profile of the inner coma was consistently shallow relative to the expected steady-state profile, and showed a persistent brightness enhancement within similar to 5000 km of the nucleus. We propose that sublimating ice grains created an ice grain halo around the nucleus, while fragmenting grains were responsible for the shallow surface brightness profile.
C1 [Jewitt, David] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Stevenson, Rachel; Jewitt, David] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
RP Stevenson, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Rachel.A.Stevenson@jpl.nasa.gov; jewitt@ucla.edu
FU NASA Outer Planets Research Program; NASA Postdoctoral Fellowship
Program; National Aeronautics and Space Administration
FX 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 is based in part on data products produced at the TERAPIX data
center located at the Institut d'Astrophysique de Paris. We appreciate
grant support from the NASA Outer Planets Research Program to D.J. R.S.
acknowledges support from the NASA Postdoctoral Fellowship Program. Part
of the research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
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JI Astron. J.
PD NOV
PY 2012
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SC Astronomy & Astrophysics
GA 029XI
UT WOS:000310530400014
ER
PT J
AU Gettings, DP
Gonzalez, AH
Stanford, SA
Eisenhardt, PRM
Brodwin, M
Mancone, C
Stern, D
Zeimann, GR
Masci, FJ
Papovich, C
Tanaka, I
Wright, EL
AF Gettings, Daniel P.
Gonzalez, Anthony H.
Stanford, S. Adam
Eisenhardt, Peter R. M.
Brodwin, Mark
Mancone, Conor
Stern, Daniel
Zeimann, Gregory R.
Masci, Frank J.
Papovich, Casey
Tanaka, Ichi
Wright, Edward L.
TI THE MASSIVE DISTANT CLUSTERS OF WISE SURVEY: THE FIRST DISTANT GALAXY
CLUSTER DISCOVERED BY WISE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: clusters: individual (MOO J2342.0+1301); galaxies: distances
and redshifts; galaxies: evolution
ID STELLAR POPULATION SYNTHESIS; DIGITAL SKY SURVEY; DARK-MATTER;
TELESCOPE; Z=1.75; RESOLUTION; EXISTENCE; UNIVERSE; CATALOG; MODELS
AB We present spectroscopic confirmation of a z = 0.99 galaxy cluster discovered using data from the Wide-field Infrared Survey Explorer (WISE). This is the first z similar to 1 cluster candidate from the Massive Distant Clusters of WISE Survey to be confirmed. It was selected as an overdensity of probable z greater than or similar to 1 sources using a combination of WISE and Sloan Digital Sky Survey DR8 photometric catalogs. Deeper follow-up imaging data from Subaru and WIYN reveal the cluster to be a rich system of galaxies, and multi-object spectroscopic observations from Keck confirm five cluster members at z = 0.99. The detection and confirmation of this cluster represents a first step toward constructing a uniformly selected sample of distant, high-mass galaxy clusters over the full extragalactic sky using WISE data.
C1 [Gettings, Daniel P.; Gonzalez, Anthony H.; Mancone, Conor] Univ Florida, Dept Astron, Bryant Space Ctr 211, Gainesville, FL 32611 USA.
[Stanford, S. Adam] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
[Stanford, S. Adam; Zeimann, Gregory R.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Eisenhardt, Peter R. M.; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Brodwin, Mark] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Masci, Frank J.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Papovich, Casey] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Papovich, Casey] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[Tanaka, Ichi] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Wright, Edward L.] UCLA Astron, Los Angeles, CA 90095 USA.
RP Gettings, DP (reprint author), Univ Florida, Dept Astron, Bryant Space Ctr 211, Gainesville, FL 32611 USA.
FU National Aeronautics and Space Administration (NASA); NASA Astrophysics
Data Analysis Program (ADAP) [NNX12AE15G]; W.M. Keck Foundation
FX The authors thank the anonymous referee whose comments improved the
quality of the manuscript. 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 (NASA). D. P. G. and A. H. G.
acknowledge support for this research from the NASA Astrophysics Data
Analysis Program (ADAP) through grant NNX12AE15G. Some of the data
presented herein were obtained at the W. M. Keck Observatory, which is
operated as a scientific partnership among the California Institute of
Technology, the University of California and the National Aeronautics
and Space Administration. The Observatory was made possible by the
generous financial support of the W.M. Keck Foundation. Based in part on
data collected at Subaru Telescope, which is operated by the National
Astronomical Observatory of Japan. D. P. G. was a Visiting Astronomer,
Kitt Peak National Observatory, National Optical Astronomy Observatory,
which is operated by the Association of Universities for Research in
Astronomy (AURA) under cooperative agreement with the National Science
Foundation. The WIY