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
TC 37
Z9 37
U1 0
U2 3
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 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).
NR 41
TC 55
Z9 55
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD 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.
NR 35
TC 7
Z9 7
U1 3
U2 15
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD 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.
NR 33
TC 5
Z9 5
U1 2
U2 25
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD 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).
NR 44
TC 10
Z9 10
U1 1
U2 40
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 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
Z9 29
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
TC 19
Z9 19
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
TC 10
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
TC 4
Z9 4
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 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.
NR 60
TC 37
Z9 37
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 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.
NR 33
TC 11
Z9 11
U1 0
U2 16
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 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.
NR 179
TC 67
Z9 68
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 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.
NR 61
TC 25
Z9 25
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 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.
NR 112
TC 30
Z9 30
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 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.
NR 41
TC 3
Z9 3
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD 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.
NR 78
TC 21
Z9 21
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 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.
NR 42
TC 35
Z9 36
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 DEC 1
PY 2012
VL 760
IS 2
AR 118
DI 10.1088/0004-637X/760/2/118
PG 11
WC Astronomy & Astrophysics
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
NR 0
TC 0
Z9 0
U1 0
U2 4
PU TAYLOR & FRANCIS INC
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.
NR 45
TC 22
Z9 22
U1 0
U2 15
PU TAYLOR & FRANCIS INC
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 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.
NR 37
TC 26
Z9 27
U1 4
U2 35
PU TAYLOR & FRANCIS INC
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
TC 9
Z9 11
U1 0
U2 9
PU TAYLOR & FRANCIS INC
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
TC 4
Z9 5
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
TC 7
Z9 7
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
TC 33
Z9 35
U1 3
U2 18
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.
NR 63
TC 29
Z9 29
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
TC 23
Z9 23
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
TC 81
Z9 82
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
TC 23
Z9 23
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
TC 74
Z9 74
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
TC 18
Z9 18
U1 2
U2 33
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
Black, E
Blackburn, JK
Blackburn, L
Blair, D
Bland, B
Blom, M
Bock, O
Bodiya, TP
Bogan, C
Bondarescu, R
Bondu, F
Bonelli, L
Bonnand, R
Bork, R
Born, M
Boschi, V
Bose, S
Bosi, L
Bouhou, B
Braccini, S
Bradaschia, C
Brady, PR
Braginsky, VB
Branchesi, M
Brau, JE
Breyer, J
Briant, T
Bridges, DO
Brillet, A
Brinkmann, M
Brisson, V
Britzger, M
Brooks, AF
Brown, DA
Bulik, T
Bulten, HJ
Buonanno, A
Burguet-Castell, J
Buskulic, D
Buy, C
Byer, RL
Cadonati, L
Calloni, E
Camp, JB
Campsie, P
Cannizzo, J
Cannon, K
Canuel, B
Cao, J
Capano, CD
Carbognani, F
Carbone, L
Caride, S
Caudill, S
Cavaglia, M
Cavalier, F
Cavalieri, R
Cella, G
Cepeda, C
Cesarini, E
Chaibi, O
Chalermsongsak, T
Charlton, P
Chassande-Mottin, E
Chelkowski, S
Chen, W
Chen, X
Chen, Y
Chincarini, A
Chiummo, A
Cho, HS
Chow, J
Christensen, N
Chua, SSY
Chung, CTY
Chung, S
Ciani, G
Clara, F
Clark, DE
Clark, J
Clayton, JH
Cleva, F
Coccia, E
Cohadon, PF
Colacino, CN
Colas, J
Colla, A
Colombini, M
Conte, A
Conte, R
Cook, D
Corbitt, TR
Cordier, M
Cornish, N
Corsi, A
Costa, CA
Coughlin, M
Coulon, JP
Couvares, P
Coward, DM
Cowart, M
Coyne, DC
Creighton, JDE
Creighton, TD
Cruise, AM
Cumming, A
Cunningham, L
Cuoco, E
Cutler, RM
Dahl, K
Danilishin, SL
Dannenberg, R
D'Antonio, S
Danzmann, K
Dattilo, V
Daudert, B
Daveloza, H
Davier, M
Daw, EJ
Day, R
Dayanga, T
De Rosa, R
Debra, D
Debreczeni, G
Degallaix, J
Del Pozzo, W
del Prete, M
Dent, T
Dergachev, V
DeRosa, R
DeSalvo, R
Dhurandhar, S
Di Fiore, L
Di Lieto, A
Di Palma, I
Emilio, MD
Di Virgilio, A
Diaz, M
Dietz, A
Donovan, F
Dooley, KL
Drago, M
Drever, RWP
Driggers, JC
Du, Z
Dumas, JC
Dwyer, S
Eberle, T
Edgar, M
Edwards, M
Effler, A
Ehrens, P
Endroczi, G
Engel, R
Etzel, T
Evans, K
Evans, M
Evans, T
Factourovich, M
Fafone, V
Fairhurst, S
Fan, Y
Farr, BF
Fazi, D
Fehrmann, H
Feldbaum, D
Feroz, F
Ferrante, I
Fidecaro, F
Finn, LS
Fiori, I
Fisher, RP
Flaminio, R
Flanigan, M
Foley, S
Forsi, E
Forte, LA
Fotopoulos, N
Fournier, JD
Franc, J
Franco, S
Frasca, S
Frasconi, F
Frede, M
Frei, M
Frei, Z
Freise, A
Frey, R
Fricke, TT
Friedrich, D
Fritschel, P
Frolov, VV
Fujimoto, MK
Fulda, PJ
Fyffe, M
Gair, J
Galimberti, M
Gammaitoni, L
Garcia, J
Garufi, F
Gaspar, ME
Gehrels, N
Gemme, G
Geng, R
Genin, E
Gennai, A
Gergely, LA
Ghosh, S
Giaime, JA
Giampanis, S
Giardina, KD
Giazotto, A
Gil-Casanova, S
Gill, C
Gleason, J
Goetz, E
Goggin, LM
Gonzalez, G
Gorodetsky, ML
Gossler, S
Gouaty, R
Graef, C
Graff, PB
Granata, M
Grant, A
Gras, S
Gray, C
Gray, N
Greenhalgh, RJS
Gretarsson, AM
Greverie, C
Grosso, R
Grote, H
Grunewald, S
Guidi, GM
Guido, C
Gupta, R
Gustafson, EK
Gustafson, R
Ha, T
Hallam, JM
Hammer, D
Hammond, G
Hanks, J
Hanna, C
Hanson, J
Hardt, A
Harms, J
Harry, GM
Harry, IW
Harstad, ED
Hartman, MT
Haughian, K
Hayama, K
Hayau, JF
Heefner, J
Heidmann, A
Heintze, MC
Heitmann, H
Hello, P
Hendry, MA
Heng, IS
Heptonstall, AW
Herrera, V
Hewitson, M
Hild, S
Hoak, D
Hodge, KA
Holt, K
Holtrop, M
Hong, T
Hooper, S
Hosken, DJ
Hough, J
Howell, EJ
Hughey, B
Husa, S
Huttner, SH
Huynh-Dinh, T
Ingram, DR
Inta, R
Isogai, T
Ivanov, A
Izumi, K
Jacobson, M
James, E
Jang, YJ
Jaranowski, P
Jesse, E
Johnson, WW
Jones, DI
Jones, G
Jones, R
Jonker, RJG
Ju, L
Kalmus, P
Kalogera, V
Kandhasamy, S
Kang, G
Kanner, JB
Kasturi, R
Katsavounidis, E
Katzman, W
Kaufer, H
Kawabe, K
Kawamura, S
Kawazoe, F
Kelley, D
Kells, W
Keppel, DG
Keresztes, Z
Khalaidovski, A
Khalili, FY
Khazanov, EA
Kim, BK
Kim, C
Kim, H
Kim, K
Kim, N
Kim, YM
King, PJ
Kinzel, DL
Kissel, JS
Klimenko, S
Kokeyama, K
Kondrashov, V
Koranda, S
Korth, WZ
Kowalska, I
Kozak, D
Kranz, O
Kringel, V
Krishnamurthy, S
Krishnan, B
Krolak, A
Kuehn, G
Kumar, P
Kumar, R
Kwee, P
Lam, PK
Landry, M
Lantz, B
Lastzka, N
Lawrie, C
Lazzarini, A
Leaci, P
Lee, CH
Lee, HK
Lee, HM
Leong, JR
Leonor, I
Leroy, N
Letendre, N
Li, J
Li, TGF
Liguori, N
Lindquist, PE
Liu, Y
Liu, Z
Lockerbie, NA
Lodhia, D
Lorenzini, M
Loriette, V
Lormand, M
Losurdo, G
Lough, J
Luan, J
Lubinski, M
Luck, H
Lundgren, AP
Macdonald, E
Machenschalk, B
MacInnis, M
Macleod, DM
Mageswaran, M
Mailand, K
Majorana, E
Maksimovic, I
Malvezzi, V
Man, N
Mandel, I
Mandic, V
Mantovani, M
Marandi, A
Marchesoni, F
Marion, F
Marka, S
Marka, Z
Markosyan, A
Maros, E
Marque, J
Martelli, F
Martin, IW
Martin, RM
Marx, JN
Mason, K
Masserot, A
Matichard, F
Matone, L
Matzner, RA
Mavalvala, N
Mazzolo, G
McCarthy, R
McClelland, DE
McGuire, SC
McIntyre, G
McIver, J
McKechan, DJA
McWilliams, S
Meadors, GD
Mehmet, M
Meier, T
Melatos, A
Melissinos, AC
Mendell, G
Mercer, RA
Meshkov, S
Messenger, C
Meyer, MS
Miao, H
Michel, C
Milano, L
Miller, J
Minenkov, Y
Mitrofanov, VP
Mitselmakher, G
Mittleman, R
Miyakawa, O
Moe, B
Mohan, M
Mohanty, SD
Mohapatra, SRP
Moraru, D
Moreno, G
Morgado, N
Morgia, A
Mori, T
Morriss, SR
Mosca, S
Mossavi, K
Mours, B
Mow-Lowry, CM
Mueller, CL
Mueller, G
Mukherjee, S
Mullavey, A
Muller-Ebhardt, H
Munch, J
Murphy, D
Murray, PG
Mytidis, A
Nash, T
Naticchioni, L
Necula, V
Nelson, J
Neri, I
Newton, G
Nguyen, T
Nishizawa, A
Nitz, A
Nocera, F
Nolting, D
Normandin, ME
Nuttall, L
Ochsner, E
O'Dell, J
Oelker, E
Ogin, GH
Oh, JJ
Oh, SH
O'Reilly, B
O'Shaughnessy, R
Osthelder, C
Ott, CD
Ottaway, DJ
Ottens, RS
Overmier, H
Owen, BJ
Page, A
Palladino, L
Palomba, C
Pan, Y
Pankow, C
Paoletti, F
Paoletti, R
Papa, MA
Parisi, M
Pasqualetti, A
Passaquieti, R
Passuello, D
Patel, P
Pedraza, M
Peiris, P
Pekowsky, L
Penn, S
Perreca, A
Persichetti, G
Phelps, M
Pichot, M
Pickenpack, M
Piergiovanni, F
Pietka, M
Pinard, L
Pinto, IM
Pitkin, M
Pletsch, HJ
Plissi, MV
Poggiani, R
Pold, J
Postiglione, F
Prato, M
Predoi, V
Prestegard, T
Price, LR
Prijatelj, M
Principe, M
Privitera, S
Prix, R
Prodi, GA
Prokhorov, LG
Puncken, O
Punturo, M
Puppo, P
Quetschke, V
Quitzow-James, R
Raab, FJ
Rabeling, DS
Racz, I
Radkins, H
Raffai, P
Rakhmanov, M
Rankins, B
Rapagnani, P
Raymond, V
Re, V
Redwine, K
Reed, CM
Reed, T
Regimbau, T
Reid, S
Reitze, DH
Ricci, F
Riesen, R
Riles, K
Robertson, NA
Robinet, F
Robinson, C
Robinson, EL
Rocchi, A
Roddy, S
Rodriguez, C
Rodruck, M
Rolland, L
Rollins, JG
Romano, JD
Romano, R
Romie, JH
Rosinska, D
Rover, C
Rowan, S
Rudiger, A
Ruggi, P
Ryan, K
Sainathan, P
Salemi, F
Sammut, L
Sandberg, V
Sannibale, V
Santamaria, L
Santiago-Prieto, I
Santostasi, G
Sassolas, B
Sathyaprakash, BS
Sato, S
Saulson, PR
Savage, RL
Schilling, R
Schnabel, R
Schofield, RMS
Schreiber, E
Schulz, B
Schutz, BF
Schwinberg, P
Scott, J
Scott, SM
Seifert, F
Sellers, D
Sentenac, D
Sergeev, A
Shaddock, DA
Shaltev, M
Shapiro, B
Shawhan, P
Shoemaker, DH
Sibley, A
Siemens, X
Sigg, D
Singer, A
Singer, L
Sintes, AM
Skelton, GR
Slagmolen, BJJ
Slutsky, J
Smith, JR
Smith, MR
Smith, RJE
Smith-Lefebvre, ND
Somiya, K
Sorazu, B
Soto, J
Speirits, FC
Sperandio, L
Stefszky, M
Stein, AJ
Stein, LC
Steinert, E
Steinlechner, J
Steinlechner, S
Steplewski, S
Stochino, A
Stone, R
Strain, KA
Strigin, SE
Stroeer, AS
Sturani, R
Stuver, AL
Summerscales, TZ
Sung, M
Susmithan, S
Sutton, PJ
Swinkels, B
Tacca, M
Taffarello, L
Talukder, D
Tanner, DB
Tarabrin, SP
Taylor, JR
Taylor, R
ter Braack, APM
Thomas, P
Thorne, KA
Thorne, KS
Thrane, E
Thuring, A
Tokmakov, KV
Tomlinson, C
Toncelli, A
Tonelli, M
Torre, O
Torres, C
Torrie, CI
Tournefier, E
Tucker, E
Travasso, F
Traylor, G
Tseng, K
Ugolini, D
Vahlbruch, H
Vajente, G
van den Brand, JFJ
Van den Broeck, C
van der Putten, S
van Veggel, AA
Vass, S
Vasuth, M
Vaulin, R
Vavoulidis, M
Vecchio, A
Vedovato, G
Veitch, J
Veitch, PJ
Veltkamp, C
Verkindt, D
Vetrano, F
Vicere, A
Villar, AE
Vinet, JY
Vitale, S
Vocca, H
Vorvick, C
Vyatchanin, SP
Wade, A
Wade, L
Wade, M
Waldman, SJ
Wallace, L
Wan, Y
Wang, M
Wang, X
Wang, Z
Wanner, A
Ward, RL
Was, M
Weinert, M
Weinstein, AJ
Weiss, R
Wen, L
Wessels, P
West, M
Westphal, T
Wette, K
Whelan, JT
Whitcomb, SE
White, DJ
Whiting, BF
Wilkinson, C
Willems, PA
Williams, L
Williams, R
Willke, B
Winkelmann, L
Winkler, W
Wipf, CC
Wiseman, AG
Wittel, H
Woan, G
Wooley, R
Worden, J
Yakushin, I
Yamamoto, H
Yamamoto, K
Yancey, CC
Yang, H
Yeaton-Massey, D
Yoshida, S
Yu, P
Yvert, M
Zadrozny, A
Zanolin, M
Zendri, JP
Zhang, F
Zhang, L
Zhang, W
Zhao, C
Zotov, N
Zucker, ME
Zweizig, J
Briggs, MS
Connaughton, V
Hurley, KC
Jenke, PA
von Kienlin, A
Rau, A
Zhang, XL
AF Abadie, J.
Abbott, B. P.
Abbott, R.
Abbott, T. D.
Abernathy, M.
Accadia, T.
Acernese, F.
Adams, C.
Adhikari, R. X.
Affeldt, C.
Agathos, M.
Agatsuma, K.
Ajith, P.
Allen, B.
Ceron, E. Amador
Amariutei, D.
Anderson, S. B.
Anderson, W. G.
Arai, K.
Arain, M. A.
Araya, M. C.
Aston, S. M.
Astone, P.
Atkinson, D.
Aufmuth, P.
Aulbert, C.
Aylott, B. E.
Babak, S.
Baker, P.
Ballardin, G.
Ballmer, S.
Barayoga, J. C. B.
Barker, D.
Barone, F.
Barr, B.
Barsotti, L.
Barsuglia, M.
Barton, M. A.
Bartos, I.
Bassiri, R.
Bastarrika, M.
Basti, A.
Batch, J.
Bauchrowitz, J.
Bauer, Th. S.
Bebronne, M.
Beck, D.
Behnke, B.
Bejger, M.
Beker, M. G.
Bell, A. S.
Belopolski, I.
Benacquista, M.
Berliner, J. M.
Bertolini, A.
Betzwieser, J.
Beveridge, N.
Beyersdorf, P. T.
Bilenko, I. A.
Billingsley, G.
Birch, J.
Biswas, R.
Bitossi, M.
Bizouard, M. A.
Black, E.
Blackburn, J. K.
Blackburn, L.
Blair, D.
Bland, B.
Blom, M.
Bock, O.
Bodiya, T. P.
Bogan, C.
Bondarescu, R.
Bondu, F.
Bonelli, L.
Bonnand, R.
Bork, R.
Born, M.
Boschi, V.
Bose, S.
Bosi, L.
Bouhou, B.
Braccini, S.
Bradaschia, C.
Brady, P. R.
Braginsky, V. B.
Branchesi, M.
Brau, J. E.
Breyer, J.
Briant, T.
Bridges, D. O.
Brillet, A.
Brinkmann, M.
Brisson, V.
Britzger, M.
Brooks, A. F.
Brown, D. A.
Bulik, T.
Bulten, H. J.
Buonanno, A.
Burguet-Castell, J.
Buskulic, D.
Buy, C.
Byer, R. L.
Cadonati, L.
Calloni, E.
Camp, J. B.
Campsie, P.
Cannizzo, J.
Cannon, K.
Canuel, B.
Cao, J.
Capano, C. D.
Carbognani, F.
Carbone, L.
Caride, S.
Caudill, S.
Cavaglia, M.
Cavalier, F.
Cavalieri, R.
Cella, G.
Cepeda, C.
Cesarini, E.
Chaibi, O.
Chalermsongsak, T.
Charlton, P.
Chassande-Mottin, E.
Chelkowski, S.
Chen, W.
Chen, X.
Chen, Y.
Chincarini, A.
Chiummo, A.
Cho, H. S.
Chow, J.
Christensen, N.
Chua, S. S. Y.
Chung, C. T. Y.
Chung, S.
Ciani, G.
Clara, F.
Clark, D. E.
Clark, J.
Clayton, J. H.
Cleva, F.
Coccia, E.
Cohadon, P. -F.
Colacino, C. N.
Colas, J.
Colla, A.
Colombini, M.
Conte, A.
Conte, R.
Cook, D.
Corbitt, T. R.
Cordier, M.
Cornish, N.
Corsi, A.
Costa, C. A.
Coughlin, M.
Coulon, J. -P.
Couvares, P.
Coward, D. M.
Cowart, M.
Coyne, D. C.
Creighton, J. D. E.
Creighton, T. D.
Cruise, A. M.
Cumming, A.
Cunningham, L.
Cuoco, E.
Cutler, R. M.
Dahl, K.
Danilishin, S. L.
Dannenberg, R.
D'Antonio, S.
Danzmann, K.
Dattilo, V.
Daudert, B.
Daveloza, H.
Davier, M.
Daw, E. J.
Day, R.
Dayanga, T.
De Rosa, R.
DeBra, D.
Debreczeni, G.
Degallaix, J.
Del Pozzo, W.
del Prete, M.
Dent, T.
Dergachev, V.
DeRosa, R.
DeSalvo, R.
Dhurandhar, S.
Di Fiore, L.
Di Lieto, A.
Di Palma, I.
Emilio, M. Di Paolo
Di Virgilio, A.
Diaz, M.
Dietz, A.
Donovan, F.
Dooley, K. L.
Drago, M.
Drever, R. W. P.
Driggers, J. C.
Du, Z.
Dumas, J. -C.
Dwyer, S.
Eberle, T.
Edgar, M.
Edwards, M.
Effler, A.
Ehrens, P.
Endroczi, G.
Engel, R.
Etzel, T.
Evans, K.
Evans, M.
Evans, T.
Factourovich, M.
Fafone, V.
Fairhurst, S.
Fan, Y.
Farr, B. F.
Fazi, D.
Fehrmann, H.
Feldbaum, D.
Feroz, F.
Ferrante, I.
Fidecaro, F.
Finn, L. S.
Fiori, I.
Fisher, R. P.
Flaminio, R.
Flanigan, M.
Foley, S.
Forsi, E.
Forte, L. A.
Fotopoulos, N.
Fournier, J. -D.
Franc, J.
Franco, S.
Frasca, S.
Frasconi, F.
Frede, M.
Frei, M.
Frei, Z.
Freise, A.
Frey, R.
Fricke, T. T.
Friedrich, D.
Fritschel, P.
Frolov, V. V.
Fujimoto, M. -K.
Fulda, P. J.
Fyffe, M.
Gair, J.
Galimberti, M.
Gammaitoni, L.
Garcia, J.
Garufi, F.
Gaspar, M. E.
Gehrels, N.
Gemme, G.
Geng, R.
Genin, E.
Gennai, A.
Gergely, L. A.
Ghosh, S.
Giaime, J. A.
Giampanis, S.
Giardina, K. D.
Giazotto, A.
Gil-Casanova, S.
Gill, C.
Gleason, J.
Goetz, E.
Goggin, L. M.
Gonzalez, G.
Gorodetsky, M. L.
Gossler, S.
Gouaty, R.
Graef, C.
Graff, P. B.
Granata, M.
Grant, A.
Gras, S.
Gray, C.
Gray, N.
Greenhalgh, R. J. S.
Gretarsson, A. M.
Greverie, C.
Grosso, R.
Grote, H.
Grunewald, S.
Guidi, G. M.
Guido, C.
Gupta, R.
Gustafson, E. K.
Gustafson, R.
Ha, T.
Hallam, J. M.
Hammer, D.
Hammond, G.
Hanks, J.
Hanna, C.
Hanson, J.
Hardt, A.
Harms, J.
Harry, G. M.
Harry, I. W.
Harstad, E. D.
Hartman, M. T.
Haughian, K.
Hayama, K.
Hayau, J. -F.
Heefner, J.
Heidmann, A.
Heintze, M. C.
Heitmann, H.
Hello, P.
Hendry, M. A.
Heng, I. S.
Heptonstall, A. W.
Herrera, V.
Hewitson, M.
Hild, S.
Hoak, D.
Hodge, K. A.
Holt, K.
Holtrop, M.
Hong, T.
Hooper, S.
Hosken, D. J.
Hough, J.
Howell, E. J.
Hughey, B.
Husa, S.
Huttner, S. H.
Huynh-Dinh, T.
Ingram, D. R.
Inta, R.
Isogai, T.
Ivanov, A.
Izumi, K.
Jacobson, M.
James, E.
Jang, Y. J.
Jaranowski, P.
Jesse, E.
Johnson, W. W.
Jones, D. I.
Jones, G.
Jones, R.
Jonker, R. J. G.
Ju, L.
Kalmus, P.
Kalogera, V.
Kandhasamy, S.
Kang, G.
Kanner, J. B.
Kasturi, R.
Katsavounidis, E.
Katzman, W.
Kaufer, H.
Kawabe, K.
Kawamura, S.
Kawazoe, F.
Kelley, D.
Kells, W.
Keppel, D. G.
Keresztes, Z.
Khalaidovski, A.
Khalili, F. Y.
Khazanov, E. A.
Kim, B. K.
Kim, C.
Kim, H.
Kim, K.
Kim, N.
Kim, Y. M.
King, P. J.
Kinzel, D. L.
Kissel, J. S.
Klimenko, S.
Kokeyama, K.
Kondrashov, V.
Koranda, S.
Korth, W. Z.
Kowalska, I.
Kozak, D.
Kranz, O.
Kringel, V.
Krishnamurthy, S.
Krishnan, B.
Krolak, A.
Kuehn, G.
Kumar, P.
Kumar, R.
Kwee, P.
Lam, P. K.
Landry, M.
Lantz, B.
Lastzka, N.
Lawrie, C.
Lazzarini, A.
Leaci, P.
Lee, C. H.
Lee, H. K.
Lee, H. M.
Leong, J. R.
Leonor, I.
Leroy, N.
Letendre, N.
Li, J.
Li, T. G. F.
Liguori, N.
Lindquist, P. E.
Liu, Y.
Liu, Z.
Lockerbie, N. A.
Lodhia, D.
Lorenzini, M.
Loriette, V.
Lormand, M.
Losurdo, G.
Lough, J.
Luan, J.
Lubinski, M.
Lueck, H.
Lundgren, A. P.
Macdonald, E.
Machenschalk, B.
MacInnis, M.
Macleod, D. M.
Mageswaran, M.
Mailand, K.
Majorana, E.
Maksimovic, I.
Malvezzi, V.
Man, N.
Mandel, I.
Mandic, V.
Mantovani, M.
Marandi, A.
Marchesoni, F.
Marion, F.
Marka, S.
Marka, Z.
Markosyan, A.
Maros, E.
Marque, J.
Martelli, F.
Martin, I. W.
Martin, R. M.
Marx, J. N.
Mason, K.
Masserot, A.
Matichard, F.
Matone, L.
Matzner, R. A.
Mavalvala, N.
Mazzolo, G.
McCarthy, R.
McClelland, D. E.
McGuire, S. C.
McIntyre, G.
McIver, J.
McKechan, D. J. A.
McWilliams, S.
Meadors, G. D.
Mehmet, M.
Meier, T.
Melatos, A.
Melissinos, A. C.
Mendell, G.
Mercer, R. A.
Meshkov, S.
Messenger, C.
Meyer, M. S.
Miao, H.
Michel, C.
Milano, L.
Miller, J.
Minenkov, Y.
Mitrofanov, V. P.
Mitselmakher, G.
Mittleman, R.
Miyakawa, O.
Moe, B.
Mohan, M.
Mohanty, S. D.
Mohapatra, S. R. P.
Moraru, D.
Moreno, G.
Morgado, N.
Morgia, A.
Mori, T.
Morriss, S. R.
Mosca, S.
Mossavi, K.
Mours, B.
Mow-Lowry, C. M.
Mueller, C. L.
Mueller, G.
Mukherjee, S.
Mullavey, A.
Mueller-Ebhardt, H.
Munch, J.
Murphy, D.
Murray, P. G.
Mytidis, A.
Nash, T.
Naticchioni, L.
Necula, V.
Nelson, J.
Neri, I.
Newton, G.
Nguyen, T.
Nishizawa, A.
Nitz, A.
Nocera, F.
Nolting, D.
Normandin, M. E.
Nuttall, L.
Ochsner, E.
O'Dell, J.
Oelker, E.
Ogin, G. H.
Oh, J. J.
Oh, S. H.
O'Reilly, B.
O'Shaughnessy, R.
Osthelder, C.
Ott, C. D.
Ottaway, D. J.
Ottens, R. S.
Overmier, H.
Owen, B. J.
Page, A.
Palladino, L.
Palomba, C.
Pan, Y.
Pankow, C.
Paoletti, F.
Paoletti, R.
Papa, M. A.
Parisi, M.
Pasqualetti, A.
Passaquieti, R.
Passuello, D.
Patel, P.
Pedraza, M.
Peiris, P.
Pekowsky, L.
Penn, S.
Perreca, A.
Persichetti, G.
Phelps, M.
Pichot, M.
Pickenpack, M.
Piergiovanni, F.
Pietka, M.
Pinard, L.
Pinto, I. M.
Pitkin, M.
Pletsch, H. J.
Plissi, M. V.
Poggiani, R.
Poeld, J.
Postiglione, F.
Prato, M.
Predoi, V.
Prestegard, T.
Price, L. R.
Prijatelj, M.
Principe, M.
Privitera, S.
Prix, R.
Prodi, G. A.
Prokhorov, L. G.
Puncken, O.
Punturo, M.
Puppo, P.
Quetschke, V.
Quitzow-James, R.
Raab, F. J.
Rabeling, D. S.
Racz, I.
Radkins, H.
Raffai, P.
Rakhmanov, M.
Rankins, B.
Rapagnani, P.
Raymond, V.
Re, V.
Redwine, K.
Reed, C. M.
Reed, T.
Regimbau, T.
Reid, S.
Reitze, D. H.
Ricci, F.
Riesen, R.
Riles, K.
Robertson, N. A.
Robinet, F.
Robinson, C.
Robinson, E. L.
Rocchi, A.
Roddy, S.
Rodriguez, C.
Rodruck, M.
Rolland, L.
Rollins, J. G.
Romano, J. D.
Romano, R.
Romie, J. H.
Rosinska, D.
Roever, C.
Rowan, S.
Ruediger, A.
Ruggi, P.
Ryan, K.
Sainathan, P.
Salemi, F.
Sammut, L.
Sandberg, V.
Sannibale, V.
Santamaria, L.
Santiago-Prieto, I.
Santostasi, G.
Sassolas, B.
Sathyaprakash, B. S.
Sato, S.
Saulson, P. R.
Savage, R. L.
Schilling, R.
Schnabel, R.
Schofield, R. M. S.
Schreiber, E.
Schulz, B.
Schutz, B. F.
Schwinberg, P.
Scott, J.
Scott, S. M.
Seifert, F.
Sellers, D.
Sentenac, D.
Sergeev, A.
Shaddock, D. A.
Shaltev, M.
Shapiro, B.
Shawhan, P.
Shoemaker, D. H.
Sibley, A.
Siemens, X.
Sigg, D.
Singer, A.
Singer, L.
Sintes, A. M.
Skelton, G. R.
Slagmolen, B. J. J.
Slutsky, J.
Smith, J. R.
Smith, M. R.
Smith, R. J. E.
Smith-Lefebvre, N. D.
Somiya, K.
Sorazu, B.
Soto, J.
Speirits, F. C.
Sperandio, L.
Stefszky, M.
Stein, A. J.
Stein, L. C.
Steinert, E.
Steinlechner, J.
Steinlechner, S.
Steplewski, S.
Stochino, A.
Stone, R.
Strain, K. A.
Strigin, S. E.
Stroeer, A. S.
Sturani, R.
Stuver, A. L.
Summerscales, T. Z.
Sung, M.
Susmithan, S.
Sutton, P. J.
Swinkels, B.
Tacca, M.
Taffarello, L.
Talukder, D.
Tanner, D. B.
Tarabrin, S. P.
Taylor, J. R.
Taylor, R.
ter Braack, A. P. M.
Thomas, P.
Thorne, K. A.
Thorne, K. S.
Thrane, E.
Thuering, A.
Tokmakov, K. V.
Tomlinson, C.
Toncelli, A.
Tonelli, M.
Torre, O.
Torres, C.
Torrie, C. I.
Tournefier, E.
Tucker, E.
Travasso, F.
Traylor, G.
Tseng, K.
Ugolini, D.
Vahlbruch, H.
Vajente, G.
van den Brand, J. F. J.
Van den Broeck, C.
van der Putten, S.
van Veggel, A. A.
Vass, S.
Vasuth, M.
Vaulin, R.
Vavoulidis, M.
Vecchio, A.
Vedovato, G.
Veitch, J.
Veitch, P. J.
Veltkamp, C.
Verkindt, D.
Vetrano, F.
Vicere, A.
Villar, A. E.
Vinet, J. -Y.
Vitale, S.
Vocca, H.
Vorvick, C.
Vyatchanin, S. P.
Wade, A.
Wade, L.
Wade, M.
Waldman, S. J.
Wallace, L.
Wan, Y.
Wang, M.
Wang, X.
Wang, Z.
Wanner, A.
Ward, R. L.
Was, M.
Weinert, M.
Weinstein, A. J.
Weiss, R.
Wen, L.
Wessels, P.
West, M.
Westphal, T.
Wette, K.
Whelan, J. T.
Whitcomb, S. E.
White, D. J.
Whiting, B. F.
Wilkinson, C.
Willems, P. A.
Williams, L.
Williams, R.
Willke, B.
Winkelmann, L.
Winkler, W.
Wipf, C. C.
Wiseman, A. G.
Wittel, H.
Woan, G.
Wooley, R.
Worden, J.
Yakushin, I.
Yamamoto, H.
Yamamoto, K.
Yancey, C. C.
Yang, H.
Yeaton-Massey, D.
Yoshida, S.
Yu, P.
Yvert, M.
Zadrozny, A.
Zanolin, M.
Zendri, J. -P.
Zhang, F.
Zhang, L.
Zhang, W.
Zhao, C.
Zotov, N.
Zucker, M. E.
Zweizig, J.
Briggs, M. S.
Connaughton, V.
Hurley, K. C.
Jenke, P. A.
von Kienlin, A.
Rau, A.
Zhang, X. -L.
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.
C1 [Abadie, J.; Abbott, B. P.; Abbott, R.; Adhikari, R. X.; Ajith, P.; Anderson, S. B.; Arai, K.; Araya, M. C.; Barayoga, J. C. B.; Betzwieser, J.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cepeda, C.; Chalermsongsak, T.; Corsi, A.; Coyne, D. C.; Dannenberg, R.; Daudert, B.; Dergachev, V.; DeSalvo, R.; Driggers, J. C.; Ehrens, P.; Engel, R.; Etzel, T.; Fotopoulos, N.; Gustafson, E. K.; Hanna, C.; Heefner, J.; Heptonstall, A. W.; Hodge, K. A.; Ivanov, A.; Jacobson, M.; James, E.; Kalmus, P.; Kells, W.; Keppel, D. G.; King, P. J.; Kondrashov, V.; Korth, W. Z.; Kozak, D.; Lazzarini, A.; Lindquist, P. E.; Mageswaran, M.; Mailand, K.; Maros, E.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Nash, T.; Ogin, G. H.; Osthelder, C.; Patel, P.; Pedraza, M.; Phelps, M.; Price, L. R.; Privitera, S.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sannibale, V.; Santamaria, L.; Seifert, F.; Singer, A.; Singer, L.; Smith, M. R.; Stochino, A.; Taylor, R.; Torrie, C. I.; Vass, S.; Villar, A. E.; Wallace, L.; Weinstein, A. J.; Whitcomb, S. E.; Willems, P. A.; Williams, R.; Yamamoto, H.; Yeaton-Massey, D.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA.
[Abbott, T. D.; Smith, J. R.] Calif State Univ Fullerton, Fullerton, CA 92831 USA.
[Abernathy, M.; Barr, B.; Bassiri, R.; Bastarrika, M.; Bell, A. S.; Beveridge, N.; Campsie, P.; Cumming, A.; Cunningham, L.; Edgar, M.; Evans, K.; Gill, C.; Grant, A.; Gray, N.; Hammond, G.; Haughian, K.; Hendry, M. A.; Heng, I. S.; Hild, S.; Hough, J.; Huttner, S. H.; Jones, R.; Kumar, R.; Lawrie, C.; Macdonald, E.; Martin, I. W.; Murray, P. G.; Nelson, J.; Newton, G.; Pitkin, M.; Plissi, M. V.; Reid, S.; Robertson, N. A.; Rowan, S.; Santiago-Prieto, I.; Scott, J.; Sorazu, B.; Speirits, F. C.; Strain, K. A.; Torrie, C. I.; van Veggel, A. A.; Woan, G.] Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland.
[Accadia, T.; Bebronne, M.; Buskulic, D.; Dietz, A.; Gouaty, R.; Letendre, N.; Marion, F.; Masserot, A.; Mours, B.; Rolland, L.; Tournefier, E.; Verkindt, D.; Yvert, M.] Univ Savoie, CNRS, Lab Annecy le Vieux Phys Particules LAPP, IN2P3, F-74941 Annecy Le Vieux, France.
[Acernese, F.; Barone, F.; Calloni, E.; De Rosa, R.; Di Fiore, L.; Forte, L. A.; Garufi, F.; Milano, L.; Mosca, S.; Parisi, M.; Persichetti, G.; Romano, R.] Complesso Univ Monte S Angelo, INFN, Sez Napoli, I-80126 Naples, Italy.
[Acernese, F.; Barone, F.; Romano, R.] Univ Salerno, I-84084 Salerno, Italy.
[Adams, C.; Birch, J.; Bridges, D. O.; Cowart, M.; Evans, T.; Forsi, E.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Guido, C.; Hanson, J.; Holt, K.; Huynh-Dinh, T.; Katzman, W.; Kinzel, D. L.; Lormand, M.; Meyer, M. S.; Nolting, D.; O'Reilly, B.; Overmier, H.; Riesen, R.; Roddy, S.; Romie, J. H.; Sellers, D.; Sibley, A.; Stuver, A. L.; Thorne, K. A.; Torres, C.; Traylor, G.; Wooley, R.; Yakushin, I.] Livingston Observ, LIGO, Livingston, LA 70754 USA.
[Affeldt, C.; Allen, B.; Aufmuth, P.; Aulbert, C.; Bauchrowitz, J.; Bertolini, A.; Bock, O.; Bogan, C.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Dahl, K.; Danzmann, K.; Di Palma, I.; Eberle, T.; Fehrmann, H.; Frede, M.; Friedrich, D.; Goetz, E.; Gossler, S.; Graef, C.; Grote, H.; Hewitson, M.; Kaufer, H.; Kawazoe, F.; Khalaidovski, A.; Kim, H.; Kranz, O.; Kringel, V.; Kuehn, G.; Kwee, P.; Lastzka, N.; Leong, J. R.; Lueck, H.; Machenschalk, B.; Mazzolo, G.; Mehmet, M.; Meier, T.; Mossavi, K.; Mueller-Ebhardt, H.; Pickenpack, M.; Pletsch, H. J.; Poeld, J.; Prijatelj, M.; Prix, R.; Puncken, O.; Roever, C.; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schreiber, E.; Schulz, B.; Shaltev, M.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Taylor, J. R.; Thuering, A.; Vahlbruch, H.; Veltkamp, C.; Wanner, A.; Was, M.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Willke, B.; Winkelmann, L.; Winkler, W.; Wittel, H.; Yamamoto, K.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
[Affeldt, C.; Allen, B.; Aufmuth, P.; Aulbert, C.; Bauchrowitz, J.; Bertolini, A.; Bock, O.; Bogan, C.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Dahl, K.; Danzmann, K.; Di Palma, I.; Eberle, T.; Fehrmann, H.; Frede, M.; Friedrich, D.; Goetz, E.; Gossler, S.; Graef, C.; Grote, H.; Hewitson, M.; Kaufer, H.; Kawazoe, F.; Khalaidovski, A.; Kim, H.; Kranz, O.; Kringel, V.; Kuehn, G.; Kwee, P.; Lastzka, N.; Leong, J. R.; Lueck, H.; Machenschalk, B.; Mazzolo, G.; Mehmet, M.; Meier, T.; Mossavi, K.; Mueller-Ebhardt, H.; Pickenpack, M.; Pletsch, H. J.; Poeld, J.; Prijatelj, M.; Prix, R.; Puncken, O.; Roever, C.; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schreiber, E.; Schulz, B.; Shaltev, M.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Taylor, J. R.; Thuering, A.; Vahlbruch, H.; Veltkamp, C.; Wanner, A.; Was, M.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Willke, B.; Winkelmann, L.; Winkler, W.; Wittel, H.; Yamamoto, K.] Leibniz Univ Hannover, D-30167 Hannover, Germany.
[Agathos, M.; Bauer, Th. S.; Beker, M. G.; Blom, M.; Bulten, H. J.; Del Pozzo, W.; Jonker, R. J. G.; Li, T. G. F.; Maksimovic, I.; Rabeling, D. S.; ter Braack, A. P. M.; van den Brand, J. F. J.; Van den Broeck, C.; van der Putten, S.; Vitale, S.] NIKHEF H, NL-1009 DB Amsterdam, Netherlands.
[Agatsuma, K.; Fujimoto, M. -K.; Hayama, K.; Izumi, K.; Kawamura, S.; Miyakawa, O.; Mori, T.; Nishizawa, A.; Sato, S.] Natl Astron Observ Japan, Tokyo 1818588, Japan.
[Allen, B.; Ceron, E. Amador; Anderson, W. G.; Brady, P. R.; Clayton, J. H.; Creighton, J. D. E.; Giampanis, S.; Goggin, L. M.; Hammer, D.; Hughey, B.; Koranda, S.; Mercer, R. A.; Moe, B.; Ochsner, E.; O'Shaughnessy, R.; Papa, M. A.; Siemens, X.; Skelton, G. R.; Wade, L.; Wade, M.; Wiseman, A. G.; Yu, P.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Amariutei, D.; Arain, M. A.; Ciani, G.; Dooley, K. L.; Feldbaum, D.; Gleason, J.; Hartman, M. T.; Heintze, M. C.; Klimenko, S.; Liu, Z.; Martin, R. M.; Mitselmakher, G.; Mueller, C. L.; Mueller, G.; Mytidis, A.; Necula, V.; Ottens, R. S.; Pankow, C.; Reitze, D. H.; Sainathan, P.; Tanner, D. B.; Whiting, B. F.; Williams, L.] Univ Florida, Gainesville, FL 32611 USA.
[Aston, S. M.; Aylott, B. E.; Carbone, L.; Chelkowski, S.; Cruise, A. M.; Cutler, R. M.; Freise, A.; Fulda, P. J.; Hallam, J. M.; Kokeyama, K.; Lodhia, D.; Mandel, I.; Page, A.; Smith, R. J. E.; Vecchio, A.; Wang, M.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England.
[Astone, P.; Colla, A.; Conte, A.; Frasca, S.; Majorana, E.; Naticchioni, L.; Palomba, C.; Puppo, P.; Rapagnani, P.; Ricci, F.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy.
[Atkinson, D.; Barker, D.; Barton, M. A.; Batch, J.; Berliner, J. M.; Bland, B.; Clara, F.; Cook, D.; Flanigan, M.; Garcia, J.; Gray, C.; Hanks, J.; Ingram, D. R.; Kawabe, K.; Landry, M.; Lubinski, M.; McCarthy, R.; Mendell, G.; Moraru, D.; Moreno, G.; Raab, F. J.; Radkins, H.; Reed, C. M.; Rodruck, M.; Ryan, K.; Sandberg, V.; Savage, R. L.; Schwinberg, P.; Sigg, D.; Steinert, E.; Thomas, P.; Vorvick, C.; Wilkinson, C.; Worden, J.] Hanford Observ, LIGO, Richland, WA 99352 USA.
[Babak, S.; Behnke, B.; Grunewald, S.; Krishnan, B.; Leaci, P.; Papa, M. A.; Robinson, E. L.; Schutz, B. F.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany.
[Baker, P.; Cornish, N.] Montana State Univ, Bozeman, MT 59717 USA.
[Ballardin, G.; Canuel, B.; Carbognani, F.; Cavalieri, R.; Chiummo, A.; Colas, J.; Cuoco, E.; Dattilo, V.; Day, R.; Fiori, I.; Genin, E.; Marque, J.; Mohan, M.; Nocera, F.; Paoletti, F.; Pasqualetti, A.; Ruggi, P.; Sentenac, D.; Swinkels, B.; Tacca, M.] EGO, I-56021 Cascina, PI, Italy.
[Ballmer, S.; Brown, D. A.; Capano, C. D.; Couvares, P.; Kelley, D.; Kumar, P.; Lough, J.; Nitz, A.; Pekowsky, L.; Perreca, A.; Saulson, P. R.; West, M.] Syracuse Univ, Syracuse, NY 13244 USA.
[Barsotti, L.; Bodiya, T. P.; Corbitt, T. R.; Donovan, F.; Dwyer, S.; Evans, M.; Foley, S.; Fritschel, P.; Harry, G. M.; Katsavounidis, E.; Kissel, J. S.; MacInnis, M.; Mandel, I.; Mason, K.; Matichard, F.; Mavalvala, N.; Mittleman, R.; Oelker, E.; Shapiro, B.; Shoemaker, D. H.; Smith-Lefebvre, N. D.; Soto, J.; Stein, A. J.; Stein, L. C.; Vaulin, R.; Waldman, S. J.; Weiss, R.; Wipf, C. C.; Zucker, M. E.] MIT, LIGO, Cambridge, MA 02139 USA.
[Barsuglia, M.; Bouhou, B.; Buy, C.; Chassande-Mottin, E.; Granata, M.; Ward, R. L.] Univ Paris Diderot, CNRS IN2P3, Observ Paris, APC,CEA Irfu,Sorbonne Paris Cite, F-75205 Paris 13, France.
[Bartos, I.; Belopolski, I.; Factourovich, M.; Marka, S.; Marka, Z.; Matone, L.; McWilliams, S.; Murphy, D.; Redwine, K.] Columbia Univ, New York, NY 10027 USA.
[Basti, A.; Bitossi, M.; Bonelli, L.; Boschi, V.; Braccini, S.; Bradaschia, C.; Cella, G.; Colacino, C. N.; Di Lieto, A.; Di Virgilio, A.; Ferrante, I.; Fidecaro, F.; Frasconi, F.; Gennai, A.; Giazotto, A.; Mantovani, M.; Paoletti, F.; Paoletti, R.; Passaquieti, R.; Passuello, D.; Poggiani, R.; Toncelli, A.; Tonelli, M.; Torre, O.; Vajente, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Basti, A.; Bonelli, L.; Colacino, C. N.; Di Lieto, A.; Ferrante, I.; Fidecaro, F.; Passaquieti, R.; Poggiani, R.; Toncelli, A.; Tonelli, M.; Vajente, G.] Univ Pisa, I-56127 Pisa, Italy.
[Beck, D.; Byer, R. L.; Clark, D. E.; DeBra, D.; Herrera, V.; Kim, N.; Lantz, B.; Marandi, A.; Markosyan, A.; Tseng, K.] Stanford Univ, Stanford, CA 94305 USA.
[Bejger, M.; Rosinska, D.] CAMK PAN, PL-00716 Warsaw, Poland.
[Benacquista, M.; Biswas, R.; Creighton, T. D.; Daveloza, H.; Diaz, M.; Grosso, R.; Mohanty, S. D.; Morriss, S. R.; Mukherjee, S.; Normandin, M. E.; Quetschke, V.; Rakhmanov, M.; Romano, J. D.; Stone, R.; Stroeer, A. S.] Univ Texas Brownsville, Brownsville, TX 78520 USA.
[Benacquista, M.; Biswas, R.; Creighton, T. D.; Daveloza, H.; Diaz, M.; Grosso, R.; Mohanty, S. D.; Morriss, S. R.; Mukherjee, S.; Normandin, M. E.; Quetschke, V.; Rakhmanov, M.; Romano, J. D.; Stone, R.; Stroeer, A. S.] Texas Southmost Coll, Brownsville, TX 78520 USA.
[Beyersdorf, P. T.; Cordier, M.] San Jose State Univ, San Jose, CA 95192 USA.
[Bilenko, I. A.; Braginsky, V. B.; Danilishin, S. L.; Gorodetsky, M. L.; Khalili, F. Y.; Mitrofanov, V. P.; Prokhorov, L. G.; Strigin, S. E.; Vyatchanin, S. P.] Moscow MV Lomonosov State Univ, Moscow 119992, Russia.
[Bizouard, M. A.; Brisson, V.; Cavalier, F.; Davier, M.; Franco, S.; Hello, P.; Leroy, N.; Robinet, F.; Vavoulidis, M.; Was, M.] Univ Paris 11, LAL, IN2P3, CNRS, F-91898 Orsay, France.
[Blackburn, L.; Camp, J. B.; Cannizzo, J.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Blair, D.; Chen, X.; Chung, S.; Coward, D. M.; Dumas, J. -C.; Fan, Y.; Gras, S.; Hooper, S.; Howell, E. J.; Ju, L.; Susmithan, S.; Wen, L.; Whitcomb, S. E.; Zhao, C.] Univ Western Australia, Crawley, WA 6009, Australia.
[Bondarescu, R.; Finn, L. S.; Fisher, R. P.; Lundgren, A. P.; Owen, B. J.] Penn State Univ, University Pk, PA 16802 USA.
[Bondu, F.; Hayau, J. -F.] Univ Rennes 1, Inst Phys Rennes, CNRS, F-35042 Rennes, France.
[Bonnand, R.; Degallaix, J.; Flaminio, R.; Franc, J.; Galimberti, M.; Michel, C.; Morgado, N.; Pinard, L.; Sassolas, B.] CNRS, IN2P3, LMA, F-69622 Lyon, France.
[Bose, S.; Dayanga, T.; Steplewski, S.; Talukder, D.] Washington State Univ, Pullman, WA 99164 USA.
[Bosi, L.; Gammaitoni, L.; Marchesoni, F.; Neri, I.; Punturo, M.; Travasso, F.; Vocca, H.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Branchesi, M.; Guidi, G. M.; Lorenzini, M.; Losurdo, G.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] Ist Nazl Fis Nucl, Sez Firenze, I-50019 Sesto Fiorentino, Italy.
[Branchesi, M.; Cesarini, E.; Guidi, G. M.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] Univ Urbino Carlo Bo, I-61029 Urbino, Italy.
[Brau, J. E.; Frey, R.; Harstad, E. D.; Leonor, I.; Quitzow-James, R.; Schofield, R. M. S.] Univ Oregon, Eugene, OR 97403 USA.
[Briant, T.; Cohadon, P. -F.; Heidmann, A.] Univ Paris 06, UPMC, CNRS, Lab Kastler Brossel,ENS, F-75005 Paris, France.
[Brillet, A.; Chaibi, O.; Cleva, F.; Coulon, J. -P.; Fournier, J. -D.; Greverie, C.; Heitmann, H.; Man, N.; Pichot, M.; Regimbau, T.; Vinet, J. -Y.] Univ Nice Sophia Antipolis, Observ Cote Azur, CNRS, F-06304 Nice, France.
[Bulik, T.; Kowalska, I.] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland.
[Bulten, H. J.; Rabeling, D. S.; van den Brand, J. F. J.] Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands.
[Buonanno, A.; Kanner, J. B.; Pan, Y.; Shawhan, P.; Yancey, C. C.] Univ Maryland, College Pk, MD 20742 USA.
[Burguet-Castell, J.; Gil-Casanova, S.; Husa, S.; Sintes, A. M.] Univ Illes Balears, E-07122 Palma de Mallorca, Spain.
[Cadonati, L.; Hoak, D.; McIver, J.; Mohapatra, S. R. P.] Univ Massachusetts, Amherst, MA 01003 USA.
[Calloni, E.; De Rosa, R.; Garufi, F.; Milano, L.; Mosca, S.; Parisi, M.; Persichetti, G.] Univ Naples Federico II, I-80126 Naples, Italy.
[Cannon, K.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Cao, J.; Chen, W.; Du, Z.; Geng, R.; Li, J.; Liu, Y.; Wan, Y.; Wang, X.; Wang, Z.; Zhang, F.; Zhang, W.] Tsinghua Univ, Beijing 100084, Peoples R China.
[Caride, S.; Gustafson, R.; Meadors, G. D.; Riles, K.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Caudill, S.; Costa, C. A.; DeRosa, R.; Effler, A.; Fricke, T. T.; Giaime, J. A.; Gonzalez, G.; Johnson, W. W.; Slutsky, J.; Sung, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA.
[Cavaglia, M.; Rankins, B.] Univ Mississippi, University, MS 38677 USA.
[Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia.
[Chen, Y.; Hong, T.; Luan, J.; Miao, H.; Ott, C. D.; Somiya, K.; Thorne, K. S.; Wen, L.; Yang, H.] CALTECH, CaRT, Pasadena, CA 91125 USA.
[Chincarini, A.; Gemme, G.; Prato, M.] Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy.
[Cho, H. S.; Kim, Y. M.; Lee, C. H.] Pusan Natl Univ, Pusan 609735, South Korea.
[Chow, J.; Chua, S. S. Y.; Inta, R.; Lam, P. K.; McClelland, D. E.; Miller, J.; Mow-Lowry, C. M.; Mullavey, A.; Nguyen, T.; Scott, S. M.; Shaddock, D. A.; Slagmolen, B. J. J.; Stefszky, M.; Wade, A.] Australian Natl Univ, Canberra, ACT 0200, Australia.
[Christensen, N.; Coughlin, M.; Hardt, A.; Isogai, T.; Tucker, E.] Carleton Coll, Northfield, MN 55057 USA.
[Chung, C. T. Y.; Melatos, A.; Sammut, L.] Univ Melbourne, Parkville, Vic 3010, Australia.
[Clark, J.; Dent, T.; Edwards, M.; Fairhurst, S.; Harry, I. W.; Jones, G.; Macleod, D. M.; McKechan, D. J. A.; Messenger, C.; Nuttall, L.; Predoi, V.; Robinson, C.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.; Veitch, J.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales.
[Coccia, E.; D'Antonio, S.; Emilio, M. Di Paolo; Fafone, V.; Malvezzi, V.; Minenkov, Y.; Morgia, A.; Palladino, L.; Re, V.; Rocchi, A.; Sperandio, L.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, Rome, Italy.
[Coccia, E.; Fafone, V.; Morgia, A.; Re, V.; Sperandio, L.] Univ Roma Tor Vergata, I-00133 Rome, Italy.
[Colla, A.; Colombini, M.; Conte, A.; Frasca, S.; Naticchioni, L.; Rapagnani, P.; Ricci, F.] Univ Roma La Sapienza, I-00185 Rome, Italy.
[Conte, R.; Postiglione, F.] Univ Salerno, I-84084 Salerno, Italy.
[Conte, R.; Pinto, I. M.; Postiglione, F.; Principe, M.] Ist Nazl Fis Nucl, Sez Napoli, Naples, Italy.
[Daw, E. J.; Tomlinson, C.; White, D. J.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England.
[Debreczeni, G.; Endroczi, G.; Gaspar, M. E.; Racz, I.; Vasuth, M.] RMKI, WIGNER RCP, H-1121 Budapest, Hungary.
[del Prete, M.; Drago, M.; Liguori, N.; Prodi, G. A.; Yamamoto, K.] Univ Trent, I-38050 Trento, Italy.
[Dhurandhar, S.; Gupta, R.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Emilio, M. Di Paolo; Palladino, L.] Univ Aquila, I-67100 Laquila, Italy.
[Drago, M.; Liguori, N.; Prodi, G. A.] Ist Nazl Fis Nucl, Grp Collegato Trento, I-38050 Trento, Italy.
[Drever, R. W. P.; Harms, J.] CALTECH, Pasadena, CA 91125 USA.
[Farr, B. F.; Fazi, D.; Jang, Y. J.; Kalogera, V.; Krishnamurthy, S.; Raymond, V.; Rodriguez, C.] Northwestern Univ, Evanston, IL 60208 USA.
[Feroz, F.; Gair, J.; Graff, P. B.] Univ Cambridge, Cambridge CB2 1TN, England.
[Frei, M.; Matzner, R. A.] Univ Texas Austin, Austin, TX 78712 USA.
[Frei, M.; Peiris, P.; Whelan, J. T.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Frei, Z.; Raffai, P.] Eotvos Lorand Univ, H-1117 Budapest, Hungary.
[Gammaitoni, L.; Neri, I.; Travasso, F.] Univ Perugia, I-06123 Perugia, Italy.
[Gergely, L. A.; Keresztes, Z.] Univ Szeged, H-6720 Szeged, Hungary.
[Greenhalgh, R. J. S.; O'Dell, J.] Rutherford Appleton Lab, HSIC, Didcot OX11 0QX, Oxon, England.
[Gretarsson, A. M.; Jesse, E.; Vitale, S.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Ha, T.; Oh, J. J.; Oh, S. H.] Natl Inst Math Sci, Taejon 305390, South Korea.
[Hanna, C.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
[Holtrop, M.] Univ New Hampshire, Durham, NH 03824 USA.
[Hosken, D. J.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Jaranowski, P.; Pietka, M.] Bialystok Univ, PL-15424 Bialystok, Poland.
[Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Kandhasamy, S.; Mandic, V.; Prestegard, T.; Thrane, E.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Kang, G.; Kim, B. K.] Korea Inst Sci & Technol Informat, Taejon 305806, South Korea.
[Kasturi, R.; Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA.
[Khazanov, E. A.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia.
[Kim, C.] Lund Observ, SE-22100 Lund, Sweden.
[Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea.
[Krolak, A.] IM PAN, PL-00956 Warsaw, Poland.
[Krolak, A.; Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland.
[Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea.
[Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland.
[Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France.
[Mantovani, M.; Torre, O.] Univ Siena, I-53100 Siena, Italy.
[McGuire, S. C.] Southern Univ, Baton Rouge, LA 70813 USA.
[McGuire, S. C.] A&M Coll, Baton Rouge, LA 70813 USA.
[Melissinos, A. C.] Univ Rochester, Rochester, NY 14627 USA.
[Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy.
[Reed, T.; Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA.
[Rosinska, D.] Inst Astron, PL-65265 Zielona Gora, Poland.
[Santostasi, G.] McNeese State Univ, Lake Charles, LA 70609 USA.
[Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Taffarello, L.; Vedovato, G.; Zendri, J. -P.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[Yamamoto, K.] Univ Padua, I-35131 Padua, Italy.
[Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA.
[Briggs, M. S.; Connaughton, V.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Hurley, K. C.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Jenke, P. A.] Marshall Space Flight Ctr Huntsville, Huntsville, AL 35811 USA.
[von Kienlin, A.; Rau, A.; Zhang, X. -L.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
RP Abadie, J (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
RI Mow-Lowry, Conor/F-8843-2015; Finn, Lee Samuel/A-3452-2009; Sigg,
Daniel/I-4308-2015; Puppo, Paola/J-4250-2012; Tacca, Matteo/J-1599-2015;
Graef, Christian/J-3167-2015; Ottaway, David/J-5908-2015; Garufi,
Fabio/K-3263-2015; Neri, Igor/F-1482-2010; Shaddock, Daniel/A-7534-2011;
Postiglione, Fabio/O-4744-2015; Rocchi, Alessio/O-9499-2015; Martelli,
Filippo/P-4041-2015; Miao, Haixing/O-1300-2013; Khazanov,
Efim/B-6643-2014; Mitrofanov, Valery/D-8501-2012; Bilenko,
Igor/D-5172-2012; Nelson, John/H-7215-2014; Losurdo,
Giovanni/K-1241-2014; Danilishin, Stefan/K-7262-2012; Canuel,
Benjamin/C-7459-2014; Lee, Chang-Hwan/B-3096-2015; Khalili,
Farit/D-8113-2012; McClelland, David/E-6765-2010; Vecchio,
Alberto/F-8310-2015; Parisi, Maria/D-2817-2013; Steinlechner,
Sebastian/D-5781-2013; Strigin, Sergey/I-8337-2012; Colla,
Alberto/J-4694-2012; Drago, Marco/E-7134-2013; Vyatchanin,
Sergey/J-2238-2012; Re, Virginia /F-6403-2013; Gorodetsky,
Michael/C-5938-2008; Bell, Angus/E-7312-2011; Hild, Stefan/A-3864-2010;
Martin, Iain/A-2445-2010; Pitkin, Matthew/I-3802-2013; Prokhorov,
Leonid/I-2953-2012; Gammaitoni, Luca/B-5375-2009; Zhao,
Chunnong/C-2403-2013; Ju, Li/C-2623-2013; Lam, Ping Koy/A-5276-2008;
Marchesoni, Fabio/A-1920-2008; Allen, Bruce/K-2327-2012; prodi,
giovanni/B-4398-2010; Chen, Yanbei/A-2604-2013; Costa,
Cesar/G-7588-2012; CONTE, ANDREA/J-6667-2012; Vicere,
Andrea/J-1742-2012; Gemme, Gianluca/C-7233-2008; Punturo,
Michele/I-3995-2012; Strain, Kenneth/D-5236-2011; Ward,
Robert/I-8032-2014; Cesarini, Elisabetta/C-4507-2017; Chow,
Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Ciani, Giacomo/G-1036-2011;
Di Virgilio, Angela Dora Vittoria/E-9078-2015; Sergeev,
Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Branchesi,
Marica/P-2296-2015; Gehring, Tobias/A-8596-2016; Howell,
Eric/H-5072-2014; Heidmann, Antoine/G-4295-2016; Ott,
Christian/G-2651-2011; mosca, simona/I-7116-2012; Frasconi,
Franco/K-1068-2016; Pinto, Innocenzo/L-3520-2016; Ferrante,
Isidoro/F-1017-2012; Prato, Mirko/D-8531-2012; Travasso,
Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Cella,
Giancarlo/A-9946-2012
OI Finn, Lee Samuel/0000-0002-3937-0688; Sigg, Daniel/0000-0003-4606-6526;
Puppo, Paola/0000-0003-4677-5015; Tacca, Matteo/0000-0003-1353-0441;
Graef, Christian/0000-0002-4535-2603; Garufi, Fabio/0000-0003-1391-6168;
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;
Losurdo, Giovanni/0000-0003-0452-746X; Danilishin,
Stefan/0000-0001-7758-7493; Lee, Chang-Hwan/0000-0003-3221-1171;
McClelland, David/0000-0001-6210-5842; Vecchio,
Alberto/0000-0002-6254-1617; Steinlechner,
Sebastian/0000-0003-4710-8548; Gorodetsky, Michael/0000-0002-5159-2742;
Bell, Angus/0000-0003-1523-0821; Pitkin, Matthew/0000-0003-4548-526X;
Gammaitoni, Luca/0000-0002-4972-7062; Veitch, John/0000-0002-6508-0713;
Principe, Maria/0000-0002-6327-0628; Kanner, Jonah/0000-0001-8115-0577;
Zhao, Chunnong/0000-0001-5825-2401; Lam, Ping Koy/0000-0002-4421-601X;
Marchesoni, Fabio/0000-0001-9240-6793; Allen, Bruce/0000-0003-4285-6256;
prodi, giovanni/0000-0001-5256-915X; Vicere, Andrea/0000-0003-0624-6231;
Gemme, Gianluca/0000-0002-1127-7406; Punturo,
Michele/0000-0001-8722-4485; Strain, Kenneth/0000-0002-2066-5355;
Vitale, Salvatore/0000-0003-2700-0767; PERSICHETTI,
GIANLUCA/0000-0001-8424-9791; Freise, Andreas/0000-0001-6586-9901; Nitz,
Alexander/0000-0002-1850-4587; Mandel, Ilya/0000-0002-6134-8946;
Whiting, Bernard F/0000-0002-8501-8669; Murphy,
David/0000-0002-8538-815X; Zweizig, John/0000-0002-1521-3397; Del Pozzo,
Walter/0000-0003-3978-2030; O'Shaughnessy, Richard/0000-0001-5832-8517;
Gray, Norman/0000-0002-1941-9202; Granata, Massimo/0000-0003-3275-1186;
Di Paolo Emilio, Maurizio/0000-0002-9558-3610; Naticchioni,
Luca/0000-0003-2918-0730; Nishizawa, Atsushi/0000-0003-3562-0990;
calloni, enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515;
Sorazu, Borja/0000-0002-6178-3198; Bondu, Francois/0000-0001-6487-5197;
Boschi, Valerio/0000-0001-8665-2293; Papa,
M.Alessandra/0000-0002-1007-5298; Vocca, Helios/0000-0002-1200-3917;
Pinto, Innocenzo M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200;
Coccia, Eugenio/0000-0002-6669-5787; Vetrano,
Flavio/0000-0002-7523-4296; Husa, Sascha/0000-0002-0445-1971; Milano,
Leopoldo/0000-0001-9487-5876; Swinkels, Bas/0000-0002-3066-3601; Guidi,
Gianluca/0000-0002-3061-9870; Drago, Marco/0000-0002-3738-2431; Hallam,
Jonathan Mark/0000-0002-7087-0461; Ward, Robert/0000-0001-5503-5241;
Ricci, Fulvio/0000-0001-5475-4447; Vedovato,
Gabriele/0000-0001-7226-1320; Cesarini, Elisabetta/0000-0001-9127-3167;
Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636;
Ciani, Giacomo/0000-0003-4258-9338; Di Virgilio, Angela Dora
Vittoria/0000-0002-2237-7533; Jaranowski, Piotr/0000-0001-8085-3414;
Fairhurst, Stephen/0000-0001-8480-1961; Whelan,
John/0000-0001-5710-6576; Aulbert, Carsten/0000-0002-1481-8319; Stein,
Leo/0000-0001-7559-9597; Matichard, Fabrice/0000-0001-8982-8418;
Gehring, Tobias/0000-0002-4311-2593; Howell, Eric/0000-0001-7891-2817;
Heidmann, Antoine/0000-0002-0784-5175; Ott,
Christian/0000-0003-4993-2055; mosca, simona/0000-0001-7869-8275;
Frasconi, Franco/0000-0003-4204-6587; Ferrante,
Isidoro/0000-0002-0083-7228; Prato, Mirko/0000-0002-2188-8059; Travasso,
Flavio/0000-0002-4653-6156; Cella, Giancarlo/0000-0002-0752-0338
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
TC 1
Z9 1
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
TC 14
Z9 14
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 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
TC 59
Z9 59
U1 0
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD 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
TC 40
Z9 41
U1 1
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD 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
TC 8
Z9 8
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
TC 93
Z9 93
U1 1
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD 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
TC 54
Z9 54
U1 2
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD 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
TC 2
Z9 2
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 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
TC 3
Z9 3
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 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
TC 35
Z9 35
U1 0
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD 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
TC 16
Z9 17
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 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
TC 11
Z9 12
U1 4
U2 26
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
TC 8
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
TC 23
Z9 23
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
TC 29
Z9 33
U1 1
U2 61
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
TC 32
Z9 35
U1 3
U2 66
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 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
TC 4
Z9 4
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
TC 11
Z9 13
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
TC 2
Z9 2
U1 1
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 10
PY 2012
VL 759
IS 2
AR 102
DI 10.1088/0004-637X/759/2/102
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.
NR 46
TC 19
Z9 19
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 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).
NR 30
TC 10
Z9 10
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 124
DI 10.1088/0004-637X/759/2/124
PG 8
WC Astronomy & Astrophysics
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.
NR 51
TC 32
Z9 32
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 146
DI 10.1088/0004-637X/759/2/146
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.
NR 43
TC 22
Z9 22
U1 1
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD 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
TC 2
Z9 3
U1 1
U2 1
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD 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
TC 1
Z9 1
U1 2
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 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
TC 1
Z9 2
U1 0
U2 2
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD 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
TC 4
Z9 5
U1 2
U2 6
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 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
TC 2
Z9 2
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
TC 0
Z9 0
U1 2
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
TC 0
Z9 0
U1 0
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
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
TC 0
Z9 0
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
TC 7
Z9 7
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
TC 1
Z9 1
U1 1
U2 9
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD 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
TC 6
Z9 6
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
TC 31
Z9 31
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
TC 10
Z9 10
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
TC 29
Z9 30
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
TC 6
Z9 6
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
TC 6
Z9 6
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
TC 10
Z9 10
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
Z9 3
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
TC 11
Z9 11
U1 0
U2 7
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD 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
Z9 20
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
TC 3
Z9 3
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
TC 11
Z9 12
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].
NR 57
TC 10
Z9 10
U1 1
U2 14
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
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD NOV
PY 2012
VL 547
AR A55
DI 10.1051/0004-6361/201219765
PG 12
WC Astronomy & Astrophysics
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.
NR 26
TC 1
Z9 1
U1 0
U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD NOV
PY 2012
VL 547
AR A2
DI 10.1051/0004-6361/201219845
PG 6
WC Astronomy & Astrophysics
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.
NR 142
TC 17
Z9 17
U1 2
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 A108
DI 10.1051/0004-6361/201219142
PG 30
WC Astronomy & Astrophysics
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
TC 26
Z9 26
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
Z9 2
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
Z9 228
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
Z9 21
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
TC 78
Z9 78
U1 0
U2 8
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 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
TC 5
Z9 5
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD 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
Z9 0
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
TC 10
Z9 10
U1 0
U2 12
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 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
TC 24
Z9 24
U1 2
U2 9
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 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
TC 2
Z9 2
U1 2
U2 4
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 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
TC 60
Z9 60
U1 2
U2 13
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 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
TC 0
Z9 0
U1 1
U2 4
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
TC 13
Z9 13
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
TC 6
Z9 6
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 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
TC 148
Z9 148
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 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
TC 2
Z9 2
U1 0
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD 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
TC 92
Z9 92
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD 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
TC 31
Z9 31
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD 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
TC 5
Z9 5
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 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.
NR 60
TC 23
Z9 23
U1 0
U2 12
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD 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
TC 16
Z9 16
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 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
TC 44
Z9 45
U1 1
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD 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
TC 7
Z9 7
U1 1
U2 17
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 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
Z9 38
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
TC 0
Z9 0
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
TC 4
Z9 4
U1 0
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD 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.
NR 27
TC 4
Z9 4
U1 0
U2 4
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 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
TC 30
Z9 30
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD 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
TC 11
Z9 11
U1 0
U2 4
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 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
TC 7
Z9 7
U1 0
U2 4
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD 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
TC 6
Z9 6
U1 0
U2 7
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 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
TC 7
Z9 7
U1 1
U2 12
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD 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.
NR 128
TC 45
Z9 45
U1 2
U2 12
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD 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
TC 34
Z9 34
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD 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
TC 11
Z9 11
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD 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
TC 7
Z9 7
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
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.
NR 176
TC 20
Z9 20
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD NOV
PY 2012
VL 144
IS 5
AR 125
DI 10.1088/0004-6256/144/5/125
PG 43
WC Astronomy & Astrophysics
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.
NR 62
TC 10
Z9 10
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD NOV
PY 2012
VL 144
IS 5
AR 135
DI 10.1088/0004-6256/144/5/135
PG 16
WC Astronomy & Astrophysics
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.
NR 33
TC 7
Z9 7
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD NOV
PY 2012
VL 144
IS 5
AR 138
DI 10.1088/0004-6256/144/5/138
PG 11
WC Astronomy & Astrophysics
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 WIYN Observatory is a joint facility of the University
of Wisconsin-Madison, Indiana University, Yale University, and the
National Optical Astronomy Observatory. 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 43
TC 11
Z9 11
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD NOV 1
PY 2012
VL 759
IS 1
AR L23
DI 10.1088/2041-8205/759/1/L23
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 028XO
UT WOS:000310458900023
ER
PT J
AU Masiero, JR
Mainzer, AK
Grav, T
Bauer, JM
Cutri, RM
Nugent, C
Cabrera, MS
AF Masiero, Joseph R.
Mainzer, A. K.
Grav, T.
Bauer, J. M.
Cutri, R. M.
Nugent, C.
Cabrera, M. S.
TI PRELIMINARY ANALYSIS OF WISE/NEOWISE 3-BAND CRYOGENIC AND POST-CRYOGENIC
OBSERVATIONS OF MAIN BELT ASTEROIDS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE minor planets, asteroids: general
ID INFRARED-SURVEY-EXPLORER; NEOWISE
AB We present preliminary diameters and albedos for 13511 Main Belt asteroids (MBAs) that were observed during the 3-Band Cryo phase of the Wide-field Infrared Survey Explorer (WISE; after the outer cryogen tank was exhausted) and as part of the NEOWISE Post-Cryo Survey (after the inner cryogen tank was exhausted). With a reduced or complete loss of sensitivity in the two long wavelength channels of WISE, the uncertainty in our fitted diameters and albedos is increased to similar to 20% for diameter and similar to 40% for albedo. Diameter fits using only the 3.4 and 4.6 mu m channels are shown to be dependent on the literature optical H absolute magnitudes. These data allow us to increase the number of size estimates for large MBAs which have been identified as members of dynamical families. We present thermal fits for 14 asteroids previously identified as the parents of a dynamical family that were not observed during the fully cryogenic mission.
C1 [Masiero, Joseph R.; Mainzer, A. K.; Bauer, J. M.; Cabrera, M. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grav, T.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Bauer, J. M.; Cutri, R. M.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Nugent, C.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Cabrera, M. S.] Calif State Polytech Univ Pomona, Pomona, CA 91768 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 National Aeronautics and Space Administration; Planetary Science
Division of the National Aeronautics and Space Administration
FX J.R.M. was supported by an appointment to the NASA Post-doctoral Program
at JPL, administered by Oak Ridge Associated Universities through a
contract with NASA. We thank the anonymous referee for their helpful
comments. 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 14
TC 20
Z9 20
U1 0
U2 3
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 1
PY 2012
VL 759
IS 1
AR L8
DI 10.1088/2041-8205/759/1/L8
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 028XO
UT WOS:000310458900008
ER
PT J
AU Miller, JM
Raymond, J
Fabian, AC
Reynolds, CS
King, AL
Kallman, TR
Cackett, EM
van der Klis, M
Steeghs, DTH
AF Miller, J. M.
Raymond, J.
Fabian, A. C.
Reynolds, C. S.
King, A. L.
Kallman, T. R.
Cackett, E. M.
van der Klis, M.
Steeghs, D. T. H.
TI THE DISK-WIND-JET CONNECTION IN THE BLACK HOLE H 1743-322
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; black hole physics; X-rays: binaries
ID X-RAY; ACCRETION DISK; GRS 1915+105; MICROQUASAR H1743-322; UNIFIED
MODEL; HARD STATE; CYG X-1; SUZAKU; J1655-40; OUTBURST
AB X-ray disk winds are detected in spectrally soft, disk-dominated phases of stellar-mass black hole outbursts. In contrast, compact, steady, relativistic jets are detected in spectrally hard states that are dominated by non-thermal X-ray emission. Although these distinctive outflows appear to be almost mutually exclusive, it is possible that a disk wind persists in hard states but cannot be detected via X-ray absorption lines owing to very high ionization. Here, we present an analysis of a deep, 60 ks Chandra/HETGS observation of the black hole candidate H 1743-322 in the low/hard state. The spectrum shows no evidence of a disk wind, with tight limits, and within the range of ionizing flux levels that were measured in prior Chandra observations wherein a wind was clearly detected. In H 1743-322, at least, disk winds are actually diminished in the low/hard state, and disk winds and jets are likely state dependent and anti-correlated. These results suggest that although the launching radii of winds and jets may differ by orders of magnitude, they may both be tied to a fundamental property of the inner accretion flow, such as the mass accretion rate and/or the magnetic field topology of the disk. We discuss these results in the context of disk winds and jets in other stellar-mass black holes, and possible launching mechanisms for black hole outflows.
C1 [Miller, J. M.; King, A. L.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Raymond, J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England.
[Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Kallman, T. R.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA.
[Cackett, E. M.] Wayne State Univ, Dept Phys & Astron, Detroit, MI 48201 USA.
[van der Klis, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Steeghs, D. T. H.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
RP Miller, JM (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA.
EM jonmm@umich.edu
RI Steeghs, Danny/C-5468-2009; XRAY, SUZAKU/A-1808-2009
OI Steeghs, Danny/0000-0003-0771-4746;
FU NASA Earth and Space Sciences Fellowship; Chandra Guest Observer program
FX We thank the anonymous referee. We thank Harvey Tananbaum for executing
this observation. A. L. K. acknowledges support through the NASA Earth
and Space Sciences Fellowship. J.M.M. acknowledges support through the
Chandra Guest Observer program.
NR 35
TC 21
Z9 21
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD NOV 1
PY 2012
VL 759
IS 1
AR L6
DI 10.1088/2041-8205/759/1/L6
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 028XO
UT WOS:000310458900006
ER
PT J
AU Ditty, JG
Salas, JA
AF Ditty, James G.
Salas, Juan A.
TI MISIDENTIFICATION OF MYSIS STAGES OF XIPHOPENAEUS KROYERI (HELLER, 1862)
AND RIMAPENAEUS PEREZ-FARFANTE AND KENSLEY, 1997 (DECAPODA: PENAEIDAE)
IN THE WESTERN ATLANTIC
SO JOURNAL OF CRUSTACEAN BIOLOGY
LA English
DT Article
DE discrimination; dorsomedian carina; Penaeidae; Rimapenaeus;
Trachypenaeus; Trachysalambria; vestigial characters; Xiphopenaeus
ID TRACHYPENAEUS-CURVIROSTRIS STIMPSON; GULF-OF-MEXICO; LARVAL DEVELOPMENT;
SHRIMP; CRUSTACEA; PENAEOIDEA; PATTERNS
AB Studies in the western Atlantic have relied primarily on the key of Cook (1966) to identify and discriminate early life stages (ELS) of Xiphopenaeus kroyeri (Heller, 1862) and Rimapenaeus spp. Perez-Farfante and Kensley, 1997, even though larvae had not been reared successfully past the zoea phase at that time. We surveyed the penaeid literature for descriptions of reared mysis stages of X. kroyeri and Rimapenaeus, compared characters with those of Cook (1966), and found that Cook had reversed illustrations and criteria to discriminate taxa. We also examined plankton-collected mysis stages and identified new characters and previously unrecognized differences between taxa. Mysis stages of X. kroyeri have a slender median spine laterally near the posterior margin of pleomere five, not those of Rimapenaeus, although some early first myses of Rimapenaeus may have a vestigial spine laterally on pleomere five. Rimapenaeus has single dorsomedian spines on pleomeres four through six with the spine on pleomeres five and six >40% (usually about 50%) of fifth pleomere length as measured along the dorsal midline. Rimapenaeus lacks a pterygiostomial spine, although a spine on the distal margin of the developing antennal peduncle near the ventrolateral border of the carapace can be confused with a pterygiostomial spine. Xiphopenaeus kroyeri has a pterygiostomial spine and single dorsomedian spines on pleomeres four through six with the spine on pleomeres five and six <35% (usually about 25%) of fifth pleomere length. Xiphopenaeus kroyeri also has a gap about the width of one spine between the longest and adjacent outer pairs of furcal spines along the posterior margin of the telson, whereas Rimapenaeus has contiguous furcal spines. Differences in spine length dorsally on pleomeres five and six, and the presence or absence of a pterygiostomial spine should be used to discriminate taxa because the low hepatic spine and median spine laterally on pleomere five can be difficult to detect in X. kroyeri, even with a biological stain applied. Likely misidentification of mysis stages and possible overexploitation of X. kroyeri and Rimapenaeus spp. stocks in the western Atlantic emphasizes the need to re-assess information on ELS and the necessity of accurate identifications.
C1 [Ditty, James G.; Salas, Juan A.] NOAA, Natl Marine Fisheries Serv, Galveston, TX 77551 USA.
RP Ditty, JG (reprint author), NOAA, Natl Marine Fisheries Serv, 4700 Ave U, Galveston, TX 77551 USA.
EM Jim.Ditty@NOAA.gov
FU NOAA's Southeast Fisheries Science Center
FX Thanks to NOAA's Southeast Fisheries Science Center for funding support.
Thanks also to Dr. Geoffrey Matthews (retired), formerly of NOAA's
Galveston Laboratory, and to Shawn Hillen of NOAA's Galveston Laboratory
who participated in sample collection. Findings and conclusions of this
study are those of the authors and do not necessarily represent the
views of NOAA.
NR 57
TC 0
Z9 0
U1 3
U2 14
PU CRUSTACEAN SOC
PI SAN ANTONIO
PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA
SN 0278-0372
J9 J CRUSTACEAN BIOL
JI J. Crustac. Biol.
PD NOV
PY 2012
VL 32
IS 6
BP 931
EP 939
DI 10.1163/1937240X-00002097
PG 9
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 026EB
UT WOS:000310256000006
ER
PT J
AU Guimond, SR
Reisner, JM
AF Guimond, Stephen R.
Reisner, Jon M.
TI A Latent Heat Retrieval and Its Effects on the Intensity and Structure
Change of Hurricane Guillermo (1997). Part II: Numerical Simulations
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID TROPICAL CYCLONES; MICROPHYSICAL PROCESSES; MODEL SIMULATIONS; DATA
ASSIMILATION; MESOSCALE MODEL; SENSITIVITY; PREDICTION; EVOLUTION;
FIELDS; IMPACT
AB In Part I of this study, a new algorithm for retrieving the latent heat field in tropical cyclones from airborne Doppler radar was presented and fields from rapidly intensifying Hurricane Guillermo (1997) were shown. In Part II, the usefulness and relative accuracy of the retrievals is assessed by inserting the heating into realistic numerical simulations at 2-km resolution and comparing the generated wind structure to the radar analyses of Guillermo. Results show that using the latent heat retrievals as forcing produces very low intensity and structure errors (in terms of tangential wind speed errors and explained wind variance) and significantly improves simulations relative to a predictive run that is highly calibrated to the latent heat retrievals by using an ensemble Kalman filter procedure to estimate values of key model parameters.
Releasing all the heating/cooling in the latent heat retrieval results in a simulation with a large positive bias in Guillermo's intensity that motivates the need to determine the saturation state in the hurricane inner-core retrieval through a procedure similar to that described in Part I of this study. The heating retrievals accomplish high-quality structure statistics by forcing asymmetries in the wind field with the generally correct amplitude, placement, and timing. In contrast, the latent heating fields generated in the predictive simulation contain a significant bias toward large values and are concentrated in bands (rather than discrete cells) stretched around the vortex. The Doppler radar based latent heat retrievals presented in this series of papers should prove useful for convection initialization and data assimilation to reduce errors in numerical simulations of tropical cyclones.
C1 [Guimond, Stephen R.] Florida State Univ, Ctr Ocean Atmospher Predict Studies, Tallahassee, FL 32306 USA.
[Guimond, Stephen R.] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA.
[Reisner, Jon M.] Los Alamos Natl Lab, Los Alamos, NM USA.
RP Guimond, SR (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
EM stephen.guimond@nasa.gov
FU Los Alamos National Laboratory; NASA; NOAA
FX The first author would like to thank Dr. Paul Reasor and Dr. Matt Eastin
for providing their Doppler radar analysis of Guillermo. Thanks go to
Dr. Mark Bourassa and Dr. Robert Hart for several discussions on the
work and for their useful suggestions. Dr. Humberto Godinez is
acknowledged for providing the parameter estimates and output from his
EnKF work. Dr. Jason Sippel and Dr. Gerald Heymsfield also provided some
helpful comments. In addition, we thank all of the reviewers for their
constructive criticism. This research was supported by the Los Alamos
National Laboratory through a project entitled "Flash Before the Storm:
Predicting Hurricane Intensification Using LANL Lightning Data" with Dr.
Chris Jeffery, the PI. Financial support was also provided by a NASA
ocean vector winds contract and a NOAA grant to Dr. Mark Bourassa.
NR 31
TC 1
Z9 1
U1 2
U2 3
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD NOV
PY 2012
VL 69
IS 11
BP 3128
EP 3146
DI 10.1175/JAS-D-11-0201.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 031OU
UT WOS:000310652500003
ER
PT J
AU Chung, D
Matheou, G
Teixeira, J
AF Chung, D.
Matheou, G.
Teixeira, J.
TI Steady-State Large-Eddy Simulations to Study the Stratocumulus to
Shallow Cumulus Cloud Transition
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID MARINE BOUNDARY-LAYER; LOWER-TROPOSPHERIC STABILITY; SUBGRID-STRESS
MODEL; CONVECTION
AB This study presents a series of steady-state large-eddy simulations (LESs) to study the stratocumulus to shallow cumulus cloud transition. To represent the different stages of what can be interpreted as an Eulerian view of the transition, each simulation is assigned a unique sea surface temperature (SST) and run until statistically steady. The LES runs are identical in every other aspect. These idealized boundary-driven steady-state LESs allow for a simple parametric assessment of cloud-controlling factors in isolation from initial conditions and time-lag effects inherent in the Lagrangian view of the transition. The analysis of the thermodynamic energy budget reveals that, as the cloud regime transitions from stratocumulus to shallow cumulus, changes in the cloud radiative cooling term are balanced by changes in the subsidence warming term. This leads to a linear regression between the cloud fraction (CF) and an integral that scales, to a first-order approximation, as the lower-tropospheric stability (LTS). The study also considers the response of the boundary layer to a step change in SST that triggers the transition from stratocumulus to shallow cumulus. An examination of the time-lag conditional average centered on events when cumulus thermals are penetrating the stratocumulus deck suggests that the net effect of cumulus thermals in the transition is not to dry the stratocumulus deck but rather to moisten it. It is shown that the Gaussian probability density function (pdf) model of Sommeria and Deardorff describes the evolution of CF well during this step-change transition, suggesting that the systematic decrease in cloud cover is essentially associated with the mean drying of the air just below the cloud top.
C1 [Chung, D.; Matheou, G.; Teixeira, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Chung, D.] Univ Melbourne, Dept Mech Engn, Melbourne, Vic, Australia.
RP Chung, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM dchung@jpl.nasa.gov
RI Chung, Daniel/F-4468-2016
OI Chung, Daniel/0000-0003-3732-364X
FU Office of Naval Research [N0001408IP20064]; NASA MAP; NOAA MAPP/CPO
FX The authors acknowledge the support provided by the Office of Naval
Research, Marine Meteorology Program under Award N0001408IP20064; the
NASA MAP Program; and the NOAA MAPP/CPO Program. 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 31
TC 17
Z9 17
U1 0
U2 21
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD NOV
PY 2012
VL 69
IS 11
BP 3264
EP 3276
DI 10.1175/JAS-D-11-0256.1
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 031OU
UT WOS:000310652500010
ER
PT J
AU van Diedenhoven, B
Fridlind, AM
Ackerman, AS
Cairns, B
AF van Diedenhoven, Bastiaan
Fridlind, Ann M.
Ackerman, Andrew S.
Cairns, Brian
TI Evaluation of Hydrometeor Phase and Ice Properties in Cloud-Resolving
Model Simulations of Tropical Deep Convection Using Radiance and
Polarization Measurements
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID SINGLE-SCATTERING PROPERTIES; ANGULAR-DISTRIBUTION MODELS;
SATELLITE-BASED RETRIEVAL; RADIATIVE FLUX ESTIMATION; PARTICLE EFFECTIVE
RADIUS; SUPERCOOLED LIQUID WATER; ENERGY SYSTEM INSTRUMENT; M GOES-12
IMAGERY; CIRRUS CLOUDS; MICROPHYSICAL PROPERTIES
AB Satellite measurements are used to evaluate the glaciation, particle shape, and effective radius in cloud-resolving model simulations of tropical deep convection. Multidirectional polarized reflectances constrain the ice crystal geometry and the thermodynamic phase of the cloud tops, which in turn are used to calculate near-infrared reflectances so as to constrain the simulated ice effective radius, thereby avoiding inconsistencies between retrieval algorithms and model simulations. Liquid index values derived from Polarization and Directionality of the Earth's Reflectances (POLDER) measurements indicate only ice-topped clouds at brightness temperatures (BTs) lower than -40 degrees C, only liquid clouds at BT > -20 degrees C, and both phases occurring at temperatures in between. Liquid index values calculated from model simulations generally reveal too many ice-topped clouds at BT > -20 degrees C. The model assumption of platelike ice crystals with an aspect ratio of 0.7 is found consistent with POLDER measurements for BT < -40 degrees C when very rough ice crystals are assumed, leading to an asymmetry parameter of 0.74, whereas measurements indicate more extreme aspect ratios of similar to 0.15 at higher temperatures, yielding an asymmetry parameter of 0.84. MODIS-retrieved ice effective radii are found to be 18-28 mu m at BT < -40 degrees C, but biased low by about 5 mu m owing primarily to the assumption of pristine crystals in the retrieval. Simulated 2.13-mu m reflectances at BT < -40 degrees C are found to be about 0.05-0.1 too large compared to measurements, suggesting that model-simulated effective radii are 7-15 mu m too small. Two simulations with contrasting ice nucleation schemes showed little difference in simulated effective radii at BT < -40 degrees C, indicating that homogeneous nucleation is dominating in the simulations. Changes around -40 degrees C in satellite observations suggest a change in cloud-top ice shape and/or size in natural deep convection possibly related to a change in the freezing mechanism.
C1 [van Diedenhoven, Bastiaan] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
[van Diedenhoven, Bastiaan; Fridlind, Ann M.; Ackerman, Andrew S.; Cairns, Brian] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP van Diedenhoven, B (reprint author), Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10025 USA.
EM bastiaan.vandiedenhoven@nasa.gov
RI Ackerman, Andrew/D-4433-2012; van Diedenhoven, Bastiaan/A-2002-2013;
OI Ackerman, Andrew/0000-0003-0254-6253; van Diedenhoven,
Bastiaan/0000-0001-5622-8619; Cairns, Brian/0000-0002-1980-1022
FU National Aeronautics and Space Administration under NASA's Earth Science
Division [06-EO5/06-100]
FX This material is based on work supported by the National Aeronautics and
Space Administration under Grant 06-EO5/06-100 issued through the Earth
Observing System Program of NASA's Earth Science Division. AMF and ASA
received computational support from the DOE's National Energy Research
Scientific Computing Center, and the NASA Advanced Supercomputing
Division. The authors are grateful to Centre National d'Etudes Spatiales
(CNES) and NASA for providing the POLDER and MODIS data. We thank the
ICARE Data and Services Center for providing access to the POLDER data
used in this study. We are grateful for the contributions from three
anonymous reviewers.
NR 144
TC 18
Z9 18
U1 2
U2 15
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD NOV
PY 2012
VL 69
IS 11
BP 3290
EP 3314
DI 10.1175/JAS-D-11-0314.1
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 031OU
UT WOS:000310652500012
ER
PT J
AU Dhir, VK
Warrier, GR
Aktinol, E
Chao, D
Eggers, J
Sheredy, W
Booth, W
AF Dhir, Vijay Kumar
Warrier, Gopinath R.
Aktinol, Eduardo
Chao, David
Eggers, Jeffery
Sheredy, William
Booth, Wendell
TI Nucleate Pool Boiling Experiments (NPBX) on the International Space
Station
SO MICROGRAVITY SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Bubble dynamics; Nucleate boiling; Critical heat flux; Microgravity
ID REDUCED GRAVITY; HEAT-TRANSFER; MICROGRAVITY; DYNAMICS; SURFACE; BUBBLE;
WATER
AB During the period of March-May 2011, a series of boiling experiments was carried out in the Boiling Experimental Facility (BXF) located in the Microgravity Science Glovebox (MSG) of the International Space Station (ISS). The BXF Facility was carried to ISS on Space Shuttle Mission STS-133 on February 24, 2011. Nucleate Pool Boiling Experiment (NPBX) was one of the two experiments housed in the BXF. Results of experiments on single bubble dynamics (e.g., inception and growth), multiple bubble dynamics (lateral merger and departure, if any), nucleate pool boiling heat transfer, and critical heat flux are described. In the experiments Perfluoro-n-hexane was used as the test liquid. The system pressure was varied from 51 to 243 kPa, pool temperature was varied from 30 degrees to 59 degrees C, and test surface temperature was varied from 40 degrees to 80 degrees C. The test surface was a polished aluminum disc (1 mm thick, 89.5 mm in diameter) heated from below with strain gage heaters. Five cylindrical cavities were formed on the surface with four cavities located at the corners of a square and one in the middle. During experiments the magnitude of mean gravity level normal to the heater surface varied from 1.2 x 10 (-7)g (e) to 6 x 10 (-7)g (e) . The results of the experiments show that a single bubble continues to grow to occupy the size of the chamber without departing from the heater surface. During lateral merger of bubbles, at high superheats a large bubble may lift off from the surface but continues to hover near the surface. Neighboring bubbles are continuously pulled into the large bubble. At low superheats bubbles at neighboring sites simply merge to yield a larger bubble. The larger bubble mostly locates in the middle of the heated surface and serves as a vapor sink. The latter mode continues to persist when boiling is occurring all over the heater surface. Heat fluxes for steady state nucleate boiling and critical heat fluxes are found to be much lower than those obtained under earth normal gravity conditions. The data are useful for calibration of results of numerical simulations. Any correlations that are developed for nucleate boiling heat transfer under microgravity condition must account for the existence of vapor escape path (sink) from the heater, size of the heater, and the size and geometry of the chamber.
C1 [Dhir, Vijay Kumar; Warrier, Gopinath R.; Aktinol, Eduardo] Univ Calif Los Angeles, Henry Samueli Sch Engn & Appl Sci, Los Angeles, CA 90024 USA.
[Chao, David; Sheredy, William] NASA Glenn Res Ctr, Cleveland, OH USA.
[Eggers, Jeffery; Booth, Wendell] Zin Technol, Cleveland, OH USA.
RP Dhir, VK (reprint author), Univ Calif Los Angeles, Henry Samueli Sch Engn & Appl Sci, Los Angeles, CA 90024 USA.
EM vdhir@seas.ucla.edu
FU NASA Microgravity Fluid Physics Program
FX This work was initially supported under the NASA Microgravity Fluid
Physics Program.
NR 24
TC 11
Z9 11
U1 1
U2 36
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0938-0108
J9 MICROGRAVITY SCI TEC
JI Microgravity Sci. Technol.
PD NOV
PY 2012
VL 24
IS 5
BP 307
EP 325
DI 10.1007/s12217-012-9315-8
PG 19
WC Engineering, Aerospace; Thermodynamics; Mechanics
SC Engineering; Thermodynamics; Mechanics
GA 031FY
UT WOS:000310625900001
ER
PT J
AU David-Uraz, A
Moffat, AFJ
Chene, AN
Rowe, JF
Lange, N
Guenther, DB
Kuschnig, R
Matthews, JM
Rucinski, SM
Sasselov, D
Weiss, WW
AF David-Uraz, Alexandre
Moffat, Anthony F. J.
Chene, Andre-Nicolas
Rowe, Jason F.
Lange, Nicholas
Guenther, David B.
Kuschnig, Rainer
Matthews, Jaymie M.
Rucinski, Slavek M.
Sasselov, Dimitar
Weiss, Werner W.
TI Using MOST to reveal the secrets of the mischievous Wolf-Rayet binary CV
Ser
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: eclipsing; stars: mass-loss; stars: winds; outflows; stars:
Wolf-Rayet
ID COROTATING INTERACTION REGIONS; MASS-LOSS RATES; COLLIDING WINDS;
INFRARED PHOTOMETRY; SYSTEMATIC SEARCH; WC STARS; O-STARS; SERPENTIS;
VARIABILITY; METALLICITY
AB The WolfRayet (WR) binary CV Serpentis (= WR113, WC8d + O8-9IV) has been a source of mystery since it was shown that its atmospheric eclipses change with time over decades, in addition to its sporadic dust production. The first high-precision time-dependent photometric observations obtained with the Microvariability and Oscillations of STars (MOST) space telescope in 2009 show two consecutive eclipses over the 29-d orbit, with varying depths. A subsequent MOST run in 2010 showed a seemingly asymmetric eclipse profile. In order to help make sense of these observations, parallel optical spectroscopy was obtained from the Mont Megantic Observatory (2009, 2010) and from the Dominion Astrophysical Observatory (2009). Assuming these depth variations are entirely due to electron scattering in a beta-law wind, an unprecedented 62 per cent increase in M? is observed over one orbital period. Alternatively, no change in mass-loss rate would be required if a relatively small fraction of the carbon ions in the wind globally recombined and coaggulated to form carbon dust grains. However, it remains a mystery as to how this could occur. There also seems to be evidence for the presence of corotating interaction regions (CIR) in the WR wind: a CIR-like signature is found in the light curves, implying a potential rotation period for the WR star of 1.6?d. Finally, a new circular orbit is derived, along with constraints for the wind collision.
C1 [David-Uraz, Alexandre; Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[David-Uraz, Alexandre; Moffat, Anthony F. J.] Univ Montreal, Ctr Rech Astrophys Quebec, Montreal, PQ H3C 3J7, Canada.
[Chene, Andre-Nicolas] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Chene, Andre-Nicolas] Univ Valparaiso, Dept Fis & Astron, Fac Ciencias, Valparaiso, Chile.
[Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Lange, Nicholas] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada.
[Guenther, David B.] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada.
[Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Kuschnig, Rainer; Matthews, Jaymie M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, 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 David-Uraz, A (reprint author), Univ Montreal, Dept Phys, CP 6128,Succursale Ctr Ville, Montreal, PQ H3C 3J7, Canada.
EM alexandre@astro.umontreal.ca; moffat@astro.umontreal.ca
OI David-Uraz, Alexandre/0000-0003-4062-0776
FU Natural Sciences and Engineering Research Council of Canada; Le Fonds
quebecois de la recherche sur la nature et les technologies; Austrian
Space Agency; Austrian Science Fund; Chilean Centro de Astrofisica
FONDAP [15010003]; Chilean Centro de Excelencia en Astrofisica y
Tecnologias Afines (CATA); Comitee Mixto ESO-GOBIERNO DE CHILE
FX AD-U would like to acknowledge the help and support of his Universite de
Montreal colleagues, in particular N. St-Louis, R. Fahed, A. de la
Chevrotiere and S. Desforges, as well as D. Soutiere and S. Peloquin for
their help in acquiring part of the data. The Natural Sciences and
Engineering Research Council of Canada supports the research of DBG,
JMM, AFJM and SMR, while AFJM is also supported by Le Fonds quebecois de
la recherche sur la nature et les technologies. RK and WWW are supported
by the Austrian Space Agency and the Austrian Science Fund. A-NC
gratefully acknowledges support from the Chilean Centro de Astrofisica
FONDAP No. 15010003 and the Chilean Centro de Excelencia en Astrofisica
y Tecnologias Afines (CATA) and Comitee Mixto ESO-GOBIERNO DE CHILE.
NR 41
TC 5
Z9 5
U1 0
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2012
VL 426
IS 3
BP 1720
EP 1730
DI 10.1111/j.1365-2966.2012.21736.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 023VE
UT WOS:000310063900003
ER
PT J
AU Roseboom, IG
Bunker, A
Sumiyoshi, M
Wang, L
Dalton, G
Akiyama, M
Bock, J
Bonfield, D
Buat, V
Casey, C
Chapin, E
Clements, DL
Conley, A
Curtis-Lake, E
Cooray, A
Dunlop, JS
Farrah, D
Ham, SJ
Ibar, E
Iwamuro, F
Kimura, M
Lewis, I
Macaulay, E
Magdis, G
Maihara, T
Marsden, G
Mauch, T
Moritani, Y
Ohta, K
Oliver, SJ
Page, MJ
Schulz, B
Scott, D
Symeonidis, M
Takato, N
Tamura, N
Totani, T
Yabe, K
Zemcov, M
AF Roseboom, I. G.
Bunker, A.
Sumiyoshi, M.
Wang, L.
Dalton, G.
Akiyama, M.
Bock, J.
Bonfield, D.
Buat, V.
Casey, C.
Chapin, E.
Clements, D. L.
Conley, A.
Curtis-Lake, E.
Cooray, A.
Dunlop, J. S.
Farrah, D.
Ham, S. J.
Ibar, E.
Iwamuro, F.
Kimura, M.
Lewis, I.
Macaulay, E.
Magdis, G.
Maihara, T.
Marsden, G.
Mauch, T.
Moritani, Y.
Ohta, K.
Oliver, S. J.
Page, M. J.
Schulz, B.
Scott, Douglas
Symeonidis, M.
Takato, N.
Tamura, N.
Totani, T.
Yabe, K.
Zemcov, M.
TI FMOS near-IR spectroscopy of Herschel-selected galaxies: star formation
rates, metallicity and dust attenuation at z similar to 1
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: evolution; submillimetre: galaxies
ID VLT DEEP SURVEY; FAR-INFRARED PROPERTIES; HIGH-REDSHIFT GALAXIES;
DIGITAL SKY SURVEY; FORMING GALAXIES; MASS-METALLICITY; EXTRAGALACTIC
SURVEY; STELLAR MASS; H-ALPHA; PHOTOMETRIC REDSHIFTS
AB We investigate the properties (e.g. star formation rate, dust attenuation, stellar mass and metallicity) of a sample of infrared (IR) luminous galaxies at z similar to 1 via near-IR spectroscopy with Subaru-FMOS. Our sample consists of Herschel SPIRE and Spitzer MIPS selected sources in the COSMOS field with photometric redshifts in the range of 0.7 < zphot < 1.8, which have been targeted in two pointings (0.5 deg2) with FMOS. We find a modest success rate for emission-line detections, with candidate Ha emission lines detected for 57 of 168 SPIRE sources (34 per cent). By stacking the near-IR spectra we directly measure the mean Balmer decrement for the Ha and H beta lines, finding a value of < E(B - V)> = 0.51 +/- 0.27 for < LIR > = 1012L circle dot sources at < z > = 1.36. By comparing star formation rates estimated from the IR and from the dust-uncorrected Ha line we find a strong relationship between dust attenuation and star formation rate. This relation is broadly consistent with that previously seen in star-forming galaxies at z similar to 0.1. Finally, we investigate the metallicity via the N2 ratio, finding that z similar to 1 IR-selected sources are indistinguishable from the local massmetallicity relation. We also find a strong correlation between dust attenuation and metallicity, with the most metal-rich IR sources experiencing the largest levels of dust attenuation.
C1 [Roseboom, I. G.; Curtis-Lake, E.; Dunlop, J. S.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Roseboom, I. G.; Wang, L.; Farrah, D.; Oliver, S. J.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
[Bunker, A.; Dalton, G.; Ham, S. J.; Lewis, I.; Macaulay, E.; Magdis, G.; Mauch, T.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Sumiyoshi, M.; Iwamuro, F.; Maihara, T.; Moritani, Y.; Ohta, K.; Totani, T.; Yabe, K.] Kyoto Univ, Dept Astron, Fac Sci, Kyoto 6068502, Japan.
[Dalton, G.] Rutherford Appleton Lab, RALSpace, Didcot OX11 0QX, Oxon, England.
[Akiyama, M.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
[Bock, J.; Schulz, B.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bonfield, D.; Mauch, T.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Buat, V.] Univ Aix Marseille, Lab Astrophys Marseille, CNRS, OAMP, F-13388 Marseille 13, France.
[Casey, C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Casey, C.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA.
[Chapin, E.; Marsden, G.; Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Kimura, M.; Takato, N.; Tamura, N.] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Page, M. J.; Symeonidis, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Schulz, B.] CALTECH, Ctr Infrared Proc & Anal, JPL, Pasadena, CA 91125 USA.
RP Roseboom, IG (reprint author), Univ Edinburgh, Royal Observ, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland.
EM igr@roe.ac.uk
RI Oliver, Seb/A-2479-2013; Magdis, Georgios/C-7295-2014;
OI Casey, Caitlin/0000-0002-0930-6466; Oliver, Seb/0000-0001-7862-1032;
Magdis, Georgios/0000-0002-4872-2294; Scott, Douglas/0000-0002-6878-9840
FU Science and Technology Facilities Council [ST/F002858/1, ST/I000976/1];
Royal Society; European Research Council; ESO Paranal Observatory
[LP175.A-0839]; Alfred P. Sloan Foundation; National Science Foundation;
US Department of Energy; National Aeronautics and Space Administration;
Japanese Monbukagakusho; Max Planck Society; Higher Education Funding
Council for England; American Museum of Natural History; Astrophysical
Institute Potsdam; University of Basel; University of Cambridge; Case
Western Reserve University; University of Chicago; Drexel University;
Fermilab; Institute for Advanced Study; Japan Participation Group; Johns
Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli
Institute for Particle Astrophysics and Cosmology; Korean Scientist
Group; Chinese Academy of Sciences (LAMOST); Los Alamos National
Laboratory; Max-Planck-Institute for Astronomy (MPIA);
Max-Planck-Institute for Astrophysics (MPA); New Mexico State
University; Ohio State University; University of Pittsburgh; University
of Portsmouth; Princeton University; United States Naval Observatory;
University of Washington; CSA (Canada); NAOC (China); CEA (France); CNES
(France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC
(UK); UKSA (UK); NASA (USA); STFC
FX IGR, SJO and LW acknowledge support from the Science and Technology
Facilities Council (grant Nos ST/F002858/1 and ST/I000976/1).; JSD
acknowledges the support of the Royal Society via a Wolfson Research
Merit award and the support of the European Research Council via the
award of an Advanced Grant.; Based on zCOSMOS observations carried out
using the Very Large Telescope at the ESO Paranal Observatory under
Programme ID: LP175.A-0839.; Funding for the SDSS and SDSS-II has been
provided by the Alfred P. Sloan Foundation, the Participating
Institutions, the National Science Foundation, the US Department of
Energy, the National Aeronautics and Space Administration, the Japanese
Monbukagakusho, the Max Planck Society and the Higher Education Funding
Council for England. The SDSS website is http://www.sdss.org/.; The SDSS
is managed by the Astrophysical Research Consortium for the
Participating Institutions. The Participating Institutions are the
American Museum of Natural History, Astrophysical Institute Potsdam,
University of Basel, University of Cambridge, Case Western Reserve
University, University of Chicago, Drexel University, Fermilab, the
Institute for Advanced Study, the Japan Participation Group, Johns
Hopkins University, the Joint Institute for Nuclear Astrophysics, the
Kavli Institute for Particle Astrophysics and Cosmology, the Korean
Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos
National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the
Max-Planck-Institute for Astrophysics (MPA), New Mexico State
University, Ohio State University, University of Pittsburgh, University
of Portsmouth, Princeton University, the United States Naval Observatory
and the University of Washington.; SPIRE has been developed by a
consortium of institutes led by Cardiff University (UK) including
University of Lethbridge (Canada); NAOC (China); CEA, LAM (France);
IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory
(Sweden); Imperial College London, RAL, UCL-MSSL, UK ATC, University of
Sussex (UK); and Caltech, JPL, NHSC, University of Colorado (USA). This
development has been supported by national funding agencies: CSA
(Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN
(Spain); SNSB (Sweden); STFC and UKSA (UK); and NASA (USA).; FMOS was
funded jointly by STFC and the Japanese Monbukagakusho, and we
gratefully acknowledge the support of the staff at the Subaru Telescope
throughout the instrument commissioning phase.
NR 70
TC 20
Z9 20
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2012
VL 426
IS 3
BP 1782
EP 1792
DI 10.1111/j.1365-2966.2012.21777.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 023VE
UT WOS:000310063900007
ER
PT J
AU Prokhorov, DA
Million, ET
Akahori, T
Zemcov, M
Moraghan, A
Nagataki, S
Yoshikawa, K
Colafrancesco, S
Rawle, TD
Egami, E
AF Prokhorov, D. A.
Million, E. T.
Akahori, T.
Zemcov, M.
Moraghan, A.
Nagataki, S.
Yoshikawa, K.
Colafrancesco, S.
Rawle, T. D.
Egami, E.
TI A high-resolution study of the X-ray emission and Sunyaev-Zel'dovich
effect in the Bullet cluster (1E 0657-56)
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: clusters: individual: 1E 0657-56
ID GALAXY CLUSTERS; RELATIVISTIC CORRECTIONS; COMPTONIZATION; ELECTRONS;
RADIATION; HALO; GAS
AB High-resolution imaging of the SunyaevZel'dovich (SZ) effect opens new possibilities for testing the presence of various high-energy particle populations in clusters of galaxies. A detailed X-ray analysis of the Bullet cluster (1E 0657-56) with Chandra has revealed the presence of additional X-ray spectral components beyond a simple, single-temperature plasma in its X-ray spectra. X-ray methods alone are insufficient to elucidate the origins of these spectral components. We show that the morphology and magnitude of the SZ effect at high frequencies are critically dependent upon the mechanism by which the additional X-ray spectra are created. We examine the differences between the predicted SZ effect emission maps at 600?GHz assuming the X-ray spectra are composed of thermal gas with a steep power-law index component and also thermal gas with a significant contribution of strongly heated gas. A two-temperature model with a hot (kT ? 3040?keV) second component is the most consistent with existing SZ data at high frequencies. However, significant morphological differences remain. High-angular-resolution SZ intensity maps at high frequencies in combination with deep X-ray data provide a new window into understanding particle energization processes in the hottest, massive merging galaxy clusters.
C1 [Prokhorov, D. A.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Million, E. T.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Akahori, T.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Zemcov, M.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Moraghan, A.] Yonsei Univ, Dept Astron, Seoul 120749, South Korea.
[Moraghan, A.] Yonsei Univ, Ctr Galaxy Evolut Res, Seoul 120749, South Korea.
[Nagataki, S.] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan.
[Yoshikawa, K.] Univ Tsukuba, Ctr Computat Sci, Tsukuba, Ibaraki 3058577, Japan.
[Colafrancesco, S.] Univ Witwatersrand, Sch Phys, ZA-2050 Johannesburg, South Africa.
[Colafrancesco, S.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Rawle, T. D.; Egami, E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Prokhorov, DA (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
EM phdmitry@stanford.edu; emillion@bama.ua.edu
FU Yonsei University; Korea Astronomy and Space Science Institute; National
Research Foundation of Korea; South African Research Chairs Initiative
of the Department of Science and Technology; National Research
Foundation; Square Kilometre Array (SKA); Korea Research Council of
Fundamental Science and Technology (KRCF)
FX AM acknowledges support from the Yonsei University Research Fund 2011
and 2012, the Korea Astronomy and Space Science Institute Research Fund
2012 and support by the National Research Foundation of Korea to the
Center for Galaxy Evolution Research. SC acknowledges support by the
South African Research Chairs Initiative of the Department of Science
and Technology and National Research Foundation and by the Square
Kilometre Array (SKA). TA acknowledges the support of the Korea Research
Council of Fundamental Science and Technology (KRCF).
NR 41
TC 1
Z9 1
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2012
VL 426
IS 3
BP 2291
EP 2299
DI 10.1111/j.1365-2966.2012.21842.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 023VE
UT WOS:000310063900044
ER
PT J
AU de Mello, DF
Urrutia-Viscarra, F
de Oliveira, CM
Torres-Flores, S
Carrasco, ER
Cypriano, E
AF de Mello, D. F.
Urrutia-Viscarra, F.
Mendes de Oliveira, C.
Torres-Flores, S.
Carrasco, E. R.
Cypriano, E.
TI Star formation in H I tails: HCG 92, HCG 100 and six interacting systems
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: interactions; intergalactic medium; galaxies: star clusters:
general; galaxies: star formation
ID TIDAL DWARF GALAXIES; STEPHANS QUINTET; COMPACT-GROUPS; EMISSION;
CLUSTERS; NGC-3079; STELLAR; REGIONS; OBJECTS; DUST
AB We present new Gemini spectra of 14 new objects found within the H?i tails of Hickson Compact Groups (HCGs) 92 and 100. Nine of them are Galaxy Evolution Explorer (GALEX) far-ultraviolet (FUV) and near-ultraviolet (NUV) sources. The spectra confirm that these objects are members of the compact groups and have metallicities close to solar, with an average value of 12+log(O/H) similar to 8.5. They have average FUV luminosities 7 x 10(40)?erg?s-1 and very young ages (<100?Myr), and two of them resemble tidal dwarf galaxy (TDG) candidates. We suggest that they were created within gas clouds that were ejected during galaxygalaxy interactions into the intergalactic medium, which would explain the high metallicities of the objects, inherited from the parent galaxies from which the gas originated. We conduct a search for similar objects in six interacting systems with extended H?i tails: NGC 2623, NGC 3079, NGC 3359, NGC 3627, NGC 3718 and NGC 4656. We found 35 ultraviolet (UV) sources with ages < 100?Myr; however, most of them are on average less luminous/massive than the UV sources found around HCG 92 and HCG 100. We speculate that this might be an environmental effect and that compact groups of galaxies are more favourable to TDG formation than other interacting systems.
C1 [de Mello, D. F.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[de Mello, D. F.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Urrutia-Viscarra, F.; Mendes de Oliveira, C.; Cypriano, E.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Dept Astron, BR-05508090 Sao Paulo, Brazil.
[Torres-Flores, S.] Univ La Serena, Dept Fis, La Serena, Chile.
[Carrasco, E. R.] So Operat Ctr, Gemini Observ AURA, La Serena, Chile.
RP de Mello, DF (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
EM demello@cua.edu
RI Cypriano, Eduardo/C-7293-2012; 7, INCT/H-6207-2013; Astrofisica,
Inct/H-9455-2013; Mendes de Oliveira, Claudia/F-2391-2012
OI Mendes de Oliveira, Claudia/0000-0002-7736-4297
FU NASA [NNG06GG45G, NNG06GG59G, NAS5-26555]; FAPESP [2007/06436-4,
2006/56213-9, 2007/07973-3]; CNPq; CAPES; FONDECYT (Chile) [3110087];
NASA Office of Space Science [NAG5-7584]
FX We are grateful to an anonymous referee for helpful comments and
suggestions. DFdM was funded by NASA Research grants NNG06GG45G and
NNG06GG59G. FU-V acknowledges the financial support of FAPESP through an
M.Sc. Fellowship, under contract 2007/06436-4. CMdO acknowledges support
from Brazilian agencies FAPESP (projeto tematico 2006/56213-9), CNPq and
CAPES. STDF acknowledges the financial support of FONDECYT (Chile)
through a post-doctoral position, under contract 3110087, and FAPESP
through the Doctoral position, under contract 2007/07973-3. 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. Some of the data presented in this paper were obtained
from the MAST. STScI is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for
MAST for non-HST data is provided by the NASA Office of Space Science
via grant NAG5-7584 and by other grants and contracts.
NR 55
TC 5
Z9 5
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2012
VL 426
IS 3
BP 2441
EP 2451
DI 10.1111/j.1365-2966.2012.21429.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 023VE
UT WOS:000310063900055
ER
PT J
AU Hoyt, D
AF Hoyt, Diana
TI The Innovation Master Plan: The CEO's Guide to Innovation, vol 2
SO RESEARCH-TECHNOLOGY MANAGEMENT
LA English
DT Book Review
C1 [Hoyt, Diana] NASA, Off Chief Technologist, Washington, DC 20546 USA.
RP Hoyt, D (reprint author), NASA, Off Chief Technologist, Washington, DC 20546 USA.
EM diana.hoyt@nasa.gov
NR 2
TC 0
Z9 0
U1 0
U2 2
PU INDUSTRIAL RESEARCH INST, INC
PI ARLINGTON
PA 2200 CLARENDON BLVD, STE 1102, ARLINGTON, VA 22201 USA
SN 0895-6308
J9 RES TECHNOL MANAGE
JI Res.-Technol. Manage.
PD NOV-DEC
PY 2012
VL 55
IS 6
BP 68
EP 69
PG 2
WC Business; Engineering, Industrial; Management
SC Business & Economics; Engineering
GA 030GT
UT WOS:000310559700014
ER
PT J
AU Potter, C
Klooster, S
Genovese, V
AF Potter, Christopher
Klooster, Steven
Genovese, Vanessa
TI Net primary production of terrestrial ecosystems from 2000 to 2009
SO CLIMATIC CHANGE
LA English
DT Article
ID DROUGHT-INDUCED REDUCTION; GROSS PRIMARY PRODUCTION; SATELLITE DATA;
TROPICAL FORESTS; CARBON; CLIMATE; MODIS; MODEL; SIMULATION; PARAMETERS
AB The CASA (Carnegie-Ames-Stanford) ecosystem model has been used to estimate monthly carbon fluxes in terrestrial ecosystems from 2000 to 2009, with global data inputs from NASA's Terra Moderate Resolution Imaging Spectroradiometer (MODIS) vegetation cover mapping. Net primary production (NPP) flux for atmospheric carbon dioxide has varied slightly from year-to-year, but was predicted to have increased over short multi-year periods in the regions of the high-latitude Northern Hemisphere, South Asia, Central Africa, and the western Amazon since the year 2000. These CASA results for global NPP were found to be in contrast to other recently published modeling trends for terrestrial NPP with high sensitivity to regional drying patterns. Nonetheless, periodic declines in regional NPP were predicted by CASA for the southern and western Untied States, the southern Amazon, and southern and eastern Africa. NPP in tropical forest zones was examined in greater detail to discover lower annual production values than previously reported in many global models across the tropical rainforest zones, likely due to the enhanced detection of lower production ecosystems replacing primary rainforest.
C1 [Potter, Christopher] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Klooster, Steven; Genovese, Vanessa] Calif State Univ Monterey Bay, Seaside, CA USA.
RP Potter, C (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM chris.potter@nasa.gov
FU Planetary Skin Institute; NASA
FX This work was supported by the Planetary Skin Institute and grants from
NASA programs in Carbon Cycle Science and the Large-scale
Biosphere-Atmosphere Experiment in Amazonia (LBA),
NR 38
TC 23
Z9 24
U1 8
U2 94
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0165-0009
EI 1573-1480
J9 CLIMATIC CHANGE
JI Clim. Change
PD NOV
PY 2012
VL 115
IS 2
BP 365
EP 378
DI 10.1007/s10584-012-0460-2
PG 14
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 021EC
UT WOS:000309867100006
ER
PT J
AU Bolton, ML
Bass, EJ
Siminiceanu, RI
AF Bolton, Matthew L.
Bass, Ellen J.
Siminiceanu, Radu I.
TI Generating phenotypical erroneous human behavior to evaluate
human-automation interaction using model checking
SO INTERNATIONAL JOURNAL OF HUMAN-COMPUTER STUDIES
LA English
DT Article
DE Human-automation interaction; Model checking; Task analysis; Human
error; Formal methods
ID USER INTERFACES; FORMAL VERIFICATION; SYSTEMATIC ANALYSIS; DESIGN RULES;
ERRORS; METHODOLOGY; CONFUSIONS; DEVIATIONS; KNOWLEDGE; PATTERNS
AB Breakdowns in complex systems often occur as a result of system elements interacting in unanticipated ways. In systems with human operators, human-automation interaction associated with both normative and erroneous human behavior can contribute to such failures. Model-driven design and analysis techniques provide engineers with formal methods tools and techniques capable of evaluating how human behavior can contribute to system failures. This paper presents a novel method for automatically generating task analytic models encompassing both normative and erroneous human behavior from normative task models. The generated erroneous behavior is capable of replicating Hollnagel's zero-order phenotypes of erroneous action for omissions, jumps, repetitions, and intrusions. Multiple phenotypical acts can occur in sequence, thus allowing for the generation of higher order phenotypes. The task behavior model pattern capable of generating erroneous behavior can be integrated into a formal system model so that system safety properties can be formally verified with a model checker. This allows analysts to prove that a human-automation interactive system (as represented by the model) will or will not satisfy safety properties with both normative and generated erroneous human behavior. We present benchmarks related to the size of the statespace and verification time of models to show how the erroneous human behavior generation process scales. We demonstrate the method with a case study: the operation of a radiation therapy machine. A potential problem resulting from a generated erroneous human action is discovered. A design intervention is presented which prevents this problem from occurring. We discuss how our method could be used to evaluate larger applications and recommend future paths of development. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Bolton, Matthew L.] NASA, Ames Res Ctr, San Jose State Univ Res Fdn, Moffett Field, CA 94035 USA.
[Bass, Ellen J.] Univ Virginia, Dept Syst & Informat Engn, Charlottesville, VA USA.
[Siminiceanu, Radu I.] Natl Inst Aerosp, Hampton, VA USA.
RP Bolton, ML (reprint author), NASA, Ames Res Ctr, San Jose State Univ Res Fdn, Moffett Field, CA 94035 USA.
EM mlb4b@virginia.edu
RI Bolton, Matthew/G-5199-2012; Bolton, Matthew/A-6390-2016
FU National Library of Medicine (NLM) [TI 5LM009462]; NASA [NCC1002043,
NNA10DE79C]
FX The majority of the work documented in this manuscript was performed
while the first author was pursuing his Ph.D. in systems engineering
from the University of Virginia. The project described was supported in
part by Grant Number TI 5LM009462 from the National Library of Medicine
(NLM), NASA Cooperative Agreement NCC1002043, and NASA award NNA10DE79C.
The content is solely the responsibility of the authors and does not
necessarily represent the official views of the NIA, NASA, the NLM, or
the National Institutes of Health.
NR 98
TC 17
Z9 17
U1 1
U2 8
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 1071-5819
J9 INT J HUM-COMPUT ST
JI Int. J. Hum.-Comput. Stud.
PD NOV
PY 2012
VL 70
IS 11
BP 888
EP 906
DI 10.1016/j.ijhcs.2012.05.010
PG 19
WC Computer Science, Cybernetics; Ergonomics; Psychology, Multidisciplinary
SC Computer Science; Engineering; Psychology
GA 023QJ
UT WOS:000310049200007
PM 23105914
ER
PT J
AU Smith, DJ
Jaffe, DA
Birmele, MN
Griffin, DW
Schuerger, AC
Hee, J
Roberts, MS
AF Smith, David J.
Jaffe, Daniel A.
Birmele, Michele N.
Griffin, Dale W.
Schuerger, Andrew C.
Hee, Jonathan
Roberts, Michael S.
TI Free Tropospheric Transport of Microorganisms from Asia to North America
SO MICROBIAL ECOLOGY
LA English
DT Article
ID SP-NOV; DIFFERENT ECOSYSTEMS; GLOBAL ATMOSPHERE; AIRBORNE BACTERIA;
BACILLUS-SUBTILIS; QUANTITATIVE PCR; DESERT DUST; FUNGI; SOIL; DIVERSITY
AB Microorganisms are abundant in the troposphere and can be transported vast distances on prevailing winds. This study measures the abundance and diversity of airborne bacteria and fungi sampled at the Mt. Bachelor Observatory (located 2.7 km above sea level in North America) where incoming free tropospheric air routinely arrives from distant sources across the Pacific Ocean, including Asia. Overall deoxyribonucleic acid (DNA) concentrations for microorganisms in the free troposphere, derived from quantitative polymerase chain reaction assays, averaged 4.94 x 10(-5) ng DNA m(-3) for bacteria and 4.77 x 10(-3) ng DNA m(-3) for fungi. Aerosols occasionally corresponded with microbial abundance, most often in the springtime. Viable cells were recovered from 27.4 % of bacterial and 47.6 % of fungal samples (N = 124), with 49 different species identified by ribosomal DNA gene sequencing. The number of microbial isolates rose significantly above baseline values on 22-23 April 2011 and 13-15 May 2011. Both events were analyzed in detail, revealing distinct free tropospheric chemistries (e.g., low water vapor, high aerosols, carbon monoxide, and ozone) useful for ruling out boundary layer contamination. Kinematic back trajectory modeling suggested air from these events probably originated near China or Japan. Even after traveling for 10 days across the Pacific Ocean in the free troposphere, diverse and viable microbial populations, including presumptive plant pathogens Alternaria infectoria and Chaetomium globosum, were detected in Asian air samples. Establishing a connection between the intercontinental transport of microorganisms and specific diseases in North America will require follow-up investigations on both sides of the Pacific Ocean.
C1 [Smith, David J.] Univ Washington, Seattle, WA 98195 USA.
[Jaffe, Daniel A.; Hee, Jonathan] Univ Washington Bothell, Dept Atmospher Sci, Bothell, WA USA.
[Birmele, Michele N.; Roberts, Michael S.] NASA, ESC Team QNA, Kennedy Space Ctr, FL USA.
[Griffin, Dale W.] US Geol Survey, Tallahassee, FL USA.
[Schuerger, Andrew C.] Univ Florida, Dept Plant Pathol, Gainesville, FL 32611 USA.
RP Smith, DJ (reprint author), Univ Washington, Seattle, WA 98195 USA.
EM djsone@uw.edu
FU National Science Foundation (NSF) Integrative Graduate Education and
Research Traineeship (IGERT) program at the University of Washington
(UW) Graduate Program in Astrobiology; National Geographic Society/Waitt
Grants Program [W177-11]; NASA Astrobiology Institute Director's
Discretionary Fund; Washington NASA Space Grant Consortium; UW Biology
Department (Sargent Award); NSF [ATM-0724327]
FX Research funding was provided by the National Science Foundation (NSF)
Integrative Graduate Education and Research Traineeship (IGERT) program
at the University of Washington (UW) Graduate Program in Astrobiology,
the National Geographic Society/Waitt Grants Program (W177-11), the NASA
Astrobiology Institute Director's Discretionary Fund, the Washington
NASA Space Grant Consortium, and the UW Biology Department (Sargent
Award). The Mt. Bachelor Observatory atmospheric chemistry measurements
were funded by NSF Grant ATM-0724327. Critical sampling support was made
possible by Bryan Hicks, Patrick Ball, Carol Higginbotham, Tom Lomax,
and the staff at Mt. Bachelor Ski Resort. The authors are grateful to
Victoria Long, Clara Wright, and Phil Howard (NASA KSC) for assistance
with SEM imaging and John Catechis, Gerard Newsham, and Martin Hayes
(NASA KSC) for help with sequencing. We would also like to thank Ray
Wheeler (NASA KSC) and the anonymous manuscript reviewers for their time
and feedback. Any use of trade names is for descriptive purposes only
and does not imply endorsement by the U.S. Government.
NR 56
TC 41
Z9 41
U1 3
U2 58
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0095-3628
EI 1432-184X
J9 MICROB ECOL
JI Microb. Ecol.
PD NOV
PY 2012
VL 64
IS 4
BP 973
EP 985
DI 10.1007/s00248-012-0088-9
PG 13
WC Ecology; Marine & Freshwater Biology; Microbiology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology;
Microbiology
GA 024SC
UT WOS:000310127900012
PM 22760734
ER
PT J
AU Blasius, TD
Monnier, JD
Tuthill, PG
Danchi, WC
Anderson, M
AF Blasius, T. D.
Monnier, J. D.
Tuthill, P. G.
Danchi, W. C.
Anderson, M.
TI The Keck Aperture Masking Experiment: dust-enshrouded red giants
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiative transfer; instrumentation: interferometers; circumstellar
matter
ID LATE-TYPE STARS; RADIATIVE-TRANSFER; CARBON STARS; SUPER-GIANTS; STELLAR
ENVIRONMENTS; INFRARED PHOTOMETRY; CLOUD FORMATION; SKY SURVEY; AGB
STARS; MU-M
AB While the importance of dusty asymptotic giant branch (AGB) stars to galactic chemical enrichment is widely recognized, a sophisticated understanding of the dust formation and wind-driving mechanisms has proven elusive due in part to the difficulty in spatially resolving the dust-formation regions themselves. We have observed 20 dust-enshrouded AGB stars as part of the Keck Aperture Masking Experiment, resolving all of them in multiple near-infrared bands between 1.5 and 3.1? mu m. We find 45 per cent of the targets to show measurable elongations that, when correcting for the greater distances of the targets, would correspond to significantly asymmetric dust shells at par with the well-known cases of IRC + 10216 or CIT 6. Using radiative transfer models, we find the sublimation temperature of Tsub (silicates) =?1130 +/- 90?K and Tsub (amorphous carbon) = 1170 +/- 60?K, both somewhat lower than expected from laboratory measurements and vastly below temperatures inferred from the inner edge of young stellar objects discs. The fact that O-rich and C-rich dust types showed the same sublimation temperature was surprising as well. For the most optically thick shells (t2.2 mu m>2), the temperature profile of the inner dust shell is observed to change substantially, an effect we suggest could arise when individual dust clumps become optically thick at the highest mass-loss rates.
C1 [Blasius, T. D.; Monnier, J. D.; Anderson, M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Blasius, T. D.] CALTECH, Dept Phys, Pasadena, CA 91106 USA.
[Tuthill, P. G.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
[Danchi, W. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Blasius, TD (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
EM tblasius@caltech.edu
FU National Aeronautics and Space Administration; National Science
Foundation; W. M. Keck Foundation
FX We thank Dr Charles Townes for his long-standing support of this work.
We also thank Angela Speck for her insightful comments upon reading a
draft of this manuscript. We acknowledge interesting discussions with
Peter Woitke regarding the effect of clumpy structures on the
temperature profile, and we thank Rita Loidl Gautschy for her help in
acquiring the C-star synthetic spectrum. This research has made use of
the SIMBAD data base, operated at CDS, Strasbourg, France. This
publication makes 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/California
Institute of Technology, funded by the National Aeronautics and Space
Administration and the National Science Foundation. The data presented
herein were obtained at the W. M. Keck Observatory, which is operated as
a scientific partnership among the California Institute of Technology,
the University of California and the National Aeronautics and Space
Administration. The Keck Observatory was made possible by the generous
financial support of the W. M. Keck Foundation. We wish to recognize and
acknowledge the very significant cultural role and reverence that the
summit of Mauna Kea has always had within the indigenous Hawaiian
community. We are most fortunate to have the opportunity to conduct
observations from this mountain.
NR 63
TC 1
Z9 1
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 426
IS 4
BP 2652
EP 2667
DI 10.1111/j.1365-2966.2012.21543.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 023VI
UT WOS:000310064400003
ER
PT J
AU Woods, PM
Walsh, C
Cordiner, MA
Kemper, F
AF Woods, Paul M.
Walsh, C.
Cordiner, M. A.
Kemper, F.
TI The chemistry of extragalactic carbon stars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Review
DE Astrochemistry; stars: AGB and post-AGB; stars: carbon; circumstellar
matter; infrared: stars; submillimetre: stars
ID LARGE-MAGELLANIC-CLOUD; GIANT BRANCH STARS; MASS-LOSS RATES; RICH
AGB-STARS; 2-DIMENSIONAL RADIATIVE-TRANSFER; ENVELOPE SURROUNDING
IRC+10216; INFRARED EXTINCTION LAW; DUST FORMATION ZONE; TO-GAS RATIO;
CIRCUMSTELLAR ENVELOPES
AB Prompted by the ongoing interest in Spitzer Infrared Spectrometer spectra of carbon stars in the Large Magellanic Cloud, we have investigated the circumstellar chemistry of carbon stars in low-metallicity environments. Consistent with observations, our models show that acetylene is particularly abundant in the inner regions of low metallicity carbon-rich asymptotic giant branch stars more abundant than carbon monoxide. As a consequence, larger hydrocarbons have higher abundances at the metallicities of the Magellanic Clouds than in stars with solar metallicity. We also find that the oxygen and nitrogen chemistry is suppressed at lower metallicity, as expected. Finally, we calculate molecular line emission from carbon stars in the Large and Small Magellanic Cloud and find that several molecules should be readily detectable with the Atacama Large Millimeter Array at Full Science operations.
C1 [Woods, Paul M.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Woods, Paul M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Walsh, C.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Cordiner, M. A.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA.
[Cordiner, M. A.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Kemper, F.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
RP Woods, PM (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England.
EM paul.woods@ucl.ac.uk
RI Kemper, Francisca/D-8688-2011; Woods, Paul/E-6926-2011
OI Kemper, Francisca/0000-0003-2743-8240; Woods, Paul/0000-0003-4340-3590
NR 118
TC 8
Z9 8
U1 0
U2 12
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 426
IS 4
BP 2689
EP 2702
DI 10.1111/j.1365-2966.2012.21771.x
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 023VI
UT WOS:000310064400006
ER
PT J
AU Mateos, S
Alonso-Herrero, A
Carrera, FJ
Blain, A
Watson, MG
Barcons, X
Braito, V
Severgnini, P
Donley, JL
Stern, D
AF Mateos, S.
Alonso-Herrero, A.
Carrera, F. J.
Blain, A.
Watson, M. G.
Barcons, X.
Braito, V.
Severgnini, P.
Donley, J. L.
Stern, D.
TI Using the Bright Ultrahard XMM-Newton survey to define an IR selection
of luminous AGN based on WISE colours
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; quasars: general; infrared: galaxies
ID ACTIVE GALACTIC NUCLEI; SPITZER-SPACE-TELESCOPE; DEEP FIELD-SOUTH;
SPECTRAL ENERGY-DISTRIBUTIONS; SWIFT-BAT SURVEY; BLACK-HOLES;
MIDINFRARED SELECTION; GALAXIES; QUASARS; SAMPLE
AB We present a highly complete and reliable mid-infrared (MIR) colour selection of luminous active galactic nucleus (AGN) candidates using the 3.4, 4.6 and 12 mu m bands of the Wide-field Infrared Survey Explorer (WISE) survey. The MIR colour wedge was defined using the wide-angle Bright Ultrahard XMMNewton survey (BUXS), one of the largest complete flux-limited samples of bright (f4.5--10 keV >6x10-14 erg s-1 cm -2) ultrahard (4.510? keV) X-ray-selected AGN to date. The BUXS includes 258 objects detected over a total sky area of 44.43?deg2 of which 251 are spectroscopically identified and classified, with 145 being type 1 AGN and 106 type 2 AGN. Our technique is designed to select objects with red MIR power-law spectral energy distributions (SEDs) in the three shortest bands of WISE and properly accounts for the errors in the photometry and deviations of the MIR SEDs from a pure power-law. The completeness of the MIR selection is a strong function of luminosity. At L210?keV >1044 ? erg?s-1, where the AGN is expected to dominate the MIR emission, 97.1-4.8+2.2 and 76.5-18.4+13.3 per cent of the BUXS type 1 and type 2 AGN, respectively, meet the selection. Our technique shows one of the highest reliability and efficiency of detection of the X-ray-selected luminous AGN population with WISE amongst those in the literature. In the area covered by BUXS our selection identifies 2755 AGN candidates detected with signal-to-noise ratio =5 in the three shorter wavelength bands of WISE with 38.5 per cent having a detection at 210?keV X-ray energies. We also analysed the possibility of including the 22? mu m WISE band to select AGN candidates, but neither the completeness nor the reliability of the selection improves. This is likely due to both the significantly shallower depth at 22 mu m compared with the first three bands of WISE and star formation contributing to the 22 mu m emission at the WISE 22 mu m sensitivity.
C1 [Mateos, S.; Alonso-Herrero, A.; Carrera, F. J.; Barcons, X.] Univ Cantabria, Inst Fis Cantabria, CSIC, E-39005 Santander, Spain.
[Mateos, S.; Blain, A.; Watson, M. G.] Univ Leicester, Leicester LE1 7RH, Leics, England.
[Braito, V.] Osserv Astron Brera, Ist Nazl Astrofis, I-23807 Merate, LC, Italy.
[Severgnini, P.] INAF Osservatorio Astron Brera, I-20121 Milan, Italy.
[Donley, J. L.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mateos, S (reprint author), Univ Cantabria, Inst Fis Cantabria, CSIC, E-39005 Santander, Spain.
EM mateos@ifca.unican.es
RI Barcons, Xavier/L-3335-2014; Mateos, Silvia/F-9524-2016; Alonso-Herrero,
Almudena/H-1426-2015;
OI Barcons, Xavier/0000-0003-1081-8861; Mateos, Silvia/0000-0002-1375-2389;
Alonso-Herrero, Almudena/0000-0001-6794-2519; Severgnini,
Paola/0000-0001-5619-5896; Braito, Valentina/0000-0002-2629-4989
FU NASA; 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; European Organisation for Astronomical Research in
the Southern hemisphere, Chile [084.A-0828, 086.A-0612, 087.A-0447];
Spanish Ministry of Economy and Competitiveness [AYA2010-21490-C02-01];
Universidad de Cantabria through the Augusto G. Linares program; Royal
Society Wolfson Research Merit Award; LANL Director's Fellowship; ASI
[I/009/10/0]
FX This work is based on observations obtained with XMM-Newton, an ESA
science mission with instruments and contributions directly funded by
ESA Member States and NASA. It is also based on data 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. 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 website is http://www.sdss.org/. This work is based on
observations collected at the European Organisation for Astronomical
Research in the Southern hemisphere, Chile, programme IDs 084.A-0828,
086.A-0612, 087.A-0447. It is also based on observations made with the
William Herschel Telescope - operated by the Isaac Newton Group, the
Telescopio Nazionale Galileo - operated by the Centro Galileo Galilei
and the Gran Telescopio de Canarias installed in the Spanish
Observatorio del Roque de los Muchachos of the Instituto de Astrofsica
de Canarias, in the island of La Palma. SM, FJC and XB acknowledge
financial support by the Spanish Ministry of Economy and Competitiveness
through grant AYA2010-21490-C02-01. AAH acknowledges support from the
Universidad de Cantabria through the Augusto G. Linares program. AB
acknowledges a Royal Society Wolfson Research Merit Award. JLD
acknowledges support from the LANL Director's Fellowship. PS
acknowledges financial support from ASI (grant No. I/009/10/0). The
authors wish to thank the anonymous referee for constructive comments.
NR 50
TC 79
Z9 79
U1 0
U2 6
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2012
VL 426
IS 4
BP 3271
EP 3281
DI 10.1111/j.1365-2966.2012.21843.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 023VI
UT WOS:000310064400047
ER
PT J
AU Jauzac, M
Jullo, E
Kneib, JP
Ebeling, H
Leauthaud, A
Ma, CJ
Limousin, M
Massey, R
Richard, J
AF Jauzac, Mathilde
Jullo, Eric
Kneib, Jean-Paul
Ebeling, Harald
Leauthaud, Alexie
Ma, Cheng-Jiun
Limousin, Marceau
Massey, Richard
Richard, Johan
TI A weak lensing mass reconstruction of the large-scale filament feeding
the massive galaxy cluster MACS J0717.5+3745
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: weak; galaxies: clusters: individual: MACS
J0717.5+3745; cosmology: observations; large-scale structure of Universe
ID HUBBLE-SPACE-TELESCOPE; VLT DEEP SURVEY; DARK-MATTER; COSMIC WEB; HOT
GAS; INTERCLUSTER FILAMENTS; PHOTOMETRIC REDSHIFTS; FUNDAMENTAL PLANE;
SKY SURVEY; EVOLUTION
AB We report the first weak lensing detection of a large-scale filament funnelling matter on to the core of the massive galaxy cluster MACS J0717.5+3745.
Our analysis is based on a mosaic of 18 multipassband images obtained with the Advanced Camera for Surveys aboard the Hubble Space Telescope, covering an area of similar to 10 x20 arcmin(2). We use a weak lensing pipeline developed for the Cosmic Evolution Survey, modified for the analysis of galaxy clusters, to produce a weak lensing catalogue. A mass map is then computed by applying a weak gravitational lensing multiscale reconstruction technique designed to describe irregular mass distributions such as the one investigated here. We test the resulting mass map by comparing the mass distribution inferred for the cluster core with the one derived from strong lensing constraints and find excellent agreement.
Our analysis detects the MACS J0717.5+3745 filament within the 3s detection contour of the lensing mass reconstruction, and underlines the importance of filaments for theoretical and numerical models of the mass distribution in the cosmic web. We measure the filament's projected length as similar to 4.5 h(74)(-1) Mpc, and its mean density as (2.92 +/- 0.66) x 10(8) h(74) M-circle dot kpc(-2). Combined with the redshift distribution of galaxies obtained after an extensive spectroscopic follow-up in the area, we can rule out any projection effect resulting from the chance alignment on the sky of unrelated galaxy group-scale structures. Assuming plausible constraints concerning the structure's geometry based on its galaxy velocity field, we construct a three-dimensional (3D) model of the large-scale filament. Within this framework, we derive the 3D length of the filament to be 18 h(74)(-1) Mpc. The filament's deprojected density in terms of the critical density of the Universe is measured as (206 +/- 46)rho(crit), a value that lies at the very high end of the range predicted by numerical simulations. Finally, we study the distribution of stellar mass in the field of MACS J0717.5+3749 and, adopting a mean mass-to-light ratio < M-*/L-K > of 0.73 +/- 0.22 and assuming a Chabrier initial mass function, measure a stellar mass fraction along the filament of (0.9 +/- 0.2) per cent, consistent with previous measurements in the vicinity of massive clusters.
C1 [Jauzac, Mathilde; Jullo, Eric; Kneib, Jean-Paul; Limousin, Marceau] Univ Aix Marseille, LAM, F-13388 Marseille 13, France.
[Jauzac, Mathilde; Jullo, Eric; Kneib, Jean-Paul; Limousin, Marceau] CNRS, UMR7326, F-13388 Marseille 13, France.
[Jauzac, Mathilde] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Jullo, Eric] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ebeling, Harald; Ma, Cheng-Jiun] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Leauthaud, Alexie] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe, WPI, Kashiwa, Chiba 2778583, Japan.
[Limousin, Marceau] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Massey, Richard] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England.
[Richard, Johan] Univ Lyon 1, Observ Lyon, CRAL, F-69561 St Genis Laval, France.
RP Jauzac, M (reprint author), Univ Aix Marseille, LAM, 38 Rue F Joliot Curie, F-13388 Marseille 13, France.
EM mathilde.jauzac@gmail.com
RI Jauzac, Mathilde/B-1966-2015; Kneib, Jean-Paul/A-7919-2015
OI Kneib, Jean-Paul/0000-0002-4616-4989
FU Jet Propulsion Laboratory under contract with the California Institute
of Technology; NASA; Centre National d'Etudes Spatiales; STScI
[GO-10420]; Centre National de la Recherche Scientifique (CNRS); Danish
National Research Foundation; World Premier International Research
Center Initiative (WPI Initiative), MEXT, Japan
FX We thank Douglas Clowe for accepting to review this paper and for his
useful comments. MJ would like to thank Graham P. Smith, Kavilan Moodley
and, Pierre-Yves Chabaud for useful discussions. EJ acknowledges support
from the Jet Propulsion Laboratory under contract with the California
Institute of Technology, the NASA Postdoctoral Program and the Centre
National d'Etudes Spatiales. MJ and EJ are indebted to Jason Rhodes for
discussions and advice. HE gratefully acknowledges financial support
from STScI grant GO-10420. We thank the UH Time Allocation Committee for
their support of the extensive ground-based follow-up observations
required for this study. JPK & ML acknowledge the Centre National de la
Recherche Scientifique (CNRS) for its support. The Dark Cosmology Centre
is funded by the Danish National Research Foundation. This work was
performed using facilities offered by Centre de donneeS Astrophysique de
Marseille (CeSAM; http://lam.oamp.fr/cesam/). This work was supported by
World Premier International Research Center Initiative (WPI Initiative),
MEXT, Japan.
NR 85
TC 40
Z9 40
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2012
VL 426
IS 4
BP 3369
EP 3384
DI 10.1111/j.1365-2966.2012.21966.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 023VI
UT WOS:000310064400054
ER
PT J
AU van Kampen, E
Smith, DJB
Maddox, S
Hopkins, AM
Valtchanov, I
Peacock, JA
Michalowski, MJ
Norberg, P
Eales, S
Dunne, L
Liske, J
Baes, M
Scott, D
Rigby, E
Robotham, A
van der Werf, P
Ibar, E
Jarvis, MJ
Loveday, J
Auld, R
Baldry, IK
Bamford, S
Cameron, E
Croom, S
Buttiglione, S
Cava, A
Cooray, A
Driver, S
Dunlop, JS
Dariush, A
Fritz, J
Ivison, RJ
Pascale, E
Pohlen, M
Rodighiero, G
Temi, P
Bonfield, DG
Hill, D
Jones, DH
Kelvin, L
Parkinson, H
Prescott, M
Sharp, R
de Zotti, G
Serjeant, S
Popescu, CC
Tuffs, RJ
AF van Kampen, E.
Smith, D. J. B.
Maddox, S.
Hopkins, A. M.
Valtchanov, I.
Peacock, J. A.
Michalowski, M. J.
Norberg, P.
Eales, S.
Dunne, L.
Liske, J.
Baes, M.
Scott, D.
Rigby, E.
Robotham, A.
van der Werf, P.
Ibar, E.
Jarvis, M. J.
Loveday, J.
Auld, R.
Baldry, I. K.
Bamford, S.
Cameron, E.
Croom, S.
Buttiglione, S.
Cava, A.
Cooray, A.
Driver, S.
Dunlop, J. S.
Dariush, A.
Fritz, J.
Ivison, R. J.
Pascale, E.
Pohlen, M.
Rodighiero, G.
Temi, P.
Bonfield, D. G.
Hill, D.
Jones, D. H.
Kelvin, L.
Parkinson, H.
Prescott, M.
Sharp, R.
de Zotti, G.
Serjeant, S.
Popescu, C. C.
Tuffs, R. J.
TI Herschel-ATLAS/GAMA: spatial clustering of low-redshift submm galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; galaxies: statistics; large-scale structure of Universe;
submillimetre: galaxies
ID MASS ASSEMBLY GAMA; DATA RELEASE; SPIRE; LUMINOSITY; COLOR; FIELD;
POPULATION; DEPENDENCE; CATALOG
AB We have measured the clustering properties of low-redshift (z < 0.3) submm galaxies detected at 250 mu m in the Herschel-ATLAS science demonstration phase field. We selected a sample for which we have high-quality spectroscopic redshifts, obtained from reliably matching the 250-mu m sources to a complete (for r < 19.4) sample of galaxies from the GAMA data base. Both the angular and spatial clustering strength are measured for all z < 0.3 sources as well as for five redshift slices with thickness Delta z = 0.05 in the range 0.05 < z < 0.3. Our measured spatial clustering length r(0) is comparable to that of optically selected, moderately star-forming (blue) galaxies: we find values around 5 Mpc. One of the redshift bins contains an interesting structure, at z = 0.164.
C1 [van Kampen, E.; Liske, J.] European So Observ, D-85748 Garching, Germany.
[Smith, D. J. B.; Maddox, S.; Dunne, L.; Rigby, E.; Bamford, S.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Smith, D. J. B.; Jarvis, M. J.; Bonfield, D. G.; Hill, D.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Maddox, S.; Dunne, L.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Hopkins, A. M.; Jones, D. H.; Sharp, R.] Australian Astron Observ, Epping, NSW 1710, Australia.
[Valtchanov, I.] ESA, ESAC, Herschel Sci Ctr, Madrid 28691, Spain.
[Peacock, J. A.; Michalowski, M. J.; Rigby, E.; van der Werf, P.; Auld, R.; Dunlop, J. S.; Parkinson, H.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Norberg, P.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England.
[Eales, S.; Pascale, E.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Robotham, A.; Driver, S.; Kelvin, L.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Ibar, E.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Loveday, J.] Univ Sussex, Dept Phys & Astron, Astron Ctr, Brighton BN1 9QH, E Sussex, England.
[Baldry, I. K.; Prescott, M.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Cameron, E.] ETH, Insitute Astron, CH-8093 Zurich, Switzerland.
[Croom, S.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Buttiglione, S.; de Zotti, G.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy.
[Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain.
[Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Driver, S.] Univ Western Australia, ICRAR, Nedlands, WA 6009, Australia.
[Dariush, A.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England.
[Rodighiero, G.] Univ Padua, I-35122 Padua, Italy.
[Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA.
[de Zotti, G.] SISSA, I-34136 Trieste, Italy.
[Serjeant, S.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[Popescu, C. C.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Tuffs, R. J.] Max Planck Inst Nucl Astrophys MPIK, D-69117 Heidelberg, Germany.
RP van Kampen, E (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM evkampen@eso.org
RI Cava, Antonio/C-5274-2017; Baes, Maarten/I-6985-2013; Robotham,
Aaron/H-5733-2014; Driver, Simon/H-9115-2014; Ivison, R./G-4450-2011;
Bamford, Steven/E-8702-2010;
OI Cava, Antonio/0000-0002-4821-1275; De Zotti,
Gianfranco/0000-0003-2868-2595; Maddox, Stephen/0000-0001-5549-195X;
Baes, Maarten/0000-0002-3930-2757; Robotham, Aaron/0000-0003-0429-3579;
Driver, Simon/0000-0001-9491-7327; Ivison, R./0000-0001-5118-1313;
Bamford, Steven/0000-0001-7821-7195; Scott, Douglas/0000-0002-6878-9840;
Smith, Daniel/0000-0001-9708-253X; Rodighiero,
Giulia/0000-0002-9415-2296; Liske, Jochen/0000-0001-7542-2927; Baldry,
Ivan/0000-0003-0719-9385
FU STFC (UK); ARC (Australia); AAO; Austrian Science Foundation FWF
[P18493, I164]; ASI-INAF [I/009/10/0]
FX 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.h-atlas.org/. GAMA is a joint
European-Australasian project based around a spectroscopic campaign
using the Anglo-Australian Telescope. The GAMA input catalogue is based
on data taken from the Sloan Digital Sky Survey and the United Kingdom
Infrared Telescope (UKIRT) Infrared Deep Sky Survey. Complementary
imaging of the GAMA regions is being obtained by a number of independent
survey programmes including GALEX MIS, VST KIDS, VISTA VIKING, WISE,
Herschel-ATLAS, GMRT and ASKAP, providing UV to radio coverage. 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 research was supported in part by the
Austrian Science Foundation FWF under grants P18493 and I164, and
received financial contribution from the agreement ASI-INAF I/009/10/0.
The authors thank Duncan Farrah for making his Limber equation inversion
code available.
NR 36
TC 9
Z9 9
U1 1
U2 9
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 426
IS 4
BP 3455
EP 3463
DI 10.1111/j.1365-2966.2012.21949.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 023VI
UT WOS:000310064400059
ER
PT J
AU Aguiar, APD
Ometto, JP
Nobre, C
Lapola, DM
Almeida, C
Vieira, IC
Soares, JV
Alvala, R
Saatchi, S
Valeriano, D
Castilla-Rubio, JC
AF Dutra Aguiar, Ana Paula
Ometto, Jean Pierre
Nobre, Carlos
Lapola, David Montenegro
Almeida, Claudio
Vieira, Ima Celia
Soares, Joao Vianei
Alvala, Regina
Saatchi, Sassan
Valeriano, Dalton
Castilla-Rubio, Juan Carlos
TI Modeling the spatial and temporal heterogeneity of deforestation-driven
carbon emissions: the INPE-EM framework applied to the Brazilian Amazon
SO GLOBAL CHANGE BIOLOGY
LA English
DT Article
DE Amazonia; carbon emissions; deforestation; LUCC; REDD; secondary forests
ID LAND-USE CHANGE; ABOVEGROUND LIVE BIOMASS; LOGGED FORESTS; TROPICAL
DEFORESTATION; SECONDARY VEGETATION; RAIN-FOREST; FIRE; DYNAMICS;
REGROWTH; REGIONS
AB We present a generic spatially explicit modeling framework to estimate carbon emissions from deforestation (INPE-EM). The framework incorporates the temporal dynamics related to the deforestation process and accounts for the biophysical and socioeconomic heterogeneity of the region under study. We build an emission model for the Brazilian Amazon combining annual maps of new clearings, four maps of biomass, and a set of alternative parameters based on the recent literature. The most important results are as follows: (a) Using different biomass maps leads to large differences in estimates of emission; for the entire region of the Brazilian Amazon in the last decade, emission estimates of primary forest deforestation range from 0.21 to 0.26 similar to Pg similar to C similar to yr-1. (b) Secondary vegetation growth presents a small impact on emission balance because of the short duration of secondary vegetation. In average, the balance is only 5% smaller than the primary forest deforestation emissions. (c) Deforestation rates decreased significantly in the Brazilian Amazon in recent years, from 27 similar to Mkm2 in 2004 to 7 similar to Mkm2 in 2010. INPE-EM process-based estimates reflect this decrease even though the agricultural frontier is moving to areas of higher biomass. The decrease is slower than a non-process instantaneous model would estimate as it considers residual emissions (slash, wood products, and secondary vegetation). The average balance, considering all biomass, decreases from 0.28 in 2004 to 0.15 similar to Pg similar to C similar to yr-1 in 2009; the non-process model estimates a decrease from 0.33 to 0.10 similar to Pg similar to C similar to yr-1. We conclude that the INPE-EM is a powerful tool for representing deforestation-driven carbon emissions. Biomass estimates are still the largest source of uncertainty in the effective use of this type of model for informing mechanisms such as REDD+. The results also indicate that efforts to reduce emissions should focus not only on controlling primary forest deforestation but also on creating incentives for the restoration of secondary forests.
C1 [Dutra Aguiar, Ana Paula; Ometto, Jean Pierre; Nobre, Carlos; Alvala, Regina] Brazilian Inst Space Res INPE, Earth Syst Sci Ctr CCST, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
[Lapola, David Montenegro] Univ Estadual Paulista UNESP, Dept Ecol, Lab Ciencia Sistema Terrestre LabTerra, BR-13506900 Rio Claro, SP, Brazil.
[Almeida, Claudio] Brazilian Inst Space Res INPE, Amazon Reg Ctr CRA, BR-66077830 Belem, Para, Brazil.
[Vieira, Ima Celia] Museu Paraense Emilio Goeldi MPEG, BR-66040170 Belem, Para, Brazil.
[Soares, Joao Vianei; Valeriano, Dalton] Brazilian Inst Space Res INPE, Earth Observat Coordinat OBT, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
[Saatchi, Sassan] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Castilla-Rubio, Juan Carlos] Planetary Skin Inst, Silicon Valley, CA USA.
RP Aguiar, APD (reprint author), Brazilian Inst Space Res INPE, Earth Syst Sci Ctr CCST, Av Astronautas 1758, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
EM ana.aguiar@inpe.br
RI Clima, Inct/I-2209-2013; SOARES, Joao/D-2576-2014; Ometto,
Jean/B-3351-2013
OI SOARES, Joao/0000-0003-3880-0006;
FU Planetary Skin Institute
FX For the biomass spatial data, we acknowledge Thelma Krug (MCT, 2010) and
Philip Fearnside (Nogueira et al., 2008). For the data preprocessing and
database organization, we acknowledge Giovana Espindola, Luciana Soler,
Talita Assis, Pedro Valle and Andre Gavlak. INPE-EM software was
developed by the authors using the TerraME modeling environment,
available at www.terrame.org. For INPE-EM software maintenance, we
acknowledge Talita Assis and Missae Yamamoto. For discussions of the
deforestation annual increment correction, we acknowledge Luis Maurano
and Marisa Motta (INPE's PRODES Project). Judith J. Hoelzemann and
Roberto Araujo are acknowledged for the critical reading of the
manuscript. Finally, we thank the Planetary Skin Institute
(www.planetaryskin.org) for discussions and for financial support for
INPE's CCST LUCC modeling group.
NR 88
TC 30
Z9 30
U1 4
U2 62
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1354-1013
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD NOV
PY 2012
VL 18
IS 11
BP 3346
EP 3366
DI 10.1111/j.1365-2486.2012.02782.x
PG 21
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 015MM
UT WOS:000309450300009
ER
PT J
AU Kronenberg, A
Cucinotta, FA
AF Kronenberg, Amy
Cucinotta, Francis A.
TI SPACE RADIATION PROTECTION ISSUES
SO HEALTH PHYSICS
LA English
DT Article
DE National Council on Radiation Protection and Measurements; charged
particles; space radiation; radiation protection; radiation risk; heavy
ions
ID GEV/NUCLEON FE-56 IONS; PERSISTENT REDUCTION; MYELOID-LEUKEMIA; RAT
SKIN; MICE; CARCINOGENESIS; HIPPOCAMPUS; IRRADIATION; EXPOSURE; RAYS
AB The complex charged particle environments in space pose considerable challenges with regard to potential health consequences that can impact mission design and crew selection. The lack of knowledge of the biological effects of different ions in isolation and in combination is a particular concern because the risk uncertainties are very high for both cancer and non-cancer late effects. Reducing the uncertainties is of high priority. Two principal components of space radiation each raise different concerns. Solar particle events (SPE) occur sporadically and are comprised primarily of low- to moderate-energy protons. Galactic cosmic radiation (GCR) is isotropic and relatively invariant in dose rate. GCR is also dominated by protons, but the energy range is wider than in SPE. In addition, the contribution of other light and heavy ions to the health risks from GCR must be addressed. This paper will introduce the principal issues under consideration for space radiation protection. Health Phys. 103(5):556-567; 2012
C1 [Kronenberg, Amy] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Life Sci, Berkeley, CA 94720 USA.
[Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Kronenberg, A (reprint author), Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Life Sci, 1 Cyclotron Rd, Berkeley, CA 94720 USA.
EM a_kronenberg@lbl.gov
FU NASA [NNJ07HC721, NNJ12HB88I]; U.S. Department of Energy
[DE-AC02-05CH11231]
FX Supported by NASA grants NNJ07HC721 and NNJ12HB88I to A. Kronenberg.
This manuscript has been authored by an author at Lawrence Berkeley
National Laboratory under Contract No. DE-AC02-05CH11231 with the U.S.
Department of Energy. The U. S. government retains, and the publisher,
by accepting the article for publication, acknowledges, that the U. S.
government retains a nonexclusive, paid-up, irrevocable, worldwide
license to publish or reproduce the published form of this manuscript,
or allow others to do so, for U. S. government purposes.
NR 38
TC 14
Z9 14
U1 2
U2 7
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA
SN 0017-9078
EI 1538-5159
J9 HEALTH PHYS
JI Health Phys.
PD NOV
PY 2012
VL 103
IS 5
BP 556
EP 567
DI 10.1097/HP.0b013e3182690caf
PG 12
WC Environmental Sciences; Public, Environmental & Occupational Health;
Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical
Imaging
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Nuclear Science & Technology; Radiology, Nuclear Medicine &
Medical Imaging
GA 016MI
UT WOS:000309522300009
PM 23032885
ER
PT J
AU Kim, MHY
Wilson, JW
Cucinotta, FA
AF Kim, Myung-Hee Y.
Wilson, John W.
Cucinotta, Francis A.
TI DESCRIPTION OF TRANSPORT CODES FOR SPACE RADIATION SHIELDING
SO HEALTH PHYSICS
LA English
DT Article
DE National Council on Radiation Protection and Measurements; risk
assessment; shielding; statistics
ID GALACTIC COSMIC-RADIATION; CROSS-SECTIONS; ENERGY-SPECTRA; HUMAN
PHANTOM; MODEL; FLUENCE; SHUTTLE; RAYS; EXPLORATION; ENVIRONMENT
AB Exposure to ionizing radiation in the space environment is one of the hazards faced by crews in space missions. As space radiations traverse spacecraft, habitat shielding, or tissues, their energies and compositions are altered by interactions with the shielding. Modifications to the radiation fields arise from atomic interactions of charged particles with orbital electrons and nuclear interactions leading to projectile and target fragmentation, including secondary particles such as neutrons, protons, mesons, and nuclear recoils. The transport of space radiation through shielding can be simulated using Monte Carlo techniques or deterministic solutions of the Boltzmann equation. To determine shielding requirements and to resolve radiation constraints for future human missions, the shielding evaluation of a spacecraft concept is required as an early step in the design process. To do this requires (1) accurate knowledge of space environmental models to define the boundary condition for transport calculations, (2) transport codes with detailed shielding and body geometry models to determine particle transmission into areas of internal shielding and at each critical body organ, and (3) the assessment of organ dosimetric quantities and biological risks by applying the corresponding response models for space radiation against the particle spectra that have been accurately determined from the transport code. This paper reviews current transport codes and analyzes their accuracy through comparison to laboratory and spaceflight data. This paper also introduces a probabilistic risk assessment approach for the evaluation of radiation shielding. Health Phys. 103(5):621-639; 2012
C1 [Kim, Myung-Hee Y.] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA.
[Wilson, John W.] NASA, Langley Res Ctr, Distinguished Res Associates, Hampton, VA 23681 USA.
[Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Space Radiat Program, Houston, TX 77058 USA.
RP Kim, MHY (reprint author), Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA.
EM myung-hee.y.kim@nasa.gov
OI Kim, Myung-Hee/0000-0001-5575-6858
NR 71
TC 4
Z9 5
U1 0
U2 7
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA
SN 0017-9078
EI 1538-5159
J9 HEALTH PHYS
JI Health Phys.
PD NOV
PY 2012
VL 103
IS 5
BP 621
EP 639
DI 10.1097/HP.0b013e318266732f
PG 19
WC Environmental Sciences; Public, Environmental & Occupational Health;
Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical
Imaging
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Nuclear Science & Technology; Radiology, Nuclear Medicine &
Medical Imaging
GA 016MI
UT WOS:000309522300016
PM 23032892
ER
PT J
AU Norbury, JW
Miller, J
AF Norbury, John W.
Miller, Jack
TI REVIEW OF NUCLEAR PHYSICS EXPERIMENTAL DATA FOR SPACE RADIATION
SO HEALTH PHYSICS
LA English
DT Review
DE National Council on Radiation Protection and Measurements; dose
assessment; modeling, dose assessment; radiation protection
AB The available nuclear fragmentation data relevant to space radiation studies are reviewed. It is found that there are serious gaps in the data. Helium data are missing in the intervals 280 MeV n(-1)-3 GeV n(-1) and >15 GeV n(-1). Carbon data are missing >15 GeV n(-1). Iron projectile data are missing at all energies except in the interval 280 MeV n(-1)-3 GeV n(-1). Health Phys. 103(5):640-642; 2012
C1 [Norbury, John W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Miller, Jack] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
RP Norbury, JW (reprint author), NASA, Langley Res Ctr, Mail Stop 188E, Hampton, VA 23681 USA.
EM john.w.norbury@nasa.gov
NR 4
TC 5
Z9 5
U1 0
U2 4
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA
SN 0017-9078
EI 1538-5159
J9 HEALTH PHYS
JI Health Phys.
PD NOV
PY 2012
VL 103
IS 5
BP 640
EP 642
DI 10.1097/HP.0b013e318261fb7f
PG 3
WC Environmental Sciences; Public, Environmental & Occupational Health;
Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical
Imaging
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Nuclear Science & Technology; Radiology, Nuclear Medicine &
Medical Imaging
GA 016MI
UT WOS:000309522300017
PM 23032893
ER
PT J
AU Cucinotta, FA
Chappell, LJ
Kim, MHY
Wang, ML
AF Cucinotta, Francis A.
Chappell, Lori J.
Kim, Myung-Hee Y.
Wang, Minli
TI RADIATION CARCINOGENESIS RISK ASSESSMENTS FOR NEVER-SMOKERS
SO HEALTH PHYSICS
LA English
DT Article
DE National Council on Radiation Protection and Measurements;
carcinogenesis; health effects; lungs; human
ID SMOKING-ATTRIBUTABLE MORTALITY; ATOMIC-BOMB SURVIVORS; LUNG-CANCER;
TOBACCO-SMOKE; CIGARETTE-SMOKING; HODGKINS-DISEASE; POOLED ANALYSIS;
URANIUM MINERS; UNITED-STATES; HISTOLOGY
AB Cigarette smoking, which is presently associated with more than 20% of adult deaths in the United States, is a large confounder to radiation risk estimates derived from epidemiology data. Astronauts and other exposed groups are classified as never-smokers (NS), defined as lifetime use of less than 100 cigarettes. In the past, radiation risk estimates have been made using average U. S. population rates for cancer and all causes of death, which may lead to overestimation of radiation risks for NS. In this report, age- and gender-specific radiation carcinogenesis risk calculations for NS and the average U. S. population are compared. Lung is the major tissue site for smoking and radiation-related cancer. However, other radiogenic cancers where tobacco has been shown to increase population cancer rates are esophagus, oral cavity, salivary gland, bladder, stomach, liver, colorectal, and leukemia. After adjusting U. S. cancer rates to remove smoking effects, radiation risks for lung and other cancers were estimated using the multiplicative risk model and a mixture model, with weighted contributions for additive and multiplicative risk transfer. Radiation mortality risks for NS were reduced compared to the average U. S. population by more than 20% and 50% in the mixture model and multiplicative transfer models, respectively. The authors discuss possible mechanisms of cancer risks from radiation and tobacco that suggest multiplicative effects could occur. These results suggest that improved understanding of possible synergisms between cancer initiators and promoters, such as radiation and tobacco, would greatly improve risk estimates and reduce uncertainties for differentially exposed groups, including NS. Health Phys. 103(5):643-651; 2012
C1 [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Chappell, Lori J.; Kim, Myung-Hee Y.; Wang, Minli] USRA, Div Life Sci, Houston, TX 77058 USA.
RP Cucinotta, FA (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM Francis.A.Cucinotta@nasa.gov
OI Kim, Myung-Hee/0000-0001-5575-6858
NR 44
TC 8
Z9 8
U1 0
U2 8
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA
SN 0017-9078
EI 1538-5159
J9 HEALTH PHYS
JI Health Phys.
PD NOV
PY 2012
VL 103
IS 5
BP 643
EP 651
DI 10.1097/HP.0b013e318267b3ad
PG 9
WC Environmental Sciences; Public, Environmental & Occupational Health;
Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical
Imaging
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Nuclear Science & Technology; Radiology, Nuclear Medicine &
Medical Imaging
GA 016MI
UT WOS:000309522300018
PM 23032894
ER
PT J
AU Zhai, PW
Kattawar, GW
Hu, YX
AF Zhai, Peng-Wang
Kattawar, George W.
Hu, Yongxiang
TI Comment on the transmission matrix for a dielectric interface
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Editorial Material
DE Atmosphere and ocean optics; Propagation, transmission, attenuation, and
radiative transfer; Scattering, polarization
ID VECTOR RADIATIVE-TRANSFER; MONTE-CARLO; ATMOSPHERE-OCEAN; POLARIZATION;
SCATTERING; SYSTEMS; MEDIA
AB In a recent paper the reflection and transmission matrices for a dielectric interface based on Fresnel formulas are derived [Garcia RDM. Fresnel boundary and interface conditions for polarized radiative transfer in a multilayer medium. J Quant Spectrosc Radiat Transfer 2012;113:306-17]. Although the final formulas appear to be correct, we found that there are some significant conceptual and logical flaws in the derivation. Here we explain that the misunderstanding is due to the different physical significances of the Stokes parameters for the coherent and diffuse radiation field and that the so-called transmission factor directly originates from the physical definition of the Stokes parameters. We also clarify a few incorrect interpretations in the aforementioned paper about previously published works. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Zhai, Peng-Wang] NASA, SSAI, MS 475, Langley Res Ctr, Hampton, VA 23681 USA.
[Kattawar, George W.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
RP Zhai, PW (reprint author), NASA, SSAI, MS 475, Langley Res Ctr, Hampton, VA 23681 USA.
EM Pengwang.zhai-1@nasa.gov
RI Hu, Yongxiang/K-4426-2012
NR 15
TC 6
Z9 6
U1 0
U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD NOV
PY 2012
VL 113
IS 16
BP 1981
EP 1984
DI 10.1016/j.jqsrt.2012.07.001
PG 4
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 017FB
UT WOS:000309574400001
ER
PT J
AU Reuter, M
Bovensmann, H
Buchwitz, M
Burrows, JP
Deutscher, NM
Heymann, J
Rozanov, A
Schneising, O
Suto, H
Toon, GC
Warneke, T
AF Reuter, M.
Bovensmann, H.
Buchwitz, M.
Burrows, J. P.
Deutscher, N. M.
Heymann, J.
Rozanov, A.
Schneising, O.
Suto, H.
Toon, G. C.
Warneke, T.
TI On the potential of the 2041-2047 nm spectral region for remote sensing
of atmospheric CO2 isotopologues
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Carbon dioxide; CO2; Isotopes; Isotopologues; Remote sensing; FTS;
Satellite; GOSAT
ID CARBON-DIOXIDE EXCHANGE; AIR-SAMPLING-NETWORK; SPECTROSCOPIC DATABASE;
STABLE-ISOTOPES; WFM-DOAS; MU-M; SCIAMACHY; RETRIEVAL; SATELLITE; GASES
AB Pressing open questions about the carbon cycle can be addressed with precise measurements of the three most abundant CO2 isotopologues (OCO)-O-16-C-12-O-16, (OCO)-O-16-C-13-O-16, and (OCO)-O-16-C-12-O-18. Such measurements can, e.g., help to further constrain oceanic and biospheric net fluxes or to differentiate between the gross biospheric fluxes photosynthesis and respiration. The 2041-2047 nm (about 4885-4900 cm(-1)) spectral region contains separated absorption lines of the three most abundant CO2 isotopologues. Their spectral properties make this spectral region well suited for the use of a light path proxy method for the retrieval of delta C-13 and delta O-18 (the ratio of heavier to lighter isotopologues relative to a standard). An optimal estimation based light path proxy retrieval for delta C-13 and delta O-18 has been set up, applicable to GOSAT (Greenhouse gases Observing Satellite) and ground-based FTS (Fourier transform spectrometer) measurements. Initial results show that it is possible to retrieve delta C-13 and delta O-18 from ground-based FTS instruments with a precision of 0.6-1.6 parts per thousand and from GOSAT with a precision of about 30 parts per thousand. Comparison of the achievable precision with the expected atmospheric signals shows that ground-based FTS remote sensing measurements have the potential to gain valuable information on delta C-13 and delta O-18 if averaging a sufficient number of measurements. It seems unlikely that this applies also to GOSAT because of the lower precision and a conceptual larger sensitivity to scattering related errors in satellite viewing geometry. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Reuter, M.; Bovensmann, H.; Buchwitz, M.; Burrows, J. P.; Deutscher, N. M.; Heymann, J.; Rozanov, A.; Schneising, O.; Warneke, T.] Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany.
[Suto, H.] Japan Aerosp Explorat Agcy, Tsukuba, Ibaraki, Japan.
[Toon, G. C.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Reuter, M (reprint author), Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany.
EM maximilian.reuter@iup.physik.uni-bremen.de
RI Reuter, Maximilian/L-3752-2014; Deutscher, Nicholas/E-3683-2015;
Bovensmann, Heinrich/P-4135-2016; Burrows, John/B-6199-2014
OI Reuter, Maximilian/0000-0001-9141-3895; Deutscher,
Nicholas/0000-0002-2906-2577; Bovensmann, Heinrich/0000-0001-8882-4108;
Burrows, John/0000-0002-6821-5580
FU ESA/ESRIN (GHG-CCI); EU FP7 (MACC-II); DLR (SADOS); State and the
University of Bremen
FX This work was in part funded by ESA/ESRIN (GHG-CCI), EU FP7 (MACC-II),
DLR (SADOS), and the State and the University of Bremen. We thank NOAA
for making available the CarbonTracker CO2 fields and ECMWF
for providing the meteorological data. LSCE is thanked for maintaining
the Orleans FTS. We thank HITRAN for providing the spectroscopic
databases. Thanks to Robert L. Kurucz for making available the solar
spectra. We further thank our reviewers for their helpful and valuable
comments to improve this work.
NR 37
TC 3
Z9 3
U1 4
U2 16
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD NOV
PY 2012
VL 113
IS 16
BP 2009
EP 2017
DI 10.1016/j.jqsrt.2012.07.013
PG 9
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 017FB
UT WOS:000309574400005
ER
PT J
AU Litvinov, P
Hasekamp, O
Dubovik, O
Cairns, B
AF Litvinov, Pavel
Hasekamp, Otto
Dubovik, Oleg
Cairns, Brian
TI Model for land surface reflectance treatment: Physical derivation,
application for bare soil and evaluation on airborne and satellite
measurements
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Satellite remote sensing; Surface bidirectional reflectance; Surface
polarized reflectance; Surface reflection models; Aerosol properties
retrieval
ID DISCRETE RANDOM-MEDIA; ANGLE PHOTOPOLARIMETRIC MEASUREMENTS; RESEARCH
SCANNING POLARIMETER; AEROSOL PROPERTIES; BIDIRECTIONAL REFLECTANCE;
COHERENT BACKSCATTERING; RADIATIVE-TRANSFER; ROUGH-SURFACE; SPACEBORNE
MEASUREMENTS; POLARIZED REFLECTANCE
AB For land surfaces and atmospheric aerosol characterization on the basis of satellite and airborne measurements models for surface reflection description are required. At present time for visible and infrared spectral regions semi-empirical model for surface reflection are usually used for these purposes. Due to the lack of physical basis, these models introduce a lot of uncertainties into the problem of aerosol and surface properties retrieval. In this paper we consider the possibility of using physically based models for bidirectional reflection matrix (BRM) which can be applied to the problem of simultaneous retrieval of aerosol and land surface properties. The physical model for the BRM is derived from the general solution of the electromagnetic scattering problems by random media. The equation for the reflection matrix is obtained within the far-field approximation when the ladder scattering diagrams are taken into account. To perform analytical averaging over orientation of the surface elements we assume that at different scales the surface can be considered as the Gaussian surface. We use multi-angle photopolarimetric airborne measurements of the Research Scanning Polarimeter (RSP) and satellite POLDER (Polarization and Directionality of the Earth's Reflectances) measurements to investigate the performance of the presented BRM model. The results of the comparison are discussed. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Litvinov, Pavel; Dubovik, Oleg] Univ Lille 1, CNRS, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France.
[Hasekamp, Otto] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Cairns, Brian] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Litvinov, P (reprint author), Univ Lille 1, CNRS, Opt Atmospher Lab, Bat P5 Cite Sci, F-59655 Villeneuve Dascq, France.
EM PVLitvinov@mail.ru
RI Dubovik, Oleg/A-8235-2009;
OI Dubovik, Oleg/0000-0003-3482-6460; Cairns, Brian/0000-0002-1980-1022
FU Dutch User Support Program (USP) [GO-AO/03]
FX We are grateful to M. Mishchenko, V. Tishkovets, M. Herman, D. Tanre and
F.-M. Breon for useful discussions. Also, we thank D. Tanre and F.-M.
Breon for providing us with POLDER BRDF/BPDF database. This research was
supported by the Dutch User Support Program (USP) under project
GO-AO/03.
NR 55
TC 12
Z9 12
U1 2
U2 17
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD NOV
PY 2012
VL 113
IS 16
BP 2023
EP 2039
DI 10.1016/j.jqsrt.2012.06.027
PG 17
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 017FB
UT WOS:000309574400007
ER
PT J
AU Korkin, SV
Lyapustin, AI
Rozanov, VV
AF Korkin, Sergey V.
Lyapustin, Alexei I.
Rozanov, Vladimir V.
TI Modifications of discrete ordinate method for computations with high
scattering anisotropy: Comparative analysis
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Radiative transfer algorithms; Discrete ordinate method; Anisotropic
part; Large particles
ID RADIATIVE-TRANSFER EQUATION; PHASE FUNCTION; ATMOSPHERE; APPROXIMATION;
THICK
AB A numerical accuracy analysis of the radiative transfer equation (RTE) solution based on separation of the diffuse light field into anisotropic and smooth parts is presented. The analysis uses three different algorithms based on the discrete ordinate method (DOM). Two methods, DOMAS and DOM2+, that do not use the truncation of the phase function, are compared against the TMS-method. DOMAS and DOM2+ use the Small-Angle Modification of RTE and the single scattering term, respectively, as anisotropic parts. The TMS method uses the Delta-M method for truncation of the phase function along with the single scattering correction. For reference, a standard discrete ordinate method, DOM, is also included in analysis. The obtained results for cases with high scattering anisotropy show that at low number of streams (16, 32) only DOMAS provides an accurate solution in the aureole area. Outside aureole, the convergence and accuracy of DOMAS, and TMS is found to be approximately similar: DOMAS was found more accurate in cases with coarse aerosol and liquid water cloud models, except low optical depth, while the TMS showed better results in case of ice cloud. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Korkin, Sergey V.; Lyapustin, Alexei I.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Korkin, Sergey V.] Univ Space Res Assoc GESTAR, Columbia, MD USA.
[Rozanov, Vladimir V.] Univ Bremen, Inst Remote Sensing, D-28359 Bremen, Germany.
RP Korkin, SV (reprint author), NASA, Goddard Space Flight Ctr, Code 613, Greenbelt, MD USA.
EM sergey.v.korkin@nasa.gov
RI Lyapustin, Alexei/H-9924-2014
OI Lyapustin, Alexei/0000-0003-1105-5739
NR 24
TC 4
Z9 4
U1 1
U2 7
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD NOV
PY 2012
VL 113
IS 16
BP 2040
EP 2048
DI 10.1016/j.jqsrt.2012.07.022
PG 9
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 017FB
UT WOS:000309574400008
ER
PT J
AU Yee, HC
Sjogreen, B
Hadjadj, A
AF Yee, Helen C.
Sjoegreen, Bjorn
Hadjadj, Abdellah
TI Comparative Study of Three High Order Schemes for LES of Temporally
Evolving Mixing Layers
SO COMMUNICATIONS IN COMPUTATIONAL PHYSICS
LA English
DT Article
DE High order numerical methods; numerical methods for turbulence with
shocks; DNS; LES; mixing layer
ID TURBULENT SHEAR-LAYER; NUMERICAL DISSIPATION; DIRECT SIMULATION;
COMPRESSIBILITY; FLOWS; BEHAVIOR
AB Three high order shock-capturing schemes are compared for large eddy simulations (LES) of temporally evolving mixing layers for different convective Mach numbers ranging from the quasi-incompressible regime to highly compressible supersonic regime. The considered high order schemes are fifth-order WENO (WENO5), seventh-order WENO (WENO7) and the associated eighth-order central spatial base scheme with the dissipative portion of WENO7 as a nonlinear post-processing filter step (WENO7fi). This high order nonlinear filter method of Yee & Sjogreen is designed for accurate and efficient simulations of shock-free compressible turbulence, turbulence with shocklets and turbulence with strong shocks with minimum tuning of scheme parameters. The LES results by WENO7fi using the same scheme parameter agree well with experimental results compiled by Barone et al., and published direct numerical simulations (DNS) work of Rogers & Moser and Pantano & Sarkar, whereas results by WENO5 and WENO7 compare poorly with experimental data and DNS computations.
C1 [Yee, Helen C.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
[Sjoegreen, Bjorn] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA.
[Hadjadj, Abdellah] CORIA, UMR 6614, F-76800 St Etienne, France.
[Hadjadj, Abdellah] INSA Rouen, F-76800 St Etienne, France.
RP Yee, HC (reprint author), NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Helen.M.Yee@nasa.gov; sjogreen2@llnl.gov; hadjadj@coria.fr
FU DOE/SciDAC SAP [DE-AI02-06ER25796]; U.S. Department of Energy by
Lawrence Livermore National Laboratory [DE-AC52-07NA27344]
FX The authors wish to express their gratitude to T. Sandstrom and C. Henze
of the Visualization Group, and A. Lazanoff and J. Chang of the
Scientific Consultant Group, Code TN, NASA Ames for their help. Special
thanks to M. Rogers and A. Wray for their valuable discussion during the
course of this research. The support of the DOE/SciDAC SAP grant
DE-AI02-06ER25796 is acknowledged. Part of the work by the first author
was performed under the NASA Fundamental Aeronautics Hypersonic Program.
Work by the second author was performed under the auspices of the U.S.
Department of Energy by Lawrence Livermore National Laboratory under
Contract DE-AC52-07NA27344.
NR 43
TC 4
Z9 5
U1 0
U2 0
PU GLOBAL SCIENCE PRESS
PI WANCHAI
PA ROOM 3208, CENTRAL PLAZA, 18 HARBOUR RD, WANCHAI, HONG KONG 00000,
PEOPLES R CHINA
SN 1815-2406
EI 1991-7120
J9 COMMUN COMPUT PHYS
JI Commun. Comput. Phys.
PD NOV
PY 2012
VL 12
IS 5
BP 1603
EP 1622
DI 10.4208/cicp.261111.130412a
PG 20
WC Physics, Mathematical
SC Physics
GA 979HA
UT WOS:000306806900015
ER
PT J
AU Benafan, O
Padula, SA
Noebe, RD
Sisneros, TA
Vaidyanathan, R
AF Benafan, O.
Padula, S. A., II
Noebe, R. D.
Sisneros, T. A.
Vaidyanathan, R.
TI Role of B19 ' martensite deformation in stabilizing two-way shape memory
behavior in NiTi
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID ZN-AL ALLOYS; TEMPERATURE; STRESS; STRAIN; TRANSFORMATION; COMPRESSION;
REFINEMENT; MECHANISM; TENSION; CYCLES
AB Deformation of a B19' martensitic, polycrystalline Ni49.9Ti50.1 (at. %) shape memory alloy and its influence on the magnitude and stability of the ensuing two-way shape memory effect (TWSME) was investigated by combined ex situ mechanical experimentation and in situ neutron diffraction measurements at stress and temperature. The microstructural changes (texture, lattice strains, and phase fractions) during room-temperature deformation and subsequent thermal cycling were captured and compared to the bulk macroscopic response of the alloy. With increasing uniaxial strain, it was observed that B19' martensite deformed by reorientation and detwinning with preferred selection of the ((1) over bar 50)(M) and (010)(M) variants, (20 (1) over bar)(B19') deformation twinning, and dislocation activity. These mechanisms were indicated by changes in bulk texture from the neutron diffraction measurements. Partial reversibility of the reoriented variants and deformation twins was also captured upon load removal and thermal cycling, which after isothermal deformation to strains between 6% and 22% resulted in a strong TWSME. Consequently, TWSME functional parameters including TWSME strain, strain reduction, and transformation temperatures were characterized and it was found that prior martensite deformation to 14% strain provided the optimum condition for the TWSME, resulting in a stable two-way shape memory strain of 2.2%. Thus, isothermal deformation of martensite was found to be a quick and efficient method for creating a strong and stable TWSME in Ni49.9Ti50.1. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4764313]
C1 [Benafan, O.; Vaidyanathan, R.] Univ Cent Florida, AMPAC, Mech Mat & Aerosp Engn Dept, Orlando, FL 32816 USA.
[Benafan, O.; Padula, S. A., II; Noebe, R. D.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
[Sisneros, T. A.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Benafan, O (reprint author), Univ Cent Florida, AMPAC, Mech Mat & Aerosp Engn Dept, Orlando, FL 32816 USA.
EM othmane.benafan@nasa.gov
RI Lujan Center, LANL/G-4896-2012
FU NASA [NNX08AB51A]; Aeronautical Sciences Project; Office of Basic Energy
Sciences DOE; DOE [DE-AC52-06NA25396]
FX Funding from the NASA Fundamental Aeronautics Program, Supersonics
Project including (Grant No. NNX08AB51A) as well as the Aeronautical
Sciences Project is gratefully acknowledged. The authors thank D. W.
Brown and B. Clausen at LANL for technical support and helpful
discussions. D. E. Nicholson's help in performing the neutron
diffraction experiments is gratefully acknowledged. O.B. thanks A.
Stebner for many helpful discussions. 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 No. DE-AC52-06NA25396.
NR 48
TC 24
Z9 24
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-8979
EI 1089-7550
J9 J APPL PHYS
JI J. Appl. Phys.
PD NOV 1
PY 2012
VL 112
IS 9
AR 093510
DI 10.1063/1.4764313
PG 11
WC Physics, Applied
SC Physics
GA 049FS
UT WOS:000311968400031
ER
PT J
AU Grugel, RN
AF Grugel, Richard N.
TI Integrity of sulfur concrete subjected to simulated lunar temperature
cycles
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Sulfur; Sulfur concrete; Compression testing; Coefficient of thermal
expansion; Lunar environment
AB In view of potential application as a construction material on the lunar surface the mechanical integrity of sulfur concrete was evaluated after being subjected to simulated temperature cycles. Here, small cubes of sulfur concrete were repeatedly cycled between room (20 degrees C) and liquid nitrogen (-191 degrees C) temperatures after which they, and non-cycled cubes, were evaluated by compression testing. The compression strength of the non-cycled samples averaged similar to 35 MPa (5076 psi) before failing whereas the cycled samples fractured at about 7 MPa (1015 psi). Microscopic examination of the fracture surfaces from the cycled samples showed clear de-bonding of the sulfur from the aggregate whereas it was seen adhering in those non-cycled. Based on a simple analysis it was concluded that the large strength discrepancy between cycled and non-cycled samples is due to differences between the coefficients of thermal expansion of the materials constituting the concrete. Published by Elsevier Ltd. on behalf of COSPAR.
C1 NASA, George C Marshall Space Flight Ctr, Mat & Proc Lab, Huntsville, AL 35812 USA.
RP Grugel, RN (reprint author), NASA, George C Marshall Space Flight Ctr, Mat & Proc Lab, MS-EM31, Huntsville, AL 35812 USA.
EM richard.n.grugel@nasa.gov
FU Marshall Space Flight Center In-Space Fabrication and Repair Element;
EM30
FX The author is grateful to Professor H. Toutanji and his group for
providing sulfur concrete samples. Appreciation is also expressed to the
Marshall Space Flight Center In-Space Fabrication and Repair Element and
EM30 for their support of this work.
NR 26
TC 7
Z9 7
U1 2
U2 13
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD NOV 1
PY 2012
VL 50
IS 9
BP 1294
EP 1299
DI 10.1016/j.asr.2012.06.027
PG 6
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 012QD
UT WOS:000309250700011
ER
PT J
AU Hanselman, DH
Clark, WG
Heifetz, J
Anderl, DM
AF Hanselman, Dana H.
Clark, William G.
Heifetz, Jonathan
Anderl, Delsa M.
TI Statistical distribution of age readings of known-age sablefish
(Anoplopoma fimbria)
SO FISHERIES RESEARCH
LA English
DT Article
DE Known-age fish; Age reading errors; Geometric distribution;
Misclassification matrix; Sablefish; Stock assessment
ID AGING ERROR; OTOLITHS; MODELS; MISCLASSIFICATION; STOCK; FISH
AB A mark-recapture experiment provided a collection of 172 known-age sablefish from Alaska waters. Otoliths from each fish were read by three readers. The readings have a positive bias among young fish and a negative bias among older fish. Among otoliths of the same age, some tended to give consistently high or low annulus counts, so that the variance of age readings at each true age was about half due to variance among otoliths and half due to variance among replicate readings of individual otoliths. The statistical distribution of age reading errors is well described by an asymmetrical two-sided geometric distribution with age-varying parameters. For comparison, the error distribution was estimated with naive methods that do not use the known ages and that assume the readings are unbiased. These estimated distributions do not match the actual error distributions very well, but they do a surprisingly good job of predicting the distribution of age readings from a stock assessment model's internal estimate of a true age composition. They also produce estimates of recruitment and biomass close to those obtained with the actual error distributions when used in the present sablefish stock assessment. Published by Elsevier B.V.
C1 [Hanselman, Dana H.; Heifetz, Jonathan] NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK 99801 USA.
[Clark, William G.] Int Pacific Halibut Commiss, Seattle, WA 98199 USA.
[Anderl, Delsa M.] NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98115 USA.
RP Hanselman, DH (reprint author), NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 17109 Pt Lena Loop Rd, Juneau, AK 99801 USA.
EM dana.hanselman@noaa.gov; wgclark@u.washington.edu; jon.heifetz@noaa.gov;
delsa.anderl@noaa.gov
NR 16
TC 2
Z9 2
U1 0
U2 11
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0165-7836
J9 FISH RES
JI Fish Res.
PD NOV
PY 2012
VL 131
BP 1
EP 8
DI 10.1016/j.fishres.2012.07.004
PG 8
WC Fisheries
SC Fisheries
GA 007QP
UT WOS:000308903500001
ER
PT J
AU Hutchinson, M
Wang, JH
Swimmer, Y
Holland, K
Kohin, S
Dewar, H
Wraith, J
Vetter, R
Heberer, C
Martinez, J
AF Hutchinson, Melanie
Wang, John H.
Swimmer, Yonat
Holland, Kim
Kohin, Suzanne
Dewar, Heidi
Wraith, James
Vetter, Russ
Heberer, Craig
Martinez, Jimmy
TI The effects of a lanthanide metal alloy on shark catch rates
SO FISHERIES RESEARCH
LA English
DT Article
DE Shark bycatch; Longline; Lanthanide metal; CPUE
ID JUVENILE SCALLOPED HAMMERHEAD; SOUTHERN CALIFORNIA BIGHT;
RARE-EARTH-METAL; CARCHARHINUS-PLUMBEUS; SANDBAR SHARKS; SPINY DOGFISH;
MOVEMENT PATTERNS; ISURUS-OXYRINCHUS; ALOPIAS-VULPINUS; PACIFIC HALIBUT
AB Bycatch of sharks in longline fisheries has contributed to declines in shark populations and prompted the need for exploring novel technologies to reduce the incidental capture of sharks. One potential strategy is to exploit the unique electrosensory system of sharks, used to detect weak electric fields. Metals from the lanthanide series, made up of neodymium (Nd) and praseodymium (Pr), produce strong electric fields in water. In this study, we tested the effects of an Nd/Pr alloy on shark catch rates. Using longline fishing gear, we compared the catch rates of baited hooks affixed with either a block of the metal alloy (experimental) or a lead weight (control). Four experiments were conducted in different regions of the Pacific Ocean. Two bottom longline experiments were conducted inside and offshore of Kaneohe Bay, Hawaii. One of these experiments targeted young of the year scalloped hammerhead sharks (Sphyrna lewini), while the other targeted sandbar (Carcharhinus plumbeus) and tiger sharks (Galeocerdo cuvier). In the Southern California Bight (SCB), pelagic longlines were deployed to target mako (Isurus oxyrinchus) and blue sharks (Prionace glauca) and longlines targeting pelagic sharks were set in the Eastern Tropical Pacific (ETP) off Ecuador. There was a significant reduction in juvenile hammerhead sharks caught on hooks with the lanthanide metal compared to the controls. In contrast, there was no difference in the catch rates for experiments targeting sandbar sharks in Hawaii or those conducted in the SCB and Ecuador. These results suggest that there are inter-specific differences regarding the effects of lanthanide metals on catch rates. This may reflect the diverse feeding strategies and sensory modalities used by shark species for detecting and attacking prey. (c) 2012 Elsevier B.V. All rights reserved.
C1 [Hutchinson, Melanie; Holland, Kim] Univ Hawaii, Hawaii Inst Marine Biol, Dept Zool, Kaneohe, HI 96744 USA.
[Wang, John H.] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA.
[Swimmer, Yonat] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA.
[Kohin, Suzanne; Dewar, Heidi; Wraith, James; Vetter, Russ] Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, La Jolla, CA 92037 USA.
[Heberer, Craig] Natl Marine Fisheries Serv, Sustainable Fisheries Div, Carlsbad, CA 92011 USA.
[Martinez, Jimmy] Subsecretaria Recursos Pesqueros ECUADOR, Planes Acc Nacl Conservac & Manejo Tiburones & Do, Manabi, America Del Sur, Ecuador.
[Martinez, Jimmy] Subsecretaria Recursos Pesqueros ECUADOR, Proyecto Reducc Bycatch, Manabi, America Del Sur, Ecuador.
RP Hutchinson, M (reprint author), Univ Hawaii, Hawaii Inst Marine Biol, Dept Zool, 46-007 Lilipuna Rd, Kaneohe, HI 96744 USA.
EM melanier@hawaii.edu
FU NOAA PIFSC; University of Hawaii - JIMAR; NOAA Bycatch Reduction
Engineering Program; WWF - Galapagos; PADI Foundation grant [2009-334]
FX We would like to thank the Captain and crews of the F/V Southern
Horizon, F/V Ventura II, and F/V Siempre Olayita. We would also like to
thank Paul Rogers and the other volunteers and participants of these
research cruises. Members of the Holland Lab at HIMB, including Jon
Dale, Yannis Papastamtiou, Tom Tinhan, Austin Stankus, James Anderson,
and all of our volunteers, deserve recognition for all of their time and
effort in assisting with our fishing activities in Hawaii. We also thank
Lianne McNaughton, T. Todd Jones, Alex Bartoli, Mariluz Parga, SUBMON,
Pablo Guerrero, WWF - Galapagos, Daniel An, Simon Dalton and Eric Stroud
for their help with this project. The authors would like to acknowledge
Keith Bigelow, Christopher Boggs, Cara Empley, John Carlson and two
anonymous reviewers for their helpful comments and edits. Funding for
this research was provided by NOAA PIFSC, University of Hawaii - JIMAR,
NOAA Bycatch Reduction Engineering Program, WWF - Galapagos and PADI
Foundation grant 2009-334. Animals used in this study were handled in
accordance with the University of Hawaii's animal care protocols and
were approved by IACUC protocol #08-623.
NR 53
TC 13
Z9 14
U1 2
U2 46
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0165-7836
J9 FISH RES
JI Fish Res.
PD NOV
PY 2012
VL 131
BP 45
EP 51
DI 10.1016/j.fishres.2012.07.006
PG 7
WC Fisheries
SC Fisheries
GA 007QP
UT WOS:000308903500007
ER
PT J
AU Stoner, AW
Mueller, KW
Brown-Peterson, NJ
Davis, MH
Booker, CJ
AF Stoner, Allan W.
Mueller, Karl W.
Brown-Peterson, Nancy J.
Davis, Martha H.
Booker, Catherine J.
TI Maturation and age in queen conch (Strombus gigas): Urgent need for
changes in harvest criteria
SO FISHERIES RESEARCH
LA English
DT Article
DE Reproduction; Gastropod; Maturity; Age; Size; Bahamas; Legal harvest
ID MARINE PROTECTED AREA; REPRODUCTIVE ACTIVITY; POPULATION-STRUCTURE;
DETERMINATE GROWTH; SEXUAL-MATURITY; GENUS STROMBUS; SIZE; FISHERY;
MANAGEMENT; ABUNDANCE
AB The queen conch (Strombus gigas) is a large economically important gastropod that has been severely depleted throughout much of the Caribbean region. The species has determinate growth and reaches maximum shell length before sexual maturation; thereafter the shell grows only in thickness. In this study, queen conch were collected in the Exuma Cays, Bahamas, to evaluate maturity with respect to shell length (SL) (170-255 mm) and shell lip thickness (LT) (2-42 mm). Soft tissue weight and gonad weight increased with SL, but these same variables, along with the gonadosomatic index (gonad weight/soft tissue weight), all had dome-shaped distributions with LT and decreased slightly with LT > 22 mm. This indicates some loss of fecundity with age; however, no loss of reproductive capability was evident in histological data. Gonad maturity lagged substantially behind first formation of the shell lip. Minimum LT for reproductive maturity was 12 mm for females and 9 mm for males, and 50% maturity for the population was achieved at 26 mm LT for females and 24 mm LT for males, higher than previous estimates. A review of fishing regulations indicates that immature queen conch are being harvested legally in most Caribbean nations, providing at least a partial explanation for widespread depletion. While relationships between shell lip thickness, age, and maturity vary geographically, sustainable management of queen conch will require a minimum shell lip thickness for harvest no less than 15 mm, along with other urgently needed management measures. Published by Elsevier B.V.
C1 [Stoner, Allan W.] NOAA, Fisheries Behav Ecol Program, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
[Stoner, Allan W.] Community Conch, Waldport, OR 97394 USA.
[Mueller, Karl W.] Lummi Indian Business Council, Lummi Nat Resources Dept, Bellingham, WA 98226 USA.
[Brown-Peterson, Nancy J.] Univ So Mississippi, Dept Coastal Sci, Ocean Springs, MS 39564 USA.
[Davis, Martha H.] Community Conch, Littleton, CO 80121 USA.
[Booker, Catherine J.] Community Conch, Savannah, GA 31405 USA.
RP Stoner, AW (reprint author), NOAA, Fisheries Behav Ecol Program, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
EM allan.stoner@gmail.com
FU Community Conch; Bahamas Department of Marine Resources (DMR)
FX Funding for this project was provided by Community Conch and the Bahamas
Department of Marine Resources (DMR), and we are also grateful to the
Bahamas National Trust (BNT) and the Perry Institute for Marine Science
for logistic and in-kind support at Warderick Wells and Lee Stocking
Island, respectively. We are especially indebted to Michael Braynen and
Lester Gittens (DMR) and Eric Carey (BNT) who were critical for
institutional support. Robert Glazer and Gabriel Delgado assisted in the
field design for the project, and they along with C. Bissada, D.
Aldana-Aranda, and O. Avila-Poveda, participated in discussions about
our approach to the study of queen conch maturity and management topics.
A. McLean, A. Olson, M. Peyton, J. Stack, T. Thompson, M. Vandenrydt, A.
Vellacott, and J. Wilchcombe all assisted in field operations. L.
Bustamante performed all histological processing. We thank L.
Rogers-Bennett for constructive comments on the manuscript.
NR 56
TC 9
Z9 9
U1 5
U2 58
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0165-7836
J9 FISH RES
JI Fish Res.
PD NOV
PY 2012
VL 131
BP 76
EP 84
DI 10.1016/j.fishres.2012.07.017
PG 9
WC Fisheries
SC Fisheries
GA 007QP
UT WOS:000308903500011
ER
PT J
AU Gherlone, M
Cerracchio, P
Mattone, M
Di Sciuva, M
Tessler, A
AF Gherlone, Marco
Cerracchio, Priscilla
Mattone, Massimiliano
Di Sciuva, Marco
Tessler, Alexander
TI Shape sensing of 3D frame structures using an inverse Finite Element
Method
SO INTERNATIONAL JOURNAL OF SOLIDS AND STRUCTURES
LA English
DT Article
DE Timoshenko beam; Shape sensing; Frame structures; Inverse Finite Element
Method; Strain gauge
ID BRAGG-GRATING SENSORS; ELASTICITY PROBLEMS; SHEAR
AB A robust and efficient computational method for reconstructing the elastodynamic structural response of truss, beam, and frame structures, using measured surface-strain data, is presented. Known as "shape sensing", this inverse problem has important implications for real-time actuation and control of smart structures, and for monitoring of structural integrity. The present formulation, based on the inverse Finite Element Method (iFEM), uses a least-squares variational principle involving section strains (also known as strain measures) of Timoshenko theory for stretching, torsion, bending, and transverse shear. The present iFEM methodology is based on strain-displacement relations only, without invoking force equilibrium. Consequently, both static and time-varying displacement fields can be reconstructed without the knowledge of material properties, applied loading, or damping characteristics. Two finite elements capable of modeling frame structures are derived using interdependent interpolations, in which interior degrees of freedom are condensed out at the element level. In addition, relationships between the order of kinematic-element interpolations and the number of required strain gauges are established. Several example problems involving cantilevered beams and three-dimensional frame structures undergoing static and dynamic response are discussed. To simulate experimentally measured strains and to establish reference displacements, high-fidelity MSC/NASTRAN finite element analyses are performed. Furthermore, numerically simulated measurement errors, based on Gaussian distribution, are also considered in order to verify the stability and robustness of the methodology. The iFEM solution accuracy is examined with respect to various levels of discretization and the number of strain gauges. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Gherlone, Marco; Cerracchio, Priscilla; Mattone, Massimiliano; Di Sciuva, Marco] Politecn Torino, Dept Mech & Aerosp Engn, I-10129 Turin, Italy.
[Tessler, Alexander] NASA Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA.
RP Cerracchio, P (reprint author), Politecn Torino, Dept Mech & Aerosp Engn, Corso Duca Abruzzi 24, I-10129 Turin, Italy.
EM marco.gherlone@polito.it; priscilla.cerracchio@polito.it;
massimiliano.mattone@polito.it; marco.disciuva@polito.it;
Alexander.Tessler-1@nasa.gov
OI Gherlone, Marco/0000-0002-5711-0046
NR 30
TC 14
Z9 14
U1 1
U2 12
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0020-7683
J9 INT J SOLIDS STRUCT
JI Int. J. Solids Struct.
PD NOV 1
PY 2012
VL 49
IS 22
BP 3100
EP 3112
DI 10.1016/j.ijsolstr.2012.06.009
PG 13
WC Mechanics
SC Mechanics
GA 010KC
UT WOS:000309092300006
ER
PT J
AU Daly, B
Stoner, AW
Eckert, GL
AF Daly, Benjamin
Stoner, Allan W.
Eckert, Ginny L.
TI Predator-induced behavioral plasticity of juvenile red king crabs
(Paralithodes camtschaticus)
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE Conditioning; Crypsis; Paralithodes camtschaticus; Predation; Predator
avoidance
ID EASTERN BERING-SEA; CHEMICAL CUES; CALLINECTES-SAPIDUS;
HOMARUS-AMERICANUS; BLUE CRABS; ANTIPREDATOR MECHANISMS;
ONCORHYNCHUS-MYKISS; HABITAT COMPLEXITY; EUROPEAN LOBSTERS; STOCK
ENHANCEMENT
AB Predation and adaptations to avoid predation during early life stages have great potential to structure population dynamics and resultant community structure. Crypsis is the primary predator-avoidance mechanism for recently-settled red king crabs (Paralithodes camtschaticus); however, it is unknown if this behavioral adaptation is innate or gained with experience. Hatchery-cultured individuals may be at a disadvantage once released into the wild if they have no experience with predators. We conducted experiments with Pacific halibut (Hippoglossus stenolepis) and Pacific cod (Gad us macrocephalus) predators to determine if red king crab predator responses could be enhanced with experience. We exposed crabs to predators for 48 h either with limited exposure (chemical and visual cues only) or complete exposure (chemical, visual, and physical cues) and used video recordings to compare (1) crab crypsis, (2) crab survival, and (3) predator behavior (attack rates, capture success) among naive and experienced crabs. Halibut and cod exposure enhanced crab crypsis and survival, but only halibut exposure resulted in a significant effect. Crabs with limited and complete halibut exposure had higher initial crypsis, and both naive and conditioned crabs increased crypsis by the end of the experiment. Complete exposure initiated a stronger response compared to limited exposure. Physical interactions with predators are likely important to initiate enhanced avoidance responses. Halibut and cod attack rates and capture success did not vary when crabs had prior experience, but halibut were generally more successful at capturing prey than cod. Our results show that juvenile red king crabs respond to some predators by increasing their cryptic behavior and that this response may be enhanced with experience. For stock enhancement programs, exposing juveniles to predators in the hatchery prior to release may enhance predator avoidance and allow quick adaptation to the natural environment. (c) 2012 Elsevier B.V. All rights reserved.
C1 [Daly, Benjamin] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Seward, AK 99664 USA.
[Stoner, Allan W.] NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
[Eckert, Ginny L.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau Ctr, Juneau, AK 99801 USA.
RP Daly, B (reprint author), Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, 201 Railway Ave, Seward, AK 99664 USA.
EM ben.daly@alaska.edu
FU Sea Grant Aquaculture grant
FX This work was funded by a Sea Grant Aquaculture grant awarded to the
University of Alaska Fairbanks. Crabs were cultured at the Alutiiq Pride
Shellfish Hatchery in Seward. AK, as part of the AKCRRAB (Alaska King
Crab Research, Rehabilitation, and Biology) program. The authors would
like to thank H. McCarty, R. Painter, J. Stephan, and L. Dochterman for
helping with broodstock acquisition, J. Swingle for hatchery-rearing
assistance, J. Hetrick for hatchery logistical support, C. Magel for
video technical support, and S. Haines and M. Ottmar for assisting in
laboratory trials, seawater systems, and crab care in Newport, OR. [SS]
NR 60
TC 10
Z9 10
U1 1
U2 30
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0981
J9 J EXP MAR BIOL ECOL
JI J. Exp. Mar. Biol. Ecol.
PD NOV 1
PY 2012
VL 429
BP 47
EP 54
DI 10.1016/j.jembe.2012.06.010
PG 8
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 999BA
UT WOS:000308282900007
ER
PT J
AU Ludovisi, D
Cha, SS
Worek, WM
Ramachandran, R
AF Ludovisi, Daniele
Cha, Soyoung S.
Worek, William M.
Ramachandran, Raranaynan
TI Numerical approach and experimental verification for interface shape
determination between layered fluids subject to a magnetic field
SO JOURNAL OF MAGNETISM AND MAGNETIC MATERIALS
LA English
DT Article
DE Ferrofluid; Meniscus; Magnetic fluid; Interfacial phenomena; Magnetic
stress; Surface tension; Hydrostatics; Layered fluid systems; Bond
number
ID LIQUID-DROP; SURFACE
AB Various applications of magnetic fluids involve interface phenomena. The analysis of the hydrostatic interface shape between two immiscible liquid layers, especially under magnetic field influence, is the first step to understand the accompanying complex dynamic phenomena as well as to providing reliable numerical capabilities for their accurate prediction. This study presents a relatively simple numerical approach, and the accompanying theory, to reliably define the meniscus shape in a two-layered fluid system in presence of a horizontal magnetic field with a vertical gradient. In the course of the study, two dimensionless parameters have been derived to describe the magnetic pressure jump at the interface and the magnetic body force throughout the volume. These parameters are used to interpret the results of the analysis and to show that a horizontal magnetic field tends to flatten the meniscus shape at the interface despite of the direction of its vertical gradient. (c) 2012 Published by Elsevier B.V.
C1 [Ludovisi, Daniele; Cha, Soyoung S.; Worek, William M.] Univ Illinois, Dept Mech & Ind Engn, Chicago, IL 60607 USA.
[Ramachandran, Raranaynan] NASA, Jacobs ESTS Grp, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Worek, WM (reprint author), Univ Illinois, Dept Mech & Ind Engn, 2039 ERF,M-C 251,842 W Taylor St, Chicago, IL 60607 USA.
EM wworek@uic.edu
NR 19
TC 1
Z9 1
U1 2
U2 11
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0304-8853
J9 J MAGN MAGN MATER
JI J. Magn. Magn. Mater.
PD NOV
PY 2012
VL 324
IS 22
BP 3633
EP 3640
DI 10.1016/j.jmmm.2012.04.007
PG 8
WC Materials Science, Multidisciplinary; Physics, Condensed Matter
SC Materials Science; Physics
GA 985VX
UT WOS:000307299700004
ER
PT J
AU Hoppe, DJ
Khayatian, B
Sosnowski, JB
Bruneau, P
Johnson, A
Reising, SC
Brown, ST
AF Hoppe, D. J.
Khayatian, B.
Sosnowski, J. B.
Bruneau, P.
Johnson, A.
Reising, S. C.
Brown, S. T.
TI A three-frequency feed for millimeter wave radiometry
SO MICROWAVE AND OPTICAL TECHNOLOGY LETTERS
LA English
DT Article
DE feed horn; millimeter wave; multifrequency; radiometer
AB A high-performance millimeter-wave feed, designed for a broad-band radiometry application is presented. The feed provides three separate output ports in the 87-97 GHz, 125-135 GHz, and 161-183 GHz bands. Measured return loss is better than 20 dB in the upper two bands and 15 dB in the lowest band, and good pattern symmetry is obtained throughout all three frequency bands. (c) 2012 Wiley Periodicals, Inc. Microwave Opt Technol Lett 54:2483-2487, 2012; View this article online at wileyonlinelibrary.com. DOI 10.1002/mop.27118
C1 [Hoppe, D. J.; Khayatian, B.; Sosnowski, J. B.; Bruneau, P.; Johnson, A.; Brown, S. T.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Reising, S. C.] Colorado State Univ, Dept Elect & Comp Engn, Ft Collins, CO 80523 USA.
RP Hoppe, DJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM daniel.j.hoppe@jpl.nasa.gov
FU NASA
FX This work was supported by the NASA Earth Science Technology Advanced
Component Technology ACT-08 Program. The research described in this
article was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, and at Colorado State University, under a
contract with the National Aeronautics and Space Administration.
NR 6
TC 0
Z9 0
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0895-2477
J9 MICROW OPT TECHN LET
JI Microw. Opt. Technol. Lett.
PD NOV
PY 2012
VL 54
IS 11
BP 2483
EP 2487
DI 10.1002/mop.27118
PG 5
WC Engineering, Electrical & Electronic; Optics
SC Engineering; Optics
GA 996NP
UT WOS:000308096800009
ER
PT J
AU Airoldi, A
Davila, CG
AF Airoldi, Alessandro
Davila, Carlos G.
TI Identification of material parameters for modelling delamination in the
presence of fibre bridging
SO COMPOSITE STRUCTURES
LA English
DT Article
DE Fibre bridging; Fracture toughness; Delamination; Finite element
analysis; Cohesive laws
ID R-CURVES; COMPOSITES; FRACTURE; SPECIMEN; STRENGTH; CRACKS
AB Delamination processes often exhibit an increase in delamination resistance, or R-curve, with crack extension. It is shown that cohesive laws can represent the R-curves due to large-scale fibre bridging and that the shape of the cohesive laws can be derived from conventional experimental results. Two approaches are investigated for determining the shape parameters of cohesive laws. The first approach consists of extracting the cohesive parameters from experimental R-curves through the use of a new semi-analytical equation. The second approach consists of a numerical optimization procedure that identifies material parameters by reducing the error between a finite element model and the experimental load-deflection results. The second approach is advantageous when fibre bridging introduces inaccuracies in the experimental energy release rate measurements. In addition, the second approach can be extended to allow more complex approximations of cohesive laws. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Airoldi, Alessandro] Politecn Milan, Dipartimento Ingn Aerosp, I-20156 Milan, Italy.
[Davila, Carlos G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Airoldi, A (reprint author), Politecn Milan, Dipartimento Ingn Aerosp, Via La Masa 34, I-20156 Milan, Italy.
EM alessandro.airoldi@polimi.it; carlos.g.davila@nasa.gov
RI Davila, Carlos/D-8559-2011; Airoldi, Alessandro/F-3906-2012
OI Airoldi, Alessandro/0000-0002-4938-3407
NR 28
TC 7
Z9 7
U1 2
U2 12
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 NOV
PY 2012
VL 94
IS 11
BP 3240
EP 3249
DI 10.1016/j.compstruct.2012.05.014
PG 10
WC Materials Science, Composites
SC Materials Science
GA 978XB
UT WOS:000306778000013
ER
PT J
AU Lall, P
Lowe, R
Goebel, K
AF Lall, Pradeep
Lowe, Ryan
Goebel, Kai
TI Prognostics Health Management of Electronic Systems Under Mechanical
Shock and Vibration Using Kalman Filter Models and Metrics
SO IEEE TRANSACTIONS ON INDUSTRIAL ELECTRONICS
LA English
DT Article
DE Health monitoring; leading indicators of failure; prognostics; solder
joint reliability
ID LEAD-FREE ELECTRONICS; THERMOMECHANICAL LOADS; FEATURE-EXTRACTION;
DAMAGE INITIATION; RELIABILITY; PROGRESSION; ASSEMBLIES; DIAGNOSIS;
VEHICLES; FAILURE
AB Structural damage to ball grid array interconnects incurred during vibration testing has been monitored in the prefailure space using resistance spectroscopy-based state space vectors, rate of change of the state variable, and acceleration of the state variable. The technique is intended for condition monitoring in high reliability applications where the knowledge of impending failure is critical and the risks in terms of loss of functionality are too high to bear. Future state of the system has been estimated based on a second-order Kalman Filter model and a Bayesian Framework. The measured state variable has been related to the underlying interconnect damage in the form of inelastic strain energy density. Performance of the prognostic health management algorithm during the vibration test has been quantified using performance evaluation metrics. The methodology has been demonstrated on leadfree area-array electronic assemblies subjected to vibration. Model predictions have been correlated with experimental data. The presented approach is applicable to functional systems where corner interconnects in area-array packages may be often redundant. Prognostic metrics including alpha - lambda precision, beta accuracy, and relative accuracy have been used to assess the performance of the damage proxies. The presented approach enables the estimation of residual life based on level of risk averseness.
C1 [Lall, Pradeep] Auburn Univ, Dept Mech Engn, NSF Elect Res Ctr CAVE3, Auburn, AL 36849 USA.
[Goebel, Kai] NASA, Ames Res Ctr, Washington, DC USA.
RP Lall, P (reprint author), Auburn Univ, Dept Mech Engn, NSF Elect Res Ctr CAVE3, Auburn, AL 36849 USA.
EM lall@auburn.edu; rdl0006@auburn.edu; kai.f.goebel@nasa.gov
FU NASA-IVHM Program from the National Aeronautics and Space Administration
[NNA08BA21C]
FX This work was supported by NASA-IVHM Program Grant NNA08BA21C from the
National Aeronautics and Space Administration.
NR 67
TC 18
Z9 19
U1 5
U2 29
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0278-0046
J9 IEEE T IND ELECTRON
JI IEEE Trans. Ind. Electron.
PD NOV
PY 2012
VL 59
IS 11
BP 4301
EP 4314
DI 10.1109/TIE.2012.2183834
PG 14
WC Automation & Control Systems; Engineering, Electrical & Electronic;
Instruments & Instrumentation
SC Automation & Control Systems; Engineering; Instruments & Instrumentation
GA 965EC
UT WOS:000305748500031
ER
PT J
AU Slavin, JA
Imber, SM
Boardsen, SA
DiBraccio, GA
Sundberg, T
Sarantos, M
Nieves-Chinchilla, T
Szabo, A
Anderson, BJ
Korth, H
Zurbuchen, TH
Raines, JM
Johnson, CL
Winslow, RM
Killen, RM
McNutt, RL
Solomon, SC
AF Slavin, James A.
Imber, Suzanne M.
Boardsen, Scott A.
DiBraccio, Gina A.
Sundberg, Torbjorn
Sarantos, Menelaos
Nieves-Chinchilla, Teresa
Szabo, Adam
Anderson, Brian J.
Korth, Haje
Zurbuchen, Thomas H.
Raines, Jim M.
Johnson, Catherine L.
Winslow, Reka M.
Killen, Rosemary M.
McNutt, Ralph L., Jr.
Solomon, Sean C.
TI MESSENGER observations of a flux-transfer-event shower at Mercury
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID MAGNETIC-FIELD; SOLAR-WIND; 1ST FLYBY; MAGNETOPAUSE; MAGNETOSPHERE;
RECONNECTION; MOTION; MODEL; MAGNETOSHEATH; CLUSTER
AB Analysis of MESSENGER magnetic field observations taken in the southern lobe of Mercury's magnetotail and the adjacent magnetosheath on 11 April 2011 indicates that a total of 163 flux transfer events (FTEs) occurred within a 25 min interval. Each FTE had a duration of similar to 2-3 s and was separated in time from the next by similar to 8-10 s. A range of values have been reported at Earth, with mean values near similar to 1-2 min and similar to 8 min, respectively. We term these intervals of quasiperiodic flux transfer events "FTE showers." The northward and sunward orientation of the interplanetary magnetic field during this shower strongly suggests that the FTEs observed during this event formed just tailward of Mercury's southern magnetic cusp. The point of origin for the shower was confirmed with the Cooling model of FTE motion. Modeling of the individual FTE-type flux ropes in the magnetosheath indicates that these flux ropes had elliptical cross sections, a mean semimajor axis of 0.15 R-M (where R-M is Mercury's radius, or 2440 km), and a mean axial magnetic flux of 1.25 MWb. The lobe magnetic field was relatively constant until the onset of the FTE shower, but thereafter the field magnitude decreased steadily until the spacecraft crossed the magnetopause. This decrease in magnetic field intensity is frequently observed during FTE showers. Such a decrease may be due to the diamagnetism of the new magnetosheath plasma being injected into the tail by the FTEs.
C1 [Slavin, James A.; Imber, Suzanne M.; DiBraccio, Gina A.; Zurbuchen, Thomas H.; Raines, Jim M.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Imber, Suzanne M.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Boardsen, Scott A.; Sundberg, Torbjorn; Sarantos, Menelaos; Nieves-Chinchilla, Teresa; Szabo, Adam] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Boardsen, Scott A.; Sarantos, Menelaos; Nieves-Chinchilla, Teresa] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Anderson, Brian J.; Korth, Haje; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Johnson, Catherine L.; Winslow, Reka M.] Univ British Columbia, Dept Earth & Ocean Sci, Vancouver, BC V5Z 1M9, Canada.
[Johnson, Catherine L.] Planetary Sci Inst, Tucson, AZ USA.
[Killen, Rosemary M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Earth Inst, Palisades, NY USA.
RP Slavin, JA (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Rm 1517,Space Res Bldg,2455 Hayward St, Ann Arbor, MI 48109 USA.
EM jaslavin@umich.edu
RI Sarantos, Menelaos/H-8136-2013; Slavin, James/H-3170-2012; DiBraccio,
Gina/C-5960-2014; McNutt, Ralph/E-8006-2010; Nieves-Chinchilla,
Teresa/F-3482-2016
OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166;
Nieves-Chinchilla, Teresa/0000-0003-0565-4890
FU NASA [NASW-00002, NAS5-97271]
FX Computational assistance and data visualization support provided by J.
Feggans are gratefully acknowledged. Discussion of the
flux-transfer-event formation process with J. Raeder is also
acknowledged. The MESSENGER project is supported by the NASA Discovery
Program under contracts NASW-00002 to the Carnegie Institution of
Washington and NAS5-97271 to the Johns Hopkins University Applied
Physics Laboratory.
NR 43
TC 36
Z9 36
U1 3
U2 20
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD OCT 30
PY 2012
VL 117
AR A00M06
DI 10.1029/2012JA017926
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 031ZU
UT WOS:000310682300001
ER
PT J
AU Li, F
Waugh, DW
Douglass, AR
Newman, PA
Strahan, SE
Ma, J
Nielsen, JE
Liang, Q
AF Li, Feng
Waugh, Darryn W.
Douglass, Anne R.
Newman, Paul A.
Strahan, Susan E.
Ma, Jun
Nielsen, J. Eric
Liang, Qing
TI Long-term changes in stratospheric age spectra in the 21st century in
the Goddard Earth Observing System Chemistry-Climate Model (GEOSCCM)
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID BREWER-DOBSON CIRCULATION; MEAN AGES; TRANSPORT; AIR; TROPOSPHERE;
CHLORINE; OZONE; GASES; CH4
AB In this study we investigate long-term variations in the stratospheric age spectra using a 21st century simulation with the Goddard Earth Observing System Chemistry-Climate Model (GEOSCCM). Our purposes are to characterize the long-term changes in the age spectra, and identify processes that cause the decrease of the mean age in a changing climate. Changes in the age spectra in the 21st century simulation are characterized by decreases in the modal age, the mean age, the spectral width, and the tail decay timescale throughout the stratosphere. Our analyses show that the decrease in the mean age is caused by two processes: the acceleration of the residual circulation that increases the young air masses in the stratosphere, and the weakening of the recirculation that leads to a decrease of the tail of the age spectra and a decrease of the old air masses. Weakening of the stratospheric recirculation is also strongly correlated with the increase of the residual circulation. One important result of this study is that the decrease of the tail of the age spectra makes an important contribution to the decrease of the mean age. Long-term changes in the stratospheric isentropic mixing are also investigated. Mixing increases in the subtropical lower stratosphere, but its impact on the age spectra is smaller than the increase of the residual circulation. The impacts of the long-term changes in the age spectra on long-lived chemical tracers are also investigated.
C1 [Li, Feng; Douglass, Anne R.; Newman, Paul A.; Strahan, Susan E.; Nielsen, J. Eric; Liang, Qing] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Li, Feng; Strahan, Susan E.; Liang, Qing] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA.
[Waugh, Darryn W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Ma, Jun] Computat Phys Inc, Springfield, VA USA.
[Nielsen, J. Eric] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Li, F (reprint author), NASA, Goddard Space Flight Ctr, Code 614, Greenbelt, MD 20771 USA.
EM feng.li@nasa.gov
RI Li, Feng/H-2241-2012; Douglass, Anne/D-4655-2012; Liang,
Qing/B-1276-2011; Newman, Paul/D-6208-2012; Waugh, Darryn/K-3688-2016
OI Newman, Paul/0000-0003-1139-2508; Waugh, Darryn/0000-0001-7692-2798
FU NASA's Modeling, Analysis and Prediction program; NASA Ames Research
Center
FX This work is supported by NASA's Modeling, Analysis and Prediction
program. We thank Stacey Frith for data management. Computational
resources for this work were provided by NASA's High-Performance
Computing through the generous award of computing time at NASA Ames
Research Center.
NR 46
TC 9
Z9 9
U1 1
U2 17
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 30
PY 2012
VL 117
AR D20119
DI 10.1029/2012JD017905
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 032BK
UT WOS:000310686600001
ER
PT J
AU Foster, JL
Skofronick-Jackson, G
Meng, H
Wang, JR
Riggs, G
Kocin, PJ
Johnson, BT
Cohen, J
Hall, DK
Nghiem, SV
AF Foster, James L.
Skofronick-Jackson, Gail
Meng, Huan
Wang, James R.
Riggs, George
Kocin, Paul J.
Johnson, Benjamin T.
Cohen, Judah
Hall, Dorothy K.
Nghiem, Son V.
TI Passive microwave remote sensing of the historic February 2010
snowstorms in the Middle Atlantic region of the USA
SO HYDROLOGICAL PROCESSES
LA English
DT Article
DE snowfall; historical; microwave; AMSR-E; AMSU-B; MHS
ID SNOW WATER EQUIVALENT; SOUNDING UNIT; DEPTH; VARIABILITY; ALGORITHM;
RADIOMETRY; VAPOR; LAND
AB The snowfall in the Baltimore/Washington metropolitan area during the winter of 2009/2010 was unprecedented and caused serious snow-related disruptions. In February 2010, snowfall totals approached 2?m, and because maximum temperatures were consistently below normal, snow remained on the ground the entire month. One of the biggest contributing factors to the unusually severe winter weather in 2009/2010, throughout much of the middle latitudes, was the Arctic Oscillation. Unusually high pressure at high latitudes and low pressure at middle latitudes forced a persistent exchange of mass from north to south. In this investigation, a concerted effort was made to link remotely sensed falling snow observations to remotely sensed snow cover and snowpack observations in the Baltimore/Washington area. Specifically, the Advanced Microwave Scanning Radiometer onboard the Aqua satellite was used to assess snow water equivalent, and the Advanced Microwave Sounding Unit-B and Microwave Humidity Sounder were employed to detect falling snow. Advanced Microwave Scanning Radiometer passive microwave signatures in this study are related to both snow on the ground and surface ice layers. In regard to falling snow, signatures indicative of snowfall can be observed in high frequency brightness temperatures of Advanced Microwave Sounding Unit-B and Microwave Humidity Sounder. Indeed, retrievals show an increase in snow water equivalent after the detection of falling snow. Yet, this work also shows that falling snow intensity and/or the presence of liquid water clouds impacts the ability to reliably detect snow water equivalent. Moreover, changes in the condition of the snowpack, especially in the surface features, negatively affect retrieval performance. Copyright (C) 2011. This article is a U.S. Government work and is in the public domain in the USA.
C1 [Foster, James L.; Skofronick-Jackson, Gail; Johnson, Benjamin T.; Hall, Dorothy K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Meng, Huan; Wang, James R.; Kocin, Paul J.] NOAA, Natl Environm Satellite Data & Informat Serv, Washington, DC 20233 USA.
[Johnson, Benjamin T.] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21201 USA.
[Nghiem, Son V.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Wang, James R.; Riggs, George] Sci Syst & Applicat Inc, Lanham, MD USA.
[Cohen, Judah] Atmospher & Environm Res Inc, Lexington, MA USA.
RP Foster, JL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM James.L.Foster@nasa.gov
RI Skofronick-Jackson, Gail/D-5354-2012; Meng, Huan/F-5613-2010; Johnson,
Benjamin/E-8557-2015
OI Meng, Huan/0000-0001-6449-890X; Johnson, Benjamin/0000-0003-3444-9669
FU NASA Terrestrial Hydrology; Precipitation Measurement Missions Programs;
National Science Foundation [ARC-0909459, ARC-0909457]
FX The authors are most appreciative of the referees' efforts in helping to
make this a stronger paper. We are also grateful to Dr Richard Kelly
(University of Waterloo, Waterloo, Ontario, Canada) for his helpful
comments. Research carried out at JPL and GSFC was supported by the NASA
Terrestrial Hydrology and also the Precipitation Measurement Missions
Programs. Quality Controlled Local Climatological Data snow accumulation
observations are from NOAA/National Climatic Data Center (NCDC) and
AMSU-B/MHS data from the CLASS data system. Judah Cohen is supported by
the National Science Foundation grants ARC-0909459 and ARC-0909457.
Research carried out at the Jet Propulsion Laboratory, California
Institute of Technology and at the Goddard Space Flight Center was
supported by the NASA Terrestrial Hydrology and also the Precipitation
Measurement Missions Programs.
NR 41
TC 4
Z9 4
U1 1
U2 9
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1099-1085
J9 HYDROL PROCESS
JI Hydrol. Process.
PD OCT 30
PY 2012
VL 26
IS 22
BP 3459
EP 3471
DI 10.1002/hyp.8418
PG 13
WC Water Resources
SC Water Resources
GA 019RG
UT WOS:000309756400016
ER
PT J
AU Vasiliou, AK
Piech, KM
Reed, B
Zhang, X
Nimlos, MR
Ahmed, M
Golan, A
Kostko, O
Osborn, DL
David, DE
Urness, KN
Daily, JW
Stanton, JF
Ellison, GB
AF Vasiliou, AnGayle K.
Piech, Krzysztof M.
Reed, Beth
Zhang, Xu
Nimlos, Mark R.
Ahmed, Musahid
Golan, Amir
Kostko, Oleg
Osborn, David L.
David, Donald E.
Urness, Kimberly N.
Daily, John W.
Stanton, John F.
Ellison, G. Barney
TI Thermal decomposition of CH3CHO studied by matrix infrared spectroscopy
and photoionization mass spectroscopy
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID AB-INITIO THERMOCHEMISTRY; REACTION-RATE CONSTANTS; ACETALDEHYDE
PYROLYSIS; VINYL ALCOHOL; GAS-PHASE; HIGH-RESOLUTION; SUPERSONIC JET;
FREE-RADICALS; SHOCK-TUBE; SPECTRUM
AB A heated SiC microtubular reactor has been used to decompose acetaldehyde and its isotopomers (CH3CDO, CD3CHO, and CD3CDO). The pyrolysis experiments are carried out by passing a dilute mixture of acetaldehyde (roughly 0.1%-1%) entrained in a stream of a buffer gas (either He or Ar) through a heated SiC reactor that is 2-3 cm long and 1 mm in diameter. Typical pressures in the reactor are 50-200 Torr with the SiC tube wall temperature in the range 1200-1900 K. Characteristic residence times in the reactor are 50-200 mu s after which the gas mixture emerges as a skimmed molecular beam at a pressure of approximately 10 mu Torr. The reactor has been modified so that both pulsed and continuous modes can be studied, and results from both flow regimes are presented. Using various detection methods (Fourier transform infrared spectroscopy and both fixed wavelength and tunable synchrotron radiation photoionization mass spectrometry), a number of products formed at early pyrolysis times (roughly 100-200 mu s) are identified: H, H-2, CH3, CO, CH2=CHOH, HC=CH, H2O, and CH2=C=O; trace quantities of other species are also observed in some of the experiments. Pyrolysis of rare isotopomers of acetaldehyde produces characteristic isotopic signatures in the reaction products, which offers insight into reaction mechanisms that occur in the reactor. In particular, while the principal unimolecular processes appear to be radical decomposition CH3CHO (+M) -> CH3 + H + CO and isomerization of acetaldehyde to vinyl alcohol, it appears that the CH2CO and HCCH are formed (perhaps exclusively) by bimolecular reactions, especially those involving hydrogen atom attacks. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4759050]
C1 [Vasiliou, AnGayle K.; Piech, Krzysztof M.; Reed, Beth; Ellison, G. Barney] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA.
[Vasiliou, AnGayle K.; Nimlos, Mark R.] Natl Renewable Energy Lab, Golden, CO 80401 USA.
[Zhang, Xu] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ahmed, Musahid; Golan, Amir; Kostko, Oleg] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Chem Sci, Berkeley, CA 94720 USA.
[Osborn, David L.] Sandia Natl Labs, Combust Res Facil, Livermore, CA 94551 USA.
[David, Donald E.] Univ Colorado, CIRES, Integrated Instrument Design Facil, Boulder, CO 80309 USA.
[Urness, Kimberly N.; Daily, John W.] Univ Colorado, Dept Mech Engn, Ctr Combust & Environm Res, Boulder, CO 80309 USA.
[Stanton, John F.] Univ Texas Austin, Dept Chem, Inst Theoret Chem, Austin, TX 78712 USA.
RP Vasiliou, AK (reprint author), Univ Colorado, Dept Chem & Biochem, Campus Box 215, Boulder, CO 80309 USA.
EM xu.zhang@jpl.nasa.gov; mark_nimlos@nrel.gov; mahmed@lbl.gov;
dlosbor@sandia.gov; john.daily@colorado.edu; jfstanton@mail.utexas.edu;
barney@jila.colorado.edu
RI Ahmed, Musahid/A-8733-2009; Kostko, Oleg/B-3822-2009
OI Kostko, Oleg/0000-0003-2068-4991
FU United States Department of Energy [DE-FG02-93ER14364]; United States
Department of Energy's Office of the Biomass Program [1544759]; National
Science Foundation [CHE-0848606, CHE-1112466]; Swiss National Science
Foundation; National Aeronautics and Space Administration (NASA); Office
of Energy Research, Office of Basic Energy Sciences, and Chemical
Sciences Division of the U.S. Department of Energy [DE-AC02-05CH11231];
Division of Chemical Sciences, Geosciences, and Biosciences, the Office
of Basic Energy Sciences, the U.S. Department of Energy; National
Nuclear Security Administration [DE-AC04-94-AL85000]; Robert A. Welch
Foundation [F-1283]; United States Department of Energy, Basic Energy
Sciences
FX We would like to acknowledge support from the United States Department
of Energy (Grant No. DE-FG02-93ER14364), the United States Department of
Energy's Office of the Biomass Program (Contract No. 1544759), and the
National Science Foundation (CHE-0848606 and CHE-1112466) for J.W.D.,
J.F.S., M.R.N., and G. B. E. K. M. P. was supported by the Swiss
National Science Foundation. X.Z. would like to acknowledge support from
the National Aeronautics and Space Administration (NASA) Planetary
Atmospheres Program. M. A., A. G., O.K. and the ALS are supported by the
Director, Office of Energy Research, Office of Basic Energy Sciences,
and Chemical Sciences Division of the U.S. Department of Energy under
Contract Nos. DE-AC02-05CH11231. D.L.O. is supported by the Division of
Chemical Sciences, Geosciences, and Biosciences, the Office of Basic
Energy Sciences, the U.S. Department of Energy. Sandia is a multiprogram
laboratory operated by Sandia Corporation, a Lockheed Martin Company,
for the National Nuclear Security Administration under Contract No.
DE-AC04-94-AL85000. J.F.S. also acknowledges support from the Robert A.
Welch Foundation (Grant No. F-1283) and the United States Department of
Energy, Basic Energy Sciences. Finally, we would like to thank John R.
Barker, Han-Heinrich Carstensen, William H. Green, Anne B. McCoy, Robert
J. McMahon, and I. W. M. Smith for provocative discussions.
NR 75
TC 16
Z9 16
U1 3
U2 64
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-9606
EI 1089-7690
J9 J CHEM PHYS
JI J. Chem. Phys.
PD OCT 28
PY 2012
VL 137
IS 16
AR 164308
DI 10.1063/1.4759050
PG 14
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 034ES
UT WOS:000310853800024
PM 23126711
ER
PT J
AU Nghiem, SV
Hall, DK
Mote, TL
Tedesco, M
Albert, MR
Keegan, K
Shuman, CA
DiGirolamo, NE
Neumann, G
AF Nghiem, S. V.
Hall, D. K.
Mote, T. L.
Tedesco, M.
Albert, M. R.
Keegan, K.
Shuman, C. A.
DiGirolamo, N. E.
Neumann, G.
TI The extreme melt across the Greenland ice sheet in 2012
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SURFACE-TEMPERATURE; MICROWAVE-FREQUENCIES; DIELECTRIC-CONSTANT;
CLEAR-SKY; MODIS; SNOW; VALIDATION; AVHRR
AB The discovery of the 2012 extreme melt event across almost the entire surface of the Greenland ice sheet is presented. Data from three different satellite sensors - including the Oceansat-2 scatterometer, the Moderate-resolution Imaging Spectroradiometer, and the Special Sensor Microwave Imager/Sounder - are combined to obtain composite melt maps, representing the most complete melt conditions detectable across the ice sheet. Satellite observations reveal that melt occurred at or near the surface of the Greenland ice sheet across 98.6% of its entire extent on 12 July 2012, including the usually cold polar areas at high altitudes like Summit in the dry snow facies of the ice sheet. This melt event coincided with an anomalous ridge of warm air that became stagnant over Greenland. As seen in melt occurrences from multiple ice core records at Summit reported in the published literature, such a melt event is rare with the last significant one occurring in 1889 and the next previous one around seven centuries earlier in the Medieval Warm Period. Given its rarity, the 2012 extreme melt across Greenland provides an exceptional opportunity for new studies in broad interdisciplinary geophysical research. Citation: Nghiem, S. V., D. K. Hall, T. L. Mote, M. Tedesco, M. R. Albert, K. Keegan, C. A. Shuman, N. E. DiGirolamo, and G. Neumann (2012), The extreme melt across the Greenland ice sheet in 2012, Geophys. Res. Lett., 39, L20502, doi:10.1029/2012GL053611.
C1 [Nghiem, S. V.; Neumann, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hall, D. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mote, T. L.] Univ Georgia, Dept Geog, Athens, GA 30602 USA.
[Tedesco, M.] CUNY, Dept Earth & Atmospher Sci, New York, NY 10021 USA.
[Albert, M. R.; Keegan, K.] Dartmouth Coll, Thayer Sch Engn, Hanover, NH 03755 USA.
[Shuman, C. A.] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21201 USA.
[DiGirolamo, N. E.] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Nghiem, SV (reprint author), CALTECH, Jet Prop Lab, MS 300-235,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM son.v.nghiem@jpl.nasa.gov
RI Tedesco, Marco/F-7986-2015;
OI Albert, Mary/0000-0001-7842-2359; Mote, Thomas/0000-0002-0021-0134
FU National Aeronautics and Space Administration (NASA) Cryospheric
Sciences Program; NASA Headquaters Science Innovation Fund (SIF); NASA
Cryospheric Program; National Science Foundation [ARC 0909388,
IGERT-0801490]
FX The research carried out at the Jet Propulsion Laboratory, California
Institute of Technology, and at NASA Goddard Space Flight Center (GSFC)
was supported by the National Aeronautics and Space Administration
(NASA) Cryospheric Sciences Program. We would like to acknowledge the
support of the NASA Headquaters Science Innovation Fund (SIF), which
helped to fund ongoing work at GSFC to blend the melt maps from the
three different instruments. The work at the City College of New York
was supported by the NASA Cryospheric Program and the National Science
Foundation grant ARC 0909388. Field observations of the melt at Summit
and NEEM were carried out under support from the National Science
Foundation grant IGERT-0801490 to Dartmouth College. Near-surface air
temperature data in July 2012 are courtesy of Thomas Mefford (NOAA Earth
System Research Laboratory Boulder, Colorado and Cooperative Institute
for Research in Environmental Sciences, University of Colorado at
Boulder) with additional processing by Michael J. Schnaubelt (University
of Maryland, Baltimore County, Joint Center for Earth Systems Technology
and Department of Physics, Baltimore, Maryland).
NR 31
TC 139
Z9 141
U1 8
U2 87
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD OCT 27
PY 2012
VL 39
AR L20502
DI 10.1029/2012GL053611
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 027IP
UT WOS:000310346000005
ER
PT J
AU Racherla, PN
Shindell, DT
Faluvegi, GS
AF Racherla, P. N.
Shindell, D. T.
Faluvegi, G. S.
TI The added value to global model projections of climate change by
dynamical downscaling: A case study over the continental US using the
GISS-ModelE2 and WRF models
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SPACE-TIME CLIMATE; PART I; GATOR-GCMM; SIMULATIONS; VARIABILITY;
PARAMETERIZATION; PRECIPITATION; SENSITIVITY; WEATHER; SYSTEM
AB Dynamical downscaling is being increasingly used for climate change studies, wherein the climates simulated by a coupled atmosphere-ocean general circulation model (AOGCM) for a historical and a future (projected) decade are used to drive a regional climate model (RCM) over a specific area. While previous studies have demonstrated that RCMs can add value to AOGCM-simulated climatologies over different world regions, it is unclear as to whether or not this translates to a better reproduction of the observed climate change therein. We address this issue over the continental U. S. using the GISS-ModelE2 and WRF models, a state-of-the-science AOGCM and RCM, respectively. As configured here, the RCM does not effect holistic improvement in the seasonally and regionally averaged surface air temperature or precipitation for the individual historical decades. Insofar as the climate change between the two decades is concerned, the RCM does improve upon the AOGCM when nudged in the domain proper, but only modestly so. Further, the analysis indicates that there is not a strong relationship between skill in capturing climatological means and skill in capturing climate change. Though additional research would be needed to demonstrate the robustness of this finding in AOGCM/RCM models generally, the evidence indicates that, for climate change studies, the most important factor is the skill of the driving global model itself, suggesting that highest priority should be given to improving the long-range climate skill of AOGCMs.
C1 [Racherla, P. N.; Shindell, D. T.; Faluvegi, G. S.] Columbia Univ, Ctr Climate Syst Res, Earth Inst, New York, NY 10025 USA.
[Racherla, P. N.; Shindell, D. T.; Faluvegi, G. S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Racherla, PN (reprint author), Columbia Univ, Ctr Climate Syst Res, Earth Inst, Armstrong Hall,2880 Broadway, New York, NY 10025 USA.
EM pavan.racherla+jpub@gmail.com
RI Shindell, Drew/D-4636-2012
FU NASA
FX This research was fully supported by NASA on an Applied Sciences Grant.
We thank the three (anonymous) reviewers who helped improve the
manuscript.
NR 41
TC 38
Z9 39
U1 1
U2 27
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 27
PY 2012
VL 117
AR D20118
DI 10.1029/2012JD018091
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 027HS
UT WOS:000310343700001
ER
PT J
AU Shriver, JF
Arbic, BK
Richman, JG
Ray, RD
Metzger, EJ
Wallcraft, AJ
Timko, PG
AF Shriver, J. F.
Arbic, B. K.
Richman, J. G.
Ray, R. D.
Metzger, E. J.
Wallcraft, A. J.
Timko, P. G.
TI An evaluation of the barotropic and internal tides in a high-resolution
global ocean circulation model
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID SATELLITE ALTIMETRY; HAWAIIAN RIDGE; GENERATION; DISSIPATION; ACCURACY
AB Global comparisons of barotropic and internal tides generated in an eddy-resolving ocean circulation model are made with tidal estimates obtained from altimetric sea surface heights and an altimetry-constrained tide model. As far as we know, our Hybrid Coordinate Ocean Model (HYCOM) simulations shown here and in an earlier paper are the only published high-resolution global simulations to contain barotropic tides, internal tides, the general circulation, and mesoscale eddies concurrently. Comparing the model barotropic tide with a global data-assimilative shallow water tide model shows that the global tidal elevation differences are approximately evenly split between discrepancies in tidal amplitude and phase. Both the model and observations show strong generation of internal tides at a limited number of "hot spot" regions with propagation of beams of energy for thousands of kilometers away from the sources. The model internal tidal amplitudes compare well with observations near these energetic tidal regions. Averaged over these regions, the model and observation internal tide amplitude estimates agree to approximately 15% for the four largest semidiurnal constituents and 23% for the four largest diurnal constituents. Away from the hot spots, the comparison between the model and altimetric amplitude is not as good due, in part, to two problems, errors in the model barotropic tides and overestimation of the altimetric tides in regions of strong mesoscale eddy activity. Examining the general energy distribution of the simulated internal tide is an important first step in the evaluation of internal tides in HYCOM.
C1 [Shriver, J. F.; Richman, J. G.; Metzger, E. J.; Wallcraft, A. J.] USN, Res Lab, Stennis Space Ctr, MS 39529 USA.
[Arbic, B. K.; Timko, P. G.] Univ Michigan, Dept Earth & Environm Sci, Ann Arbor, MI 48109 USA.
[Ray, R. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Shriver, JF (reprint author), USN, Res Lab, Stennis Space Ctr, MS 39529 USA.
EM jay.shriver@nrlssc.navy.mil
RI Ray, Richard/D-1034-2012;
OI Arbic, Brian K/0000-0002-7969-2294
FU Eddy Resolving Global Ocean Prediction Including Tides; Office of Naval
Research (ONR) [0602435N]; Naval Research Laboratory
[N000173-06-2-C003]; ONR [N00014-09-1-1003, N00014-11-1-0487]
FX J.F.S., J.G.R., E.J.M., and A.J.W. were supported by the project "Eddy
Resolving Global Ocean Prediction Including Tides" sponsored by the
Office of Naval Research (ONR) under program element number 0602435N.
B.K.A. and P.G.T. acknowledge support from Naval Research Laboratory
contract N000173-06-2-C003 and ONR grants N00014-09-1-1003 and
N00014-11-1-0487. The model results were obtained under the FY09-11
Department of Defense HPC Challenge Project "Eddy Resolving Global Ocean
Prediction including Tides." This is NRL contribution
NRL/JA/7320-12-1201.
NR 24
TC 25
Z9 25
U1 1
U2 16
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD OCT 27
PY 2012
VL 117
AR C10024
DI 10.1029/2012JC008170
PG 14
WC Oceanography
SC Oceanography
GA 027HX
UT WOS:000310344200002
ER
PT J
AU Fassett, CI
Head, JW
Baker, DMH
Zuber, MT
Smith, DE
Neumann, GA
Solomon, SC
Klimczak, C
Strom, RG
Chapman, CR
Prockter, LM
Phillips, RJ
Oberst, J
Preusker, F
AF Fassett, Caleb I.
Head, James W.
Baker, David M. H.
Zuber, Maria T.
Smith, David E.
Neumann, Gregory A.
Solomon, Sean C.
Klimczak, Christian
Strom, Robert G.
Chapman, Clark R.
Prockter, Louise M.
Phillips, Roger J.
Oberst, Juergen
Preusker, Frank
TI Large impact basins on Mercury: Global distribution, characteristics,
and modification history from MESSENGER orbital data
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID CRATERING RECORD; LONGITUDE RANGE; CALORIS BASIN; MOON-MERCURY; SURFACE;
EVOLUTION; LUNAR; RELAXATION; TOPOGRAPHY; VOLCANISM
AB The formation of large impact basins (diameter D >= 300 km) was an important process in the early geological evolution of Mercury and influenced the planet's topography, stratigraphy, and crustal structure. We catalog and characterize this basin population on Mercury from global observations by the MESSENGER spacecraft, and we use the new data to evaluate basins suggested on the basis of the Mariner 10 flybys. Forty-six certain or probable impact basins are recognized; a few additional basins that may have been degraded to the point of ambiguity are plausible on the basis of new data but are classified as uncertain. The spatial density of large basins (D >= 500 km) on Mercury is lower than that on the Moon. Morphological characteristics of basins on Mercury suggest that on average they are more degraded than lunar basins. These observations are consistent with more efficient modification, degradation, and obliteration of the largest basins on Mercury than on the Moon. This distinction may be a result of differences in the basin formation process (producing fewer rings), relaxation of topography after basin formation (subduing relief), or rates of volcanism (burying basin rings and interiors) during the period of heavy bombardment on Mercury from those on the Moon.
C1 [Fassett, Caleb I.] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA.
[Head, James W.; Baker, David M. H.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Zuber, Maria T.; Smith, David E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Smith, David E.; Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Solomon, Sean C.; Klimczak, Christian] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20005 USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Strom, Robert G.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Chapman, Clark R.; Phillips, Roger J.] SW Res Inst, Dept Space Sci, Boulder, CO USA.
[Prockter, Louise M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Oberst, Juergen; Preusker, Frank] German Aerosp Ctr, Inst Planetary Res, Berlin, Germany.
RP Fassett, CI (reprint author), Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA.
EM cfassett@mtholyoke.edu
RI Neumann, Gregory/I-5591-2013;
OI Neumann, Gregory/0000-0003-0644-9944; Fassett, Caleb/0000-0001-9155-3804
FU NASA [NAS5-97271]; Carnegie Institution of Washington [NASW-00002]
FX The Integrated Software for Imagers and Spectrometers (ISIS) software
package of the United States Geological Survey was used for data
processing in this study. We thank Thomas Kneissl for developing and
sharing the CraterTools extension to ArcMap. Mapping by Seth Kadish from
MESSENGER flyby data helped contribute to this analysis. Reviews by Ken
Tanaka and an anonymous reviewer improved this manuscript. The MESSENGER
project is supported by NASA Discovery program through contracts to The
Johns Hopkins Applied Physics Laboratory (NAS5-97271) and the Carnegie
Institution of Washington (NASW-00002).
NR 72
TC 28
Z9 28
U1 1
U2 19
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 OCT 27
PY 2012
VL 117
AR E00L08
DI 10.1029/2012JE004154
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 027HE
UT WOS:000310342300001
ER
PT J
AU Margot, JL
Peale, SJ
Solomon, SC
Hauck, SA
Ghigo, FD
Jurgens, RF
Yseboodt, M
Giorgini, JD
Padovan, S
Campbell, DB
AF Margot, Jean-Luc
Peale, Stanton J.
Solomon, Sean C.
Hauck, Steven A., II
Ghigo, Frank D.
Jurgens, Raymond F.
Yseboodt, Marie
Giorgini, Jon D.
Padovan, Sebastiano
Campbell, Donald B.
TI Mercury's moment of inertia from spin and gravity data
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MOLTEN CORE; LIBRATION; LONGITUDE; BODY
AB Earth-based radar observations of the spin state of Mercury at 35 epochs between 2002 and 2012 reveal that its spin axis is tilted by (2.04 +/- 0.08) arc min with respect to the orbit normal. The direction of the tilt suggests that Mercury is in or near a Cassini state. Observed rotation rate variations clearly exhibit an 88-day libration pattern which is due to solar gravitational torques acting on the asymmetrically shaped planet. The amplitude of the forced libration, (38.5 +/- 1.6) arc sec, corresponds to a longitudinal displacement of similar to 450 m at the equator. Combining these measurements of the spin properties with second-degree gravitational harmonics (Smith et al., 2012) provides an estimate of the polar moment of inertia of Mercury C/MR2 = 0.346 +/- 0.014, where M and R are Mercury's mass and radius. The fraction of the moment that corresponds to the outer librating shell, which can be used to estimate the size of the core, is C-m/C = 0.431 +/- 0.025.
C1 [Margot, Jean-Luc; Padovan, Sebastiano] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Margot, Jean-Luc] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Peale, Stanton J.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Hauck, Steven A., II] Case Western Reserve Univ, Dept Earth Environm & Planetary Sci, Cleveland, OH 44106 USA.
[Ghigo, Frank D.] Natl Radio Astron Lab, Green Bank, WV USA.
[Jurgens, Raymond F.; Giorgini, Jon D.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Yseboodt, Marie] Royal Observ Belgium, Uccle, Belgium.
[Campbell, Donald B.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
RP Margot, JL (reprint author), Univ Calif Los Angeles, Dept Earth & Space Sci, 595 Charles Young Dr E, Los Angeles, CA 90095 USA.
EM jlm@ess.ucla.edu
RI Margot, Jean-Luc/A-6154-2012; Hauck, Steven/A-7865-2008
OI Margot, Jean-Luc/0000-0001-9798-1797; Hauck, Steven/0000-0001-8245-146X
FU Jet Propulsion Laboratory
FX We are very grateful to Igor Holin for bringing the radar speckle
displacement technique to our attention. We thank J. Jao, R. Rose, J.
Van Brimmer, L. Juare, M. Silva, L. Snedeker, D. Choate, D. Kelley, C.
Snedeker, C. Franck, L. Teitlebaum, M. Slade, R. Maddalena, C. Bignell,
T. Minter, M. Stennes, and F. Lo for assistance with the observations.
The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc. Part of this work was supported by the Jet Propulsion
Laboratory, operated by Caltech under contract with the National
Aeronautics and Space Administration.
NR 29
TC 34
Z9 34
U1 0
U2 14
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 OCT 27
PY 2012
VL 117
AR E00L09
DI 10.1029/2012JE004161
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 027HE
UT WOS:000310342300002
ER
PT J
AU Burlaga, LF
Ness, NF
AF Burlaga, L. F.
Ness, N. F.
TI Magnetic field fluctuations observed in the heliosheath by Voyager 1 at
114 +/- 2 AU during 2010
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID COSMIC-RAY MODULATION; SOLAR-WIND; TERMINATION SHOCK; HELIOSPHERE;
TURBULENCE; ACCELERATION; TRANSPORT; PLASMA
AB The radial component of the flow speed VR in the heliosheath was decreasing between 2009.0 (108.5 AU) and 2010.3, at which time it reached the "stagnation region" where VR approximate to 0 km/s from 2010.3 to at least to 2011.0 (115.7 AU). The fluctuations of the hour averages of the magnetic field B observed by Voyager 1 (V1) each day throughout 2010 were primarily compressive (longitudinal) fluctuations, along the T (average B) direction in HG coordinates. The yearly average of the daily standard deviations (SD) of the compressive component of B was < SDc > = < SD(BT)> approximate to < SD(B)> approximate to 0.015 nT. The corresponding standard deviations of the transverse components < SDt > = SD(BR) > approximate to < SD(BN)> approximate to 0.006 nT. During 2010, < SDc >/< SDt > > 2.6 and < SDc >/< B > = 0.15. The counting rate of cosmic rays >70 MeV/nuc tends to increase with increasing B and SDc, contrary to expectations.
C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Code 673, Greenbelt, MD 20771 USA.
EM lburlagahsp@verizon.net
FU NASA [NASA NNX 07AW09G, NNX 09AT41G]
FX Daniel Berdichevsky computed the zero level offsets for the instrument.
The data were processed by T. McClanahan and S. Kramer. N. F. Ness was
partially supported by NASA grants NASA NNX 07AW09G and NASA NNX 09AT41G
to the Catholic University of America.
NR 26
TC 3
Z9 3
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD OCT 27
PY 2012
VL 117
AR A10107
DI 10.1029/2012JA017894
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 027II
UT WOS:000310345300001
ER
PT J
AU Hulley, GC
Hook, SJ
AF Hulley, Glynn C.
Hook, Simon J.
TI A radiance-based method for estimating uncertainties in the Atmospheric
Infrared Sounder (AIRS) land surface temperature product
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID REMOTE-SENSING DATA; GRAN DESIERTO; EMISSIVITY DATABASE; VALIDATION;
MODIS; MEXICO; CALIBRATION; ASTER; SPECTROSCOPY; RETRIEVALS
AB Land Surface Temperature (LST) has been identified by NASA and other international organizations as an important Earth System Data Record (ESDR). An ESDR is defined as a long-term, well calibrated and validated data set. Identifying uncertainties in LST products with coarse spatial resolutions (>10 km) such as those from hyperspectral infrared sounders is notoriously difficult due to the challenges of making reliable in situ measurements representative of the spatial scales of the output products. In this study we utilize a Radiance-based (R-based) LST method for estimating uncertainties in the Atmospheric Infrared Sounder (AIRS) v5 LST product. The R-based method provides estimates of the true LST using a radiative closure simulation without the need for in situ measurements, and requires input air temperature, relative humidity profiles and emissivity data. The R-based method was employed at three validation sites over the Namib Desert, Gran Desierto, and Redwood National Park for all AIRS observations from 2002 to 2010. Results showed daytime LST root-mean square errors (RMSE) of 2-3 K at the Namib and Desierto sites, and 1.5 K at the Redwood site. Nighttime LST RMSEs at the two desert sites were a factor of two less when compared to daytime results. Positive daytime LST biases were found at each site due to an underestimation of the daytime AIRS v5 longwave spectral emissivity, while the reverse occurred at nighttime. In the AIRS v6 product (release 2012), LST biases and RMSEs will be reduced significantly due to improved methodologies for the surface retrieval and emissivity first guess.
C1 [Hulley, Glynn C.; Hook, Simon J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Hulley, GC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM glynn.hulley@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX We would like to thank Stephen Scheidt, from the Smithsonian Center for
Earth and Planetary Studies, for providing the Gran Desierto emissivity
lab spectra. The research described in this paper was carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under the
contract with the National Aeronautics and Space Administration.
NR 39
TC 8
Z9 8
U1 2
U2 16
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 26
PY 2012
VL 117
AR D20117
DI 10.1029/2012JD018102
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 027HP
UT WOS:000310343400004
ER
PT J
AU Murray, LT
Jacob, DJ
Logan, JA
Hudman, RC
Koshak, WJ
AF Murray, Lee T.
Jacob, Daniel J.
Logan, Jennifer A.
Hudman, Rynda C.
Koshak, William J.
TI Optimized regional and interannual variability of lightning in a global
chemical transport model constrained by LIS/OTD satellite data
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID OPTICAL TRANSIENT DETECTOR; TROPOSPHERIC OZONE PRODUCTION;
GENERAL-CIRCULATION MODEL; TROPICAL DEEP CONVECTION; LONG-RANGE
TRANSPORT; EL-NINO EVENT; NITROGEN-OXIDES; MONITORING INSTRUMENT;
AIRBORNE MEASUREMENTS; IMAGING SENSOR
AB Nitrogen oxides (NOx = NO + NO2) produced by lightning make a major contribution to the global production of tropospheric ozone and OH. Lightning distributions inferred from standard convective parameterizations in global chemical transport models (CTMs) fail to reproduce observations from the Lightning Imaging Sensor (LIS) and the Optical Transient Detector (OTD) satellite instruments. We present an optimal regional scaling algorithm for CTMs to fit the lightning NOx source to the satellite lightning data in a way that preserves the coupling to deep convective transport. We show that applying monthly scaling factors over similar to 37 regions globally significantly improves the tropical ozone simulation in the GEOS-Chem CTM as compared to a simulation unconstrained by the satellite data and performs equally well to a simulation with local scaling. The coarse regional scaling preserves sufficient statistics in the satellite data to constrain the interannual variability (IAV) of lightning. After processing the LIS data to remove their diurnal sampling bias, we construct a monthly time series of lightning flash rates for 1998-2010 and 35 degrees S-35 degrees N. We find a correlation of IAV in total tropical lightning with El Nino but not with the solar cycle or the quasi-biennial oscillation. The global lightning NOx source +/- IAV standard deviation in GEOS-Chem is 6.0 +/- 0.5 Tg N yr(-1), compared to 5.5 +/- 0.8 Tg N yr(-1) for the biomass burning source. Lightning NOx could have a large influence on the IAV of tropospheric ozone because it is released in the upper troposphere where ozone production is most efficient.
C1 [Murray, Lee T.; Jacob, Daniel J.; Logan, Jennifer A.; Hudman, Rynda C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Koshak, William J.] NASA Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL USA.
RP Murray, LT (reprint author), Harvard Univ, Sch Engn & Appl Sci, 29 Oxford St, Cambridge, MA 02138 USA.
EM ltmurray@seas.harvard.edu
RI Chem, GEOS/C-5595-2014; Murray, Lee/F-2296-2014; Hudman,
Rynda/C-6118-2009
OI Murray, Lee/0000-0002-3447-3952;
FU NASA Atmospheric Composition Modeling and Analysis Program (ACMAP); NASA
Graduate Student Researchers Program; NASA Earth and Space Science
Fellowship; NASA [NNX08AJ16G, NNH09ZDA001N]
FX We acknowledge useful discussions with R. V. Martin and B. Sauvage
(Dalhousie), K. E. Pickering, D. Allen, L. E. Ott (UMD/UMBC/GSFC), H.
Huntrieser (DLR), D. B. A. Jones (University of Toronto), and L.
Jourdain (JPL). This work was supported by the NASA Atmospheric
Composition Modeling and Analysis Program (ACMAP). L. T. M. was also
partly supported by the NASA Graduate Student Researchers Program and a
NASA Earth and Space Science Fellowship. J.A.L. was supported by NASA
grants NNX08AJ16G and NNH09ZDA001N.
NR 90
TC 63
Z9 64
U1 1
U2 39
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 26
PY 2012
VL 117
AR D20307
DI 10.1029/2012JD017934
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 027HP
UT WOS:000310343400003
ER
PT J
AU Zhang, X
Sander, SP
Stanton, JF
AF Zhang, Xu
Sander, Stanley P.
Stanton, John F.
TI Detection of the Far-IR v(12) Bending Level in Propargyl: A Complete Set
of Fundamentals for an Important Radical
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID MATRIX-ISOLATION; SPECTROSCOPY; SPECTRUM; ALLENE; H2CCCH;
METHYLACETYLENE; PHOTOLYSIS; BENZENE; HCCCH2; AR
AB Propargyl (HCCCH2) radicals have been generated by expanding precursors through a supersonic pyrolysis nozzle, and their infrared (IR) absorption spectra have been recorded in a rare gas matrix. Besides the 10 vibrational modes observed in our previous studies, this investigation detected the HCCCH2 (X) over bar B-2(1) in-plane bending mode (v(12)) at 344.2 (+/- 0.8) cm(-1) in a cryogenic argon matrix. This is the first experimental observation of v(12) for the propargyl radical. In the previous study, v(12) had been fixed at 333 (+/- 10) cm(-1) based on detection of its overtone (2v(12), 667.7 +/- 1.0 cm(-1)) and a possible combination band (v(10) + v(12), 1339.0 +/- 0.8 cm(-1)). The new observation is in reasonable agreement with this previous experimental estimation of v(12). Ab initio coupled cluster anharmonic force field calculations were used to guide the analysis. Our finding completes the fundamental frequency database for propargyl.
C1 [Zhang, Xu; Sander, Stanley P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Stanton, John F.] Univ Texas Austin, Inst Theoret Chem, Dept Chem, Austin, TX 78712 USA.
RP Zhang, X (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM xu.zhang@jpl.nasa.gov; Stanley.p.sander@jpl.nasa.gov;
jfstanton@mail.utexas.edu
FU NASA planetary atmosphere program; U.S. Department of Energy; Robert A.
Welch Foundations
FX This research was carried out by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration (NASA). This work was supported by
the grant from the NASA planetary atmosphere program. Additional support
for this work comes from the U.S. Department of Energy and the Robert A.
Welch Foundations (to J.F.S.). The authors would also like to thank Dave
Nazic for his laboratory support. Copyright 2012 California Institute of
Technology. Government sponsorship is acknowledged.
NR 31
TC 3
Z9 3
U1 1
U2 13
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD OCT 25
PY 2012
VL 116
IS 42
BP 10338
EP 10343
DI 10.1021/jp305390p
PG 6
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 024PJ
UT WOS:000310120800009
PM 22970766
ER
PT J
AU Tadic, JM
AF Tadic, Jovan M.
TI Comment on "308 nm Photolysis of Nitric Acid in the Gas Phase, on
Aluminum Surfaces, and on Ice Films"
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Editorial Material
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Tadic, JM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RI Tadic, Jovan/P-3677-2016
NR 2
TC 1
Z9 1
U1 1
U2 7
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD OCT 25
PY 2012
VL 116
IS 42
BP 10463
EP 10464
DI 10.1021/jp307052w
PG 2
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 024PJ
UT WOS:000310120800024
PM 23016500
ER
PT J
AU Ham, YG
Rienecker, MM
Schubert, S
Marshak, J
Yeh, SW
Yang, SC
AF Ham, Yoo-Geun
Rienecker, Michele M.
Schubert, Siegfried
Marshak, Jelena
Yeh, Sang-Wook
Yang, Shu-Chih
TI The decadal modulation of coupled bred vectors
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID EL-NINO; ENSO; OCEAN; PACIFIC; MODEL
AB This study investigates the nature of a decadal modulation in the coupled bred vectors (BVs) developed to capture the dominant instabilities related to seasonal-to-interannual variability in the Equatorial Pacific using the GEOS-5 atmosphereocean general circulation model. It is found that the coupled BVs, with a monthly rescaling period, successfully reflect the observed decadal modulation of zonal location in the El Nino action center over the equatorial Pacific. By dividing the 30 years of BVs into two epochs, it is shown that the leading Empirical Orthogonal Function (EOF) of BV oceanic temperature shifts from the eastern Pacific during 1981-1999 to the central Pacific during 2000-2010, consistent with decadal changes in the location of the El Nino action center. By performing a budget analysis for BV temperature, it is found that the westward shift of the BV temperature is due to the strengthening of the mean zonal temperature gradient, which acts to amplify the BV temperature growth due to the zonal advection of background temperature by the BV current. Citation: Ham, Y.-G., M. M. Rienecker, S. Schubert, J. Marshak, S.-W. Yeh, and S.-C. Yang (2012), The decadal modulation of coupled bred vectors, Geophys. Res. Lett., 39, L20712, doi: 10.1029/2012GL053719.
C1 [Ham, Yoo-Geun; Rienecker, Michele M.; Schubert, Siegfried; Marshak, Jelena] NASA GSFC, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Ham, Yoo-Geun] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Studies & Invest, Columbia, MD USA.
[Yeh, Sang-Wook] Hanyang Univ, Dept Environm Marine Sci, Ansan, South Korea.
[Yang, Shu-Chih] Natl Cent Univ, Dept Atmospher Sci, Jhongli, Taiwan.
RP Ham, YG (reprint author), NASA GSFC, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
EM yoo-geun.ham@nasa.gov
RI Yeh, Sang-Wook/G-3007-2014
OI Yeh, Sang-Wook/0000-0003-4549-1686
FU NASA Modeling, Analysis and Prediction (MAP) Program [WBS
802678.02.17.01.25]; Korea Meteorological Administration Research and
Development Program [CATER 2012-3041]; NASA Center for Climate
Simulation at the Goddard Space Flight Center
FX The authors thank the reviewer for helpful comments to improve the
paper. Support for this project was provided by the NASA Modeling,
Analysis and Prediction (MAP) Program under WBS 802678.02.17.01.25.
S.-W. Yeh was funded by the Korea Meteorological Administration Research
and Development Program under grant CATER 2012-3041. Computing resources
for this study were provided by the NASA Center for Climate Simulation
at the Goddard Space Flight Center.
NR 17
TC 3
Z9 3
U1 1
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD OCT 25
PY 2012
VL 39
AR L20712
DI 10.1029/2012GL053719
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 027IJ
UT WOS:000310345400002
ER
PT J
AU Cooray, A
Smidt, J
De Bernardis, F
Gong, Y
Stern, D
Ashby, MLN
Eisenhardt, PR
Frazer, CC
Gonzalez, AH
Kochanek, CS
Kozlowski, S
Wright, EL
AF Cooray, Asantha
Smidt, Joseph
De Bernardis, Francesco
Gong, Yan
Stern, Daniel
Ashby, Matthew L. N.
Eisenhardt, Peter R.
Frazer, Christopher C.
Gonzalez, Anthony H.
Kochanek, Christopher S.
Kozlowski, Szymon
Wright, Edward L.
TI Near-infrared background anisotropies from diffuse intrahalo light of
galaxies
SO NATURE
LA English
DT Article
ID BRIGHTEST CLUSTER GALAXIES; WIDE-FIELD SURVEY; INTRACLUSTER LIGHT;
POPULATION-III; STELLAR HALOS; FLUCTUATIONS; STARS; DEEP; REIONIZATION;
CALIBRATION
AB Unresolved anisotropies of the cosmic near-infrared background radiation are expected to have contributions from the earliest galaxies during the epoch of reionization(1-5) and from faint, dwarf galaxies at intermediate redshifts(6,7). Previous measurements(8-12) were unable to pinpoint conclusively the dominant origin because they did not sample spatial scales that were sufficiently large to distinguish between these two possibilities. Here we report a measurement of the anisotropy power spectrum from subarcminute to one-degree angular scales, and find the clustering amplitude to be larger than predicted by the models based on the two existing explanations. As the shot-noise level of the power spectrum is consistent with that expected from faint galaxies, a new source population on the sky is not necessary to explain the observations. However, a physical mechanism that increases the clustering amplitude is needed. Motivated by recent results related to the extended stellar light profile in dark-matter haloes(13-15), we consider the possibility that the fluctuations originate from intrahalo stars of all galaxies. We find that the measured power spectrum can be explained by an intrahalo light fraction of 0.07 to 0.2 per cent relative to the total luminosity in dark-matter haloes of 10(9) to 10(12) solar masses at redshifts of about 1 to 4.
C1 [Cooray, Asantha; Smidt, Joseph; De Bernardis, Francesco; Gong, Yan; Frazer, Christopher C.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Stern, Daniel; Eisenhardt, Peter R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ashby, Matthew L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Kochanek, Christopher S.; Kozlowski, Szymon] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Kozlowski, Szymon] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
[Wright, Edward L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Cooray, A (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
EM acooray@uci.edu
RI Kozlowski, Szymon/G-4799-2013
OI Kozlowski, Szymon/0000-0003-4084-880X
FU NSF CAREER; NASA ADAP; JPL/Caltech
FX We acknowledge support from NSF CAREER (to A.C.), NASA ADAP and an award
from JPL/Caltech. We thank R. Arendt for sharing his IRAC
self-calibration code. We thank J. Bock and M. Zemcov for their
contributions to the SDWFS project. This work is based on observations
made with the Spitzer Space Telescope. This work also made use of data
products provided by the NOAO Deep Wide-Field Survey. A.C. thanks the
Aspen Center for Physics for hospitality.
NR 30
TC 33
Z9 33
U1 1
U2 7
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 OCT 25
PY 2012
VL 490
IS 7421
BP 514
EP 516
DI 10.1038/nature11474
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 025NK
UT WOS:000310196200036
PM 23099405
ER
PT J
AU Painter, TH
Brodzik, MJ
Racoviteanu, A
Armstrong, R
AF Painter, Thomas H.
Brodzik, Mary J.
Racoviteanu, Adina
Armstrong, Richard
TI Automated mapping of Earth's annual minimum exposed snow and ice with
MODIS
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID COVERED AREA; GRAIN-SIZE; GLACIER; ALBEDO; RETRIEVAL; HIMALAYA
AB Global snow and ice have been diminishing during the Anthropocene but we still lack a complete mapping of annual minimum exposed snow and ice with a consistent, repeatable algorithm. The Global Land Ice Measurements from Space (GLIMS) project has compiled digital glacier outlines and related metadata for the majority of the world's glaciers but inconsistency among product algorithms and time periods represented precludes the production of a consistently derived global data set. Here we present the MODIS Persistent Ice (MODICE) algorithm that leverages the time series of fractional snow and ice cover from the MODIS Snow Covered Area and Grain size (MODSCAG) algorithm. The end product of MODICE is a consistently derived map of annual minimum exposed snow and ice. Comparisons of MODICE with GLIMS glacier outlines derived from SPOT, ASTER, and Landsat Thematic Mapper show strong agreement with the higher resolution outlines subject to uncertainties with spatial resolution, deep mountain shadows, and GLIMS interpretation errors. Citation: Painter, T. H., M. J. Brodzik, A. Racoviteanu, and R. Armstrong (2012), Automated mapping of Earth's annual minimum exposed snow and ice with MODIS, Geophys. Res. Lett., 39, L20501, doi:10.1029/2012GL053340.
C1 [Painter, Thomas H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Brodzik, Mary J.; Armstrong, Richard] Natl Snow & Ice Data Ctr, Boulder, CO USA.
[Racoviteanu, Adina] Lab Glaciol & Geophys Environm, F-38402 St Martin Dheres, France.
RP Painter, TH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM thomas.painter@jpl.nasa.gov
RI Painter, Thomas/B-7806-2016;
OI Racoviteanu, Adina/0000-0003-4954-1871
FU Cryospheric Sciences program of NASA; Centre National d'Etudes Spatiales
(CNES), France; NASA
FX Funding for this work came from the Cryospheric Sciences program of
NASA. A. Racoviteanu's current work is supported by the Centre National
d'Etudes Spatiales (CNES), France. We acknowledge Ken Knowles for his
original idea for MODICE persistence and his initial implementation. We
also thank S. McKenzie Skiles, Karl Rittger, and the Snow Data System
team at JPL for assistance with GIS and comparisons. Thanks also to
Bruce Raup at the NSIDC GLIMS archive and to the French IRD for
providing access to SPOT imagery. Part of this work was performed at the
Jet Propulsion Laboratory, California Institute of Technology under a
contract with NASA.
NR 19
TC 2
Z9 2
U1 0
U2 25
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD OCT 24
PY 2012
VL 39
AR L20501
DI 10.1029/2012GL053340
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 027IH
UT WOS:000310345200001
ER
PT J
AU Wu, LT
Su, H
Fovell, RG
Wang, B
Shen, JT
Kahn, BH
Hristova-Veleva, SM
Lambrigtsen, BH
Fetzer, EJ
Jiang, JH
AF Wu, Longtao
Su, Hui
Fovell, Robert G.
Wang, Bin
Shen, Janice T.
Kahn, Brian H.
Hristova-Veleva, Svetla M.
Lambrigtsen, Bjorn H.
Fetzer, Eric J.
Jiang, Jonathan H.
TI Relationship of environmental relative humidity with North Atlantic
tropical cyclone intensity and intensification rate
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID VERTICAL WIND SHEAR; ATMOSPHERIC INFRARED SOUNDER; HURRICANE INTENSITY;
PACIFIC BASINS; STORM MOTION; SIMULATIONS; ASYMMETRIES; FORECASTS; FLOW
AB Quantifying the relationship of large-scale environmental conditions such as relative humidity with hurricane intensity and intensity change is important for statistical hurricane intensity forecasts. Our composite analysis of 9 years of Atmospheric Infrared Sounder (AIRS) humidity data spanning 198 Atlantic tropical cyclones (TCs) shows that environmental relative humidity (ERH) above the boundary layer generally decreases with time as TCs evolve. Near the surface, ERH stays approximately constant. ERH generally increases with increasing TC intensity and intensification rate. Rapidly intensifying TCs are associated with free tropospheric ERH more than 10% (relative to the averaged ERH for all TCs) larger than that for weakening TCs. Substantial azimuthal asymmetry in ERH is also found, especially for the TCs attaining the highest intensities and largest intensification rates at distances greater than 400 km away from the TC center. In the front-right quadrant relative to TC motion, rapid intensification is associated with a sharp gradient of ERH in the upper troposphere, with a decrease from the near to the far environment between 400 hPa and 300 hPa. The ERH gradient weakens with the decrease of intensification rate. This radial ERH gradient might be a useful predictor for the statistical forecast of TC intensification. Citation: Wu, L., H. Su, R. G. Fovell, B. Wang, J. T. Shen, B. H. Kahn, S. M. Hristova-Veleva, B. H. Lambrigtsen, E. J. Fetzer, and J. H. Jiang (2012), Relationship of environmental relative humidity with North Atlantic tropical cyclone intensity and intensification rate, Geophys. Res. Lett., 39, L20809, doi:10.1029/2012GL053546.
C1 [Wu, Longtao; Su, Hui; Shen, Janice T.; Kahn, Brian H.; Hristova-Veleva, Svetla M.; Fetzer, Eric J.; Jiang, Jonathan H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wu, Longtao] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Fovell, Robert G.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Wang, Bin] Univ Hawaii Manoa, Int Pacific Res Ctr, Honolulu, HI 96822 USA.
RP Wu, LT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 183-701, Pasadena, CA 91109 USA.
EM longtao.wu@jpl.nasa.gov
RI Wu, Longtao/G-5509-2012
FU NASA; NASA HSRP program
FX The authors thank Sundararaman Gopalakrishnan and Tomislava Vukicevic
for valuable discussions, and Mark DeMaria for suggestions. The helpful
comments from two anonymous reviewers are appreciated. The work is
conducted at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with NASA. The authors thank the funding
support from the NASA HSRP program.
NR 26
TC 16
Z9 16
U1 2
U2 22
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD OCT 24
PY 2012
VL 39
AR L20809
DI 10.1029/2012GL053546
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA 027IH
UT WOS:000310345200002
ER
PT J
AU Argus, DF
AF Argus, Donald F.
TI Uncertainty in the velocity between the mass center and surface of Earth
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
ID GLACIAL ISOSTATIC-ADJUSTMENT; SEA-LEVEL RISE; TERRESTRIAL REFERENCE
FRAME; BASE-LINE INTERFEROMETRY; COORDINATE TIME-SERIES; SPACE GEODESY;
SOLID EARTH; ICE-5G VM2; SERVICE; MODEL
AB Using spectral analysis and data decimation, we estimate the uncertainty in the velocity between the cumulative mass center of Earth (CM) and geodetic sites on Earth's surface. Knowing this velocity is crucial for evaluating space geodetic observations of continental uplift and subsidence in terms of postglacial rebound and sea level rise. We find SLR observations of satellite LAGEOS to constrain the X and Y components of the velocity of CM to +/- 0.4 mm/yr and the Z component to +/- 0.9 mm/yr. (95% confidence limits, X is in the direction of 0 degrees N 0 degrees E, Y of 0 degrees N 90 degrees E, and Z of 90 degrees N.) The uncertainty in Z is high, so that the estimate includes the independent inference made jointly using site velocities, the rigid plate hypothesis, and models of postglacial rebound that the true velocity of CM has a Z component of 0.5-1.0 mm/yr relative to that in ITRF2008. Uncertainty in scale rate, an intermediate parameter in the determination of an ITRF, is +/- 0.36 mm/yr for VLBI, +/- 0.52 mm/yr for SLR, and +/- 0.20 mm/yr for GPS. The scale of GPS depends on that of VLBI and SLR, but the low GPS uncertainty indicates that GPS results are, for the first time, unbiased by changing satellite Block types, evidently due to newly incorporated satellite phase center variations. GPS constrains the velocity of CM nearly as well as SLR, representing a technical advance given that a GPS satellite is not a sphere and responds strongly to solar radiation pressure.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Argus, DF (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM donald.f.argus@jpl.nasa.gov
FU NASA at Jet Propulsion Laboratory, California Institute of Technology
FX We are grateful to Z. Altamimi, X. Collilieux, and L. Metivier for
determining the Helmert transformations from SLR, VLBI, and DORIS to
ITRF2008; to R. Ferland for the IGS Helmert transformations from GPS to
ITRF2008; to S. Desai, W. Bertiger, J. Gross, B. Haines, N. Harvey, C.
Selle, A. Sibthorpe, and J. P. Weiss for the JPL GPS solution; to M. B.
Heflin and A. Moore for JPL's position-time series; to S. D. P. Williams
and M. S. Bos for instruction on CATS spectral analysis; and to F. W.
Landerer for GRACE estimates of seasonal mass fluctuations. We thank
Erricos Pavlis and two anonymous reviewers for their suggestions and
constructive criticism. D. Argus performed this research under contract
by NASA at Jet Propulsion Laboratory, California Institute of
Technology.
NR 54
TC 16
Z9 17
U1 2
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9313
EI 2169-9356
J9 J GEOPHYS RES-SOL EA
JI J. Geophys. Res.-Solid Earth
PD OCT 24
PY 2012
VL 117
AR B10405
DI 10.1029/2012JB009196
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 027HK
UT WOS:000310342900001
ER
PT J
AU Field, SE
Galley, CR
Ochsner, E
AF Field, Scott E.
Galley, Chad R.
Ochsner, Evan
TI Towards beating the curse of dimensionality for gravitational waves
using reduced basis
SO PHYSICAL REVIEW D
LA English
DT Article
ID COALESCENCE; BINARIES; FORMS
AB Using the reduced basis approach, we efficiently compress and accurately represent the space of waveforms for nonprecessing binary black hole inspirals, which constitutes a four-dimensional parameter space (two masses, two spin magnitudes). Compared to the nonspinning case, we find that only a marginal increase in the (already relatively small) number of reduced basis elements is required to represent any nonprecessing waveform to nearly numerical round-off precision. Most parameters selected by the algorithm are near the boundary of the parameter space, leaving the bulk of its volume sparse. Our results suggest that the full eight-dimensional space (two masses, two spin magnitudes, four spin orientation angles on the unit sphere) may be highly compressible and represented with very high accuracy by a remarkably small number of waveforms, thus providing some hope that the number of numerical relativity simulations of binary black hole coalescences needed to represent the entire space of configurations is not intractable. Finally, we find that the distribution of selected parameters is robust to different choices of seed values starting the algorithm, a property which should be useful for indicating parameters for numerical relativity simulations of binary black holes. In particular, we find that the mass ratios m(1)/m(2) of nonspinning binaries selected by the algorithm are mostly in the interval [1,3] and that the median of the distribution follows a power-law behavior similar to(m(1)/m(2))(-5.25).
C1 [Field, Scott E.] Univ Maryland, Ctr Sci Computat & Math Modeling, Joint Space Sci Inst, Maryland Ctr Fundamental Phys,Dept Phys, College Pk, MD 20742 USA.
[Galley, Chad R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Galley, Chad R.] CALTECH, Pasadena, CA 91125 USA.
[Ochsner, Evan] Univ Wisconsin, Ctr Gravitat & Cosmol, Milwaukee, WI 53201 USA.
RP Field, SE (reprint author), Univ Maryland, Ctr Sci Computat & Math Modeling, Joint Space Sci Inst, Maryland Ctr Fundamental Phys,Dept Phys, College Pk, MD 20742 USA.
FU NSF [PHY1208861, PHY1005632, PHY0970074]; Oak Ridge Associated
Universities; NASA
FX This work has been supported by NSF Grants No. PHY1208861 and No.
PHY1005632 to the University of Maryland, and NSF Grant No. PHY0970074
to the University of Wisconsin-Milwaukee. C. G. was supported by an
appointment to the NASA Postdoctoral Program at the Jet Propulsion
Laboratory administered by Oak Ridge Associated Universities through a
contract with NASA. Copyright 2012. All rights reserved. We thank
Alessandra Buonanno, Sarah Caudill, Tom Dent, Alexandre Le Tiec, Drew
Keppel, and Dianne O'Leary for very helpful comments on the manuscript
and/or suggestions. We especially thank Manuel Tiglio for helpful
discussions and comments on the manuscript as well as generating much of
the data used in this paper.
NR 36
TC 8
Z9 8
U1 0
U2 1
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD OCT 23
PY 2012
VL 86
IS 8
AR 084046
DI 10.1103/PhysRevD.86.084046
PG 7
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 025NA
UT WOS:000310194900002
ER
PT J
AU Abdo, AA
Ackermann, M
Ajello, M
Atwoo, WB
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Blandford, RD
Bonamente, E
Borgland, AW
Bottacini, E
Bouvier, A
Bregeon, J
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Casandjian, JM
Cecchi, C
Charles, E
Chekhtman, A
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Cutini, S
D'Ammando, F
de Angelis, A
de Palma, F
Dermer, CD
Digel, SW
Silva, EDE
Drell, PS
Drlica-Wagner, A
Dubois, R
Favuzzi, C
Fegan, SJ
Focke, WB
Fortin, P
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gehrels, N
Germani, S
Giglietto, N
Giommi, P
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Gomez-Vargas, GA
Grenier, IA
Grove, JE
Guiriec, S
Hadasch, D
Hays, E
Hill, AB
Horan, D
Hou, X
Hughes, RE
Iafrate, G
Jackson, MS
Johannesson, G
Johnson, AS
Kamae, T
Katagiri, H
Kataoka, J
Knodlseder, J
Kuss, M
Lande, J
Larsson, S
Latronico, L
Lemoine-Goumard, M
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Mazziotta, MN
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
Nolan, PL
Norris, JP
Nuss, E
Ohno, M
Ohsugi, T
Okumura, A
Omodei, N
Orienti, M
Orlando, E
Ormes, JF
Ozaki, M
Paneque, D
Panetta, JH
Parent, D
Pesce-Rollins, M
Pierbattista, M
Piron, F
Pivato, G
Poon, H
Porter, TA
Prokhorov, D
Raino, S
Rando, R
Razzano, M
Razzaque, S
Reimer, A
Reimer, O
Reposeur, T
Rochester, LS
Roth, M
Sadrozinski, HFW
Sanchez, DA
Sbarra, C
Schalk, TL
Sgro, C
Share, GH
Siskind, EJ
Spandre, G
Spinelli, P
Stawarz, L
Takahashi, H
Tanaka, T
Thayer, JG
Thayer, JB
Thompson, DJ
Tibaldo, L
Tinivella, M
Torres, DF
Tosti, G
Troja, E
Uchiyama, Y
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Waite, AP
Wang, P
Winer, BL
Wood, DL
Wood, KS
Yang, Z
Zimmer, S
AF Abdo, A. A.
Ackermann, M.
Ajello, M.
Atwoo, W. B.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bonamente, E.
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.
Casandjian, J. M.
Cecchi, C.
Charles, E.
Chekhtman, A.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Cutini, S.
D'Ammando, F.
de Angelis, A.
de Palma, F.
Dermer, C. D.
Digel, S. W.
Silva, E. do Couto E
Drell, P. S.
Drlica-Wagner, A.
Dubois, R.
Favuzzi, C.
Fegan, S. J.
Focke, W. B.
Fortin, P.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gehrels, N.
Germani, S.
Giglietto, N.
Giommi, P.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Gomez-Vargas, G. A.
Grenier, I. A.
Grove, J. E.
Guiriec, S.
Hadasch, D.
Hays, E.
Hill, A. B.
Horan, D.
Hou, X.
Hughes, R. E.
Iafrate, G.
Jackson, M. S.
Johannesson, G.
Johnson, A. S.
Kamae, T.
Katagiri, H.
Kataoka, J.
Knoedlseder, J.
Kuss, M.
Lande, J.
Larsson, S.
Latronico, L.
Lemoine-Goumard, M.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Mazziotta, M. N.
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.
Nolan, P. L.
Norris, J. P.
Nuss, E.
Ohno, M.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orienti, M.
Orlando, E.
Ormes, J. F.
Ozaki, M.
Paneque, D.
Panetta, J. H.
Parent, D.
Pesce-Rollins, M.
Pierbattista, M.
Piron, F.
Pivato, G.
Poon, H.
Porter, T. A.
Prokhorov, D.
Raino, S.
Rando, R.
Razzano, M.
Razzaque, S.
Reimer, A.
Reimer, O.
Reposeur, T.
Rochester, L. S.
Roth, M.
Sadrozinski, H. F. -W.
Sanchez, D. A.
Sbarra, C.
Schalk, T. L.
Sgro, C.
Share, G. H.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Stawarz, L.
Takahashi, H.
Tanaka, T.
Thayer, J. G.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Tinivella, M.
Torres, D. F.
Tosti, G.
Troja, E.
Uchiyama, Y.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Waite, A. P.
Wang, P.
Winer, B. L.
Wood, D. L.
Wood, K. S.
Yang, Z.
Zimmer, S.
TI FERMI OBSERVATIONS OF gamma-RAY EMISSION FROM THE MOON
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astroparticle physics; gamma rays: general; Moon
ID LARGE-AREA TELESCOPE; LUNAR-SURFACE; ELEMENTAL COMPOSITION;
SOLAR-SYSTEM; EGRET DATA; SPECTROMETER; ALBEDO; SPECTROSCOPY;
PROSPECTOR; ASTRONOMY
AB We report on the detection of high-energy gamma-ray emission from the Moon during the first 24 months of observations by the Fermi Large Area Telescope (LAT). This emission comes from particle cascades produced by cosmic-ray (CR) nuclei and electrons interacting with the lunar surface. The differential spectrum of the Moon is soft and can be described as a log-parabolic function with an effective cutoff at 2-3 GeV, while the average integral flux measured with the LAT from the beginning of observations in 2008 August to the end of 2010 August is F(> 100 MeV) = (1.04 +/- 0.01 [statistical error] +/- 0.1 [systematic error]) x 10(-6) cm(-2) s(-1). This flux is about a factor 2-3 higher than that observed between 1991 and 1994 by the EGRET experiment on board the Compton Gamma Ray Observatory, F(> 100 MeV) approximate to 5 x 10(-7) cm-2 s-1, when solar activity was relatively high. The higher gamma-ray flux measured by Fermi is consistent with the deep solar minimum conditions during the first 24 months of the mission, which reduced effects of heliospheric modulation, and thus increased the heliospheric flux of Galactic CRs. A detailed comparison of the light curve with McMurdo Neutron Monitor rates suggests a correlation of the trends. The Moon and the Sun are so far the only known bright emitters of gamma-rays with fast celestial motion. Their paths across the sky are projected onto the Galactic center and high Galactic latitudes as well as onto other areas crowded with high-energy gamma-ray sources. Analysis of the lunar and solar emission may thus be important for studies of weak and transient sources near the ecliptic.
C1 [Chekhtman, A.; Parent, D.; Razzaque, S.] George Mason Univ, Ctr Earth Observing & Space Res, Coll Sci, Fairfax, VA 22030 USA.
[Ackermann, M.; Tinivella, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Silva, E. do Couto E; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Prokhorov, D.; Reimer, A.; Reimer, O.; Rochester, L. S.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Borgland, A. W.; Bottacini, E.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Silva, E. do Couto E; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Prokhorov, D.; Reimer, A.; Reimer, O.; Rochester, L. S.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Atwoo, W. B.; Bouvier, A.; Razzano, M.; Sadrozinski, H. F. -W.; Schalk, T. L.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Atwoo, W. B.; Bouvier, A.; Razzano, M.; Sadrozinski, H. F. -W.; Schalk, T. L.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.; Pierbattista, M.] Univ Paris Diderot, Lab AIM, CNRS, CEA IRFU,CEA Saclay,Serv Astrophys, 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.; Pivato, G.; Poon, H.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Bonamente, E.; Cecchi, C.; D'Ammando, F.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Fortin, P.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] CSIC, Inst Ciencies Espai IEEE, E-08193 Barcelona, Spain.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Ciprini, S.] ASI Sci Data Ctr, I-00044 Frascati, Roma, Italy.
[Conrad, J.; Larsson, S.; Yang, Z.; Zimmer, S.] Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.; Jackson, M. S.; Larsson, S.; Yang, Z.; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle 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 Collegato Udine, I-33100 Udine, Italy.
[Dermer, C. D.; Grove, J. E.; Lovellette, M. N.; Wood, K. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
[Fukazawa, Y.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Gehrels, N.; Hays, E.; McEnery, J. E.; 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.
[Gomez-Vargas, G. A.; Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Gomez-Vargas, G. A.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain.
[Gomez-Vargas, G. A.] Univ Autonoma Madrid, CSIC, UAM, IFT, E-28049 Madrid, Spain.
[Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Hou, X.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Iafrate, G.] Osserv Astron Trieste, Ist Nazl Astrofis, I-34143 Trieste, Italy.
[Jackson, M. S.] Royal Inst Technol KTH, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden.
[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.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Knoedlseder, J.] Univ Toulouse, IRAP, UPS OMP, 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.
[Lemoine-Goumard, M.; Lott, B.; Reposeur, T.] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France.
[Lemoine-Goumard, M.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Lemoine-Goumard, M.; 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.
[Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA.
[Moiseev, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA.
[Ohno, M.; Ozaki, M.; Stawarz, L.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Okumura, A.] 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.
[Reimer, A.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Sanchez, D. A.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Share, G. H.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[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 Abdo, AA (reprint author), George Mason Univ, Ctr Earth Observing & Space Res, Coll Sci, Fairfax, VA 22030 USA.
EM imos@stanford.edu
RI Sgro, Carmelo/K-3395-2016; Reimer, Olaf/A-3117-2013; Tosti,
Gino/E-9976-2013; Ozaki, Masanobu/K-1165-2013; Rando,
Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Funk,
Stefan/B-7629-2015; Gomez-Vargas, German/C-7138-2015; Johannesson,
Gudlaugur/O-8741-2015; 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; Torres,
Diego/O-9422-2016; Orlando, E/R-5594-2016;
OI Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080;
Johannesson, Gudlaugur/0000-0003-1458-7036; 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; Giordano, Francesco/0000-0002-8651-2394;
giommi, paolo/0000-0002-2265-5003; De Angelis,
Alessandro/0000-0002-3288-2517; Iafrate, Giulia/0000-0002-6185-8292;
Caraveo, Patrizia/0000-0003-2478-8018; Sgro',
Carmelo/0000-0001-5676-6214; Rando, Riccardo/0000-0001-6992-818X
FU K. A. Wallenberg Foundation; European Community [ERC-StG-259391]; NASA
[NNX11AQ06G]
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.; 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. I.V.M. acknowledges support from NASA Grant
NNX11AQ06G.; 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.
NR 33
TC 12
Z9 12
U1 1
U2 17
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2012
VL 758
IS 2
AR 140
DI 10.1088/0004-637X/758/2/140
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030HO
UT WOS:000310562000069
ER
PT J
AU Chen, CHK
Mallet, A
Schekochihin, AA
Horbury, TS
Wicks, RT
Bale, SD
AF Chen, C. H. K.
Mallet, A.
Schekochihin, A. A.
Horbury, T. S.
Wicks, R. T.
Bale, S. D.
TI THREE-DIMENSIONAL STRUCTURE OF SOLAR WIND TURBULENCE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic fields; magnetohydrodynamics (MHD); plasmas; solar wind;
turbulence
ID INTERPLANETARY MAGNETIC-FIELD; MAGNETOHYDRODYNAMIC TURBULENCE;
DENSITY-FLUCTUATIONS; ALFVENIC TURBULENCE; INERTIAL-RANGE; COMPRESSIVE
FLUCTUATIONS; HYDRODYNAMIC TURBULENCE; DISSIPATION RANGE; ULYSSES
MISSION; POWER SPECTRA
AB We present a measurement of the scale-dependent, three-dimensional structure of the magnetic field fluctuations in inertial range solar wind turbulence with respect to a local, physically motivated coordinate system. The Alfvenic fluctuations are three-dimensionally anisotropic, with the sense of this anisotropy varying from large to small scales. At the outer scale, the magnetic field correlations are longest in the local fluctuation direction, consistent with Alfven waves. At the proton gyroscale, they are longest along the local mean field direction and shortest in the direction perpendicular to the local mean field and the local field fluctuation. The compressive fluctuations are highly elongated along the local mean field direction, although axially symmetric perpendicular to it. Their large anisotropy may explain why they are not heavily damped in the solar wind.
C1 [Chen, C. H. K.; Bale, S. D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Mallet, A.; Schekochihin, A. A.] Univ Oxford, Rudolf Peierls Ctr Theoret Phys, Oxford OX1 3NP, England.
[Horbury, T. S.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England.
[Wicks, R. T.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bale, S. D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
RP Chen, CHK (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM chen@ssl.berkeley.edu
RI Bale, Stuart/E-7533-2011; Wicks, Robert/A-1180-2009
OI Bale, Stuart/0000-0002-1989-3596; Wicks, Robert/0000-0002-0622-5302
FU NASA [NNN06AA01C, NNX09AE41G]; Leverhulme Trust Network for Magnetized
Plasma Turbulence
FX This work was supported by NASA contract NNN06AA01C, NASA grant
NNX09AE41G, and the Leverhulme Trust Network for Magnetized Plasma
Turbulence. Ulysses data were obtained from CDAWeb
(http://cdaweb.gsfc.nasa.gov).
NR 71
TC 34
Z9 34
U1 0
U2 11
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2012
VL 758
IS 2
AR 120
DI 10.1088/0004-637X/758/2/120
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030HO
UT WOS:000310562000049
ER
PT J
AU Clowe, D
Markevitch, M
Bradac, M
Gonzalez, AH
Chung, SM
Massey, R
Zaritsky, D
AF Clowe, Douglas
Markevitch, Maxim
Bradac, Marusa
Gonzalez, Anthony H.
Chung, Sun Mi
Massey, Richard
Zaritsky, Dennis
TI ON DARK PEAKS AND MISSING MASS: A WEAK-LENSING MASS RECONSTRUCTION OF
THE MERGING CLUSTER SYSTEM A520
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark matter; galaxies: clusters: individual (A520); gravitational
lensing: weak
ID HUBBLE-SPACE-TELESCOPE; CHARGE-TRANSFER INEFFICIENCY; INTERACTION
CROSS-SECTION; PHOTOMETRIC REDSHIFTS; GALAXY CLUSTERS; NUMERICAL
SIMULATIONS; MODIFIED GRAVITY; BULLET CLUSTER; DATA REDUCTION; MATTER
AB Merging clusters of galaxies are unique in their power to directly probe and place limits on the self-interaction cross-section of dark matter. Detailed observations of several merging clusters have shown the intracluster gas to be displaced from the centroids of dark matter and galaxy density by ram pressure, while the latter components are spatially coincident, consistent with collisionless dark matter. This has been used to place upper limits on the dark matter particle self-interaction cross-section of order 1 cm(2) g(-1). The cluster A520 has been seen as a possible exception. We revisit A520 presenting new Hubble Space Telescope Advanced Camera for Surveys mosaic images and a Magellan image set. We perform a detailed weak-lensing analysis and show that the weak-lensing mass measurements and morphologies of the core galaxy-filled structures are mostly in good agreement with previous works. There is, however, one significant difference: We do not detect the previously claimed "dark core" that contains excess mass with no significant galaxy overdensity at the location of the X-ray plasma. This peak has been suggested to be indicative of a large self-interaction cross-section for dark matter (at least similar to 5 sigma larger than the upper limit of 0.7 cm(2) g(-1) determined by observations of the Bullet Cluster). We find no such indication and instead find that the mass distribution of A520, after subtraction of the X-ray plasma mass, is in good agreement with the luminosity distribution of the cluster galaxies. We conclude that A520 shows no evidence to contradict the collisionless dark matter scenario.
C1 [Clowe, Douglas] Ohio Univ, Dept Phys & Astron, Clippinger Labs 251B, Athens, OH 45701 USA.
[Markevitch, Maxim] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20706 USA.
[Bradac, Marusa] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Gonzalez, Anthony H.; Chung, Sun Mi] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Massey, Richard] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Zaritsky, Dennis] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Clowe, D (reprint author), Ohio Univ, Dept Phys & Astron, Clippinger Labs 251B, Athens, OH 45701 USA.
EM clowe@ohio.edu
FU NASA [NAS 5-26555]; NASA through a grant from the Space Telescope
Science Institute [NAS 5-26555, 12253]
FX Based on observations made with the NASA/ESA Hubble Space Telescope,
obtained at the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS 5-26555. These observations are associated with
program 12253.; We wish to thank Alexie Leauthaud and James Taylor for
useful discussions on the shear measurement errors seen in COSMOS, and
Dan Coe for providing a copy of the UDF photometric redshift catalog
matched to our observed passbands. We also wish to thank James Jee,
Andisheh Mahdavi, and Henk Hoekstra for both discussions on possible
differences between the observed shear catalogs and additional
information on their techniques that helped rule out several
possibilities for differences between the mass reconstructions. Support
for program 12253 was provided by NASA through a grant from the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract NAS
5-26555.
NR 67
TC 33
Z9 33
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 OCT 20
PY 2012
VL 758
IS 2
AR 128
DI 10.1088/0004-637X/758/2/128
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030HO
UT WOS:000310562000057
ER
PT J
AU Crowder, SG
Barger, KA
Brandl, DE
Eckart, ME
Galeazzi, M
Kelley, RL
Kilbourne, CA
McCammon, D
Pfendner, CG
Porter, FS
Rocks, L
Szymkowiak, AE
Teplin, IM
AF Crowder, S. G.
Barger, K. A.
Brandl, D. E.
Eckart, M. E.
Galeazzi, M.
Kelley, R. L.
Kilbourne, C. A.
McCammon, D.
Pfendner, C. G.
Porter, F. S.
Rocks, L.
Szymkowiak, A. E.
Teplin, I. M.
TI OBSERVED LIMITS ON CHARGE EXCHANGE CONTRIBUTIONS TO THE DIFFUSE X-RAY
BACKGROUND
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instrumentation: detectors; instrumentation: spectrographs;
interplanetary medium; solar wind; X-rays: diffuse background; X-rays:
ISM
ID BUBBLE HOT GAS; SOLAR-WIND; EMISSION; SUZAKU; INFERENCES; ABUNDANCES;
SPECTRA; MAPS
AB We present a high-resolution spectrum of the diffuse X-ray background from 0.1 to 1 keV for a similar to 1 sr region of the sky centered at l = 90 degrees, b = +60 degrees using a 36 pixel array of microcalorimeters flown on a sounding rocket. With an energy resolution of 11 eV FWHM below 1 keV, the spectrum's observed line ratios help separate charge exchange contributions originating within the heliosphere from thermal emission of hot gas in the interstellar medium. The X-ray sensitivity below 1 keV was reduced by about a factor of four from contamination that occurred early in the flight, limiting the significance of the results. The observed centroid of helium-like O VII is 568(-3)(+2) eV at 90% confidence. Since the centroid expected for thermal emission is 568.4 eV and for charge exchange is 564.2 eV, thermal emission appears to dominate for this line complex. The dominance of thermal emission is consistent with much of the high-latitude O VII emission originating in 2-3 x 10(6) K gas in the Galactic halo. On the other hand, the observed ratio of C VI Ly gamma to Ly alpha is 0.3 +/- 0.2. The expected ratios are 0.04 for thermal emission and 0.24 for charge exchange, indicating that charge exchange must contribute strongly to this line and therefore potentially to the rest of the ROSAT R12 band usually associated with 10(6) K emission from the Local Hot Bubble. The limited statistics of this experiment and systematic uncertainties due to the contamination require only > 32% thermal emission for O VII and > 20% from charge exchange for C VI at the 90% confidence level. An experimental gold coating on the silicon substrate of the array greatly reduced extraneous signals induced on nearby pixels from cosmic rays passing through the substrate, reducing the triggered event rate by a factor of 15 from a previous flight of the instrument.
C1 [Crowder, S. G.; Barger, K. A.; Brandl, D. E.; McCammon, D.; Pfendner, C. G.; Rocks, L.; Teplin, I. M.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Eckart, M. E.; Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Eckart, M. E.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Galeazzi, M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA.
[Szymkowiak, A. E.] Yale Univ, Dept Phys, New Haven, CT 06511 USA.
RP Crowder, SG (reprint author), Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
EM crowder@physics.umn.edu
RI Kelley, Richard/K-4474-2012; Porter, Frederick/D-3501-2012
OI Porter, Frederick/0000-0002-6374-1119
FU NASA [NNX09AF09G]
FX Many graduate and undergraduate students have been involved with the
development and improvement of this instrument and we greatly appreciate
their assistance. We particularly thank Greg Jaehnig for his
contributions. We also thank Kari Kripps, Regis Brekosky, and John Gygax
for their work on the fabrication and assembly of the filters and
detectors. We appreciate Dimitra Koutroumpa providing us with charge
exchange predictions of C VI and O VII for our line of sight. We thank
the Luxel Corporation for developing the polyimide filters. We are
grateful for the support of the sounding rocket staff at Wallops Flight
Facility and White Sands Missile Range. We thank the anonymous referee
for suggestions that have significantly improved the clarity of the
paper. This work was supported in part by NASA grant NNX09AF09G.
NR 31
TC 7
Z9 7
U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2012
VL 758
IS 2
AR 143
DI 10.1088/0004-637X/758/2/143
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030HO
UT WOS:000310562000072
ER
PT J
AU Kassin, SA
Weiner, BJ
Faber, SM
Gardner, JP
Willmer, CNA
Coil, AL
Cooper, MC
Devriendt, J
Dutton, AA
Guhathakurta, P
Koo, DC
Metevier, AJ
Noeske, KG
Primack, JR
AF Kassin, Susan A.
Weiner, Benjamin J.
Faber, S. M.
Gardner, Jonathan P.
Willmer, C. N. A.
Coil, Alison L.
Cooper, Michael C.
Devriendt, Julien
Dutton, Aaron A.
Guhathakurta, Puragra
Koo, David C.
Metevier, A. J.
Noeske, Kai G.
Primack, Joel R.
TI THE EPOCH OF DISK SETTLING: z similar to 1 TO NOW
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: fundamental
parameters; galaxies: kinematics and dynamics
ID TULLY-FISHER RELATION; STAR-FORMING GALAXIES; INTEGRAL FIELD
SPECTROSCOPY; EXTENDED GROTH STRIP; TKRS/GOODS-N FIELD; MEDIUM DEEP
SURVEY; HIGH-REDSHIFT; SPIRAL GALAXIES; PHYSICAL-PROPERTIES; ASSEMBLY
HISTORY
AB We present evidence from a sample of 544 galaxies from the DEEP2 Survey for evolution of the internal kinematics of blue galaxies with stellar masses ranging 8.0 < log M-*(M-circle dot) < 10.7 over 0.2 < z < 1.2. DEEP2 provides galaxy spectra and Hubble imaging from which we measure emission-line kinematics and galaxy inclinations, respectively. Our large sample allows us to overcome scatter intrinsic to galaxy properties in order to examine trends in kinematics. We find that at a fixed stellar mass, galaxies systematically decrease in disordered motions and increase in rotation velocity and potential well depth with time. Massive galaxies are the most well ordered at all times examined, with higher rotation velocities and less disordered motions than less massive galaxies. We quantify disordered motions with an integrated gas velocity dispersion corrected for beam smearing (sigma(g)). It is unlike the typical pressure-supported velocity dispersion measured for early type galaxies and galaxy bulges. Because both seeing and the width of our spectral slits comprise a significant fraction of the galaxy sizes, sigma(g) integrates over velocity gradients on large scales which can correspond to non-ordered gas kinematics. We compile measurements of galaxy kinematics from the literature over 1.2 < z < 3.8 and do not find any trends with redshift, likely for the most part, because these data sets are biased toward the most highly star-forming systems. In summary, over the last similar to 8 billion years since z = 1.2, blue galaxies evolve from disordered to ordered systems as they settle to become the rotation-dominated disk galaxies observed in the universe today, with the most massive galaxies being the most evolved at any time.
C1 [Kassin, Susan A.; Gardner, Jonathan P.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Weiner, Benjamin J.; Willmer, C. N. A.] Univ Arizona, Steward Observ, Tucson, AZ USA.
[Faber, S. M.; Guhathakurta, Puragra; Koo, David C.] Univ Calif Santa Cruz, UCO Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Coil, Alison L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Cooper, Michael C.] Univ Calif Irvine, Dept Phys & Astron, Ctr Galaxy Evolut, Irvine, CA 92697 USA.
[Devriendt, Julien] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Dutton, Aaron A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Metevier, A. J.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA.
[Noeske, Kai G.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Primack, Joel R.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
RP Kassin, SA (reprint author), NASA, Postdoctoral Program, Washington, DC 20546 USA.
EM susan.kassin@nasa.gov
FU NASA [NAS 5-26555]; NSF [AST 95-29098, 00-71198]; NASA through Hubble
Fellowship by the Space Telescope Science Institute [HF-51269.01-A];
Southern California Center for Galaxy Evolution; University of
California Office of Research
FX S.A.K is supported by an appointment to the NASA Postdoctoral Program at
NASA's Goddard Space Flight Center, administered by Oak Ridge Associated
Universities through a contract with NASA. The authors also acknowledge
NSF grants AST 95-29098 and 00-71198 to UC Santa Cruz. S. A. K. kindly
thanks F. Bournaud, N. Forster-Schreiber, A. Gnerucci, M. Puech, P. van
der Werf, and S. Wright for providing tables of measurements and/or
further information on how their measurements were performed. We wish to
extend thanks to those of Hawaiian ancestry on whose sacred mountain we
are privileged guests. M. C. C. acknowledges support provided by NASA
through Hubble Fellowship grant No. HF-51269.01-A, awarded by the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., for NASA, under contract
NAS 5-26555. M. C. C. also acknowledges support from the Southern
California Center for Galaxy Evolution, a multi-campus research program
funded by the University of California Office of Research.
NR 80
TC 52
Z9 52
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 OCT 20
PY 2012
VL 758
IS 2
AR 106
DI 10.1088/0004-637X/758/2/106
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030HO
UT WOS:000310562000035
ER
PT J
AU LaMassa, SM
Heckman, TM
Ptak, A
AF LaMassa, Stephanie M.
Heckman, T. M.
Ptak, A.
TI DISENTANGLING AGN AND STAR FORMATION IN SOFT X-RAYS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: Seyfert; galaxies: starburst; infrared: galaxies; X-rays:
galaxies
ID ACTIVE GALACTIC NUCLEUS; SUPERMASSIVE BLACK-HOLES; LUMINOUS INFRARED
GALAXIES; SPACE-TELESCOPE SURVEY; SEYFERT-GALAXIES; HOST GALAXIES;
VELOCITY DISPERSION; STARBURST GALAXIES; NEARBY GALAXIES; DISK GALAXIES
AB We have explored the interplay of star formation and active galactic nucleus (AGN) activity in soft X-rays (0.5-2 keV) in two samples of Seyfert 2 galaxies (Sy2s). Using a combination of low-resolution CCD spectra from Chandra and XMM-Newton, we modeled the soft emission of 34 Sy2s using power-law and thermal models. For the 11 sources with high signal-to-noise Chandra imaging of the diffuse host galaxy emission, we estimate the luminosity due to star formation by removing the AGN, fitting the residual emission. The AGN and star formation contributions to the soft X-ray luminosity (i.e., L-x,L-AGN and L-x,L-SF) for the remaining 24 Sy2s were estimated from the power-law and thermal luminosities derived from spectral fitting. These luminosities were scaled based on a template derived from XSINGS analysis of normal star-forming galaxies. To account for errors in the luminosities derived from spectral fitting and the spread in the scaling factor, we estimated L-x,L-AGN and L-x,L-SF from Monte Carlo simulations. These simulated luminosities agree with L-x,L-AGN and L-x,L-SF derived from Chandra imaging analysis within a 3 sigma confidence level. Using the infrared [Ne II]12.8 mu m and [O IV]26 mu m lines as a proxy of star formation and AGN activity, respectively, we independently disentangle the contributions of these two processes to the total soft X-ray emission. This decomposition generally agrees with L-x,L-SF and L-x,L-AGN at the 3 sigma level. In the absence of resolvable nuclear emission, our decomposition method provides a reasonable estimate of emission due to star formation in galaxies hosting type 2 AGNs.
C1 [LaMassa, Stephanie M.; Heckman, T. M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Ptak, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP LaMassa, SM (reprint author), Yale Univ, New Haven, CT 06520 USA.
FU ADAP [10-ADAP10-0167]; Alfred P. Sloan Foundation; American Museum of
Natural History; Astrophysical Institute Potsdam; University of Basel;
University of Cambridge; Case Western Reserve University; University of
Chicago; Drexel University; Fermilab; Institute for Advanced Study;
Japan Participation Group; Johns Hopkins University; Joint Institute for
Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and
Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST);
Los Alamos National Laboratory; Max-Planck-Institute for Astronomy
(MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State
University; Ohio State University; University of Pittsburgh; University
of Portsmouth; Princeton University; United States Naval Observatory;
University of Washington; National Science Foundation; U.S. Department
of Energy; National Aeronautics and Space Administration; Japanese
Monbukagakusho; Max Planck Society; Higher Education Funding Council for
England
FX This work is funded by ADAP grant number 10-ADAP10-0167. We thank the
anonymous referee for comments and suggestions that improved the
manuscript. 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/. The SDSS is managed
by the Astrophysical Research Consortium for the Participating
Institutions. The Participating Institutions are the American Museum of
Natural History, Astrophysical Institute Potsdam, University of Basel,
University of Cambridge, Case Western Reserve University, University of
Chicago, Drexel University, Fermilab, the Institute for Advanced Study,
the Japan Participation Group, Johns Hopkins University, the Joint
Institute for Nuclear Astrophysics, the Kavli Institute for Particle
Astrophysics and Cosmology, the Korean Scientist Group, the Chinese
Academy of Sciences (LAMOST), Los Alamos National Laboratory, the
Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for
Astrophysics (MPA), New Mexico State University, Ohio State University,
University of Pittsburgh, University of Portsmouth, Princeton
University, the United States Naval Observatory, and the University of
Washington.
NR 51
TC 7
Z9 7
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2012
VL 758
IS 2
AR 82
DI 10.1088/0004-637X/758/2/82
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030HO
UT WOS:000310562000011
ER
PT J
AU Nissanke, S
Vallisneri, M
Nelemans, G
Prince, TA
AF Nissanke, Samaya
Vallisneri, Michele
Nelemans, Gijs
Prince, Thomas A.
TI GRAVITATIONAL-WAVE EMISSION FROM COMPACT GALACTIC BINARIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; Galaxy: general; gravitational waves; methods: data
analysis; white dwarfs
ID WHITE-DWARF BINARIES; AM CVN STARS; INTERFEROMETER-SPACE-ANTENNA;
POPULATION SYNTHESIS; MILKY-WAY; MASS-TRANSFER; DETACHED SYSTEMS; SDSS
1257+5428; X-RAY; EVOLUTION
AB Compact Galactic binaries where at least one member is a white dwarf (WD) or neutron star constitute the majority of individually detectable sources for future low-frequency space-based gravitational-wave (GW) observatories; they also form an unresolved continuum, the dominant Galactic foreground at frequencies below a few mHz. Due to the paucity of electromagnetic observations, the majority of studies of Galactic-binary populations so far have been based on population-synthesis simulations. However, recent surveys have reported several new detections of WD binaries, providing new constraints for population estimates. In this article, we evaluate the impact of revised local densities of interacting WD binaries on future GW observations. Specifically, we consider five scenarios that explain these densities with different assumptions on the formation of interacting systems; we simulate corresponding populations of detached and interacting WD binaries; we estimate the number of individually detectable GW sources and the magnitude of the confusion-noise foreground, as observed by space-based detectors with 5 and 1 Mkm arms. We confirm earlier estimates of thousands of detached-binary detections, but project only a few ten to a few hundred detections of interacting systems. This reduction is partly due to our assessment of detection prospects, based on the iterative identification and subtraction of bright sources with respect to both instrument and confusion noise. We also confirm earlier estimates for the confusion-noise foreground, except in one scenario that explains smaller local densities of interacting systems with smaller numbers of progenitor detached systems.
C1 [Nissanke, Samaya; Vallisneri, Michele; Prince, Thomas A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Nissanke, Samaya; Vallisneri, Michele; Prince, Thomas A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Nelemans, Gijs] Radboud Univ Nijmegen, Dept Astrophys, NL-6525 AJ Nijmegen, Netherlands.
[Nelemans, Gijs] Katholieke Univ Leuven, Inst Astron, B-3001 Louvain, Belgium.
[Nelemans, Gijs] Nikhef, NL-1098 XG Amsterdam, Netherlands.
RP Nissanke, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RI Nelemans, Gijs/D-3177-2012
OI Nelemans, Gijs/0000-0002-0752-2974
FU NSF [1066293]; NWO; FOM; LISA Mission Science Office
FX For useful discussions and interactions, we are grateful to Lars
Bildsten, Roseanne Di Stefano, Paul Groot, Mukremin Kilic, Shri
Kulkarni, David Levitan, Avi Loeb, Sterl Phinney, Tony Piro, and Ken
Shen. Part of this work was performed by TAP while at the Aspen Center
for Physics, which is supported by NSF grant No. 1066293. G.N. is
supported by NWO and FOM. M.V. is grateful for support from the LISA
Mission Science Office. Part of this work was performed at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration.
Government sponsorship acknowledged. Copyright 2011.
NR 100
TC 28
Z9 28
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 OCT 20
PY 2012
VL 758
IS 2
AR 131
DI 10.1088/0004-637X/758/2/131
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030HO
UT WOS:000310562000060
ER
PT J
AU Orosz, JA
Welsh, WF
Carter, JA
Brugamyer, E
Buchhave, LA
Cochran, WD
Endl, M
Ford, EB
MacQueen, P
Short, DR
Torres, G
Windmiller, G
Agol, E
Barclay, T
Caldwell, DA
Clarke, BD
Doyle, LR
Fabrycky, DC
Geary, JC
Haghighipour, N
Holman, MJ
Ibrahim, KA
Jenkins, JM
Kinemuchi, K
Li, J
Lissauer, JJ
Prsa, A
Ragozzine, D
Shporer, A
Still, M
Wade, RA
AF Orosz, Jerome A.
Welsh, William F.
Carter, Joshua A.
Brugamyer, Erik
Buchhave, Lars A.
Cochran, William D.
Endl, Michael
Ford, Eric B.
MacQueen, Phillip
Short, Donald R.
Torres, Guillermo
Windmiller, Gur
Agol, Eric
Barclay, Thomas
Caldwell, Douglas A.
Clarke, Bruce D.
Doyle, Laurance R.
Fabrycky, Daniel C.
Geary, John C.
Haghighipour, Nader
Holman, Matthew J.
Ibrahim, Khadeejah A.
Jenkins, Jon M.
Kinemuchi, Karen
Li, Jie
Lissauer, Jack J.
Prsa, Andrej
Ragozzine, Darin
Shporer, Avi
Still, Martin
Wade, Richard A.
TI THE NEPTUNE-SIZED CIRCUMBINARY PLANET KEPLER-38b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; planets and satellites: detection; planets and
satellites: fundamental parameters; planets and satellites: individual
(Kepler-38b); stars: fundamental parameters
ID LOW-MASS STARS; CLOSE BINARY-SYSTEMS; ECLIPSING BINARIES; INITIAL
CHARACTERISTICS; HIERARCHICAL TRIPLE; TIDAL EVOLUTION; LIGHT CURVES;
CADENCE DATA; DATA RELEASE; ORBITS
AB We discuss the discovery and characterization of the circumbinary planet Kepler-38b. The stellar binary is single-lined, with a period of 18.8 days, and consists of a moderately evolved main-sequence star (M-A = 0.949+/-0.059 M-circle dot and R-A = 1.757+/-0.034 R-circle dot) paired with a low-mass star (M-B = 0.249+/-0.010 M-circle dot and R-B = 0.2724+/-0.0053 R-circle dot) in a mildly eccentric (e = 0.103) orbit. A total of eight transits due to a circumbinary planet crossing the primary star were identified in the Kepler light curve (using Kepler Quarters 1-11), from which a planetary period of 105.595+/-0.053 days can be established. A photometric dynamical model fit to the radial velocity curve and Kepler light curve yields a planetary radius of 4.35+/-0.11 R-circle plus, or equivalently 1.12+/-0.03 R-Nep. Since the planet is not sufficiently massive to observably alter the orbit of the binary from Keplerian motion, we can only place an upper limit on the mass of the planet of 122 M-circle dot(7.11 M-Nep or equivalently 0.384 M-Jup) at 95% confidence. This upper limit should decrease as more Kepler data become available.
C1 [Orosz, Jerome A.; Welsh, William F.; Short, Donald R.; Windmiller, Gur] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Carter, Joshua A.; Torres, Guillermo; Geary, John C.; Holman, Matthew J.; Ragozzine, Darin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brugamyer, Erik; Cochran, William D.; Endl, Michael; MacQueen, Phillip] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Ford, Eric B.; Ragozzine, Darin] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.
[Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Barclay, Thomas; Kinemuchi, Karen; Still, Martin] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA.
[Caldwell, Douglas A.; Clarke, Bruce D.; Doyle, Laurance R.; Jenkins, Jon M.; Li, Jie] SETI Inst, Mountain View, CA 94043 USA.
[Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Haghighipour, Nader] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Haghighipour, Nader] Univ Hawaii Manoa, NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
[Ibrahim, Khadeejah A.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA.
[Shporer, Avi] Global Telescope Network, Las Cumbres Observ, Santa Barbara, CA 93117 USA.
[Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Shporer, Avi] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Wade, Richard A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
RP Orosz, JA (reprint author), San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 92182 USA.
RI Carter, Joshua/A-8280-2013; Agol, Eric/B-8775-2013; Ragozzine,
Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014;
OI Agol, Eric/0000-0002-0802-9145; Caldwell, Douglas/0000-0003-1963-9616;
Buchhave, Lars A./0000-0003-1605-5666; /0000-0001-6545-639X; Barclay,
Thomas/0000-0001-7139-2724; Fabrycky, Daniel/0000-0003-3750-0183
FU NASA, Science Mission Directorate; NASA [NNX12AD23G]; National Science
Foundation [AST-1109928, AST-0908642, AST-0645416, AST-1007992]
FX Kepler was selected as the 10th mission of the Discovery Program.
Funding for this mission is provided by NASA, Science Mission
Directorate. J.A.O. and W. F. W. acknowledge support from the Kepler
Participating Scientist Program via NASA Grant NNX12AD23G. Support was
also provided by the National Science Foundation via grants AST-1109928
to J.A.O., W.F.W., and G.W., AST-0908642 to R. W., AST-0645416 to E. A.,
and AST-1007992 to G.T.
NR 53
TC 99
Z9 99
U1 0
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2012
VL 758
IS 2
AR 87
DI 10.1088/0004-637X/758/2/87
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030HO
UT WOS:000310562000016
ER
PT J
AU Poomvises, W
Gopalswamy, N
Yashiro, S
Kwon, RY
Olmedo, O
AF Poomvises, Watanachak
Gopalswamy, Nat
Yashiro, Seiji
Kwon, Ryun-Young
Olmedo, Oscar
TI DETERMINATION OF THE HELIOSPHERIC RADIAL MAGNETIC FIELD FROM THE
STANDOFF DISTANCE OF A CME-DRIVEN SHOCK OBSERVED BY THE STEREO
SPACECRAFT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE coronal mass ejections (CMEs); solar-terrestrial relations
ID CORONAL MASS EJECTIONS; FARADAY-ROTATION MEASUREMENTS; SOLAR CORONA;
STRENGTH; PROPAGATION; MISSION
AB We report on the determination of radial magnetic field strength in the heliocentric distance range from 6 to 120 solar radii (R-circle dot) using data from Coronagraph 2 (COR2) and Heliospheric Imager I (HI1) instruments on board the Solar Terrestrial Relations Observatory spacecraft following the standoff-distance method of Gopalswamy & Yashiro. We measured the shock standoff distance of the 2008 April 5 coronal mass ejection (CME) and determined the flux-rope curvature by fitting the three-dimensional shape of the CME using the Graduated Cylindrical Shell model. The radial magnetic field strength is computed from the Alfven speed and the density of the ambient medium. We also compare the derived magnetic field strength with in situ measurements made by the Helios spacecraft, which measured the magnetic field at the heliocentric distance range from 60 to 215 R-circle dot. We found that the radial magnetic field strength decreases from 28 mG at 6 R-circle dot to 0.17 mG at 120 R-circle dot. In addition, we found that the radial profile can be described by a power law.
C1 [Poomvises, Watanachak; Gopalswamy, Nat; Yashiro, Seiji; Kwon, Ryun-Young] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Poomvises, Watanachak; Yashiro, Seiji; Kwon, Ryun-Young] Catholic Univ Amer, Inst Astrophys & Computat Sci, Dept Phys, Washington, DC 20064 USA.
[Olmedo, Oscar] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
[Olmedo, Oscar] USN, NRC Res, Res Lab, Washington, DC 20375 USA.
RP Poomvises, W (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
OI Gopalswamy, Nat/0000-0001-5894-9954
FU NASA LWS TRT
FX This research is supported by NASA LWS TR&T.
NR 27
TC 15
Z9 15
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 OCT 20
PY 2012
VL 758
IS 2
AR 118
DI 10.1088/0004-637X/758/2/118
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030HO
UT WOS:000310562000047
ER
PT J
AU Xue, YQ
Wang, SX
Brandt, WN
Luo, B
Alexander, DM
Bauer, FE
Comastri, A
Fabian, AC
Gilli, R
Lehmer, BD
Schneider, DP
Vignali, C
Young, M
AF Xue, Y. Q.
Wang, S. X.
Brandt, W. N.
Luo, B.
Alexander, D. M.
Bauer, F. E.
Comastri, A.
Fabian, A. C.
Gilli, R.
Lehmer, B. D.
Schneider, D. P.
Vignali, C.
Young, M.
TI TRACKING DOWN THE SOURCE POPULATION RESPONSIBLE FOR THE UNRESOLVED
COSMIC 6-8 keV BACKGROUND
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE diffuse radiation; galaxies: active; surveys; X-rays: diffuse
background; X-rays: galaxies
ID DEEP FIELD-SOUTH; ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; MS
SOURCE CATALOGS; X-RAY SOURCES; EXTRAGALACTIC LEGACY SURVEY;
ALPHA-EMITTING GALAXIES; LARGE-SCALE STRUCTURE; BLACK-HOLE GROWTH;
STELLAR-MASS
AB Using the 4 Ms Chandra Deep Field-South (CDF-S) survey, we have identified a sample of 6845 X-ray-undetected galaxies that dominates the unresolved approximate to 20%-25% of the 6-8 keV cosmic X-ray background (XRB). This sample was constructed by applying mass and color cuts to sources from a parent catalog based on GOODS-South Hubble Space Telescope z-band imaging of the central 6'radius area of the 4 Ms CDF-S. The stacked 6-8 keV detection is significant at the 3.9 sigma level, but the stacked emission was not detected in the 4-6 keV band, which indicates the existence of an underlying population of highly obscured active galactic nuclei (AGNs). Further examinations of these 6845 galaxies indicate that the galaxies on the top of the blue cloud and with redshifts of 1 less than or similar to z less than or similar to 3, magnitudes of 25 less than or similar to z(850) less than or similar to 28, and stellar masses of 2 x 10(8) less than or similar to M-star/M-circle dot less than or similar to 2 x 10(9) make the majority contributions to the unresolved 6-8 keV XRB. Such a population is seemingly surprising given that the majority of the X-ray-detected AGNs reside in massive (greater than or similar to 10(10) M-circle dot) galaxies. We discuss constraints upon this underlying AGN population, supporting evidence for relatively low mass galaxies hosting highly obscured AGNs, and prospects for further boosting the stacked signal.
C1 [Xue, Y. Q.; Wang, S. X.; Brandt, W. N.; Luo, B.; Young, M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Xue, Y. Q.; Wang, S. X.; Brandt, W. N.; Luo, B.; Schneider, D. P.; Young, M.] Penn State Univ, Inst Gravitat, University Pk, PA 16802 USA.
[Xue, Y. Q.; Wang, S. X.; Brandt, W. N.; Luo, B.; Schneider, D. P.; Young, M.] Penn State Univ, Cosmos, University Pk, PA 16802 USA.
[Xue, Y. Q.] Univ Sci & Technol China, Chinese Acad Sci, Key Lab Res Galaxies & Cosmol, Dept Astron, Hefei 230026, Anhui, Peoples R China.
[Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Bauer, F. E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Comastri, A.] INAF Osservatorio Astron Bologna, Bologna, Italy.
[Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, 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.
[Vignali, C.] Univ Bologna, Dipartimento Astron, Bologna, Italy.
RP Xue, YQ (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
EM xuey@ustc.edu.cn
RI Vignali, Cristian/J-4974-2012; Brandt, William/N-2844-2015; Comastri,
Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015
OI Alexander, David/0000-0002-5896-6313; Vignali,
Cristian/0000-0002-8853-9611; Brandt, William/0000-0002-0167-2453;
Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177
FU NASA through Chandra Award by the Chandra X-ray Observatory Center
[SP1-12007A]; NASA ADP grant [NNX10AC99G]; Youth 1000 Plan
(QingNianQianRen) program; USTC; Science and Technology Facilities
Council; Chandra Award [SP1-12007B]; Programa de Financiamiento Basal;
CONICYT-Chile [FONDECYT 1101024, FONDAP-CATA 15010003]; Italian Space
Agency (ASI) under the ASI-INAF [I/009/10/0]; Einstein Fellowship
Program
FX We thank the referee for helpful feedback that improved this work. We
thank T. Dahlen for providing the GOODS-S HST z-band-selected
photometric catalog, J. R. Mullaney and M. Pannella for making
comparisons between stellar-mass estimates, and R. Ciardullo and C.
Gronwall for helpful discussions. Support for this work was provided by
NASA through Chandra Award SP1-12007A (Y.Q.X., S.X.W., W.N.B.) issued by
the Chandra X-ray Observatory Center, which is operated by the
Smithsonian Astrophysical Observatory, and by NASA ADP grant NNX10AC99G
(Y.Q.X., S.X.W., W.N.B.). We also acknowledge the financial support of
the Youth 1000 Plan (QingNianQianRen) program and the USTC startup
funding (Y.Q.X.), the Science and Technology Facilities Council
(D.M.A.), Chandra Award SP1-12007B (F.E.B.), the Programa de
Financiamiento Basal (F.E.B.), the CONICYT-Chile grants FONDECYT 1101024
and FONDAP-CATA 15010003 (F.E.B.), the Italian Space Agency (ASI) under
the ASI-INAF contract I/009/10/0 (A.C., R.G., C.V.), and the Einstein
Fellowship Program (B.D.L.).
NR 95
TC 34
Z9 34
U1 0
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2012
VL 758
IS 2
AR 129
DI 10.1088/0004-637X/758/2/129
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030HO
UT WOS:000310562000058
ER
PT J
AU Yukita, M
Swartz, DA
Tennant, AF
Soria, R
Irwin, JA
AF Yukita, Mihoko
Swartz, Douglas A.
Tennant, Allyn F.
Soria, Roberto
Irwin, Jimmy A.
TI HOT DIFFUSE EMISSION IN THE NUCLEAR STARBURST REGION OF NGC 2903
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: individual (NGC 2903); galaxies: nuclei;
X-rays: galaxies
ID ACTIVE GALACTIC NUCLEUS; BARRED SPIRAL GALAXIES; X-RAY-EMISSION;
SUPERMASSIVE BLACK-HOLES; BH-SIGMA DIAGRAM; STAR-FORMATION; XMM-NEWTON;
H-ALPHA; CIRCUMNUCLEAR REGIONS; INTERSTELLAR BUBBLES
AB We present a deep Chandra observation of the central regions of the late-type barred spiral galaxy NGC 2903. The Chandra data reveal soft (kT(e) similar to 0.2-0.5 keV) diffuse emission in the nuclear starburst region and extending similar to 2' (similar to 5 kpc) to the north and west of the nucleus. Much of this soft hot gas is likely to be from local active star-forming regions; however, besides the nuclear region, the morphology of hot gas does not strongly correlate with the bar or other known sites of active star formation. The central similar to 650 pc radius starburst zone exhibits much higher surface brightness diffuse emission than the surrounding regions and a harder spectral component in addition to a soft component similar to the surrounding zones. We interpret the hard component as also being of thermal origin with kT(e) similar to 3.6 keV and to be directly associated with a wind fluid produced by supernovae and massive star winds similar to the hard diffuse emission seen in the starburst galaxy M82. The inferred terminal velocity for this hard component, similar to 1100 km s(-1), exceeds the local galaxy escape velocity suggesting a potential outflow into the halo and possibly escape from the galaxy gravitational potential. Morphologically, the softer extended emission from nearby regions does not display an obvious outflow geometry. However, the column density through which the X-rays are transmitted is lower in the zone to the west of the nucleus compared to that from the east and the surface brightness is relatively higher suggesting some of the soft hot gas originates from above the disk: viewed directly from the western zone but through the intervening disk of the host galaxy along sight lines from the eastern zone. There are several point-like sources embedded in the strong diffuse nuclear emission zone. Their X-ray spectra show them to likely be compact binaries. None of these detected point sources are coincident with the mass center of the galaxy and we place an upper limit luminosity from any point-like nuclear source to be <2 x 10(38) erg s(-1) in the 0.5-8.0 keV band, which indicates that NGC 2903 lacks an active galactic nucleus. Heating from the nuclear starburst and a galactic wind may be responsible for preventing cold gas from accreting onto the galactic center.
C1 [Yukita, Mihoko; Irwin, Jimmy A.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Swartz, Douglas A.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA.
[Tennant, Allyn F.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
[Soria, Roberto] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
RP Yukita, M (reprint author), Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
FU National Aeronautics and Space Administration through Chandra Award by
Chandra X-ray Observatory Center [GO0-11099A, NAS8-03060]
FX Support for this work was provided in part by the National Aeronautics
and Space Administration through Chandra Award GO0-11099A issued by the
Chandra X-ray Observatory Center, which is operated by the Smithsonian
Astrophysical Observatory for and on behalf of the National Aeronautics
Space Administration under contract NAS8-03060. M.Y. acknowledges R.
Buta and K. Wong for fruitful discussions.
NR 78
TC 5
Z9 5
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 OCT 20
PY 2012
VL 758
IS 2
AR 105
DI 10.1088/0004-637X/758/2/105
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030HO
UT WOS:000310562000034
ER
PT J
AU Green-Garcia, AM
Engel, AS
AF Green-Garcia, Angela M.
Engel, Annette Summers
TI Bacterial diversity of siliciclastic sediments in a Thalassia testudinum
meadow and the implications for Lucinisca nassula chemosymbiosis
SO ESTUARINE COASTAL AND SHELF SCIENCE
LA English
DT Article
DE 16S rRNA; marine sediments; seagrass; lucinid; endosymbiosis; Florida
ID RIBOSOMAL-RNA SEQUENCES; TROPICAL SEAGRASS; CODAKIA-ORBICULARIS;
GILL-ENDOSYMBIONTS; SPECIES RICHNESS; SULFIDE DYNAMICS; WEST-INDIES;
SULFUR; COMMUNITIES; BIVALVIA
AB Despite the ecological and economic importance of Thalassia testudinum (turtle grass) meadows along the Caribbean and Gulf of Mexico coasts, and recognition that microbial activities are critical to plant growth and health, the bacterial diversity of these habitats has been poorly studied. Based on comparative analyses of 165 rRNA gene sequences from sediments in a T. testudinum meadow, 25 major taxonomic groups (excluding candidate divisions) were retrieved, including Alpha- Delta-, and Gamma-proteobacteria, Chloroflexi, Bacteroidetes, Acidobacteria, Spirochaetes, and Firmicutes. The distribution of bacterial groups was linked to a strongly hypoxic and sulfidic redox gradient. The diversity is potentially novel because phylogenetic affinities of sediment sequences compared to contextually annotated environmental clones from different habitats or to cultured representatives indicated approximately 41% were more closely related to each other than to sequences retrieved from these other habitats. Of all the relationships, very few (2.4%) were to cultured organisms, but 27% were to environmental clones retrieved from shallow marine shelf and coastal sediments or from mangroves, estuarine, or wetland sediments. Rare sequences were closely related to endosymbiont groups of Lucinisca nassula (Lucinidea: Bivalvia) hosts collected from the same meadow, which may indicate that the sediment is a potential reservoir for free-living symbionts. This study provides insight into the ecological and evolutionary relationships of the Thalassia lucinid bacteria system in tropical to sub-tropical regions. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Engel, Annette Summers] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Green-Garcia, Angela M.; Engel, Annette Summers] Louisiana State Univ, Dept Geol & Geophys, Baton Rouge, LA 70803 USA.
[Green-Garcia, Angela M.] NASA, Lyndon B Johnson Space Ctr, Astromat Curat & Explorat Sci, Houston, TX 77058 USA.
RP Engel, AS (reprint author), Univ Tennessee, Dept Earth & Planetary Sci, 1412 Circle Dr, Knoxville, TN 37996 USA.
EM aengel1@utk.edu
RI Engel, Annette/E-3662-2016
OI Engel, Annette/0000-0003-2469-744X
FU Geoscience Alliance to Enhance Minority Participation (GAEMP) by a
National Science Foundation (OEDG) [0303138]; Sigma Xi; National Science
Foundation [IOS-1239903]
FX Field and laboratory assistance and support were provided by L.
Anderson, A. Aronowsky, and I. Kohl. W. LeBlanc assisted with
geochemical and mineralogical analyses. Funding for A.G.G. was provided
by the Geoscience Alliance to Enhance Minority Participation (GAEMP) by
a National Science Foundation award (OEDG #0303138) to Louisiana State
University, Department of Geology and Geophysics, and Sigma Xi by a
Grants-in-Aid Research award. Continued financial support to A.S.E. was
provided by the National Science Foundation (IOS-1239903).
NR 82
TC 4
Z9 4
U1 2
U2 26
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0272-7714
J9 ESTUAR COAST SHELF S
JI Estuar. Coast. Shelf Sci.
PD OCT 20
PY 2012
VL 112
SI SI
BP 153
EP 161
DI 10.1016/j.ecss.2012.07.010
PG 9
WC Marine & Freshwater Biology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA 031OQ
UT WOS:000310652000016
ER
PT J
AU Dols, V
Delamere, PA
Bagenal, F
Kurth, WS
Paterson, WR
AF Dols, Vincent
Delamere, Peter A.
Bagenal, Fran
Kurth, William S.
Paterson, William R.
TI Asymmetry of Io's outer atmosphere: Constraints from five Galileo flybys
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID PLASMA-WAVE OBSERVATIONS; JOVIAN MAGNETOSPHERE; CYCLOTRON WAVES;
ELECTRON-BEAMS; NEUTRAL CLOUDS; TORUS; SPACECRAFT; MODEL; SIMULATION;
ECLIPSE
AB The Galileo spacecraft probed the Io atmosphere/torus interaction region along six flybys between 1995 and 2001. The instruments on board provided measurements of the plasma density, average ion temperature, composition, flow, and magnetic perturbations to which we compare models and from which we constrain Io's atmosphere asymmetries. We have developed a model of the local interaction at Io that couples an MHD model of the flow and magnetic perturbations around the moon with a multispecies chemistry model that includes the physical chemistry of the main species: atoms, molecules, and ions derived from Io's volcanic gases ( S, O, SO2, SO). We prescribe several scenarios of the multicomponent neutral atmosphere of Io based on observations and compare our results with the plasma properties inferred from the Galileo measurements. Owing to limited data on the I25 flyby, it is excluded to make a total of five flybys for our comparisons. We show that the ion average temperature profile is a key quantity to constrain the radial extension and longitudinal asymmetries of the atmosphere of Io. We propose that the atmosphere has longitudinal asymmetries: its radial extension is limited upstream and significantly larger on the anti-Jovian downstream side. A very extended corona of SO2 and SO is present mainly downstream of Io. We discuss the possible temporal variability of Io's plasma-atmosphere interaction by comparing two flybys at different times at approximately the same location in the wake. We also discuss the plasma composition in the wake and the O1356A auroral emissions observed on the flanks of Io.
C1 [Dols, Vincent; Delamere, Peter A.; Bagenal, Fran] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Kurth, William S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Paterson, William R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Dols, V (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
EM dols@lasp.colorado.edu
OI Kurth, William/0000-0002-5471-6202
FU NASA OPR grant [NNX09AU29G]
FX We thank K. Khurana, M. Kivelson, X. Jia, N. Schneider, and B. Fleshman
for discussions on this topic; J. Groene for providing the Galileo
trajectories; D. Strobel for providing the electron energy equation and
the related cross sections; D. Shemansky for the SO2 cross
sections; and Steve Bartlett for graphics. Work for this paper was
supported by NASA OPR grant NNX09AU29G.
NR 67
TC 11
Z9 11
U1 2
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 OCT 20
PY 2012
VL 117
AR E10010
DI 10.1029/2012JE004076
PG 34
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 023ZN
UT WOS:000310076800001
ER
PT J
AU De Sanctis, MC
Combe, JP
Ammannito, E
Palomba, E
Longobardo, A
McCord, TB
Marchi, S
Capaccioni, F
Capria, MT
Mittlefehldt, DW
Pieters, CM
Sunshine, J
Tosi, F
Zambon, F
Carraro, F
Fonte, S
Frigeri, A
Magni, G
Raymond, CA
Russell, CT
Turrini, D
AF De Sanctis, M. C.
Combe, J. -Ph.
Ammannito, E.
Palomba, E.
Longobardo, A.
McCord, T. B.
Marchi, S.
Capaccioni, F.
Capria, M. T.
Mittlefehldt, D. W.
Pieters, C. M.
Sunshine, J.
Tosi, F.
Zambon, F.
Carraro, F.
Fonte, S.
Frigeri, A.
Magni, G.
Raymond, C. A.
Russell, C. T.
Turrini, D.
TI DETECTION OF WIDESPREAD HYDRATED MATERIALS ON VESTA BY THE VIR IMAGING
SPECTROMETER ON BOARD THE DAWN MISSION
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE minor planets, asteroids: general; minor planets, asteroids: individual:
(Vesta)
ID V-TYPE ASTEROIDS; MINERALOGICAL CHARACTERIZATION; PARENT BODY;
CARBONACEOUS CHONDRITES; SOLAR-SYSTEM; MU-M; HOWARDITES; EUCRITE;
SURFACE; CLASTS
AB Water plays a key role in the evolution of terrestrial planets, and notably in the occurrence of Earth's oceans. However, the mechanism by which water has been incorporated into these bodies-including Earth-is still extensively debated. Here we report the detection of widespread 2.8 mu m OH absorption bands on the surface of the asteroid Vesta by the VIR imaging spectrometer on board Dawn. These observations are surprising as Vesta is fully differentiated with a basaltic surface. The 2.8 mu m OH absorption is distributed across Vesta's surface and shows areas enriched and depleted in hydrated materials. The uneven distribution of hydrated mineral phases is unexpected and indicates ancient processes that differ from those believed to be responsible for OH on other airless bodies, like the Moon. The origin of Vestan OH provides new insight into the delivery of hydrous materials in the main belt and may offer new scenarios on the delivery of hydrous minerals in the inner solar system, suggesting processes that may have played a role in the formation of terrestrial planets.
C1 [De Sanctis, M. C.; Ammannito, E.; Palomba, E.; Longobardo, A.; Capaccioni, F.; Capria, M. T.; Tosi, F.; Zambon, F.; Carraro, F.; Fonte, S.; Frigeri, A.; Magni, G.; Turrini, D.] INAF, Ist Astrofis & Planetol Spaziali, Rome, Italy.
[Combe, J. -Ph.; McCord, T. B.] Bear Fight Inst, Winthrop, WA USA.
[Marchi, S.] NASA, Lunar Sci Inst, Boulder, CO USA.
[Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Pieters, C. M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Sunshine, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
RP De Sanctis, MC (reprint author), INAF, Ist Astrofis & Planetol Spaziali, Rome, Italy.
EM mariacristina.desanctis@iaps.inaf.it
RI Russell, Christopher/E-7745-2012; De Sanctis, Maria
Cristina/G-5232-2013; Frigeri, Alessandro/F-2151-2010
OI capria, maria teresa/0000-0002-9814-9588; Russell,
Christopher/0000-0003-1639-8298; Turrini, Diego/0000-0002-1923-7740;
Capaccioni, Fabrizio/0000-0003-1631-4314; De Sanctis, Maria
Cristina/0000-0002-3463-4437; Palomba, Ernesto/0000-0002-9101-6774;
Tosi, Federico/0000-0003-4002-2434; Zambon,
Francesca/0000-0002-4190-6592; Frigeri, Alessandro/0000-0002-9140-3977
FU Italian Space Agency; Dawn Science, Instrument, and Operations Teams;
NASA's Dawn at Vesta Participating Scientists Program
FX VIR is funded by the Italian Space Agency and was developed under the
leadership of INAF-Istituto di Astrofisica e Planetologia Spaziali,
Rome, Italy. The instrument was built by Selex-Galileo, Florence, Italy.
The authors acknowledge the support of the Dawn Science, Instrument, and
Operations Teams. This work was supported by the Italian Space Agency
and NASA's Dawn at Vesta Participating Scientists Program. A portion of
this work was performed at the Jet Propulsion Laboratory, under contract
with NASA.
NR 40
TC 51
Z9 52
U1 1
U2 17
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 20
PY 2012
VL 758
IS 2
AR L36
DI 10.1088/2041-8205/758/2/L36
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 018RH
UT WOS:000309679300012
ER
PT J
AU Godfrey, LEH
Lovell, JEJ
Burke-Spolaor, S
Ekers, R
Bicknell, GV
Birkinshaw, M
Worrall, DM
Jauncey, DL
Schwartz, DA
Marshall, HL
Gelbord, J
Perlman, ES
Georganopoulos, M
AF Godfrey, L. E. H.
Lovell, J. E. J.
Burke-Spolaor, S.
Ekers, R.
Bicknell, G. V.
Birkinshaw, M.
Worrall, D. M.
Jauncey, D. L.
Schwartz, D. A.
Marshall, H. L.
Gelbord, J.
Perlman, E. S.
Georganopoulos, M.
TI PERIODIC STRUCTURE IN THE MEGAPARSEC-SCALE JET OF PKS 0637-752
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: active; galaxies: jets; quasars: individual (PKS0637-752)
ID ACTIVE GALACTIC NUCLEI; BINARY BLACK-HOLE; II RADIO-SOURCES;
HUBBLE-SPACE-TELESCOPE; X-RAY-EMISSION; ACCRETION DISK; RELATIVISTIC
JETS; GALAXY; INSTABILITY; CHANDRA
AB We present 18 GHz Australia Telescope Compact Array imaging of the megaparsec-scale quasar jet PKS 0637-752 with angular resolution similar to 0 ''.58. We draw attention to a spectacular train of quasi-periodic knots along the inner 11 '' of the jet, with average separation similar to 1.1 arcsec (7.6 kpc projected). We consider two classes of model to explain the periodic knots: those that involve a static pattern through which the jet plasma travels (e.g., stationary shocks) and those that involve modulation of the jet engine. Interpreting the knots as re-confinement shocks implies the jet kinetic power Q(jet) similar to 10(46) erg s(-1), but the constant knot separation along the jet is not expected in a realistic external density profile. For models involving modulation of the jet engine, we find that the required modulation period is 2 x 10(3) yr < tau < 3 x 10(5) yr. The lower end of this range is applicable if the jet remains highly relativistic on kiloparsec scales, as implied by the IC/CMB model of jet X-ray emission. We suggest that the periodic jet structure in PKS 0637-752 may be analogous to the quasi-periodic jet modulation seen in the microquasar GRS 1915+105, believed to result from limit cycle behavior in an unstable accretion disk. If variations in the accretion rate are driven by a binary black hole, the predicted orbital radius is 0.7 pc less than or similar to a less than or similar to 30 pc, which corresponds to a maximum angular separation of similar to 0.1-5 mas.
C1 [Godfrey, L. E. H.; Ekers, R.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6102, Australia.
[Godfrey, L. E. H.; Bicknell, G. V.; Jauncey, D. L.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Lovell, J. E. J.; Ekers, R.; Jauncey, D. L.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Hobart, Tas 2121, Australia.
[Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001`, Australia.
[Burke-Spolaor, S.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Birkinshaw, M.; Worrall, D. M.; Schwartz, D. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Birkinshaw, M.; Worrall, D. M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England.
[Marshall, H. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Gelbord, J.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Perlman, E. S.] Florida Inst Technol, Phys & Space Sci Dept, Melbourne, FL 32901 USA.
[Georganopoulos, M.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Dept Phys, Baltimore, MD 21250 USA.
RP Godfrey, LEH (reprint author), Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6102, Australia.
EM L.Godfrey@curtin.edu.au
RI Godfrey, Leith/B-5283-2013
FU Commonwealth of Australia; NASA [NAS8-03060]; CXC [GO9-0121B]
FX The Australia Telescope Compact Array is part of the Australia Telescope
which is funded by the Commonwealth of Australia for operation as a
National Facility managed by CSIRO. D.A.S. is supported by NASA contract
NAS8-03060 and CXC grant GO9-0121B.
NR 48
TC 13
Z9 13
U1 1
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 20
PY 2012
VL 758
IS 2
AR L27
DI 10.1088/2041-8205/758/2/L27
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 018RH
UT WOS:000309679300003
ER
PT J
AU McGuire, BA
Loomis, RA
Charness, CM
Corby, JF
Blake, GA
Hollis, JM
Lovas, FJ
Jewell, PR
Remijan, AJ
AF McGuire, Brett A.
Loomis, Ryan A.
Charness, Cameron M.
Corby, Joanna F.
Blake, Geoffrey A.
Hollis, Jan M.
Lovas, Frank J.
Jewell, Philip R.
Remijan, Anthony J.
TI INTERSTELLAR CARBODIIMIDE (HNCNH): A NEW ASTRONOMICAL DETECTION FROM THE
GBT PRIMOS SURVEY VIA MASER EMISSION FEATURES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrochemistry; ISM: clouds; ISM: individual objects (Sagittarius
B2(N)); ISM: molecules
ID WATER-ICE; CYANAMIDE; LINE; THZ
AB In this work, we identify carbodiimide (HNCNH), which is an isomer of the well-known interstellar species cyanamide (NH2CN), in weak maser emission, using data from the Green Bank Telescope PRIMOS survey toward Sgr B2(N). All spectral lines observed are in emission and have energy levels in excess of 170 K, indicating that the molecule likely resides in relatively hot gas that characterizes the denser regions of this star-forming region. The anticipated abundance of this molecule from ice mantle experiments is similar to 10% of the abundance of NH2CN, which in Sgr B2(N) corresponds to similar to 2 x 10(13) cm(-2). Such an abundance results in transition intensities well below the detection limit of any current astronomical facility and, as such, HNCNH could only be detected by those transitions which are amplified by masing.
C1 [McGuire, Brett A.; Blake, Geoffrey A.] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
[Loomis, Ryan A.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA.
[Charness, Cameron M.; Corby, Joanna F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Hollis, Jan M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lovas, Frank J.] NIST, Gaithersburg, MD 20899 USA.
[Jewell, Philip R.; Remijan, Anthony J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
RP McGuire, BA (reprint author), CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
OI McGuire, Brett/0000-0003-1254-4817
FU NSF Graduate Research Fellowship
FX All authors dedicate this work to Lewis E. Snyder who pioneered the
astronomical detection of molecules at radio frequencies. B.A.M.
gratefully acknowledges funding by an NSF Graduate Research Fellowship,
and M. Emprechtinger for helpful discussions regarding masers. We thank
the anonymous referee for very helpful comments. The National Radio
Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc.
NR 18
TC 9
Z9 9
U1 2
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 20
PY 2012
VL 758
IS 2
AR L33
DI 10.1088/2041-8205/758/2/L33
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 018RH
UT WOS:000309679300009
ER
PT J
AU Behrangi, A
Lebsock, M
Wong, S
Lambrigtsen, B
AF Behrangi, Ali
Lebsock, Matthew
Wong, Sun
Lambrigtsen, Bjorn
TI On the quantification of oceanic rainfall using spaceborne sensors
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CLOUD CLASSIFICATION-SYSTEM; TRMM PRECIPITATION RADAR; MICROWAVE
SOUNDING UNIT; PROFILING ALGORITHM; TROPICAL PACIFIC; WATER-VAPOR;
CYCLE; CLIMATE; VARIABILITY; MODEL
AB Much of our knowledge about oceanic rainfall comes from spaceborne sensors. These sensors provide direct or indirect information used for precipitation retrievals through various algorithms. A thorough understanding of rain frequency and intensity and its regional distribution, which is especially important in a warming climate, requires an evaluation of the performance of rain-measuring sensors and identification of strengths and limitations offered by each sensor. The Tropical Rainfall Measuring Mission (TRMM) has enabled significant advancement in quantification of moderate to intense rainfall. However, a common limitation of the current suite of rain-measuring sensors is their lack of sensitivity to light rainfall, especially over subtropical and high-latitude oceans. Among various spaceborne sensors, CloudSat enables superior retrieval of light rainfall and drizzle. By using 3 years (2007-2009) of rainfall data from CloudSat and the precipitation radar aboard TRMM, it was determined that the quasi-global (60 degrees S-60 degrees N) oceanic mean rain rate is about 3.05 mm/d, considerably larger than that obtained from any individual sensor product. In the deep tropics, especially within 20 degrees S-20 degrees N, the sensors show the highest agreement, with a large fraction of total rain volume captured by the majority of sensors. However, toward higher latitudes and within the subtropical high-pressure regions, a significant fraction of rainfall, which can exceed 50% or more of total rain volume, is missed by the majority of the sensors.
C1 [Behrangi, Ali; Lebsock, Matthew; Wong, Sun; Lambrigtsen, Bjorn] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Behrangi, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ali.behrangi@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The research described in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
Government sponsorship is acknowledged. Comments by George Huffman and
the anonymous reviewers improved the final paper.
NR 48
TC 31
Z9 31
U1 3
U2 28
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 19
PY 2012
VL 117
AR D20105
DI 10.1029/2012JD017979
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 024AQ
UT WOS:000310080100003
ER
PT J
AU Gettelman, A
Liu, X
Barahona, D
Lohmann, U
Chen, C
AF Gettelman, A.
Liu, X.
Barahona, D.
Lohmann, U.
Chen, C.
TI Climate impacts of ice nucleation
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CIRRUS CLOUD FORMATION; COMMUNITY ATMOSPHERE MODEL; TROPICAL TROPOPAUSE;
UPPER TROPOSPHERE; AEROSOL; PARAMETERIZATION; NUCLEI; MICROPHYSICS;
SENSITIVITY; SUPERSATURATIONS
AB Several different ice nucleation parameterizations in two different General Circulation Models (GCMs) are used to understand the effects of ice nucleation on the mean climate state, and the Aerosol Indirect Effects (AIE) of cirrus clouds on climate. Simulations have a range of ice microphysical states that are consistent with the spread of observations, but many simulations have higher present-day ice crystal number concentrations than in-situ observations. These different states result from different parameterizations of ice cloud nucleation processes, and feature different balances of homogeneous and heterogeneous nucleation. Black carbon aerosols have a small (-0.06 Wm(-2)) and not statistically significant AIE when included as ice nuclei, for nucleation efficiencies within the range of laboratory measurements. Indirect effects of anthropogenic aerosols on cirrus clouds occur as a consequence of increasing anthropogenic sulfur emissions with different mechanisms important in different models. In one model this is due to increases in homogeneous nucleation fraction, and in the other due to increases in heterogeneous nucleation with coated dust. The magnitude of the effect is the same however. The resulting ice AIE does not seem strongly dependent on the balance between homogeneous and heterogeneous ice nucleation. Regional effects can reach several Wm(-2). Indirect effects are slightly larger for those states with less homogeneous nucleation and lower ice number concentration in the base state. The total ice AIE is estimated at 0.27 +/- 0.10 Wm(-2) (1 sigma uncertainty). This represents a 20% offset of the simulated total shortwave AIE for ice and liquid clouds of -1.6 Wm(-2).
C1 [Gettelman, A.; Chen, C.] Natl Ctr Atmospher Res, Boulder, CO 80305 USA.
[Gettelman, A.; Lohmann, U.] ETH, Inst Atmospher & Climate Sci, Zurich, Switzerland.
[Liu, X.] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Barahona, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Barahona, D.] IM Syst Grp, Rockville, MD USA.
RP Gettelman, A (reprint author), Natl Ctr Atmospher Res, 1850 Table Mesa Dr, Boulder, CO 80305 USA.
EM andrew@ucar.edu
RI Barahona, Donifan/G-4157-2011; Liu, Xiaohong/E-9304-2011; Lohmann,
Ulrike/B-6153-2009
OI Liu, Xiaohong/0000-0002-3994-5955; Lohmann, Ulrike/0000-0001-8885-3785
FU U.S. National Science Foundation; Aviation Climate Change Research
Initiative (ACCRI) [DTRT57-10-C-10012]; NASA Modeling Analysis and
Prediction program [NNX09AJ05G, WBS 802678.02.17.01.07]; US NSF/DOE/USDA
Decadal and Regional Climate Prediction using Earth System Models (EaSM)
program
FX Computing resources were provided by the Climate Simulation Laboratory
at National Center for Atmospheric Research (NCAR) Computational and
Information Systems Laboratory. NCAR is sponsored by the U.S. National
Science Foundation. This work was supported at NCAR by the Aviation
Climate Change Research Initiative (ACCRI) contract DTRT57-10-C-10012
and the NASA Modeling Analysis and Prediction program, award NNX09AJ05G.
D. Barahona was supported by the NASA Modeling, Analysis and Prediction
program under WBS 802678.02.17.01.07. X. Liu acknowledges support of the
US NSF/DOE/USDA Decadal and Regional Climate Prediction using Earth
System Models (EaSM) program. The Pacific Northwest National Laboratory
is operated for the US DOE by the Batelle Memorial Institute under
contract DE-AC06-76RLO 1830. We thank S. T. Massie and C. Bardeen for
comments, and M. Wang and K. Zhang for making available ice crystal
observations.
NR 58
TC 45
Z9 46
U1 3
U2 72
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 19
PY 2012
VL 117
AR D20201
DI 10.1029/2012JD017950
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 024AQ
UT WOS:000310080100002
ER
PT J
AU Mischna, MA
Lee, C
Richardson, M
AF Mischna, Michael A.
Lee, Christopher
Richardson, Mark
TI Development of a fast, accurate radiative transfer model for the Martian
atmosphere, past and present
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MOLECULAR SPECTROSCOPIC DATABASE; K-DISTRIBUTION METHOD;
GENERAL-CIRCULATION; SOLAR-RADIATION; EARLY EARTH; INHOMOGENEOUS
ATMOSPHERES; MULTIPLE-SCATTERING; THERMAL EMISSION; WATER-VAPOR;
ABSORPTION
AB We present details of an approach to creating a k-distribution radiative transfer model (KDM) for use in the Martian atmosphere. Such models preserve the accuracy of more rigorous line-by-line models, but are orders of magnitude faster, and can be effectively implemented in 3-D general circulation models. The approach taken here is sufficiently generalized that it can be employed for atmospheres of any arbitrary composition and mass, and demonstrations are provided for simulated atmospheres with a present-day Martian surface pressure (similar to 6 mb) and a putative thick early Mars atmosphere (similar to 500 mb), both with and without atmospheric water vapor. KDM-derived absorption coefficients are placed into a look-up table at a set of gridded points in pressure, temperature and atmospheric composition, and a tri-linear interpolation scheme is used to obtain the coefficients appropriate for the local atmospheric conditions. These coefficients may then be used within any of a variety of commonly used flux solvers to obtain atmospheric heating rates. A series of validation tests are performed with the KDM for both present-day and early Mars atmospheric conditions, and the model is compared against several other widely used radiative transfer schemes, including several used in contemporary general circulation models. These validation results identify weaknesses in some other approaches and demonstrate the efficacy of the KDM, providing a rigorous test of these types of models for use in the Martian atmosphere. A demonstration of results obtained by implementing the KDM in a Mars general circulation model is provided.
C1 [Mischna, Michael A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lee, Christopher; Richardson, Mark] Ashima Res, Pasadena, CA USA.
RP Mischna, MA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 183-601, Pasadena, CA 91109 USA.
EM michael.a.mischna@jpl.nasa.gov
FU NASA Mars Fundamental Research Program grant [NNH10ZDA001N]; NASA
Planetary Atmospheres grant [NNX10AB42G]
FX The authors would like to thank Ramses Ramirez and Jim Kasting for data
from their model, and for useful discussions that improved the output of
our 1-D model. Also, Karen Cady-Pereira and Eli Mlawer of AER, Inc. who
assisted with implementation of the LBLRTM code as well as incorporation
of continuum absorption in our line-by-line code. Resources supporting
this work were provided by the NASA High- End Computing (HEC) Program
through the NASA Advanced Supercomputing (NAS) Division at Ames Research
Center as well as from the JPL Office of the Chief Information Officer.
M.A.M. and C.L. were supported by a NASA Mars Fundamental Research
Program grant NNH10ZDA001N to JPL. Additional support for C.L. and
M.I.R. was provided by a NASA Planetary Atmospheres grant NNX10AB42G to
Ashima Research. 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. The
authors would like to thank two anonymous reviewers for their comments
on and suggestions for this manuscript.
NR 57
TC 15
Z9 15
U1 0
U2 14
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 OCT 19
PY 2012
VL 117
AR E10009
DI 10.1029/2012JE004110
PG 22
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 023ZM
UT WOS:000310076700001
ER
PT J
AU Gong, Y
Andrews, L
Bauschlicher, CW
AF Gong, Yu
Andrews, Lester
Bauschlicher, Charles W., Jr.
TI Reactions of Group 3 Metals with OF2: Infrared Spectroscopic and
Theoretical Investigations of the Group 3 Oxydifluoride OMF2 and
Oxyfluoride OMF Molecules
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID DENSITY-FUNCTIONAL CALCULATIONS; AB-INITIO PSEUDOPOTENTIALS; BOND
COVALENT RADII; GAUSSIAN-BASIS SETS; LASER-ABLATED-Y; SOLID ARGON;
ELECTRONIC-STRUCTURE; MATRIX-ISOLATION; F-ATOMS;
PHOTOELECTRON-SPECTROSCOPY
AB The oxidifluoride molecules, OYF2 and OLaF2, are produced via the reactions of laser ablated metal atoms with OF2 in solid argon. The product structures are characterized using matrix isolation infrared spectroscopy as well as theoretical calculations. Similar to the very recently characterized OScF2 molecule, OYF2 is predicted to have a B-2(2) ground state with C-2, symmetry while the heavier OLaF2, has a (2)A '' ground state with near C-2, symmetry. The unpaired electron is mainly located on the terminal oxygen atom, suggesting radical character for the group 3 OMF2 molecules. In addition, the closed shell singlet OMF molecules with bent geometries are also observed, and they are found to have triple metal-oxygen bonds with higher stretching frequencies and shorter bond lengths than their OMF2 counterparts. alpha-Fluorine transfer from OF2 to metal centers is predicted to be highly exothermic, which is very favorable for the formation of new OMF2 and OMF species.
C1 [Gong, Yu; Andrews, Lester] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA.
[Bauschlicher, Charles W., Jr.] NASA, Ames Res Ctr, Entry Syst & Technol Div, Moffett Field, CA 94035 USA.
RP Andrews, L (reprint author), Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA.
EM lsa@virginia.edu
FU DOE [DE-SC0001034]
FX We gratefully acknowledge financial support from DOE Grant DE-SC0001034
and helpful discussions with our colleague Lin Pu.
NR 72
TC 1
Z9 1
U1 5
U2 17
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD OCT 18
PY 2012
VL 116
IS 41
BP 10115
EP 10121
DI 10.1021/jp3079315
PG 7
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 047WM
UT WOS:000311872200010
PM 22994287
ER
PT J
AU Han, JW
Kim, B
Li, J
Meyyappan, M
AF Han, Jin-Woo
Kim, Beomseok
Li, Jing
Meyyappan, M.
TI Carbon Nanotube Based Humidity Sensor on Cellulose Paper
SO JOURNAL OF PHYSICAL CHEMISTRY C
LA English
DT Article
ID SUBSTRATE; SENSITIVITY; DEVICES
AB A humidity sensor on cellulose paper is demonstrated using single-walled carbon nanotubes functionalized with carboxylic acid. The conductance shift of the nanotube network entangled on the microfibril cellulose is utilized for the humidity sensing. Compared to the control sensor made on a glass substrate, the cellulose-mediated charge transport on the paper substrate enhances the sensitivity. The sensor response exhibits linear behavior up to a relative humidity of 75% with good repeatability and low hysteresis. A simple circuit model is used to explain the sensor results. This approach is a step toward future paper electronics for low-cost disposable applications.
C1 [Han, Jin-Woo; Kim, Beomseok; Li, Jing; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
RP Han, JW (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
EM jin-woo.han@nasa.gov
NR 26
TC 51
Z9 51
U1 7
U2 57
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1932-7447
J9 J PHYS CHEM C
JI J. Phys. Chem. C
PD OCT 18
PY 2012
VL 116
IS 41
BP 22094
EP 22097
DI 10.1021/jp3080223
PG 4
WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science,
Multidisciplinary
SC Chemistry; Science & Technology - Other Topics; Materials Science
GA 021RD
UT WOS:000309902100057
ER
PT J
AU Shim, JS
Kuznetsova, M
Rastatter, L
Bilitza, D
Butala, M
Codrescu, M
Emery, BA
Foster, B
Fuller-Rowell, TJ
Huba, J
Mannucci, AJ
Pi, X
Ridley, A
Scherliess, L
Schunk, RW
Sojka, JJ
Stephens, P
Thompson, DC
Weimer, D
Zhu, L
Sutton, E
AF Shim, J. S.
Kuznetsova, M.
Rastaetter, L.
Bilitza, D.
Butala, M.
Codrescu, M.
Emery, B. A.
Foster, B.
Fuller-Rowell, T. J.
Huba, J.
Mannucci, A. J.
Pi, X.
Ridley, A.
Scherliess, L.
Schunk, R. W.
Sojka, J. J.
Stephens, P.
Thompson, D. C.
Weimer, D.
Zhu, L.
Sutton, E.
TI CEDAR Electrodynamics Thermosphere Ionosphere (ETI) Challenge for
systematic assessment of ionosphere/thermosphere models: Electron
density, neutral density, NmF2, and hmF2 using space based observations
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID LOWER ATMOSPHERE; PROFILES; MIDDLE
AB In an effort to quantitatively assess the current capabilities of Ionosphere/Thermosphere (IT) models, an IT model validation study using metrics was performed. This study is a main part of the CEDAR Electrodynamics Thermosphere Ionosphere (ETI) Challenge, which was initiated at the CEDAR workshop in 2009 to better comprehend strengths and weaknesses of models in predicting the IT system, and to trace improvements in ionospheric/thermospheric specification and forecast. For the challenge, two strong geomagnetic storms, four moderate storms, and three quiet time intervals were selected. For the selected events, we obtained four scores (i.e., RMS error, prediction efficiency, ratio of the maximum change in amplitudes, and ratio of the maximum amplitudes) to compare the performance of models in reproducing the selected physical parameters such as vertical drifts, electron and neutral densities, NmF2, and hmF2. In this paper, we present the results from comparing modeled values against space-based measurements including NmF2 and hmF2 from the CHAMP and COSMIC satellites, and electron and neutral densities at the CHAMP satellite locations. It is found that the accuracy of models varies with the metrics used, latitude and geomagnetic activity level.
C1 [Shim, J. S.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bilitza, D.] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA.
[Butala, M.; Mannucci, A. J.; Pi, X.; Stephens, P.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Codrescu, M.; Fuller-Rowell, T. J.] NOAA, Space Weather Predict Ctr, Boulder, CO USA.
[Emery, B. A.; Foster, B.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Huba, J.] USN, Div Plasma Phys, Res Lab, Washington, DC USA.
[Ridley, A.] Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA.
[Scherliess, L.; Schunk, R. W.; Sojka, J. J.; Zhu, L.] Utah State Univ, Ctr Atmospher & Space Sci, Logan, UT 84322 USA.
[Thompson, D. C.; Sutton, E.] USAF, Res Lab, Albuquerque, NM USA.
[Weimer, D.] Virginia Polytech Inst & State Univ, Ctr Space Sci & Engn Res, Blacksburg, VA 24061 USA.
RP Shim, JS (reprint author), Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM jasoon.shim@nasa.gov
RI Rastaetter, Lutz/D-4715-2012; Ridley, Aaron/F-3943-2011; Scherliess,
Ludger/A-7499-2016; Sutton, Eric/A-1574-2016
OI Rastaetter, Lutz/0000-0002-7343-4147; Ridley, Aaron/0000-0001-6933-8534;
Scherliess, Ludger/0000-0002-7388-5255; Sutton, Eric/0000-0003-1424-7189
FU National Aeronautics and Space Administration
FX The CHAMP neutral density data used in this study are obtained from
http://sisko.colorado.edu/sutton/data.html. Portions of this research
were performed at the Jet Propulsion Laboratory, California Institute of
Technology under contract with the National Aeronautics and Space
Administration.
NR 33
TC 16
Z9 16
U1 0
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD OCT 18
PY 2012
VL 10
AR S10004
DI 10.1029/2012SW000851
PG 16
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 023XP
UT WOS:000310071300001
ER
PT J
AU Mikellides, IG
Katz, I
AF Mikellides, Ioannis G.
Katz, Ira
TI Numerical simulations of Hall-effect plasma accelerators on a
magnetic-field-aligned mesh
SO PHYSICAL REVIEW E
LA English
DT Article
ID 2-DIMENSIONAL HYBRID MODEL; THRUSTER; DISCHARGE; SHEATH; OSCILLATIONS;
TURBULENCE; TRANSPORT; DRIFT; FLOW
AB The ionized gas in Hall-effect plasma accelerators spans a wide range of spatial and temporal scales, and exhibits diverse physics some of which remain elusive even after decades of research. Inside the acceleration channel a quasiradial applied magnetic field impedes the current of electrons perpendicular to it in favor of a significant component in the E x B direction. Ions are unmagnetized and, arguably, of wide collisional mean free paths. Collisions between the atomic species are rare. This paper reports on a computational approach that solves numerically the 2D axisymmetric vector form of Ohm's law with no assumptions regarding the resistance to classical electron transport in the parallel relative to the perpendicular direction. The numerical challenges related to the large disparity of the transport coefficients in the two directions are met by solving the equations on a computational mesh that is aligned with the applied magnetic field. This approach allows for a large physical domain that extends more than five times the thruster channel length in the axial direction and encompasses the cathode boundary where the lines of force can become nonisothermal. It also allows for the self-consistent solution of the plasma conservation laws near the anode boundary, and for simulations in accelerators with complex magnetic field topologies. Ions are treated as an isothermal, cold (relative to the electrons) fluid, accounting for the ion drag in the momentum equation due to ion-neutral (charge-exchange) and ion-ion collisions. The density of the atomic species is determined using an algorithm that eliminates the statistical noise associated with discrete-particle methods. Numerical simulations are presented that illustrate the impact of the above-mentioned features on our understanding of the plasma in these accelerators.
C1 [Mikellides, Ioannis G.; Katz, Ira] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mikellides, IG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ioannis.g.mikellides@jpl.nasa.gov
NR 46
TC 14
Z9 14
U1 2
U2 12
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0045
EI 2470-0053
J9 PHYS REV E
JI Phys. Rev. E
PD OCT 17
PY 2012
VL 86
IS 4
AR 046703
DI 10.1103/PhysRevE.86.046703
PN 2
PG 17
WC Physics, Fluids & Plasmas; Physics, Mathematical
SC Physics
GA 021SE
UT WOS:000309904900006
PM 23214706
ER
PT J
AU Collinson, GA
Wilson, LB
Sibeck, DG
Shane, N
Zhang, TL
Moore, TE
Coates, AJ
Barabash, S
AF Collinson, G. A.
Wilson, L. B.
Sibeck, D. G.
Shane, N.
Zhang, T. L.
Moore, T. E.
Coates, A. J.
Barabash, S.
TI Short large-amplitude magnetic structures (SLAMS) at Venus
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID COMET GIACOBINI-ZINNER; QUASI-PARALLEL SHOCKS; EARTHS BOW SHOCK;
MAGNETOSONIC WAVES; UPSTREAM; EXPRESS; IONS; SIMULATIONS; PULSATIONS;
LOCATION
AB We present the first observation of magnetic fluctuations consistent with short large-amplitude magnetic structures (SLAMS) in the foreshock of the planet Venus. Three monolithic magnetic field spikes were observed by the Venus Express on 11 April 2009. The structures were similar to 1.5-11 s in duration, had magnetic compression ratios between similar to 3 and 6, and exhibited elliptical polarization. These characteristics are consistent with the SLAMS observed at Earth, Jupiter, and Comet Giacobini-Zinner, and thus we hypothesize that it is possible SLAMS may be found at any celestial body with a foreshock.
C1 [Collinson, G. A.; Wilson, L. B.; Sibeck, D. G.; Moore, T. E.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Shane, N.; Coates, A. J.] Univ Coll London, Mullard Space Sci Lab, Holmbury, England.
[Shane, N.] UCL Birkbeck, Ctr Planetary Sci, London, England.
[Zhang, T. L.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria.
[Barabash, S.] Swedish Inst Space Phys, S-98128 Kiruna, Sweden.
RP Collinson, GA (reprint author), NASA, Heliophys Sci Div, Goddard Space Flight Ctr, 8080 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM glyn.a.collinson@nasa.gov
RI Moore, Thomas/D-4675-2012; Wilson III, Lynn/D-4425-2012; Coates,
Andrew/C-2396-2008;
OI Moore, Thomas/0000-0002-3150-1137; Wilson III, Lynn/0000-0002-4313-1970;
Coates, Andrew/0000-0002-6185-3125; Shane, Neville/0000-0003-1024-7739
FU NASA
FX This work was supported by an appointment to the NASA Postdoctoral
Program at NASA Goddard Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA.
NR 49
TC 5
Z9 5
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD OCT 16
PY 2012
VL 117
AR A10221
DI 10.1029/2012JA017838
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 024CB
UT WOS:000310084200001
ER
PT J
AU Sherwin, BD
Das, S
Hajian, A
Addison, G
Bond, JR
Crichton, D
Devlin, MJ
Dunkley, J
Gralla, MB
Halpern, M
Hill, JC
Hincks, AD
Hughes, JP
Huffenberger, K
Hlozek, R
Kosowsky, A
Louis, T
Marriage, TA
Marsden, D
Menanteau, F
Moodley, K
Niemack, MD
Page, LA
Reese, ED
Sehgal, N
Sievers, J
Sifon, C
Spergel, DN
Staggs, ST
Switzer, ER
Wollack, E
AF Sherwin, Blake D.
Das, Sudeep
Hajian, Amir
Addison, Graeme
Bond, J. Richard
Crichton, Devin
Devlin, Mark J.
Dunkley, Joanna
Gralla, Megan B.
Halpern, Mark
Hill, J. Colin
Hincks, Adam D.
Hughes, John P.
Huffenberger, Kevin
Hlozek, Renee
Kosowsky, Arthur
Louis, Thibaut
Marriage, Tobias A.
Marsden, Danica
Menanteau, Felipe
Moodley, Kavilan
Niemack, Michael D.
Page, Lyman A.
Reese, Erik D.
Sehgal, Neelima
Sievers, Jon
Sifon, Cristobal
Spergel, David N.
Staggs, Suzanne T.
Switzer, Eric R.
Wollack, Ed
TI The Atacama Cosmology Telescope: Cross-correlation of cosmic microwave
background lensing and quasars
SO PHYSICAL REVIEW D
LA English
DT Article
ID GALACTIC NUCLEI; MODEL; ANISOTROPIES; POLARIZATION; CALIBRATION; MATTER;
SKY; CMB
AB We measure the cross-correlation of Atacama cosmology telescope cosmic microwave background (CMB) lensing convergence maps with quasar maps made from the Sloan Digital Sky Survey DR8 SDSS-XDQSO photometric catalog. The CMB lensing quasar cross-power spectrum is detected for the first time at a significance of 3.8 sigma, which directly confirms that the quasar distribution traces the mass distribution at high redshifts z > 1. Our detection passes a number of null tests and systematic checks. Using this cross-power spectrum, we measure the amplitude of the linear quasar bias assuming a template for its redshift dependence, and find the amplitude to be consistent with an earlier measurement from clustering; at redshift z approximate to 1.4, the peak of the distribution of quasars in our maps, our measurement corresponds to a bias of b = 2.5 +/- 0.6. With the signal-to-noise ratio on CMB lensing measurements likely to improve by an order of magnitude over the next few years, our results demonstrate the potential of CMB lensing cross-correlations to probe astrophysics at high redshifts.
C1 [Sherwin, Blake D.; Das, Sudeep; Niemack, Michael D.; Page, Lyman A.; Sievers, Jon; Staggs, Suzanne T.; Switzer, Eric R.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Das, Sudeep; Hill, J. Colin; Hlozek, Renee; Marriage, Tobias A.; Sehgal, Neelima; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Hajian, Amir; Bond, J. Richard; Hincks, Adam D.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Addison, Graeme; Dunkley, Joanna; Louis, Thibaut] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Crichton, Devin; Gralla, Megan B.; Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Devlin, Mark J.; Reese, Erik D.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Halpern, Mark] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada.
[Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Huffenberger, Kevin] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA.
[Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Marsden, Danica] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Moodley, Kavilan] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Niemack, Michael D.] Natl Inst Stand & Technol, Quantum Devices Grp, Boulder, CO 80305 USA.
[Sifon, Cristobal] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile.
[Switzer, Eric R.] Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Wollack, Ed] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sherwin, BD (reprint author), Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
EM bsherwin@princeton.edu
RI Wollack, Edward/D-4467-2012; Spergel, David/A-4410-2011
OI Wollack, Edward/0000-0002-7567-4451; Huffenberger,
Kevin/0000-0001-7109-0099; Sievers, Jonathan/0000-0001-6903-5074; Sifon,
Cristobal/0000-0002-8149-1352;
FU U.S. NSF [AST-0408698, PHY-0355328, AST-0707731, PIRE-0507768];
Princeton University; University of Pennsylvania; FONDAP; Basal; Centre
AIUC; RCUK Fellowship; NASA Grant [NNX08AH30G]; NSERC PGSD; NSF PFC
Grant [PHY-0114422]; KICP Fellowship; SLAC Grant [DE-AC3-76SF00515]; ERC
Grant [259505]; BCCP; NSF GRFP; Programa de Astronomia, a program of the
Comision Nacional de Investigacion Cientifica y Tecnologica de Chile
(CONICYT); CFI; Compute Canada; government of Ontario; Ontario Research
Fund-Research Excellence; University of Toronto
FX We thank Jo Bovy and Michael Strauss for discussions and helpful
comments on the draft, and acknowledge useful discussions with Kendrick
Smith and Alex van Engelen. This work was supported by the U.S. NSF
through Grants No. AST-0408698, No. PHY-0355328, No. AST-0707731, and
No. PIRE-0507768, as well as by Princeton University, the University of
Pennsylvania, FONDAP, Basal, Centre AIUC, RCUK Fellowship (J. D.), NASA
Grant No. NNX08AH30G (S. D., A. H., T. M.), NSERC PGSD (A. D. H.), NSF
PFC Grant No. PHY-0114422 (E. S.), KICP Fellowship (E. S.), SLAC Grant
No. DE-AC3-76SF00515 (N. S.), ERC Grant No. 259505 (J. D.), BCCP (S.
D.), and the NSF GRFP (B. D. S., B. L. S.). We thank B. Berger, R.
Escribano, T. Evans, D. Faber, P. Gallardo, A. Gomez, M. Gordon, D.
Holtz, M. McLaren, W. Page, R. Plimpton, D. Sanchez, O. Stryzak, M.
Uehara, and Astro-Norte for assistance with ACT. ACT operates in the
Parque Astronomico Atacama in northern Chile under the auspices of
Programa de Astronomia, a program of the Comision Nacional de
Investigacion Cientifica y Tecnologica de Chile (CONICYT). Computations
were performed on the GPC supercomputer at the SciNet HPC Consortium.
SciNet is funded by the CFI under the auspices of Compute Canada, the
government of Ontario, the Ontario Research Fund-Research Excellence,
and the University of Toronto.
NR 38
TC 49
Z9 49
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 OCT 16
PY 2012
VL 86
IS 8
AR 083006
DI 10.1103/PhysRevD.86.083006
PG 8
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 021BC
UT WOS:000309859300001
ER
PT J
AU Xue, Y
Balmaseda, MA
Boyer, T
Ferry, N
Good, S
Ishikawa, I
Kumar, A
Rienecker, M
Rosati, AJ
Yin, YH
AF Xue, Yan
Balmaseda, Magdalena A.
Boyer, Tim
Ferry, Nicolas
Good, Simon
Ishikawa, Ichiro
Kumar, Arun
Rienecker, Michele
Rosati, Anthony J.
Yin, Yonghong
TI A Comparative Analysis of Upper-Ocean Heat Content Variability from an
Ensemble of Operational Ocean Reanalyses
SO JOURNAL OF CLIMATE
LA English
DT Article
ID TROPICAL INDIAN-OCEAN; SEA-SURFACE TEMPERATURE; IMPROVED COUPLED MODEL;
ENSO PREDICTION; INTERANNUAL VARIABILITY; CLIMATE VARIABILITY; DECADAL
PREDICTION; DATA ASSIMILATION; ANALYSIS SYSTEM; LEVEL
AB Ocean heat content (HC) is one of the key indicators of climate variability and also provides ocean memory critical for seasonal and decadal predictions. The availability of multiple operational ocean analyses (ORAs) now routinely produced around the world is an opportunity for estimation of uncertainties in HC analysis and development of ensemble-based operational HC climate indices. In this context, the spread across the ORAs is used to quantify uncertainties in HC analysis and the ensemble mean of ORAs to identify, and to monitor, climate signals. Toward this goal, this study analyzed 10 ORAs, two objective analyses based on in situ data only, and eight model analyses based on ocean data assimilation systems. The mean, annual cycle, interannual variability, and long-term trend of HC in the upper 300 m (HC300) from 1980 to 2009 are compared. The spread across HC300 analyses generally decreased with time and reached a minimum in the early 2000s when the Argo data became available. There was a good correspondence between the increase of data counts and reduction of the spread. The agreement of HC300 anomalies among different ORAs, measured by the signal-to-noise ratio (SIN), is generally high in the tropical Pacific, tropical Indian Ocean, North Pacific, and North Atlantic but low in the tropical Atlantic and extratropical southern oceans where observations are very sparse. A set of climate indices was derived as HC300 anomalies averaged over the areas where the covariability between SST and HC300 represents the major climate modes such as ENS, Indian Ocean dipole, Atlantic Nino, Pacific decadal oscillation, and Atlantic multidecadal oscillation.
C1 [Xue, Yan; Kumar, Arun] NOAA, NWS, NCEP, Climate Predict Ctr,WWB, Camp Springs, MD 20746 USA.
[Balmaseda, Magdalena A.] ECMWF, Reading, Berks, England.
[Boyer, Tim] NOAA Natl Oceanog Data Ctr, Silver Spring, MD USA.
[Ferry, Nicolas] Mercator Ocean, Toulouse, France.
[Good, Simon] Hadley Ctr, Met Off, Exeter, Devon, England.
[Ishikawa, Ichiro] Japan Meteorol Agcy, Tokyo, Japan.
[Rienecker, Michele] NASA GSFC, Global Modeling & Assimilat Off, Greenbelt, MD USA.
[Rosati, Anthony J.] Princeton Univ, Geophys Fluid Dynam Lab, Princeton, NJ 08544 USA.
[Yin, Yonghong] Ctr Australia Weather & Climate Res, Melbourne, Vic, Australia.
[Yin, Yonghong] Bur Meteorol, Melbourne, Vic, Australia.
RP Xue, Y (reprint author), NOAA, NWS, NCEP, Climate Predict Ctr,WWB, Room 605-A,5200 Auth Rd, Camp Springs, MD 20746 USA.
EM yan.xue@noaa.gov
FU NOAA Climate Observation Division of Climate Program Office
FX We thank support from the NOAA Climate Observation Division of Climate
Program Office for this study. The EN3 analysis was supported by the
Joint DECC/Defra Met Office Hadley Centre Climate Program (GA01101); The
GMAO analysis was supported by the NASA Modeling, Analysis and
Prediction (MAP) Program; The BOM analysis was supported by the
Australian Managing Climate Variability Program. We also thank Dr. David
Behringer, Dr. Oscar Alves, Dr. Zeng-Zhen Hu, and Dr. Caihong Wen for
helpful comments on the manuscript.
NR 60
TC 37
Z9 37
U1 0
U2 32
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
J9 J CLIMATE
JI J. Clim.
PD OCT 15
PY 2012
VL 25
IS 20
BP 6905
EP 6929
DI 10.1175/JCLI-D-11-00542.1
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 022GB
UT WOS:000309944500002
ER
PT J
AU Kug, JS
Ham, YG
AF Kug, Jong-Seong
Ham, Yoo-Geun
TI Indian Ocean Feedback to the ENSO Transition in a Multimodel Ensemble
SO JOURNAL OF CLIMATE
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; EQUATORIAL WARM POOL; EAST-ASIAN CLIMATE;
EL-NINO; COUPLED GCM; INTERANNUAL VARIABILITY; INTERACTIVE FEEDBACK;
RECHARGE PARADIGM; PACIFIC CLIMATE; DIPOLE MODE
AB Observational studies hypothesized that Indian Ocean (IO) feedback plays a role in leading to a fast transition of El Nino. When El Nino accompanies IO warming, IO warming induces the equatorial easterlies over the western Pacific (WP), leading to a rapid termination of El Nino via an oceanic adjust process. In this study, this IO feedback is reinvestigated using the Coupled Model Intercomparison Project phase 3 (CMIP3) coupled GCM simulations. It is found that most of the climate models mimic this IO feedback reasonably, supporting the observational hypothesis. However, most climate models tend to underestimate the strength of the IO feedback, which means the phase transition of ENSO due to the IO feedback is less effective than the observed one. Furthermore, there is great intermodel diversity in simulating the strength of the IO feedback. It is shown that the strength of the IO feedback is related to the precipitation responses to El Nino and IO SST forcings over the warm-pool regions. Moreover, the authors suggest that the distribution of climatological precipitation is one important component in controlling the strength of the IO feedback.
C1 [Kug, Jong-Seong] Korea Inst Ocean Sci & Technol, Ansan, South Korea.
[Ham, Yoo-Geun] NASA GSFC, Global Modeling & Assimilat Off, Greenbelt, MD USA.
[Ham, Yoo-Geun] Univ Space Res Assoc, Columbia, MD USA.
RP Ham, YG (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA.
EM yoo-geun.ham@nasa.gov
RI KUG, JONG-SEONG/A-8053-2013
FU Korea Meteorological Administration Research and Development Program
[CATER 2012-3042]
FX This work is supported by the Korea Meteorological Administration
Research and Development Program under Grant CATER 2012-3042.
NR 50
TC 5
Z9 5
U1 0
U2 12
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
J9 J CLIMATE
JI J. Clim.
PD OCT 15
PY 2012
VL 25
IS 20
BP 6942
EP 6957
DI 10.1175/JCLI-D-12-00078.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 022GB
UT WOS:000309944500004
ER
PT J
AU Zhu, XS
Zong, J
Miller, A
Wiersma, K
Norwood, RA
Prasad, NS
Chavez-Pirson, A
Peyghambarian, N
AF Zhu, Xiushan
Zong, Jie
Miller, Andy
Wiersma, Kort
Norwood, R. A.
Prasad, Narasimha S.
Chavez-Pirson, Arturo
Peyghambarian, N.
TI Single-frequency Ho3+-doped ZBLAN fiber laser at 1200 nm
SO OPTICS LETTERS
LA English
DT Article
AB A single-frequency (SF) fiber laser at 1200 nm was developed with a distributed Bragg reflector (DBR) configuration by splicing a 22 mm long highly holmium-doped ZBLAN (ZrF4-BaF2-LaF3-AlF3-NaF) fiber with a pair of silica fiber Bragg gratings. The linewidth was estimated to be less than 100 kHz based on the measured frequency noise. The relative intensity noise was measured to be < 110 dB/Hz at the relaxation oscillation peak and the polarization extinction ratio was measured to be >19 dB. Our results highlight the exciting prospect that wavelength coverage of SF DBR fiber lasers can be expanded significantly by using rare-earth-doped ZBLAN fibers. (C) 2012 Optical Society of America
C1 [Zhu, Xiushan; Zong, Jie; Miller, Andy; Wiersma, Kort; Chavez-Pirson, Arturo; Peyghambarian, N.] NP Photon Inc, Tucson, AZ 85747 USA.
[Zhu, Xiushan; Norwood, R. A.; Peyghambarian, N.] Univ Arizona, Coll Opt Sci, Tucson, AZ 85721 USA.
[Prasad, Narasimha S.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Zhu, XS (reprint author), NP Photon Inc, 9030 S Rita Rd, Tucson, AZ 85747 USA.
EM xzhu@npphotonics.com
FU NASA SBIR [NNX10CB39C]
FX This work was supported by NASA SBIR Project "1.26 mu m SF fiber
oscillator" under contract no. NNX10CB39C.
NR 13
TC 14
Z9 14
U1 0
U2 21
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 OCT 15
PY 2012
VL 37
IS 20
BP 4185
EP 4187
PG 3
WC Optics
SC Optics
GA 023RP
UT WOS:000310052800007
PM 23073405
ER
PT J
AU Cataldo, G
Beall, JA
Cho, HM
McAndrew, B
Niemack, MD
Wollack, EJ
AF Cataldo, Giuseppe
Beall, James A.
Cho, Hsiao-Mei
McAndrew, Brendan
Niemack, Michael D.
Wollack, Edward J.
TI Infrared dielectric properties of low-stress silicon nitride
SO OPTICS LETTERS
LA English
DT Article
ID FILMS
AB Silicon nitride thin films play an important role in the realization of sensors, filters, and high-performance circuits. Estimates of the dielectric function in the far- and mid-IR regime are derived from the observed transmittance spectra for a commonly employed low-stress silicon nitride formulation. The experimental, modeling, and numerical methods used to extract the dielectric parameters with an accuracy of approximately 4% are presented. (C) 2012 Optical Society of America
C1 [Cataldo, Giuseppe; McAndrew, Brendan; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cataldo, Giuseppe] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Beall, James A.; Cho, Hsiao-Mei; Niemack, Michael D.] NIST, Boulder, CO 80305 USA.
RP Cataldo, G (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Giuseppe.Cataldo@nasa.gov
RI Wollack, Edward/D-4467-2012
OI Wollack, Edward/0000-0002-7567-4451
NR 18
TC 15
Z9 16
U1 1
U2 11
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0146-9592
J9 OPT LETT
JI Opt. Lett.
PD OCT 15
PY 2012
VL 37
IS 20
BP 4200
EP 4202
PG 3
WC Optics
SC Optics
GA 023RP
UT WOS:000310052800012
PM 23073410
ER
PT J
AU Rossmanith, G
Modest, H
Rath, C
Banday, AJ
Gorski, KM
Morfill, G
AF Rossmanith, G.
Modest, H.
Raeth, C.
Banday, A. J.
Gorski, K. M.
Morfill, G.
TI Probing non-Gaussianities in the cosmic microwave background on an
incomplete sky using surrogates
SO PHYSICAL REVIEW D
LA English
DT Article
ID HEMISPHERICAL POWER ASYMMETRY; TIME-SERIES DATA; WMAP DATA; PRIMORDIAL
INHOMOGENEITY; INFLATIONARY UNIVERSE; FULL SKY; MAPS; TEMPERATURE;
SPECTRUM; ISOTROPY
AB We demonstrate the feasibility to generate surrogates by Fourier-based methods for an incomplete data set. This is performed for the case of a cosmic microwave background analysis, where astrophysical foreground emission, mainly present in the Galactic plane, is a major challenge. The shuffling of the Fourier phases for generating surrogates is now enabled by transforming the spherical harmonics into a new set of basis functions that are orthonormal on the cut sky. The results show that non-Gaussianities and hemispherical asymmetries in the cosmic microwave background as identified in several former investigations, can still be detected even when the complete Galactic plane (vertical bar b vertical bar < 30 degrees) is removed. We conclude that the Galactic plane cannot be the dominant source for these anomalies. The results point towards a violation of statistical isotropy.
C1 [Rossmanith, G.; Modest, H.; Raeth, C.; Morfill, G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Banday, A. J.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Banday, A. J.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse, France.
[Gorski, K. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
RP Rossmanith, G (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
FU NASA Office of Space Science
FX Many of the results in this paper have been obtained using HEALPix [35].
We acknowledge the use of LAMBDA. Support for LAMBDA is provided by the
NASA Office of Space Science. We want to thank the referees for their
comments and suggestions.
NR 40
TC 5
Z9 5
U1 0
U2 1
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD OCT 15
PY 2012
VL 86
IS 8
AR 083005
DI 10.1103/PhysRevD.86.083005
PG 9
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 020MA
UT WOS:000309812300001
ER
PT J
AU Frei, A
Tedesco, M
Lee, S
Foster, J
Hall, DK
Kelly, R
Robinson, DA
AF Frei, Allan
Tedesco, Marco
Lee, Shihyan
Foster, James
Hall, Dorothy K.
Kelly, Richard
Robinson, David A.
TI A review of global satellite-derived snow products
SO ADVANCES IN SPACE RESEARCH
LA English
DT Review
DE Snow; Remote sensing
ID PASSIVE MICROWAVE DATA; INTERACTIVE MULTISENSOR SNOW; WATER EQUIVALENT
RETRIEVALS; GROUND-BASED MEASUREMENTS; WESTERN NORTH-AMERICA; MACKENZIE
RIVER-BASIN; ICE MAPPING SYSTEM; CLIMATE-CHANGE; COVER PRODUCTS;
ARCTIC-OCEAN
AB Snow cover over the Northern Hemisphere plays a crucial role in the Earth's hydrology and surface energy balance, and modulates feedbacks that control variations of global climate. While many of these variations are associated with exchanges of energy and mass between the land surface and the atmosphere, other expected changes are likely to propagate downstream and affect oceanic processes in coastal zones. For example, a large component of the freshwater flux into the Arctic Ocean comes from snow melt. The timing and magnitude of this flux affects biological and thermodynamic processes in the Arctic Ocean, and potentially across the globe through their impact on North Atlantic Deep Water formation.
Several recent global remotely sensed products provide information at unprecedented temporal, spatial, and spectral resolutions. In this article we review the theoretical underpinnings and characteristics of three key products. We also demonstrate the seasonal and spatial patterns of agreement and disagreement amongst them, and discuss current and future directions in their application and development. Though there is general agreement amongst these products, there can be disagreement over certain geographic regions and under conditions of ephemeral, patchy and melting snow. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Frei, Allan] CUNY Hunter Coll, Dept Geog, New York, NY 10065 USA.
[Tedesco, Marco] CUNY City Coll, Dept Earth & Atmospher Sci, New York, NY 10031 USA.
[Lee, Shihyan] Sigma Space Corp, Lanham, MD 20706 USA.
[Foster, James; Hall, Dorothy K.] NASA, Hydrospher & Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kelly, Richard] Univ Waterloo, Dept Geog & Environm Management, Waterloo, ON N2L 3G1, Canada.
[Robinson, David A.] Rutgers State Univ, Dept Geog, Piscataway, NJ 08854 USA.
RP Frei, A (reprint author), CUNY Hunter Coll, Dept Geog, Rm 1006N,695 Pk Ave, New York, NY 10065 USA.
EM afrei@hunter.cuny.edu
RI Tedesco, Marco/F-7986-2015
FU NASA [NNX08AQ70G, NNX08AI02G, NNX08AP34A]; NOAA Climate Program Office
[EA133E10SE2623, NA08AR 4310678]
FX Frei is supported by the NASA Cryospheric Sciences Program award
#NNX08AQ70G, and began work on this article while on sabbatical leave at
the Climate Research Division of Environment Canada in Downsview,
Ontario. M. Tedesco is supported by NASA Grant # NNX08AI02G. D. Robinson
acknowledges funding support from NASA MEaSUREs award NNX08AP34A and
NOAA Climate Program Office awards EA133E10SE2623 and NA08AR 4310678.
Two anonymous reviewers made valuable contributions to, and helped
clarify, our manuscript; and we thank T. Estilow and Jeff Miller for
contributions to the figures.
NR 163
TC 55
Z9 61
U1 7
U2 105
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD OCT 15
PY 2012
VL 50
IS 8
BP 1007
EP 1029
DI 10.1016/j.asr.2011.12.021
PG 23
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 010LG
UT WOS:000309095300003
ER
PT J
AU Su, CM
Puls, RW
Krug, TA
Watling, MT
O'Hara, SK
Quinn, JW
Ruiz, NE
AF Su, Chunming
Puls, Robert W.
Krug, Thomas A.
Watling, Mark T.
O'Hara, Suzanne K.
Quinn, Jacqueline W.
Ruiz, Nancy E.
TI A two and half-year-performance evaluation of a field test on treatment
of source zone tetrachloroethene and its chlorinated daughter products
using emulsified zero valent iron nanoparticles
SO WATER RESEARCH
LA English
DT Article
DE Tetrachloroethene; Emulsified zero valent iron nanoparticles;
Groundwater remediation; Pneumatic and direct injections; Reductive
dechlorination; Mass flux
ID MICROBIAL REDUCTIVE DECHLORINATION; MODIFIED FE-0 NANOPARTICLES;
PARTICLE CONCENTRATION; TCE DECHLORINATION; VINYL-CHLORIDE; MASS FLUXES;
NANOSCALE; GROUNDWATER; WATER; TRANSPORT
AB A field test of emulsified zero valent iron (EZVI) nanoparticles was conducted at Parris Island, SC, USA and was monitored for two and half years to assess the treatment of subsurface-source zone chlorinated volatile organic compounds (CVOCs) dominated by tetrachloroethene (PCE) and its chlorinated daughter products. Two EZVI delivery methods were used: pneumatic injection and direct injection. In the pneumatic injection plot, 2180 L of EZVI containing 225 kg of iron (Toda RNIP-10DS), 856 kg of corn oil, and 22.5 kg of surfactant were injected to remedy an estimated 38 kg of CVOCs. In the direct injection plot, 572 L of EZVI were injected to treat an estimated 0.155 kg of CVOCs. After injection of the EZVI, significant reductions in PCE and trichloroethene (TCE) concentrations were observed in downgradient wells with corresponding increases in degradation products including significant increases in ethene. In the pneumatic injection plot, there were significant reductions in the downgradient groundwater mass flux values for PCE (>85%) and TCE (>85%) and a significant increase in the mass flux of ethene. There were significant reductions in total CVOC mass (86%); an estimated reduction of 63% in the sorbed and dissolved phases and 93% reduction in the PCE DNAPL mass. There are uncertainties in these estimates because DNAPL may have been mobilized during and after injection. Following injection, significant increases in dissolved sulfide, volatile fatty acids (VFA), and total organic carbon (TOC) were observed. In contrast, dissolved sulfate and pH decreased in many wells. The apparent effective remediation seems to have been accomplished by direct abiotic dechlorination by nanoiron followed by biological reductive dechlorination stimulated by the corn oil in the emulsion. Published by Elsevier Ltd.
C1 [Su, Chunming; Puls, Robert W.] US EPA, Ground Water & Ecosyst Restorat Div, Natl Risk Management Res Lab, Off Res & Dev, Ada, OK 74820 USA.
[Krug, Thomas A.; Watling, Mark T.; O'Hara, Suzanne K.] Geosyntec Consultants Inc, Guelph, ON N1G 5G3, Canada.
[Quinn, Jacqueline W.] NASA, Kennedy Space Ctr, FL 32899 USA.
[Ruiz, Nancy E.] USN, Facil Engn Command, Engn Serv Ctr, Port Hueneme, CA 93043 USA.
RP Su, CM (reprint author), US EPA, Ground Water & Ecosyst Restorat Div, Natl Risk Management Res Lab, Off Res & Dev, 919 Kerr Res Dr, Ada, OK 74820 USA.
EM su.chunming@epa.gov
FU ESTCP [ER-0431]; U.S.EPA
FX This project is a collaboration among the United States Environmental
Protection Agency through its Office of Research and Development,
Geosyntec Consultants Inc., NASA, and the Naval Facilities Engineering
Service Center. Funding was provided by ESTCP (project ER-0431) and the
U.S.EPA. Although the research described in this article has been funded
partly by the U.S.EPA, it has not been subjected to the Agency's peer
and administrative review and, therefore, does not necessarily reflect
the views of the Agency, and no official endorsement should be inferred.
Mention of trade names or commercial products does not constitute
endorsement or recommendation for use. We are grateful to the following
individuals and organizations: Deborah Schnell, Cornel Plebani, and
their team of Pneumatic Fracturing, Inc. (Alpha, NJ) for high-pressure
pneumatic injection of EZVI, Andrew Thornton and Corey Gamwell of
Vironex Environmental Field Service (Golden, CO) for direct push
injection of EZVI, Drs. Cherie Geiger and Christian Clausen of the
University of Central Florida for assisting with on-site preparation of
EZVI, Mr. Tim Harrington of MCRD at Parris Island and Ms. Bridget Toews
(Independent Contractor) for providing logistical support, Messrs.
Justin Groves, Brad Scroggins, Ken Jewell, Russell Neil, Tim Lankford,
and Pat Clark of EPA, and Steve Randall of Geosyntec for field support,
Ms. Lynda Callaway and Kristie Hargrove and Mr. Mark White of EPA for
TOC/TIC and anions analyses, Messrs. Steve Markham and Andrew Greenwood
and Ms. Sandra Saye of Shaw Environmental & Infrastructure, Inc. for
metals analysis, and Columbia Analytical Services, In. (Rochester, NY)
for VOC, DHG, and VFA analysis, and TestAmerica (Knoxville, TN) for
soils CVOC analysis.
NR 51
TC 35
Z9 35
U1 3
U2 84
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0043-1354
J9 WATER RES
JI Water Res.
PD OCT 15
PY 2012
VL 46
IS 16
BP 5071
EP 5084
DI 10.1016/j.watres.2012.06.051
PG 14
WC Engineering, Environmental; Environmental Sciences; Water Resources
SC Engineering; Environmental Sciences & Ecology; Water Resources
GA 010LL
UT WOS:000309095800018
PM 22868086
ER
PT J
AU Diner, DJ
Hodos, RA
Davis, AB
Garay, MJ
Martonchik, JV
Sanghavi, SV
von Allmen, P
Kokhanovsky, AA
Zhai, PW
AF Diner, David J.
Hodos, Rachel A.
Davis, Anthony B.
Garay, Michael J.
Martonchik, John V.
Sanghavi, Suniti V.
von Allmen, Paul
Kokhanovsky, Alexander A.
Zhai, Pengwang
TI An optimization approach for aerosol retrievals using simulated MISR
radiances
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Aerosols; Optimization; MISR
ID IMAGING SPECTRORADIOMETER MISR; RADIATIVE-TRANSFER MODEL; OCEAN;
MULTIANGLE; LAND; ALGORITHMS; INTENSITY; MIXTURES
AB Currently, many satellite-based aerosol retrievals make use of lookup tables (LUTs) containing precomputed solutions to the radiative transfer (RT) equation. The benefit of this strategy is the avoidance of expensive runtime calculations, but its main drawback is that the LUTs discretize what is inherently a continuous, multivariate solution space. The operational retrieval algorithm for the Multi-angle Imaging SpectroRadiometer (MISR), for example, compares the observations to a set of 74 aerosol mixtures, each composed of particle models having prescribed optical properties and size distributions. In a recent "blind" study comparing the performance of several satellite retrieval algorithms on simulated data over a black surface, the MISR algorithm performed reasonably well in recovering the "true" spectral aerosol optical depths (AODs), but because the correct aerosol model was not contained within the MISR LUT, the retrieved AODs were biased low by similar to 14%. This motivated an investigation of whether an optimization approach, in which the aerosols are modeled by a set of continuously variable parameters recovered using nonlinear least-squares, could improve the results. In this paper, we demonstrate that such an approach using Levenberg-Marquardt optimization yields superior accuracy. Advances in computer speed, development of more efficient RI codes, and algorithm innovations will be necessary for this approach to satisfy the demands of a global, production-level satellite aerosol retrieval process, especially when used in conjunction with future instruments having enhanced sensitivity to diverse aerosol properties. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Diner, David J.; Hodos, Rachel A.; Davis, Anthony B.; Martonchik, John V.; Sanghavi, Suniti V.; von Allmen, Paul] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Garay, Michael J.] Raytheon Co, Pasadena, CA USA.
[Kokhanovsky, Alexander A.] Univ Bremen, D-28359 Bremen, Germany.
[Zhai, Pengwang] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Diner, DJ (reprint author), CALTECH, Jet Prop Lab, MS 169-237,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM David.J.Diner@jpl.nasa.gov
RI Kokhanovsky, Alexander/C-6234-2016
OI Kokhanovsky, Alexander/0000-0001-7370-1164
NR 31
TC 8
Z9 8
U1 0
U2 12
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
J9 ATMOS RES
JI Atmos. Res.
PD OCT 15
PY 2012
VL 116
BP 1
EP 14
DI 10.1016/j.atmosres.2011.05.020
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 004LF
UT WOS:000308682500001
ER
PT J
AU Yang, WD
Marshak, A
Varnai, T
Liu, ZY
AF Yang, Weidong
Marshak, Alexander
Varnai, Tamas
Liu, Zhaoyan
TI Effect of CALIPSO cloud-aerosol discrimination (CAD) confidence levels
on observations of aerosol properties near clouds
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Backscatter enhancement; Transition zone; Twilight zone; CALIPSO;
Aerosol; Remote sensing
ID MODIS OBSERVATIONS; CUMULUS CLOUDS; ART.; PRODUCTS; HUMIDITY; OCEAN;
CERES; LIDAR
AB CALIPSO aerosol backscatter enhancement in the transition zone between clouds and clear sky areas is revisited with particular attention to effects of data selection based on the confidence level of cloud-aerosol discrimination (CAD). The results show that backscatter behavior in the transition zone strongly depends on the CAD confidence level. Higher confidence level data has a flatter backscatter far away from clouds and a much sharper increase near clouds (within 4 km), thus a smaller transition zone. For high confidence level data it is shown that the overall backscatter enhancement is more pronounced for small clear-air segments and horizontally larger clouds. The results suggest that data selection based on CAD reduces the possible effects of cloud contamination when studying aerosol properties in the vicinity of clouds. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Yang, Weidong] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Marshak, Alexander] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Varnai, Tamas] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Liu, Zhaoyan] Natl Inst Aerosp, Hampton, VA 23666 USA.
RP Yang, WD (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
EM weidong.yang@nasa.gov; Alexander.marshak@nasa.gov;
tamas.varnai@nasa.gov; zhaoyan.liu-1@nasa.gov
RI Liu, Zhaoyan/B-1783-2010; Marshak, Alexander/D-5671-2012
OI Liu, Zhaoyan/0000-0003-4996-5738;
FU NASA Radiation Sciences Program; CALIPSO/CLOUDSAT science team
FX We gratefully acknowledge support for this research by the NASA
Radiation Sciences Program and the CALIPSO/CLOUDSAT science team.
NR 35
TC 11
Z9 11
U1 0
U2 17
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
J9 ATMOS RES
JI Atmos. Res.
PD OCT 15
PY 2012
VL 116
BP 134
EP 141
DI 10.1016/j.atmosres.2012.03.013
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 004LF
UT WOS:000308682500013
ER
PT J
AU Hurley, JV
Galewsky, J
Worden, J
Noone, D
AF Hurley, John V.
Galewsky, Joseph
Worden, John
Noone, David
TI A test of the advection-condensation model for subtropical water vapor
using stable isotopologue observations from Mauna Loa Observatory,
Hawaii
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID VOSTOK ICE CORE; HYDROLOGIC-CYCLE; LAST SATURATION; HUMIDITY;
CONVECTION; TRANSPORT; ISOTOPES; CLIMATE; STRATOSPHERE; SIMULATIONS
AB Subtropical humidity plays a critical role in the radiative balance of the planet, and there is a need for adequate description of the controls on water vapor distributions. This study tests whether an advection-condensation model, combined with Rayleigh distillation, can describe observed humidity and water vapor isotope ratios of the subtropical free troposphere. A field campaign, from 9 October to 6 November, 2008, included continuous in situ measurement of water vapor stable isotope ratios at the NOAA Mauna Loa Observatory (MLO), Hawaii. Last saturation patterns for air at the MLO were determined using both Lagrangian back-trajectory and Eulerian model techniques. Last saturation occurs primarily along midlatitude storm tracks (similar to 65%), and secondarily near Hawaii (similar to 10%) within mesoscale convective systems. Periods of lower delta D values at MLO correspond to extra-tropical last saturation, while elevated delta D corresponds with saturation locations near Hawaii. To a first order, the conditions of last saturation are found to set not only the humidity but also the water vapor isotope ratio. In the absence of mixing, reconstructed q and delta D values underestimate the observations. Experimental reconstructions demonstrate that variable amounts of mixing within the free troposphere and about 2% vapor influx mixing per hour from the boundary layer can explain the observed q and delta D values. A last saturation model provides a reasonable description of humidity and water vapor isotope ratios of the subtropical free troposphere and results are sensitive to the treatment of mixing of air parcels last saturated in distinctly different regions of the atmosphere.
C1 [Hurley, John V.; Galewsky, Joseph] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
[Worden, John] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Noone, David] Univ Colorado Boulder, Dept Atmospher & Ocean Sci, Boulder, CO USA.
[Noone, David] Univ Colorado Boulder, Cooperat Inst Res Environm Sci, Boulder, CO USA.
RP Hurley, JV (reprint author), Yale Univ, Dept Geol & Geophys, POB 6666, New Haven, CT 06520 USA.
EM john.hurley@yale.edu
RI hurley, john/A-8707-2015
FU NSF [ATM-0840-168, ATM-0840-129]; NASA ROSES Aura Science Team
[NNH07ZDA001N-AST 07-AST07-0069]; National Aeronautics and Space
Administration
FX We thank Editor Yinon Rudich and three anonymous reviewers for
persistently helpful comments. We also thank Zachary D. Sharp, David
Gutzler, Peter Fawcett, and Ken Minschwaner for thoughtful comments on
an earlier version of the manuscript. NSF grant ATM-0840-168 supported
J. Galewsky and NSF grant ATM-0840-129 supported D. Noone for this
research. 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. The NASA ROSES Aura
Science Team NNH07ZDA001N-AST 07-AST07-0069 contributed to the support
of the analysis.
NR 63
TC 11
Z9 11
U1 1
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 13
PY 2012
VL 117
AR D19118
DI 10.1029/2012JD018029
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 020RN
UT WOS:000309831300004
ER
PT J
AU Painemal, D
Minnis, P
Ayers, JK
O'Neill, L
AF Painemal, David
Minnis, Patrick
Ayers, J. Kirk
O'Neill, Larry
TI GOES-10 microphysical retrievals in marine warm clouds: Multi-instrument
validation and daytime cycle over the southeast Pacific
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID LIQUID WATER PATH; DIURNAL CYCLE; VOCALS-REX; BOUNDARY-LAYER;
STRATOCUMULUS CLOUDS; STRATIFORM CLOUDS; SATELLITE; VARIABILITY; TERRA;
MODIS
AB The daytime evolution of warm cloud microphysical properties over the southeast Pacific during October-November 2008 is investigated with optical/infrared retrievals from the Tenth Geostationary Operational Environmental Satellite (GOES-10) imager. GOES-10 retrievals, produced at NASA Langley Research Center, are validated against in situ aircraft observations and with independent satellite observations. Comparisons with in situ observations reveal high linear correlations (r) for cloud effective radius (r(e)) and optical thickness (tau) (r = 0.89 and 0.69 respectively); nevertheless, a GOES-10 positive mean r(e) bias of 2.3 mu m is apparent, and consistent with other previously reported satellite biases. Smaller biases are found for liquid water path (LWP) and an adiabatic-based cloud droplet number concentration (N-d), both variables derived by combining r(e) and tau. In addition, GOES-10 observations are well correlated with their Moderate Resolution Imaging Spectroradiometer (MODIS) counterparts, but with smaller biases and root-mean-square errors for the Aqua satellite passes, arguably associated with a better calibrated MODIS-Aqua instrument relative to MODIS-Terra. Furthermore, the excellent agreement between GOES-10 LWP and microwave-based satellite retrievals, especially at high solar zenith angles (>60 degrees), provide further evidence of the utility of using GOES-10 retrievals to represent the daytime cloud cycle. In terms of the daytime cycle, GOES-10 observations show an afternoon minimum in LWP and an increase thereafter, consistent with satellite microwave climatologies. The tau cycle explains most of the LWP variance with both variables in phase, minima near noon along the coast, and a 13:30-14:00 local solar time (LST) minimum offshore. In contrast, r(e) is not exactly in phase with LWP and tau, having a minimum approximately at 12: 30 LST throughout the domain. A unique feature is a striking r(e) maximum along the coast at 16: 15 LST, concomitant with a faster tau recovery. An explanation for a coastal r(e) afternoon maximum is lacking although this is consistent with an enhancement of the updraft velocity reported in previous modeling studies. Finally, the GOES-derived Nd (N-d (proportional to) tau(1/2) r(e) (5/2)) shows a complex daytime cycle with maxima at 7: 15 and 13: 15 LST. While the first maximum is driven by large tau, the second one is mainly explained by a minimum in r(e).
C1 [Painemal, David; Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Ayers, J. Kirk] Sci Syst & Applicat Inc, Hampton, VA USA.
[O'Neill, Larry] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
RP Painemal, D (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM david.painemal@nasa.gov
RI Minnis, Patrick/G-1902-2010
OI Minnis, Patrick/0000-0002-4733-6148
FU NASA Postdoctoral Program at the NASA Langley Research Center; NASA
Modeling, Analysis, and Prediction and CERES Programs; U.S. Department
of Energy's Atmospheric Science Program Atmospheric System Research
interagency [DE-SC0000991/003]; NASA [NNX11AF31G]; Institutional
Postdoctoral Fellowship through Oregon State University
FX D. Painemal was supported by the NASA Postdoctoral Program at the NASA
Langley Research Center, administered by Oak Ridge Associated
Universities (ORAU). P. Minnis and J. K. Ayers were supported by the
NASA Modeling, Analysis, and Prediction and CERES Programs, and by the
U.S. Department of Energy's Atmospheric Science Program Atmospheric
System Research interagency Agreement, DE-SC0000991/003. L. O'Neill was
supported by NASA grant NNX11AF31G for funding of NASA's Ocean Vector
Winds Science Team activities and an Institutional Postdoctoral
Fellowship through Oregon State University. The suggestions made by
three anonymous reviewers are also greatly acknowledged.
NR 50
TC 14
Z9 14
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 13
PY 2012
VL 117
AR D19212
DI 10.1029/2012JD017822
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 020RN
UT WOS:000309831300003
ER
PT J
AU Ehlmann, BL
Bish, DL
Ruff, SW
Mustard, JF
AF Ehlmann, B. L.
Bish, D. L.
Ruff, S. W.
Mustard, J. F.
TI Mineralogy and chemistry of altered Icelandic basalts: Application to
clay mineral detection and understanding aqueous environments on Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID THERMAL EMISSION-SPECTROSCOPY; RAY-POWDER DIFFRACTION; LOW-GRADE
METAMORPHISM; MAWRTH VALLIS REGION; GEOTHERMAL SYSTEMS; DIOCTAHEDRAL
SMECTITES; INFRARED-SPECTROSCOPY; REFLECTANCE SPECTRA; CONCEPTUAL
MODELS; TEMPERATURE AREAS
AB We used a suite of techniques, including those emulating compositional data sets obtained from Mars orbit and obtainable at the Mars surface, to examine aqueous alteration of basaltic rocks from Iceland as a mineralogic and geochemical analog for Noachian environments on Mars. A sample suite was collected for laboratory measurement of (1) whole-rock visible/near-infrared (VNIR) reflectance and thermal infrared (TIR) emission spectra; (2) VNIR and TIR reflectance spectra of particle-size separates derived from the bulk rock and from materials extracted from fractures/vesicles; (3) X-ray diffraction (XRD) patterns for determination of quantitative modal mineralogy; (4) major element chemistry using flux fusion of whole-rock powders; and (5) electron microprobe analyses of minerals in thin sections. Conclusions about aqueous alteration can be influenced by technique. For these basalts, whole-rock chemical data showed scant evidence for chemical fractionation, but TIR, VNIR, and XRD measurements identified distinctive assemblages of hydrous silicate minerals, differing by sample. XRD provided the most complete and accurate quantitative determination of sample mineralogy. However, VNIR spectroscopy was the technique most useful for determining composition of low-abundance smectite clays, and TIR spectroscopy was the most useful for recognizing hydrated silicates in thin surface coatings. High spatial resolution mineralogical and chemical data sets were useful for understanding the texture and distribution of alteration products and variations in fluid chemistry. No single approach provides a complete assessment of the environment of alteration, demonstrating the importance of employing multiple, synergistic mineralogical and geochemical techniques and instruments in exploration of rock strata from aqueous paleoenvironments on Mars.
C1 [Ehlmann, B. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Bish, D. L.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA.
[Ruff, S. W.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
[Mustard, J. F.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
RP Ehlmann, BL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM ehlmann@caltech.edu
NR 91
TC 25
Z9 26
U1 4
U2 37
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD OCT 13
PY 2012
VL 117
AR E00J16
DI 10.1029/2012JE004156
PG 27
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 020SD
UT WOS:000309833300002
ER
PT J
AU Milbury, C
Schubert, G
Raymond, CA
Smrekar, SE
Langlais, B
AF Milbury, C.
Schubert, G.
Raymond, C. A.
Smrekar, S. E.
Langlais, B.
TI The history of Mars' dynamo as revealed by modeling magnetic anomalies
near Tyrrhenus Mons and Syrtis Major
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID THERMAL EVOLUTION; PALEOMAGNETIC POLES; MARTIAN DYNAMO; FIELD; CRUSTAL;
GRAVITY; PATERA; TOPOGRAPHY; HEMISPHERE; INVERSION
AB The lack of magnetic anomalies within the major impact basins (Hellas, Argyre, and Isidis) has led many investigators to the conclusion that Mars' dynamo shut down prior to the time when these basins formed (similar to 4.0 Ga). We test this hypothesis by analyzing gravity and magnetic anomalies in the regions surrounding Tyrrhenus Mons and Syrtis Major, two volcanoes that were active during the late Noachian and Hesperian. We model magnetic anomalies that are associated with gravity anomalies and generally find that sources located below Noachian surface units tend to favor paleopoles near the equator and sources located below Hesperian surface features favor paleopoles near the geographical poles, suggesting polar wander during the Noachian-Hesperian. Both paleopole clusters have positive and negative polarities, indicating reversals of the field during the Noachian and Hesperian. Magnetization of sources below Hesperian surfaces is evidence that the dynamo persisted beyond the formation of the major impact basins. The demagnetization associated with the volcanic construct of Syrtis Major implies dynamo cessation occurred while it was geologically active approximately 3.6 billion years ago. Timing of dynamo activity is fundamentally linked to Mars' climate via the stability of its atmosphere, and is coupled to the extent and duration of surface geologic activity. Thus, the dynamo history is key for understanding both when Mars was most geologically active and when it may have been most hospitable to life.
C1 [Milbury, C.; Langlais, B.] CNRS, LPGNantes, F-44300 Nantes, France.
[Milbury, C.; Langlais, B.] Univ Nantes, CNRS, UMR 6112, F-44300 Nantes, France.
[Milbury, C.; Schubert, G.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA.
[Raymond, C. A.; Smrekar, S. E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Milbury, C (reprint author), CNRS, LPGNantes, 2 Rue Houssiniere, F-44300 Nantes, France.
EM cmilbury@ucla.edu
RI Langlais, Benoit/K-5366-2012
OI Langlais, Benoit/0000-0001-5207-304X
FU NASA [NNG05GL93H]; Region Pays de la Loire; NSF [0909206]; Agence
Nationale de la Recherche [ANR-08-JCJC-0126-01]
FX All graphs and maps have been plotted using the Generic Mapping Tools
software [Wessel and Smith, 1991]. C. Milbury was initially supported by
NASA Graduate Student Researcher Program Grant NNG05GL93H and received
additional support from Region Pays de la Loire. G. Schubert
acknowledges partial support from NSF 0909206. A portion of this
research was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA. This study was
supported by Agence Nationale de la Recherche (Project
ANR-08-JCJC-0126-01). We thank two anonymous reviewers for their
comments, which helped to improve this paper.
NR 85
TC 10
Z9 10
U1 0
U2 11
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 OCT 13
PY 2012
VL 117
AR E10007
DI 10.1029/2012JE004099
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 020SD
UT WOS:000309833300001
ER
PT J
AU Qian, LY
Burns, AG
Liu, HL
Chamberlin, PC
AF Qian, Liying
Burns, Alan G.
Liu, Hanli
Chamberlin, Phillip C.
TI Effect of a solar flare on a traveling atmospheric disturbance
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; GRAVITY-WAVES; THERMOSPHERE; DISSIPATION;
MISSION
AB It is known that the sudden injection of energy during geomagnetic storms can excite atmospheric gravity waves (AGWs) or traveling atmospheric disturbances (TADs). Together with large-scale circulation, these AGWs/TADs transport energy and momentum away from their sources. In this paper, we investigate possible involvement of AGWs/TADs during solar flares. Model simulations of an X17 flare that occurred on October 28, 2003 shows that AGWs/TADS contributed to flare energy transport from the sunlit South-Pole region to the nightside equatorial region in 3-4 h, resulting in similar to 10% nightside equatorial neutral density enhancement in the upper thermosphere. These nightside AGWs/TADs have a phase speed on the order of similar to 750 m/s and a horizontal wavelength on the order of 4000 km. Enhanced solar heating to the thermosphere through enhanced ionization during flares occurs on the entire dayside, with the spatial scale of the increased solar heating being too large to excite AGWs/TADs. Further analysis revealed that strong localized enhancement of Joule heating was produced during the October 28, 2003 flare. This sudden injection of the localized heating, together with preexisting AGWs/TADs excited by moderate geomagnetic activity prior to the flare, produced intensified AGWs/TADs, which propagated energy and momentum to the equatorial region. On the other hand, model simulations showed that, under assumed geomagnetically quiet conditions, strong localized enhancement of Joule heating and AGWs/TADs were not produced during the flare. This interplay between geomagnetic activity and solar flares can be a challenge to space weather monitoring, specification, and forecasting.
C1 [Qian, Liying; Burns, Alan G.; Liu, Hanli] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80301 USA.
[Chamberlin, Phillip C.] NASA, Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Qian, LY (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80301 USA.
EM lqian@ucar.edu
RI Liu, Han-Li/A-9549-2008; Chamberlin, Phillip/C-9531-2012; Qian,
Liying/D-9236-2013; Burns, Alan/L-1547-2013
OI Liu, Han-Li/0000-0002-6370-0704; Chamberlin,
Phillip/0000-0003-4372-7405; Qian, Liying/0000-0003-2430-1388;
FU NASA [NNX08AQ31G, NNX09AJ60G]; National Science Foundation's STC program
[ATM-0120950]; National Science Foundation
FX This research was supported by NASA grants NNX08AQ31G and NNX09AJ60G to
the National Center for Atmospheric Research. We would also like to
acknowledge the Center for Integrated Space Weather Modeling (CISM),
which is funded by the National Science Foundation's STC program under
agreement number ATM-0120950. NCAR is sponsored by the National Science
Foundation.
NR 20
TC 2
Z9 2
U1 2
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD OCT 13
PY 2012
VL 117
AR A10319
DI 10.1029/2012JA017806
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 020QZ
UT WOS:000309829800002
ER
PT J
AU Mandt, KE
Gell, DA
Perry, M
Waite, JH
Crary, FA
Young, D
Magee, BA
Westlake, JH
Cravens, T
Kasprzak, W
Miller, G
Wahlund, JE
Agren, K
Edberg, NJT
Heays, AN
Lewis, BR
Gibson, ST
de la Haye, V
Liang, MC
AF Mandt, Kathleen E.
Gell, David A.
Perry, Mark
Waite, J. Hunter, Jr.
Crary, Frank A.
Young, David
Magee, Brian A.
Westlake, Joseph H.
Cravens, Thomas
Kasprzak, Wayne
Miller, Greg
Wahlund, Jan-Erik
Agren, Karin
Edberg, Niklas J. T.
Heays, Alan N.
Lewis, Brenton R.
Gibson, Stephen T.
de la Haye, V.
Liang, Mao-Chang
TI Ion densities and composition of Titan's upper atmosphere derived from
the Cassini Ion Neutral Mass Spectrometer: Analysis methods and
comparison of measured ion densities to photochemical model simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID IONOSPHERE; CHEMISTRY; PLASMA; HYDROCARBONS; SPECTRA
AB The Cassini Ion Neutral Mass Spectrometer (INMS) has measured both neutral and ion species in Titan's upper atmosphere and ionosphere and the Enceladus plumes. Ion densities derived from INMS measurements are essential data for constraining photochemical models of Titan's ionosphere. The objective of this paper is to present an optimized method for converting raw data measured by INMS to ion densities. To do this, we conduct a detailed analysis of ground and in-flight calibration to constrain the instrument response to ion energy, the critical parameter on which the calibration is based. Data taken by the Cassini Radio Plasma Wave Science Langmuir Probe and the Cassini Plasma Spectrometer Ion Beam Spectrometer are used as independent measurement constraints in this analysis. Total ion densities derived with this method show good agreement with these data sets in the altitude region (similar to 1100-1400 km) where ion drift velocities are low and the mass of the ions is within the measurement range of the INMS (1-99 Daltons). Although ion densities calculated by the method presented here differ slightly from those presented in previous INMS publications, we find that the implications for the science presented in previous publications is mostly negligible. We demonstrate the role of the INMS ion densities in constraining photochemical models and find that (1) cross sections having high resolution as a function of wavelength are necessary for calculating the initial photoionization products and (2) there are disagreements between the measured ion densities representative of the initial steps in Titan photochemistry that require further investigation.
C1 [Mandt, Kathleen E.; Gell, David A.; Waite, J. Hunter, Jr.; Crary, Frank A.; Young, David; Magee, Brian A.; Miller, Greg] SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78228 USA.
[Mandt, Kathleen E.] Univ Texas San Antonio, Dept Environm & Civil Engn, San Antonio, TX USA.
[Perry, Mark; Westlake, Joseph H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Cravens, Thomas] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Kasprzak, Wayne] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wahlund, Jan-Erik; Agren, Karin; Edberg, Niklas J. T.] Swedish Inst Space Phys, Uppsala, Sweden.
[Heays, Alan N.] Leiden Univ, Leiden Observ, Leiden, Netherlands.
[Lewis, Brenton R.; Gibson, Stephen T.] Australian Natl Univ, Res Sch Phys & Engn, Canberra, ACT, Australia.
[de la Haye, V.] Univ Calif San Diego, Dept Psychiat, La Jolla, CA 92093 USA.
[Liang, Mao-Chang] Acad Sinica, Ctr Environm Changes, Taipei 115, Taiwan.
RP Mandt, KE (reprint author), SW Res Inst, Space Sci & Engn Div, 6220 Culebra Rd, San Antonio, TX 78228 USA.
EM kmandt@swri.edu
RI Mandt, Kathleen/M-9812-2013; Westlake, Joseph/G-2732-2015; Perry,
Mark/B-8870-2016;
OI Mandt, Kathleen/0000-0001-8397-3315; Westlake,
Joseph/0000-0003-0472-8640; Perry, Mark/0000-0003-1600-6856; Gibson,
Stephen/0000-0002-3767-6114; Heays, Alan/0000-0002-7716-9192
FU NASA; Australian Research Council [DP0558962, DP0773050, LX0882438]
FX This research was funded by NASA through the Cassini project. The
authors thank Hasso Niemann for his invaluable input on the work
involved. We also thank Pascal Pernot and two anonymous reviewers for
their valuable input during the review process. N2
cross-section calculations were supported by the Australian Research
Council, through grants DP0558962, DP0773050, and LX0882438.
NR 64
TC 24
Z9 24
U1 1
U2 25
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD OCT 12
PY 2012
VL 117
AR E10006
DI 10.1029/2012JE004139
PG 22
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 020SA
UT WOS:000309833000001
ER
PT J
AU Prettyman, TH
Mittlefehldt, DW
Yamashita, N
Lawrence, DJ
Beck, AW
Feldman, WC
McCoy, TJ
McSween, HY
Toplis, MJ
Titus, TN
Tricarico, P
Reedy, RC
Hendricks, JS
Forni, O
Le Corre, L
Li, JY
Mizzon, H
Reddy, V
Raymond, CA
Russell, CT
AF Prettyman, Thomas H.
Mittlefehldt, David W.
Yamashita, Naoyuki
Lawrence, David J.
Beck, Andrew W.
Feldman, William C.
McCoy, Timothy J.
McSween, Harry Y.
Toplis, Michael J.
Titus, Timothy N.
Tricarico, Pasquale
Reedy, Robert C.
Hendricks, John S.
Forni, Olivier
Le Corre, Lucille
Li, Jian-Yang
Mizzon, Hugau
Reddy, Vishnu
Raymond, Carol A.
Russell, Christopher T.
TI Elemental Mapping by Dawn Reveals Exogenic H in Vesta's Regolith
SO SCIENCE
LA English
DT Article
ID ASTEROID 4 VESTA; BASALTIC ACHONDRITE; GAMMA-RAY; MINERALOGY;
METEORITES; MISSION; WATER
AB Using Dawn's Gamma Ray and Neutron Detector, we tested models of Vesta's evolution based on studies of howardite, eucrite, and diogenite (HED) meteorites. Global Fe/O and Fe/Si ratios are consistent with HED compositions. Neutron measurements confirm that a thick, diogenitic lower crust is exposed in the Rheasilvia basin, which is consistent with global magmatic differentiation. Vesta's regolith contains substantial amounts of hydrogen. The highest hydrogen concentrations coincide with older, low-albedo regions near the equator, where water ice is unstable. The young, Rheasilvia basin contains the lowest concentrations. These observations are consistent with gradual accumulation of hydrogen by infall of carbonaceous chondrites-observed as clasts in some howardites-and subsequent removal or burial of this material by large impacts.
C1 [Prettyman, Thomas H.; Yamashita, Naoyuki; Feldman, William C.; Tricarico, Pasquale; Reedy, Robert C.; Li, Jian-Yang] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Mittlefehldt, David W.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
[Lawrence, David J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Beck, Andrew W.; McCoy, Timothy J.] Smithsonian Inst, Washington, DC 20560 USA.
[McSween, Harry Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Toplis, Michael J.; Forni, Olivier; Mizzon, Hugau] Univ Toulouse, CNRS, Inst Rech Astrophys & Planetol, Toulouse, France.
[Titus, Timothy N.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Hendricks, John S.] TechSource, Los Alamos, NM 87544 USA.
[Le Corre, Lucille; Reddy, Vishnu] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Reddy, Vishnu] Univ N Dakota, Dept Space Studies, Grand Forks, ND USA.
[Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Russell, Christopher T.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
RP Prettyman, TH (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA.
EM prettyman@psi.edu
RI Russell, Christopher/E-7745-2012; Lujan Center, LANL/G-4896-2012; Beck,
Andrew/J-7215-2015; Lawrence, David/E-7463-2015;
OI Russell, Christopher/0000-0003-1639-8298; Beck,
Andrew/0000-0003-4455-2299; Lawrence, David/0000-0002-7696-6667; Forni,
Olivier/0000-0001-6772-9689; Reedy, Robert/0000-0002-2189-1303; Reddy,
Vishnu/0000-0002-7743-3491; Prettyman, Thomas/0000-0003-0072-2831; Le
Corre, Lucille/0000-0003-0349-7932
FU Jet Propulsion Laboratory (JPL), California Institute of Technology;
NASA; NASA Dawn Participating Scientist Program; NASA Discovery Program
Office
FX We thank the Dawn team for spacecraft and instrument operations at
Vesta. Portions of this work were performed by the Planetary Science
Institute under contract with the Jet Propulsion Laboratory (JPL),
California Institute of Technology; by JPL under contract with NASA; and
by the NASA Dawn Participating Scientist Program. D. Bazell and P.
Peplowski of Johns Hopkins University Applied Physics Laboratory
assisted in fast-neutron data analysis. The Dawn mission is led by the
University of California, Los Angeles, and managed by JPL under the
auspices of the NASA Discovery Program Office. The Dawn data are
archived with the NASA Planetary Data System.
NR 36
TC 107
Z9 108
U1 7
U2 28
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 OCT 12
PY 2012
VL 338
IS 6104
BP 242
EP 246
DI 10.1126/science.1225354
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 019BQ
UT WOS:000309712300042
PM 22997135
ER
PT J
AU Denevi, BW
Blewett, DT
Buczkowski, DL
Capaccioni, F
Capria, MT
De Sanctis, MC
Garry, WB
Gaskell, RW
Le Corre, L
Li, JY
Marchi, S
McCoy, TJ
Nathues, A
O'Brien, DP
Petro, NE
Pieters, CM
Preusker, F
Raymond, CA
Reddy, V
Russell, CT
Schenk, P
Scully, JEC
Sunshine, JM
Tosi, F
Williams, DA
Wyrick, D
AF Denevi, B. W.
Blewett, D. T.
Buczkowski, D. L.
Capaccioni, F.
Capria, M. T.
De Sanctis, M. C.
Garry, W. B.
Gaskell, R. W.
Le Corre, L.
Li, J. -Y.
Marchi, S.
McCoy, T. J.
Nathues, A.
O'Brien, D. P.
Petro, N. E.
Pieters, C. M.
Preusker, F.
Raymond, C. A.
Reddy, V.
Russell, C. T.
Schenk, P.
Scully, J. E. C.
Sunshine, J. M.
Tosi, F.
Williams, D. A.
Wyrick, D.
TI Pitted Terrain on Vesta and Implications for the Presence of Volatiles
SO SCIENCE
LA English
DT Article
ID CARBONACEOUS CHONDRITES; ASTEROID 4-VESTA; CERES; DAWN; MARS
AB We investigated the origin of unusual pitted terrain on asteroid Vesta, revealed in images from the Dawn spacecraft. Pitted terrain is characterized by irregular rimless depressions found in and around several impact craters, with a distinct morphology not observed on other airless bodies. Similar terrain is associated with numerous martian craters, where pits are thought to form through degassing of volatile-bearing material heated by the impact. Pitted terrain on Vesta may have formed in a similar manner, which indicates that portions of the surface contain a relatively large volatile component. Exogenic materials, such as water-rich carbonaceous chondrites, may be the source of volatiles, suggesting that impactor materials are preserved locally in relatively high abundance on Vesta and that impactor composition has played an important role in shaping the asteroid's geology.
C1 [Denevi, B. W.; Blewett, D. T.; Buczkowski, D. L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Capaccioni, F.; Capria, M. T.; De Sanctis, M. C.; Tosi, F.] Ist Nazl Astrofis, Ist Astrofis & Planetol Spaziali, Rome, Italy.
[Garry, W. B.; Gaskell, R. W.; Li, J. -Y.; O'Brien, D. P.] Planetary Sci Inst, Tucson, AZ USA.
[Le Corre, L.; Nathues, A.; Reddy, V.] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany.
[Li, J. -Y.; Sunshine, J. M.] Univ Maryland, College Pk, MD 20742 USA.
[Marchi, S.] NASA, Lunar Sci Inst, Boulder, CO USA.
[McCoy, T. J.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Petro, N. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pieters, C. M.] Brown Univ, Providence, RI 02912 USA.
[Preusker, F.] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Planetary Res, Berlin, Germany.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Reddy, V.] Univ N Dakota, Grand Forks, ND 58201 USA.
[Russell, C. T.; Scully, J. E. C.] Univ Calif Los Angeles, Los Angeles, CA USA.
[Schenk, P.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Williams, D. A.] Arizona State Univ, Tempe, AZ USA.
[Wyrick, D.] SW Res Inst, San Antonio, TX USA.
RP Denevi, BW (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
EM brett.denevi@jhuapl.edu
RI Denevi, Brett/I-6502-2012; Russell, Christopher/E-7745-2012; Petro,
Noah/F-5340-2013; Garry, Brent/I-5920-2013; De Sanctis, Maria
Cristina/G-5232-2013; Blewett, David/I-4904-2012; Buczkowski,
Debra/I-7842-2015;
OI Capaccioni, Fabrizio/0000-0003-1631-4314; Le Corre,
Lucille/0000-0003-0349-7932; Tosi, Federico/0000-0003-4002-2434; Denevi,
Brett/0000-0001-7837-6663; Russell, Christopher/0000-0003-1639-8298; De
Sanctis, Maria Cristina/0000-0002-3463-4437; Blewett,
David/0000-0002-9241-6358; Buczkowski, Debra/0000-0002-4729-7804;
capria, maria teresa/0000-0002-9814-9588; Reddy,
Vishnu/0000-0002-7743-3491
FU Dawn at Vesta Participating Scientist program; NASA; Italian Space
Agency
FX We thank the Dawn Science, Instrument, and Operations Teams and the Dawn
at Vesta Participating Scientist program for support. A portion of this
work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA, and portions were
supported by the Italian Space Agency. Dawn data are archived with the
NASA Planetary Data System.
NR 28
TC 43
Z9 44
U1 2
U2 22
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 OCT 12
PY 2012
VL 338
IS 6104
BP 246
EP 249
DI 10.1126/science.1225374
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 019BQ
UT WOS:000309712300043
PM 22997131
ER
PT J
AU Mather, J
Mao, M
AF Mather, John
Mao, Minnie
TI ASTRONOMY A conversation about observation
SO NATURE
LA English
DT Editorial Material
C1 [Mao, Minnie] Natl Radio Astron Observ, Socorro, NM 87801 USA.
RP Mather, J (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 3
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD OCT 11
PY 2012
VL 490
IS 7419
BP S5
EP S7
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 019IY
UT WOS:000309733300003
PM 23051770
ER
PT J
AU Bolten, JD
Crow, WT
AF Bolten, J. D.
Crow, W. T.
TI Improved prediction of quasi-global vegetation conditions using
remotely-sensed surface soil moisture
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID AMSR-E; RETRIEVAL; MISSION; INDEXES
AB The added value of satellite-based surface soil moisture retrievals for agricultural drought monitoring is assessed by calculating the lagged rank correlation between remotely-sensed vegetation indices (VI) and soil moisture estimates obtained both before and after the assimilation of surface soil moisture retrievals derived from the Advanced Microwave Scanning Radiometer-EOS (AMSR-E) into a soil water balance model. Higher soil moisture/VI lag correlations imply an enhanced ability to predict future vegetation conditions using estimates of current soil moisture. Results demonstrate that the assimilation of AMSR-E surface soil moisture retrievals substantially improve the performance of a global drought monitoring system - particularly in sparsely-instrumented areas of the world where high-quality rainfall observations are unavailable. Citation: Bolten, J. D., and W. T. Crow (2012), Improved prediction of quasi-global vegetation conditions using remotely-sensed surface soil moisture, Geophys. Res. Lett., 39, L19406, doi: 10.1029/2012GL053470.
C1 [Bolten, J. D.] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20705 USA.
[Crow, W. T.] USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
RP Bolten, JD (reprint author), NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20705 USA.
EM john.bolten@nasa.gov
FU NASA Applied Sciences Program
FX Research was funded by a grant from the NASA Applied Sciences Program.
NR 24
TC 18
Z9 18
U1 1
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD OCT 11
PY 2012
VL 39
AR L19406
DI 10.1029/2012GL053470
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 020TK
UT WOS:000309837300005
ER
PT J
AU Wood, R
Leon, D
Lebsock, M
Snider, J
Clarke, AD
AF Wood, Robert
Leon, David
Lebsock, Matthew
Snider, Jefferson
Clarke, Antony D.
TI Precipitation driving of droplet concentration variability in marine low
clouds
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TOPPED BOUNDARY-LAYER; VOCALS-REX; STRATOCUMULUS CLOUDS; CONDENSATION
NUCLEI; SIZE DISTRIBUTION; WRF-CHEM; ATMOSPHERE; AEROSOLS; SATELLITE;
ENTRAINMENT
AB The concentration N-d of cloud droplets in marine low clouds is a primary determinant of their ability to reflect sunlight and modulates their ability to precipitate. Previous studies have focused upon aerosol source variability as the key driver of variability in N-d. Here, we use a highly simplified aerosol budget model to examine the impact of precipitation on N-d. This model considers: precipitation (coalescence) scavenging, constrained using new satellite measurements of light precipitation; entrainment of aerosol from above cloud combined with constant aerosol concentration based on recent field observations of aerosol particles in the free troposphere; and sea-surface aerosol production estimated using a wind speed dependent source function. Despite the highly simplified nature of this model, it skillfully predicts the geographical variability of N-d in regions of extensive marine low clouds. Inclusion of precipitation results in reduction in N-d by factors of 2-3 over the remote oceans. Within 500 km of coastlines the reduction in N-d due to precipitation is weak but in these regions the model is not able to accurately predict N-d because of strong pollution sources. In general, neither free-tropospheric nor surface CCN sources alone are sufficient to maintain N-d against precipitation losses. The results demonstrate that even the light precipitation rates typical of marine stratocumulus profoundly impact the radiative properties of marine low clouds.
C1 [Wood, Robert] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Leon, David; Snider, Jefferson] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA.
[Lebsock, Matthew] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Clarke, Antony D.] Univ Hawaii Manoa, Dept Oceanog, Honolulu, HI 96822 USA.
RP Wood, R (reprint author), Univ Washington, Dept Atmospher Sci, 408 ATG Bldg, Seattle, WA 98195 USA.
EM robwood@atmos.washington.edu
RI Wood, Robert/A-2989-2008; Snider, Jefferson/F-9175-2016
OI Wood, Robert/0000-0002-1401-3828; Snider, Jefferson/0000-0002-9318-1343
FU NASA Ocean Vector Winds Science Team; NASA [NNX10AN78G, NNX10AM29G]; NSF
[ATM-0745702, ATM-0745368, ATM-0745986]; National Aeronautics and Space
Administration
FX The authors would like to thank the staff and crew of the NSF/NCAR C-130
aircraft whose dedication resulted in the in situ observational VOCALS
Regional Experiment data set. The CloudSat data were distributed by the
CloudSat Data Processing Center at Colorado State University. MODIS data
were obtained from the NASA Goddard Land Processes data archive.
QuikScat data were produced by Remote Sensing Systems and sponsored by
the NASA Ocean Vector Winds Science Team. This work was supported by
NASA awards NNX10AN78G and NNX10AM29G and NSF awards ATM-0745702,
ATM-0745368 and ATM-0745986. Part of this research was carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with the National Aeronautics and Space Administration.
NR 64
TC 15
Z9 15
U1 2
U2 35
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 11
PY 2012
VL 117
AR D19210
DI 10.1029/2012JD018305
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 020RB
UT WOS:000309830000001
ER
PT J
AU Dotson, A
Georganopoulos, M
Kazanas, D
Perlman, ES
AF Dotson, Amanda
Georganopoulos, Markos
Kazanas, Demosthenes
Perlman, Eric S.
TI A METHOD FOR LOCALIZING ENERGY DISSIPATION IN BLAZARS USING FERMI
VARIABILITY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: active; gamma rays: galaxies; quasars: general; radiation
mechanisms: non-thermal
ID ACTIVE GALACTIC NUCLEI; SELF-COMPTON MODEL; HIGH-POWER BLAZARS;
BROAD-LINE REGION; GAMMA-RAY FLARE; DETECTED BLAZARS; RADIATION-FIELDS;
RADIO-SOURCES; HOT DUST; EMISSION
AB The distance of a Fermi-detected blazar gamma-ray emission site from a supermassive black hole is a matter of active debate. Here we present a method for testing if the GeV emission of powerful blazars is produced within the subparsec-scale broad-line region (BLR) or farther out in the parsec-scale molecular torus (MT) environment. If the GeV emission takes place within the BLR, the inverse Compton (IC) scattering of the BLR ultraviolet (UV) seed photons that produces the gamma-rays takes place at the onset of the Klein-Nishina regime. This causes the electron cooling time to become practically energy-independent and the variation of the gamma-ray emission to be almost achromatic. If, on the other hand, the gamma-ray emission is produced farther out in the parsec-scale MT, the IC scattering of the infrared (IR) MT seed photons that produces the gamma-rays takes place in the Thomson regime, resulting in energy-dependent electron cooling times, manifested as faster cooling times for higher Fermi energies. We demonstrate these characteristics and discuss the applicability and limitations of our method.
C1 [Dotson, Amanda; Georganopoulos, Markos] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Georganopoulos, Markos; Kazanas, Demosthenes] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Perlman, Eric S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
RP Dotson, A (reprint author), Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
EM adot1@umbc.edu
OI Perlman, Eric/0000-0002-3099-1664
FU NASA ATFP [NNX08AG77G]; Fermi grant [NNX12AF01G]; LTSA [NNX07AM17G]
FX We thank the referee, Luigi Foschini, for his thoughtful comments and
suggestions. We acknowledge support from NASA ATFP grant NNX08AG77G and
Fermi grant NNX12AF01G. E.P. and M.G. acknowledge support from LTSA
grant NNX07AM17G.
NR 46
TC 15
Z9 15
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 10
PY 2012
VL 758
IS 1
AR L15
DI 10.1088/2041-8205/758/1/L15
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016TK
UT WOS:000309542200015
ER
PT J
AU Hashimoto, J
Dong, R
Kudo, T
Honda, M
McClure, MK
Zhu, Z
Muto, T
Wisniewski, J
Abe, L
Brandner, W
Brandt, T
Carson, J
Egner, S
Feldt, M
Fukagawa, M
Goto, M
Grady, CA
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, S
Henning, T
Hodapp, K
Ishii, M
Iye, M
Janson, M
Kandori, R
Knapp, G
Kusakabe, N
Kuzuhara, M
Kwon, J
Matsuo, T
Mayama, S
McElwain, MW
Miyama, S
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, S
Serabyn, G
Suenaga, T
Suto, H
Suzuki, R
Takahashi, Y
Takami, M
Takato, N
Terada, H
Thalmann, C
Tomono, D
Turner, EL
Watanabe, M
Yamada, T
Takami, H
Usuda, T
Tamura, M
AF Hashimoto, J.
Dong, R.
Kudo, T.
Honda, M.
McClure, M. K.
Zhu, Z.
Muto, T.
Wisniewski, J.
Abe, L.
Brandner, W.
Brandt, T.
Carson, J.
Egner, S.
Feldt, M.
Fukagawa, M.
Goto, M.
Grady, C. A.
Guyon, O.
Hayano, Y.
Hayashi, M.
Hayashi, S.
Henning, T.
Hodapp, K.
Ishii, M.
Iye, M.
Janson, M.
Kandori, R.
Knapp, G.
Kusakabe, N.
Kuzuhara, M.
Kwon, J.
Matsuo, T.
Mayama, S.
McElwain, M. W.
Miyama, S.
Morino, J. -I.
Moro-Martin, A.
Nishimura, T.
Pyo, S.
Serabyn, G.
Suenaga, T.
Suto, H.
Suzuki, R.
Takahashi, Y.
Takami, M.
Takato, N.
Terada, H.
Thalmann, C.
Tomono, D.
Turner, E. L.
Watanabe, M.
Yamada, T.
Takami, H.
Usuda, T.
Tamura, M.
TI POLARIMETRIC IMAGING OF LARGE CAVITY STRUCTURES IN THE PRE-TRANSITIONAL
PROTOPLANETARY DISK AROUND PDS 70: OBSERVATIONS OF THE DISK
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planetary systems; polarization; protoplanetary disks; stars: individual
(PDS 70); stars: pre-main sequence
ID T-TAURI STARS; EVOLUTIONARY MODELS; TRANSITIONAL DISK; PLANET FORMATION;
DUST; GAP; IMAGES; LIGHT; LKCA-15; CATALOG
AB We present high-resolution H-band polarized intensity (FWHM = 0.'' 1:14 AU) and L'-band imaging data (FWHM = 0.'' 11:15 AU) of the circumstellar disk around the weak-lined T Tauri star PDS 70 in Centaurus at a radial distance of 28 AU (0.'' 2) up to 210 AU (1.'' 5). In both images, a giant inner gap is clearly resolved for the first time, and the radius of the gap is similar to 70 AU. Our data show that the geometric center of the disk shifts by similar to 6 AU toward the minor axis. We confirm that the brown dwarf companion candidate to the north of PDS 70 is a background star based on its proper motion. As a result of spectral energy distribution fitting by Monte Carlo radiative transfer modeling, we infer the existence of an optically thick inner disk at a few AU. Combining our observations and modeling, we classify the disk of PDS 70 as a pre-transitional disk. Furthermore, based on the analysis of L'-band imaging data, we put an upper limit of similar to 30 to similar to 50 M-J on the mass of companions within the gap. Taking into account the presence of the large and sharp gap, we suggest that the gap could be formed by dynamical interactions of sub-stellar companions or multiple unseen giant planets in the gap.
C1 [Hashimoto, J.; Hayashi, M.; Iye, M.; Kandori, R.; Kusakabe, N.; Kuzuhara, M.; Kwon, J.; Morino, J. -I.; Suenaga, T.; Suto, H.; Suzuki, R.; Takahashi, Y.; Tamura, M.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Dong, R.; Zhu, Z.; Brandt, T.; Janson, M.; Knapp, G.; Moro-Martin, A.; Turner, E. L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Kudo, T.; Egner, S.; Guyon, O.; Hayano, Y.; Hayashi, S.; Ishii, M.; Nishimura, T.; Pyo, 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.
[Honda, M.] Kanagawa Univ, Hiratsuka, Kanagawa 2591293, Japan.
[McClure, M. K.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Muto, T.] Kogakuin Univ, Div Liberal Arts, Shinjuku Ku, Tokyo 1638677, Japan.
[Wisniewski, J.] Univ Washington, Seattle, WA 98195 USA.
[Wisniewski, J.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Abe, L.] Univ Nice Sophia Antipolis, Lab Hippolyte Fizeau, UMR6525, F-06108 Nice 02, France.
[Brandner, W.; Carson, J.; Feldt, M.; Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Carson, J.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Fukagawa, M.] Osaka Univ, Toyonaka, Osaka 5600043, Japan.
[Goto, M.] Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Grady, C. A.; McElwain, M. W.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Grady, C. A.] Eureka Sci, Oakland, CA 96002 USA.
[Hodapp, K.] Univ Hawaii, Hilo, HI 96720 USA.
[Kuzuhara, M.] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan.
[Kwon, J.; Suenaga, T.] Grad Univ Adv Studies Sokendai, Dept Astron Sci, Tokyo 1818588, Japan.
[Matsuo, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Mayama, S.] Grad Univ Adv Studies, Hayama, Kanagawa 2400193, Japan.
[Miyama, S.] Hiroshima Univ, Higashihiroshima 7398511, Japan.
[Moro-Martin, A.] CAB CSIC INTA, Dept Astrophys, E-28850 Madrid, Spain.
[Serabyn, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Takahashi, Y.] Univ Tokyo, Dept Astron, Tokyo 1130033, Japan.
[Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Thalmann, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Turner, E. L.] Univ Tokyo, Kavli 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 Hashimoto, J (reprint author), Natl Inst Nat Sci, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
EM jun.hashimoto@nao.ac.jp
RI Turner, Edwin/A-4295-2011; MIYAMA, Shoken/A-3598-2015;
OI McClure, Melissa/0000-0003-1878-327X
FU MEXT; Mitsubishi Foundation; U.S. National Science Foundation [1009203,
1009314]
FX We are grateful to an anonymous referee for providing many useful
comments leading to an improved version of this Letter. We appreciate
support from the Subaru Telescope and the Gemini South Telescope staff,
especially from Jennie Berghuis and Dr. Tom Hayward. This work is partly
supported by a Grant-in-Aid for Science Research in a Priority Area from
MEXT, by the Mitsubishi Foundation, and by the U.S. National Science
Foundation under Award Nos. 1009203 and 1009314.
NR 46
TC 54
Z9 54
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 10
PY 2012
VL 758
IS 1
AR L19
DI 10.1088/2041-8205/758/1/L19
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016TK
UT WOS:000309542200019
ER
PT J
AU Helgason, K
Kashlinsky, A
AF Helgason, Kari
Kashlinsky, Alexander
TI RECONSTRUCTING THE gamma-RAY PHOTON OPTICAL DEPTH OF THE UNIVERSE TO z
similar to 4 FROM MULTIWAVELENGTH GALAXY SURVEY DATA
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmic background radiation; galaxies: evolution; gamma rays: general
ID EXTRAGALACTIC BACKGROUND LIGHT; STAR-FORMATION RATE;
SPITZER-SPACE-TELESCOPE; ULTRAVIOLET LUMINOSITY DENSITY; POPULATION-III
STARS; SOURCE COUNTS; DEPENDENT EVOLUTION; NUMBER COUNTS; HIGH-REDSHIFT;
DEEP
AB We reconstruct the gamma-ray opacity of the universe out to z less than or similar to 3-4 using an extensive library of 342 observed galaxy luminosity function (LF) surveys extending to high redshifts. We cover the whole range from UV to mid-IR (0.15-25 mu m) providing for the first time a robust empirical calculation of the gamma gamma optical depth out to several TeV. Here, we use the same database as Helgason et al. where the extragalactic background light was reconstructed from LFs out to 4.5 mu m and was shown to recover observed galaxy counts to high accuracy. We extend our earlier library of LFs to 25 mu m such that it covers the energy range of pair production with gamma-rays (1) in the entire Fermi/LAT energy range, and (2) at higher TeV energies probed by ground-based Cherenkov telescopes. In the absence of significant contributions to the cosmic diffuse background from unknown populations, such as the putative Population III era sources, the universe appears to be largely transparent to gamma-rays at all Fermi/LAT energies out to z similar to 2 whereas it becomes opaque to TeV photons already at z less than or similar to 0.2 and reaching tau similar to 10 at z = 1. Comparing with the currently available Fermi/LAT gamma-ray burst and blazar data shows that there is room for significant emissions originating in the first stars era.
C1 [Helgason, Kari] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Helgason, Kari; Kashlinsky, Alexander] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kashlinsky, Alexander] SSAI, Lanham, MD 20706 USA.
RP Helgason, K (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM kari@astro.umd.edu; alexander.kashlinsky@nasa.gov
FU NASA [NNX11AO05H]; Leifur Eiriksson Foundation
FX Our reconstructed EBL and optical depths are available upon request.
This work was supported by NASA Headquarters under the NASA Earth and
Space Sciences Fellowship Program-Grant NNX11AO05H. K.H. is also
grateful to The Leifur Eiriksson Foundation for its support. We thank W.
McConville, B. Magnelli, and M. Ricotti for useful communications.
NR 46
TC 13
Z9 13
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 10
PY 2012
VL 758
IS 1
AR L13
DI 10.1088/2041-8205/758/1/L13
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016TK
UT WOS:000309542200013
ER
PT J
AU Rappazzo, AF
Matthaeus, WH
Ruffolo, D
Servidio, S
Velli, M
AF Rappazzo, A. F.
Matthaeus, W. H.
Ruffolo, D.
Servidio, S.
Velli, M.
TI INTERCHANGE RECONNECTION IN A TURBULENT CORONA
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE magnetic reconnection; magnetohydrodynamics (MHD); solar wind; Sun:
corona; Sun: magnetic topology; turbulence
ID SLOW SOLAR-WIND; DEPENDENT BOUNDARY-CONDITIONS; OPEN MAGNETIC-FIELD;
DIFFERENTIAL ROTATION; HYPERBOLIC SYSTEMS; ACTIVE-REGION; DYNAMICS;
SHEET; HOLES; LINES
AB Magnetic reconnection at the interface between coronal holes and loops, the so-called interchange reconnection, can release the hotter, denser plasma from magnetically confined regions into the heliosphere, contributing to the formation of the highly variable slow solar wind. The interchange process is often thought to develop at the apex of streamers or pseudo-streamers, near Y - and X-type neutral points, but slow streams with loop composition have been recently observed along fanlike open field lines adjacent to closed regions, far from the apex. However, coronal heating models, with magnetic field lines shuffled by convective motions, show that reconnection can occur continuously in unipolar magnetic field regions with no neutral points: photospheric motions induce a magnetohydrodynamic turbulent cascade in the coronal field that creates the necessary small scales, where a sheared magnetic field component orthogonal to the strong axial field is created locally and can reconnect. We propose that a similar mechanism operates near and around boundaries between open and closed regions inducing a continual stochastic rearrangement of connectivity. We examine a reduced magnetohydrodynamic model of a simplified interface region between open and closed corona threaded by a strong unipolar magnetic field. This boundary is not stationary, becomes fractal, and field lines change connectivity continuously, becoming alternatively open and closed. This model suggests that slow wind may originate everywhere along loop-coronal-hole boundary regions and can account naturally and simply for outflows at and adjacent to such boundaries and for the observed diffusion of slow wind around the heliospheric current sheet.
C1 [Rappazzo, A. F.; Matthaeus, W. H.] Univ Delaware, Bartol Res Inst, Dept Phys & Astron, Newark, DE 19716 USA.
[Ruffolo, D.] Mahidol Univ, Dept Phys, Fac Sci, Bangkok 10400, Thailand.
[Ruffolo, D.] Minist Educ, CHE, Thailand Ctr Excellence Phys, Bangkok 10400, Thailand.
[Servidio, S.] Univ Calabria, Dipartimento Fis, I-87036 Cosenza, Italy.
[Velli, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Rappazzo, AF (reprint author), Univ Delaware, Bartol Res Inst, Dept Phys & Astron, Newark, DE 19716 USA.
EM rappazzo@udel.edu
OI Servidio, Sergio/0000-0001-8184-2151
FU NASA Heliophysics Theory program [NNX11AJ44G, 12-3188]; NSF Solar
Terrestrial and SHINE programs [AGS-1063439, AGS-1156094]; NASA MMS,
Solar probe Plus Projects; Thailand Research Fund, POR Calabria
[FSE-2007/2013]; EU
FX This research is supported in part by NASA Heliophysics Theory program
NNX11AJ44G, NSF Solar Terrestrial and SHINE programs AGS-1063439 and
AGS-1156094, NASA MMS, Solar probe Plus Projects, the Thailand Research
Fund, POR Calabria FSE-2007/2013, and by EU project "Turboplasmas." This
work is carried out in part at the Jet Propulsion Laboratory under a
contract with NASA. Simulations performed through the NASA Advanced
Supercomputing SMD award 12-3188.
NR 49
TC 15
Z9 15
U1 2
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 10
PY 2012
VL 758
IS 1
AR L14
DI 10.1088/2041-8205/758/1/L14
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016TK
UT WOS:000309542200014
ER
PT J
AU Yusef-Zadeh, F
Arendt, R
Bushouse, H
Cotton, W
Haggard, D
Pound, MW
Roberts, DA
Royster, M
Wardle, M
AF Yusef-Zadeh, F.
Arendt, R.
Bushouse, H.
Cotton, W.
Haggard, D.
Pound, M. W.
Roberts, D. A.
Royster, M.
Wardle, M.
TI A 3 pc SCALE JET-DRIVEN OUTFLOW FROM SGRA
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion; accretion disks; black hole physics; Galaxy: center
ID SAGITTARIUS-A-ASTERISK; GALACTIC-CENTER; CENTRAL PARSEC; IONIZED-GAS;
PROPER MOTION; GALAXY; RADIO; ACCRETION; EMISSION; DYNAMICS
AB The compact radio source Sgr A* is coincident with a 4 x 10(6) M-circle dot black hole at the dynamical center of the Galaxy and is surrounded by dense orbiting ionized and molecular gas. We present high-resolution radio continuum images of the central 3' and report a faint continuous linear structure centered on Sgr A* with a P.A. similar to 60 degrees. The extension of this feature appears to be terminated symmetrically by two linearly polarized structures at 8.4 GHz, similar to 75 '' from Sgr A*. A number of weak blobs of radio emission with X-ray counterparts are detected along the axis of the linear structure. The linear structure is best characterized by a mildly relativistic jet from Sgr A* with an outflow rate 10(-6) M-circle dot yr(-1). The near and far sides of the jet are interacting with orbiting ionized and molecular gas over the last 1-3 hundred years and are responsible for a 2 '' hole, the "minicavity," characterized by disturbed kinematics, enhanced Fe II/III line emission, and diffuse X-ray gas. The estimated kinetic luminosity of the outflow is similar to 1.2 x 10(41) erg s(-1), so the interaction with the bar may be responsible for the Galactic center X-ray flash inferred to be responsible for much of the fluorescent Fe K alpha line emission from the inner 100 pc of the Galaxy.
C1 [Yusef-Zadeh, F.; Haggard, D.; Roberts, D. A.; Royster, M.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
[Arendt, R.] NASA, CRESST, UMBC, GSFC, Greenbelt, MD 20771 USA.
[Bushouse, H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Cotton, W.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Pound, M. W.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Wardle, M.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia.
RP Yusef-Zadeh, F (reprint author), Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
OI Wardle, Mark/0000-0002-1737-0871; Arendt, Richard/0000-0001-8403-8548
FU NSF [AST-0807400]; Australian Research Council [DP0986386]; CARMA
partner universities
FX This work is partially supported by the grant AST-0807400 from the NSF
and DP0986386 from the Australian Research Council. Ongoing CARMA
development and operations are supported by the National Science
Foundation under a cooperative agreement, and by the CARMA partner
universities.
NR 28
TC 18
Z9 18
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 10
PY 2012
VL 758
IS 1
AR L11
DI 10.1088/2041-8205/758/1/L11
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016TK
UT WOS:000309542200011
ER
PT J
AU A'Hearn, MF
Feaga, LM
Keller, HU
Kawakita, H
Hampton, DL
Kissel, J
Klaasen, KP
McFadden, LA
Meech, KJ
Schultz, PH
Sunshine, JM
Thomas, PC
Veverka, J
Yeomans, DK
Besse, S
Bodewits, D
Farnham, TL
Groussin, O
Kelley, MS
Lisse, CM
Merlin, F
Protopapa, S
Wellnitz, DD
AF A'Hearn, Michael F.
Feaga, Lori M.
Keller, H. Uwe
Kawakita, Hideyo
Hampton, Donald L.
Kissel, Jochen
Klaasen, Kenneth P.
McFadden, Lucy A.
Meech, Karen J.
Schultz, Peter H.
Sunshine, Jessica M.
Thomas, Peter C.
Veverka, Joseph
Yeomans, Donald K.
Besse, Sebastien
Bodewits, Dennis
Farnham, Tony L.
Groussin, Olivier
Kelley, Michael S.
Lisse, Carey M.
Merlin, Frederic
Protopapa, Silvia
Wellnitz, Dennis D.
TI COMETARY VOLATILES AND THE ORIGIN OF COMETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets: general; Oort cloud; protoplanetary disks
ID C/1996 B2 HYAKUTAKE; C/2009 P1 GARRADD; O1 HALE-BOPP; CARBON-MONOXIDE;
CHEMICAL-COMPOSITION; SPECTROSCOPIC OBSERVATIONS; ORGANIC COMPOSITION;
RADIO TELESCOPES; 103P/HARTLEY 2; SOLAR NEBULA
AB We describe recent results on the CO/CO2/H2O composition of comets together with a survey of older literature (primarily for CO/H2O) and compare these with models of the protoplanetary disk. Even with the currently small sample, there is a wide dispersion in abundance ratios and little if any systematic difference between Jupiter-family comets (JFCs) and long-period and Halley-type comets (LPCs and HTCs). We argue that the cometary observations require reactions on grain surfaces to convert CO to CO2 and also require formation of all types of comets in largely, but not entirely, overlapping regions, probably between the CO and CO2 snow lines. Any difference in the regions of formation is in the opposite direction from the classical picture with the JFCs having formed closer to the Sun than the LPCs. In the classical picture, the LPCs formed in the region of the giant planets and the JFCs formed in the Kuiper Belt. However, these data suggest, consistent with suggestions on dynamical grounds, that the JFCs and LPCs formed in largely overlapping regions where the giant planets are today and with JFCs on average forming slightly closer to the Sun than did the LPCs. Presumably at least the JFCs passed through the scattered disk on their way to their present dynamical family.
C1 [A'Hearn, Michael F.; Feaga, Lori M.; Sunshine, Jessica M.; Besse, Sebastien; Bodewits, Dennis; Farnham, Tony L.; Kelley, Michael S.; Protopapa, Silvia; Wellnitz, Dennis D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Keller, H. Uwe] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany.
[Kawakita, Hideyo] Kyoto Sangyo Univ, Dept Phys, Kamigamo JP Kita Ku, Kyoto 6038555, Japan.
[Hampton, Donald L.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA.
[Kissel, Jochen] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Klaasen, Kenneth P.; Yeomans, Donald K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[McFadden, Lucy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Meech, Karen J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Schultz, Peter H.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Thomas, Peter C.; Veverka, Joseph] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Groussin, Olivier] Univ Aix Marseille, Astrophys Lab, F-13388 Marseille 13, France.
[Groussin, Olivier] CNRS, UMR7326, F-13388 Marseille 13, France.
[Lisse, Carey M.] JHU APL, Dept Space, Laurel, MD 20723 USA.
[Merlin, Frederic] Univ Paris 07, Observ Paris, LESIA, F-92195 Meudon, France.
RP A'Hearn, MF (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM ma@astro.umd.edu
RI McFadden, Lucy-Ann/I-4902-2013; Lisse, Carey/B-7772-2016;
OI McFadden, Lucy-Ann/0000-0002-0537-9975; Lisse,
Carey/0000-0002-9548-1526; Kelley, Michael/0000-0002-6702-7676;
Bodewits, Dennis/0000-0002-2668-7248; Besse,
Sebastien/0000-0002-1052-5439
FU NASA [NNM07AA99 C, NMO711002]
FX This work benefited significantly from discussions with numerous
colleagues, including alphabetically Chas Beichman, Sally
Dodson-Robinson, Paul Feldman, Hal Levison, Hans Rickman, Kevin Walsh,
and an anonymous referee. This work was funded by NASA, through the
Discovery Program, via contract NNM07AA99 C to the University of
Maryland and task order NMO711002 to the Jet Propulsion Laboratory. The
Jet Propulsion Laboratory is operated by the California Institute of
Technology.
NR 51
TC 42
Z9 42
U1 0
U2 20
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2012
VL 758
IS 1
AR 29
DI 10.1088/0004-637X/758/1/29
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016LS
UT WOS:000309520500029
ER
PT J
AU Bauer, JM
Kramer, E
Mainzer, AK
Stevenson, R
Grav, T
Masiero, JR
Walker, RG
Fernandez, YR
Meech, KJ
Lisse, CM
Weissman, PR
Cutri, RM
Dailey, JW
Masci, FJ
Tholen, DJ
Pearman, G
Wright, EL
AF Bauer, James M.
Kramer, Emily
Mainzer, A. K.
Stevenson, Rachel
Grav, Tommy
Masiero, Joseph R.
Walker, Russell G.
Fernandez, Yan R.
Meech, Karen J.
Lisse, Carey M.
Weissman, Paul R.
Cutri, Roc M.
Dailey, John W.
Masci, Frank J.
Tholen, David J.
Pearman, George
Wright, Edward L.
CA WISE Team
TI WISE/NEOWISE PRELIMINARY ANALYSIS AND HIGHLIGHTS OF THE
67P/CHURYUMOV-GERASIMENKO NEAR NUCLEUS ENVIRONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets: individual (67P)
ID SPACE-TELESCOPE OBSERVATIONS; THERMAL-MODEL CALIBRATION;
INFRARED-SURVEY-EXPLORER; NEAR-EARTH ASTEROIDS; COMET 103P/HARTLEY 2;
DUST TRAIL; PHYSICAL-PROPERTIES; SOLAR-SYSTEM; 2P/ENCKE
AB On 2010 January 18-19 and June 28-29, the Wide-field Infrared Survey Explorer (WISE) spacecraft imaged the Rosetta mission target, comet 67P/Churyumov-Gerasimenko. We present a preliminary analysis of the images, which provide a characterization of the dust environment at heliocentric distances similar to those planned for the initial spacecraft encounter, but on the outbound leg of its orbit rather than the inbound. Broadband photometry yields low levels of CO2 production at a comet heliocentric distance of 3.32 AU and no detectable production at 4.18 AU. We find that at these heliocentric distances, large dust grains with mean grain diameters on the order of a millimeter or greater dominate the coma and evolve to populate the tail. This is further supported by broadband photometry centered on the nucleus, which yield an estimated differential dust particle size distribution with a power-law relation that is considerably shallower than average. We set a 3 sigma upper limit constraint on the albedo of the large-grain dust at <= 0.12. Our best estimate of the nucleus radius (1.82 +/- 0.20 km) and albedo (0.04 +/- 0.01) are in agreement with measurements previously reported in the literature.
C1 [Bauer, James M.; Kramer, Emily; Mainzer, A. K.; Stevenson, Rachel; Masiero, Joseph R.; Weissman, Paul R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bauer, James M.; Cutri, Roc M.; Dailey, John W.; Masci, Frank J.; Pearman, George] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Kramer, Emily; Fernandez, Yan R.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA.
[Grav, Tommy] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Walker, Russell G.] Monterey Inst Res Astron, Marina, CA 93933 USA.
[Meech, Karen J.] Univ Hawaii, Inst Astron, Manoa, HI 96822 USA.
[Meech, Karen J.; Tholen, David J.] Univ Hawaii, NASA, Astrobiol Inst, Manoa, HI 96822 USA.
[Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Wright, Edward L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Bauer, JM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-401, Pasadena, CA 91109 USA.
EM bauer@scn.jpl.nasa.gov
RI Lisse, Carey/B-7772-2016;
OI Lisse, Carey/0000-0002-9548-1526; Masiero, Joseph/0000-0003-2638-720X;
Fernandez, Yanga/0000-0003-1156-9721
FU National Aeronautics and Space Administration; Planetary Science
Division of NASA; NASA through NASA Astrobiology Institute issued
through Office of Space Science [NNA09DA77A]; NASA Postdoctoral Program;
JPL graduate internship program
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 JPL/Caltech, funded by the Planetary
Science Division of NASA. This material is based in part upon work
supported by the NASA through the NASA Astrobiology Institute under
Cooperative Agreement No. NNA09DA77A issued through the Office of Space
Science. R. Stevenson is supported by the NASA Postdoctoral Program, and
E. Kramer acknowledges her support through the JPL graduate internship
program.
NR 39
TC 11
Z9 11
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2012
VL 758
IS 1
AR 18
DI 10.1088/0004-637X/758/1/18
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016LS
UT WOS:000309520500018
ER
PT J
AU Bradshaw, SJ
Klimchuk, JA
Reep, JW
AF Bradshaw, S. J.
Klimchuk, J. A.
Reep, J. W.
TI DIAGNOSING THE TIME-DEPENDENCE OF ACTIVE REGION CORE HEATING FROM THE
EMISSION MEASURE. I. LOW-FREQUENCY NANOFLARES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona
ID EXTREME-ULTRAVIOLET OBSERVATIONS; CORONAL LOOPS; SOLAR CORONA; MEASURE
DISTRIBUTIONS; ATOMIC DATABASE; PLASMA; DYNAMICS; ENERGY; IONIZATION;
SPECTRUM
AB Observational measurements of active region emission measures contain clues to the time dependence of the underlying heating mechanism. A strongly nonlinear scaling of the emission measure with temperature indicates a large amount of hot plasma relative to warm plasma. A weakly nonlinear (or linear) scaling of the emission measure indicates a relatively large amount of warm plasma, suggesting that the hot active region plasma is allowed to cool and so the heating is impulsive with a long repeat time. This case is called low-frequency nanoflare heating, and we investigate its feasibility as an active region heating scenario here. We explore a parameter space of heating and coronal loop properties with a hydrodynamic model. For each model run, we calculate the slope alpha of the emission measure distribution EM(T) alpha T-alpha . Our conclusions are: (1) low-frequency nanoflare heating is consistent with about 36% of observed active region cores when uncertainties in the atomic data are not accounted for; (2) proper consideration of uncertainties yields a range in which as many as 77% of observed active regions are consistent with low-frequency nanoflare heating and as few as zero; (3) low-frequency nanoflare heating cannot explain observed slopes greater than 3; (4) the upper limit to the volumetric energy release is in the region of 50 erg cm(-3) to avoid unphysical magnetic field strengths; (5) the heating timescale may be short for loops of total length less than 40 Mm to be consistent with the observed range of slopes; (6) predicted slopes are consistently steeper for longer loops.
C1 [Bradshaw, S. J.; Reep, J. W.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.
[Klimchuk, J. A.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
RP Bradshaw, SJ (reprint author), Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.
EM stephen.bradshaw@rice.edu; james.a.klimchuk@nasa.gov;
jeffrey.reep@rice.edu
OI Reep, Jeffrey/0000-0003-4739-1152
FU NASA
FX S.J.B. and J.A.K. acknowledge support for this work by the NASA SR&T
program. We thank the International Space Science Institute (ISSI) for
hosting the International Team led by S.J.B. and Helen Mason, and the
team members for the fruitful discussions that took place during the
meeting held there in 2012 February. We also thank the referee for their
comments and suggestions.
NR 37
TC 32
Z9 32
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2012
VL 758
IS 1
AR 53
DI 10.1088/0004-637X/758/1/53
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016LS
UT WOS:000309520500053
ER
PT J
AU Cargill, PJ
Bradshaw, SJ
Klimchuk, JA
AF Cargill, P. J.
Bradshaw, S. J.
Klimchuk, J. A.
TI ENTHALPY-BASED THERMAL EVOLUTION OF LOOPS. III. COMPARISON OF
ZERO-DIMENSIONAL MODELS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: transition region
ID CLOSED CORONAL STRUCTURES; ACTIVE-REGION CORE; TRANSITION REGION;
FLARING LOOPS; SOLAR-FLARES; PLASMA; HYDRODYNAMICS; TEMPERATURE;
EVAPORATION; STABILITY
AB Zero-dimensional (0D) hydrodynamic models provide a simple and quick way to study the thermal evolution of coronal loops subjected to time-dependent heating. This paper presents a comparison of a number of 0D models that have been published in the past and is intended to provide a guide for those interested in either using the old models or developing new ones. The principal difference between the models is the way the exchange of mass and energy between corona, transition region, and chromosphere is treated, as plasma cycles into and out of a loop during a heating-cooling cycle. It is shown that models based on the principles of mass and energy conservation can give satisfactory results at some or, in the case of the Enthalpy-based Thermal Evolution of Loops model, all stages of the loop evolution. Empirical models can have significant difficulties in obtaining accurate behavior due to invocation of assumptions incompatible with the correct exchange of mass and energy between corona, transition region, and chromosphere.
C1 [Cargill, P. J.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BW, England.
[Cargill, P. J.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland.
[Bradshaw, S. J.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.
[Klimchuk, J. A.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
RP Cargill, PJ (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BW, England.
FU NASA; International Space Science Institute (ISSI)
FX J.A.K. and S.J.B acknowledge support from the NASA SR&T program. We are
grateful to the International Space Science Institute (ISSI) for
supporting our team, and to Helen Mason for acting as co-leader of this
team with S.J.B.
NR 41
TC 21
Z9 21
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2012
VL 758
IS 1
AR 5
DI 10.1088/0004-637X/758/1/5
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016LS
UT WOS:000309520500005
ER
PT J
AU Freedman, WL
Madore, BF
Scowcroft, V
Burns, C
Monson, A
Persson, SE
Seibert, M
Rigby, J
AF Freedman, Wendy L.
Madore, Barry F.
Scowcroft, Victoria
Burns, Chris
Monson, Andy
Persson, S. Eric
Seibert, Mark
Rigby, Jane
TI CARNEGIE HUBBLE PROGRAM: A MID-INFRARED CALIBRATION OF THE HUBBLE
CONSTANT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmological parameters; cosmology: observations; distance scale;
galaxies: distances and redshifts; stars: variables: Cepheids
ID OBSERVATIONS COSMOLOGICAL INTERPRETATION; PERIOD-LUMINOSITY RELATIONS;
SPITZER-SPACE-TELESCOPE; LARGE-MAGELLANIC-CLOUD; LIGHT CURVES; DARK
ENERGY; IA SUPERNOVAE; CONSTRAINTS; PARALLAXES; PARAMETERS
AB Using a mid-infrared calibration of the Cepheid distance scale based on recent observations at 3.6 mu m with the Spitzer Space Telescope, we have obtained a new, high-accuracy calibration of the Hubble constant. We have established the mid-IR zero point of the Leavitt law (the Cepheid period-luminosity relation) using time-averaged 3.6 mu m data for 10 high-metallicity, Milky Way Cepheids having independently measured trigonometric parallaxes. We have adopted the slope of the PL relation using time-averaged 3.6 mu m data for 80 long-period Large Magellanic Cloud (LMC) Cepheids falling in the period range 0.8 < log(P) < 1.8. We find a new reddening-corrected distance to the LMC of 18.477 +/- 0.033 (systematic) mag. We re-examine the systematic uncertainties in H-0, also taking into account new data over the past decade. In combination with the new Spitzer calibration, the systematic uncertainty in H-0 over that obtained by the Hubble Space Telescope Key Project has decreased by over a factor of three. Applying the Spitzer calibration to the Key Project sample, we find a value of H-0 = 74.3 with a systematic uncertainty of +/- 2.1 (systematic) km s(-1) Mpc(-1), corresponding to a 2.8% systematic uncertainty in the Hubble constant. This result, in combination with WMAP7 measurements of the cosmic microwave background anisotropies and assuming a flat universe, yields a value of the equation of state for dark energy, w(0) = -1.09 +/- 0.10. Alternatively, relaxing the constraints on flatness and the numbers of relativistic species, and combining our results with those of WMAP7, Type Ia supernovae and baryon acoustic oscillations yield w(0) = -1.08 +/- 0.10 and a value of N-eff = 4.13 +/- 0.67, mildly consistent with the existence of a fourth neutrino species.
C1 [Freedman, Wendy L.; Madore, Barry F.; Scowcroft, Victoria; Burns, Chris; Monson, Andy; Persson, S. Eric; Seibert, Mark] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Rigby, Jane] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Freedman, WL (reprint author), Observ Carnegie Inst Washington, 813 Santa Barbara St, Pasadena, CA 91101 USA.
EM wendy@obs.carnegiescience.edu; barry@obs.carnegiescience.edu;
vs@obs.carnegiescience.edu; cburns@obs.carnegiescience.edu;
amonson@obs.carnegiescience.edu; persson@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 NASA through JPL/Caltech; Ahmanson Foundation
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. We thank the staff of the Spitzer Science Center for the
rapid processing of the data that went into this and other papers in the
series. Computing resources used for this work were made possible by a
grant from the Ahmanson Foundation. This research made use of the
NASA/IPAC Extragalactic Database (NED).
NR 41
TC 180
Z9 181
U1 1
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2012
VL 758
IS 1
AR 24
DI 10.1088/0004-637X/758/1/24
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016LS
UT WOS:000309520500024
ER
PT J
AU High, FW
Hoekstra, H
Leethochawalit, N
de Haan, T
Abramson, L
Aird, KA
Armstrong, R
Ashby, MLN
Bautz, M
Bayliss, M
Bazin, G
Benson, BA
Bleem, LE
Brodwin, M
Carlstrom, JE
Chang, CL
Cho, HM
Clocchiatti, A
Conroy, M
Crawford, TM
Crites, AT
Desai, S
Dobbs, MA
Dudley, JP
Foley, RJ
Forman, WR
George, EM
Gladders, MD
Gonzalez, AH
Halverson, NW
Harrington, NL
Holder, GP
Holzapfel, WL
Hoover, S
Hrubes, JD
Jones, C
Joy, M
Keisler, R
Knox, L
Lee, AT
Leitch, EM
Liu, J
Lueker, M
Luong-Van, D
Mantz, A
Marrone, DP
McDonald, M
McMahon, JJ
Mehl, J
Meyer, SS
Mocanu, L
Mohr, JJ
Montroy, TE
Murray, SS
Natoli, T
Nurgaliev, D
Padin, S
Plagge, T
Pryke, C
Reichardt, CL
Rest, A
Ruel, J
Ruhl, JE
Saliwanchik, BR
Saro, A
Sayre, JT
Schaffer, KK
Shaw, L
Schrabback, T
Shirokoff, E
Song, J
Spieler, HG
Stalder, B
Staniszewski, Z
Stark, AA
Story, K
Stubbs, CW
Suhada, R
Tokarz, S
van Engelen, A
Vanderlinde, K
Vieira, JD
Vikhlinin, A
Williamson, R
Zahn, O
Zenteno, A
AF High, F. W.
Hoekstra, H.
Leethochawalit, N.
de Haan, T.
Abramson, L.
Aird, K. A.
Armstrong, R.
Ashby, M. L. N.
Bautz, M.
Bayliss, M.
Bazin, G.
Benson, B. A.
Bleem, L. E.
Brodwin, M.
Carlstrom, J. E.
Chang, C. L.
Cho, H. M.
Clocchiatti, A.
Conroy, M.
Crawford, T. M.
Crites, A. T.
Desai, S.
Dobbs, M. A.
Dudley, J. P.
Foley, R. J.
Forman, W. R.
George, E. M.
Gladders, M. D.
Gonzalez, A. H.
Halverson, N. W.
Harrington, N. L.
Holder, G. P.
Holzapfel, W. L.
Hoover, S.
Hrubes, J. D.
Jones, C.
Joy, M.
Keisler, R.
Knox, L.
Lee, A. T.
Leitch, E. M.
Liu, J.
Lueker, M.
Luong-Van, D.
Mantz, A.
Marrone, D. P.
McDonald, M.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Mocanu, L.
Mohr, J. J.
Montroy, T. E.
Murray, S. S.
Natoli, T.
Nurgaliev, D.
Padin, S.
Plagge, T.
Pryke, C.
Reichardt, C. L.
Rest, A.
Ruel, J.
Ruhl, J. E.
Saliwanchik, B. R.
Saro, A.
Sayre, J. T.
Schaffer, K. K.
Shaw, L.
Schrabback, T.
Shirokoff, E.
Song, J.
Spieler, H. G.
Stalder, B.
Staniszewski, Z.
Stark, A. A.
Story, K.
Stubbs, C. W.
Suhada, R.
Tokarz, S.
van Engelen, A.
Vanderlinde, K.
Vieira, J. D.
Vikhlinin, A.
Williamson, R.
Zahn, O.
Zenteno, A.
TI WEAK-LENSING MASS MEASUREMENTS OF FIVE GALAXY CLUSTERS IN THE SOUTH POLE
TELESCOPE SURVEY USING MAGELLAN/MEGACAM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: clusters: individual
ID DIGITAL SKY SURVEY; X-RAY-PROPERTIES; DARK-MATTER; PHOTOMETRIC
REDSHIFTS; COSMOLOGICAL CONSTRAINTS; HALO CONCENTRATIONS; SCALING
RELATIONS; OBSERVED GROWTH; CATALOG; PROFILE
AB We use weak gravitational lensing to measure the masses of five galaxy clusters selected from the South Pole Telescope (SPT) survey, with the primary goal of comparing these with the SPT Sunyaev-Zel'dovich (SZ) and X-ray-based mass estimates. The clusters span redshifts 0.28 < z < 0.43 and have masses M-500 > 2 x 10(14) h(-1)M(circle dot), and three of the five clusters were discovered by the SPT survey. We observed the clusters in the g'r'i' passbands with the Megacam imager on the Magellan Clay 6.5 m telescope. We measure a mean ratio of weak-lensing (WL) aperture masses to inferred aperture masses from the SZ data, both within an aperture of R-500,R-SZ derived from the SZ mass, of 1.04 +/- 0.18. We measure a mean ratio of spherical WL masses evaluated at R-500,R-SZ to spherical SZ masses of 1.07 +/- 0.18, and a mean ratio of spherical WL masses evaluated at R-500,R-WL to spherical SZ masses of 1.10 +/- 0.24. We explore potential sources of systematic error in the mass comparisons and conclude that all are subdominant to the statistical uncertainty, with dominant terms being cluster concentration uncertainty and N-body simulation calibration bias. Expanding the sample of SPT clusters with WL observations has the potential to significantly improve the SPT cluster mass calibration and the resulting cosmological constraints from the SPT cluster survey. These are the first WL detections using Megacam on the Magellan Clay telescope.
C1 [High, F. W.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mantz, A.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Natoli, T.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[High, F. W.; Abramson, L.; Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Hoekstra, H.] Leiden Univ, Leiden Observ, Leiden, Netherlands.
[Leethochawalit, N.; Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[de Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Shaw, L.; van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Armstrong, R.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA.
[Ashby, M. L. N.; Conroy, M.; Foley, R. J.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.; Tokarz, S.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bautz, M.; McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Bayliss, M.; Nurgaliev, D.; Ruel, J.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Bazin, G.; Desai, S.; Liu, J.; Mohr, J. J.; Saro, A.; Suhada, R.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Bazin, G.; Desai, S.; Liu, J.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; McMahon, J. J.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
[Clocchiatti, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[George, E. M.; Harrington, N. L.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.; Shirokoff, E.; Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Joy, M.] NASA, Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA.
[Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[Lueker, M.; Padin, S.; Shirokoff, E.; Vieira, J. D.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[McMahon, J. J.; Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI USA.
[Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Dept Phys, Cleveland, OH 44106 USA.
[Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA.
[Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Schrabback, T.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Zahn, O.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA.
RP High, FW (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
EM fwhigh@kicp.uchicago.edu
RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; Stubbs,
Christopher/C-2829-2012;
OI Williamson, Ross/0000-0002-6945-2975; Stubbs,
Christopher/0000-0003-0347-1724; Marrone, Daniel/0000-0002-2367-1080;
Aird, Kenneth/0000-0003-1441-9518; Reichardt,
Christian/0000-0003-2226-9169; Hoekstra, Henk/0000-0002-0641-3231;
Stark, Antony/0000-0002-2718-9996
FU National Science Foundation [ANT-0638937]; NSF Physics Frontier Center
[PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation;
Marie Curie IRG [230924]; Netherlands Organisation for Scientific
Research (NWO) [639.042.814]; Excellence Cluster Universe; DFG research
program [TR33]; NSF [AST-1009012, AST-1009649, MRI-0723073]; National
Sciences and Engineering Research Council of Canada; Canada Research
Chairs program; Canadian Institute for Advanced Research; Clay
fellowship; Smithsonian Astrophysical Observatory
FX The South Pole Telescope program is supported by the National Science
Foundation through grant ANT-0638937. Partial support is also provided
by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli
Institute of Cosmological Physics at the University of Chicago, the
Kavli Foundation, and the Gordon and Betty Moore Foundation. H.H.
acknowledges support from Marie Curie IRG grant 230924 and the
Netherlands Organisation for Scientific Research (NWO) grant No.
639.042.814. The Munich group acknowledges support from the Excellence
Cluster Universe and the DFG research program TR33 The Dark Universe.
Galaxy cluster research at Harvard is supported by NSF grant
AST-1009012, and research at SAO is supported in part by NSF grants
AST-1009649 and MRI-0723073. The McGill group acknowledges funding from
the National Sciences and Engineering Research Council of Canada, Canada
Research Chairs program, and the Canadian Institute for Advanced
Research. R.J.F. is supported by a Clay fellowship.; This paper used
data products produced by the OIR Telescope Data Center, supported by
the Smithsonian Astrophysical Observatory.
NR 80
TC 30
Z9 30
U1 1
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2012
VL 758
IS 1
AR 68
DI 10.1088/0004-637X/758/1/68
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016LS
UT WOS:000309520500068
ER
PT J
AU LaMassa, SM
Heckman, TM
Ptak, A
Schiminovich, D
O'Dowd, M
Bertincourt, B
AF LaMassa, Stephanie M.
Heckman, T. M.
Ptak, A.
Schiminovich, D.
O'Dowd, M.
Bertincourt, B.
TI EXPLORING THE CONNECTION BETWEEN STAR FORMATION AND ACTIVE GALACTIC
NUCLEUS ACTIVITY IN THE LOCAL UNIVERSE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: Seyfert; galaxies: star formation; infrared:
galaxies; techniques: spectroscopic
ID ULTRALUMINOUS INFRARED GALAXIES; SPITZER-SPACE-TELESCOPE; POLYCYCLIC
AROMATIC-HYDROCARBONS; STARBURST-AGN CONNECTION; BLACK-HOLE MASS;
SEYFERT-GALAXIES; FORMING GALAXIES; VELOCITY DISPERSION;
STATISTICAL-METHODS; ASTRONOMICAL DATA
AB We study a combined sample of 264 star-forming, 51 composite, and 73 active galaxies using optical spectra from the Sloan Digital Sky Survey (SDSS) and mid-infrared (mid-IR) spectra from the Spitzer Infrared Spectrograph. We examine optical and mid-IR spectroscopic diagnostics that probe the amount of star formation and relative energetic contributions from star formation and an active galactic nucleus (AGN). Overall we find good agreement between optical and mid-IR diagnostics. Misclassifications of galaxies based on the SDSS spectra are rare despite the presence of dust obscuration. The luminosity of the [Ne II] 12.8 mu m emission line is well correlated with the star formation rate measured from the SDSS spectra, and this holds for the star-forming, composite, and AGN-dominated systems. AGNs show a clear excess of [Ne III] 15.6 mu m emission relative to star-forming and composite systems. We find good qualitative agreement between various parameters that probe the relative contributions of the AGN and star formation, including the mid-IR spectral slope, the ratio of the [Ne v] 14.3 mu m to [Ne II] mu m 12.8 fluxes, the equivalent widths of the 7.7 mu m, 11.3 mu m, and 17 mu m polycyclic aromatic hydrocarbon (PAH) features, and the optical "D" parameter which measures the distance at which a source lies from the locus of star-forming galaxies in the optical BPT emission-line diagnostic diagram. We also consider the behavior of the three individual PAH features by examining how their flux ratios depend upon the degree of AGN dominance. We find that the PAH 11.3 mu m feature is significantly suppressed in the most AGN-dominated systems.
C1 [LaMassa, Stephanie M.; Heckman, T. M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Ptak, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Schiminovich, D.; Bertincourt, B.] Columbia Univ, Dept Astron, New York, NY 10027 USA.
[O'Dowd, M.] CUNY Herbert H Lehman Coll, Bronx, NY 10468 USA.
RP LaMassa, SM (reprint author), Yale Univ, New Haven, CT 06520 USA.
FU ADAP [10-ADAP10-0167]; 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; American Museum of Natural
History; Astrophysical Institute Potsdam; University of Basel;
University of Cambridge; Case Western Reserve University; University of
Chicago; Drexel University; Fermilab; Institute for Advanced Study;
Japan Participation Group; Johns Hopkins University; Joint Institute for
Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and
Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST);
Los Alamos National Laboratory; Max-Planck-Institute for Astronomy
(MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State
University; Ohio State University; University of Pittsburgh; University
of Portsmouth; Princeton University; United States Naval Observatory;
University of Washington
FX This work is funded by ADAP grant number 10-ADAP10-0167. We thank the
anonymous referee whose comments have improved this manuscript. We thank
D. M. Alexander for thoughtful discussions. 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. 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/. The SDSS
is managed by the Astrophysical Research Consortium for the
Participating Institutions. The Participating Institutions are the
American Museum of Natural History, Astrophysical Institute Potsdam,
University of Basel, University of Cambridge, Case Western Reserve
University, University of Chicago, Drexel University, Fermilab, the
Institute for Advanced Study, the Japan Participation Group, Johns
Hopkins University, the Joint Institute for Nuclear Astrophysics, the
Kavli Institute for Particle Astrophysics and Cosmology, the Korean
Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos
National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the
Max-Planck-Institute for Astrophysics (MPA), New Mexico State
University, Ohio State University, University of Pittsburgh, University
of Portsmouth, Princeton University, the United States Naval
Observatory, and the University of Washington.
NR 49
TC 27
Z9 27
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2012
VL 758
IS 1
AR 1
DI 10.1088/0004-637X/758/1/1
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016LS
UT WOS:000309520500001
ER
PT J
AU Mostl, C
Farrugia, CJ
Kilpua, EKJ
Jian, LK
Liu, Y
Eastwood, JP
Harrison, RA
Webb, DF
Temmer, M
Odstrcil, D
Davies, JA
Rollett, T
Luhmann, JG
Nitta, N
Mulligan, T
Jensen, EA
Forsyth, R
Lavraud, B
de Koning, CA
Veronig, AM
Galvin, AB
Zhang, TL
Anderson, BJ
AF Moestl, C.
Farrugia, C. J.
Kilpua, E. K. J.
Jian, L. K.
Liu, Y.
Eastwood, J. P.
Harrison, R. A.
Webb, D. F.
Temmer, M.
Odstrcil, D.
Davies, J. A.
Rollett, T.
Luhmann, J. G.
Nitta, N.
Mulligan, T.
Jensen, E. A.
Forsyth, R.
Lavraud, B.
de Koning, C. A.
Veronig, A. M.
Galvin, A. B.
Zhang, T. L.
Anderson, B. J.
TI MULTI-POINT SHOCK AND FLUX ROPE ANALYSIS OF MULTIPLE INTERPLANETARY
CORONAL MASS EJECTIONS AROUND 2010 AUGUST 1 IN THE INNER HELIOSPHERE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE shock waves; solar-terrestrial relations; Sun: coronal mass ejections
(CMEs); Sun: heliosphere
ID IN-SITU OBSERVATIONS; CME-CME INTERACTION; MAGNETIC CLOUDS; SOLAR-WIND;
RING CURRENT; STEREO OBSERVATIONS; GEOMAGNETIC STORMS; INTERACTION
REGION; INTERNAL STRUCTURE; COMPLEX EJECTA
AB We present multi-point in situ observations of a complex sequence of coronal mass ejections (CMEs) which may serve as a benchmark event for numerical and empirical space weather prediction models. On 2010 August 1, instruments on various space missions, Solar Dynamics Observatory/Solar and Heliospheric Observatory/Solar-TErrestrial-RElations-Observatory (SDO/SOHO/STEREO), monitored several CMEs originating within tens of degrees from the solar disk center. We compare their imprints on four widely separated locations, spanning 120 degrees in heliospheric longitude, with radial distances from the Sun ranging from MESSENGER (0.38 AU) to Venus Express (VEX, at 0.72 AU) to Wind, ACE, and ARTEMIS near Earth and STEREO-B close to 1 AU. Calculating shock and flux rope parameters at each location points to a non-spherical shape of the shock, and shows the global configuration of the interplanetary coronal mass ejections (ICMEs), which have interacted, but do not seem to have merged. VEX and STEREO-B observed similar magnetic flux ropes (MFRs), in contrast to structures at Wind. The geomagnetic storm was intense, reaching two minima in the Dst index (approximate to-100 nT), and was caused by the sheath region behind the shock and one of two observed MFRs. MESSENGER received a glancing blow of the ICMEs, and the events missed STEREO-A entirely. The observations demonstrate how sympathetic solar eruptions may immerse at least 1/3 of the heliosphere in the ecliptic with their distinct plasma and magnetic field signatures. We also emphasize the difficulties in linking the local views derived from single-spacecraft observations to a consistent global picture, pointing to possible alterations from the classical picture of ICMEs.
C1 [Moestl, C.; Liu, Y.; Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Moestl, C.; Temmer, M.; Rollett, T.; Veronig, A. M.] Graz Univ, Inst Phys, Kanzelhohe Observ IGAM, A-8010 Graz, Austria.
[Moestl, C.; Rollett, T.; Zhang, T. L.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria.
[Farrugia, C. J.; Galvin, A. B.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Farrugia, C. J.; Galvin, A. B.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA.
[Kilpua, E. K. J.] Univ Helsinki, Dept Phys, FI-00560 Helsinki, Finland.
[Jian, L. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Jian, L. K.; Odstrcil, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Liu, Y.] Chinese Acad Sci, Natl Space Sci Ctr, State Key Lab Space Weather, Beijing, Peoples R China.
[Eastwood, J. P.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London, England.
[Harrison, R. A.; Davies, J. A.] Harwell Oxford, RAL Space, Didcot, Oxon, England.
[Webb, D. F.] Boston Coll, Inst Sci Res, Newton, MA USA.
[Nitta, N.] Lockheed Martin Adv Technol Ctr, Solar & Astrophys Lab, Palo Alto, CA USA.
[Mulligan, T.] Aerosp Corp, Space Sci Applicat Lab, El Segundo, CA 90245 USA.
[Jensen, E. A.] ACS Consulting, Houston, TX USA.
[Lavraud, B.] Univ Toulouse UPS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France.
[Lavraud, B.] Ctr Natl Rech Sci, UMR 5277, F-31400 Toulouse, France.
[de Koning, C. A.] NOAA SWPC, Boulder, CO USA.
[Anderson, B. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
RP Mostl, C (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM christian.moestl@uni-graz.at
RI Anderson, Brian/I-8615-2012; Galvin, Antoinette/A-6114-2013; Jian,
Lan/B-4053-2010; Veronig, Astrid/B-8422-2009; Kilpua,
Emilia/G-8994-2012;
OI Amerstorfer, Tanja/0000-0001-9024-6706; Temmer,
Manuela/0000-0003-4867-7558; Jian, Lan/0000-0002-6849-5527; Liu,
Ying/0000-0002-3483-5909; Moestl, Christian/0000-0001-6868-4152
FU Marie Curie International Outgoing Fellowship within the 7th European
Community Framework Programme; Austrian Science Fund (FWF) [P20145-N16,
V195-N16]; European Union [263252]; NASA [NAS5-00132, NNG06GD41G,
NNX08AD11G, NNX10AQ29G, NNX08AQ16G]; NSF [AGS-1140211]; STEREO
[NAS5-03131]; Navy [N00173-07-1-G016, N00173-10-1-G001]
FX We thank all the people involved in building and maintaining the great
variety of instruments from which data was used to make this work
possible. This work would also not have been possible without the
enthusiasm of the attendees of the three workshops held in early 2011.
We additionally thank Paulett Liewer, Karel Schrijver, and Volker
Bothmer for enlightening discussions. This research was supported by a
Marie Curie International Outgoing Fellowship within the 7th European
Community Framework Programme. C. M., M. T., and T. R. were supported by
the Austrian Science Fund (FWF): P20145-N16, V195-N16. The presented
work has received funding from the European Union Seventh Framework
Programme (FP7/2007-2013) under grant agreement No. 263252 [COMESEP]. It
is also supported by NASA grants NAS5-00132, NNG06GD41G, NNX08AD11G,
NNX10AQ29G, NNX08AQ16G, and NSF grant AGS-1140211. Work at the
University of California, Berkeley, was supported from STEREO grant
NAS5-03131. D. F. W. was supported by Navy contracts N00173-07-1-G016
and N00173-10-1-G001. We also acknowledge the use of Wind data provided
by the magnetometer and the solar wind experiment teams at GSFC, and
thank the centers for geomagnetism in Kyoto and Potsdam for providing
the Kp and Dst indices.
NR 94
TC 42
Z9 42
U1 3
U2 16
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2012
VL 758
IS 1
AR 10
DI 10.1088/0004-637X/758/1/10
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016LS
UT WOS:000309520500010
ER
PT J
AU Sultana, J
Kazanas, D
Fukumura, K
AF Sultana, J.
Kazanas, D.
Fukumura, K.
TI LUMINOSITY CORRELATIONS FOR GAMMA-RAY BURSTS AND IMPLICATIONS FOR THEIR
PROMPT AND AFTERGLOW EMISSION MECHANISMS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmological parameters; gamma-ray burst: general
ID SPECTRAL LAGS; BATSE OBSERVATIONS; TIGHT CORRELATION; ALERT-TELESCOPE;
PEAK LUMINOSITY; HUBBLE DIAGRAM; LIGHT CURVES; SWIFT; CONNECTION;
SPECTROSCOPY
AB We present the relation between the (z- and k-corrected) spectral lags, tau, for the standard Swift energy bands 50-100 keV and 100-200 keV and the peak isotropic luminosity, L-iso (a relation reported first by Norris et al.), for a subset of 12 long Swift gamma-ray bursts (GRBs) taken from a recent study of this relation by Ukwatta et al. The chosen GRBs are also a subset of the Dainotti et al. sample, a set of Swift GRBs of known redshift, employed in establishing a relation between the (GRB frame) luminosity, L-X, of the shallow (or constant) flux portion of the typical X-Ray Telescope GRB-afterglow light curve and the (GRB frame) time of transition to the normal decay rate, T-brk. We also present the L-X-T-brk relation using only the bursts common in the two samples. The two relations exhibit a significant degree of correlation (rho = -0.65 for the L-iso-tau and rho = -0.88 for the L-X-T-brk relation) and have surprisingly similar best-fit power-law indices (-1.19 +/- 0.17 for L-iso-tau and -1.10 +/- 0.03 for L-X-T-brk). Even more surprisingly, we noted that although tau and T-brk represent different GRB time variables, it appears that the first relation (L-iso-tau) extrapolates into the second one for timescales tau similar or equal to T-brk. This fact suggests that these two relations have a common origin, which we conjecture to be kinematic. This relation adds to the recently discovered relations between properties of the prompt and afterglow GRB phases, indicating a much more intimate relation between these two phases than hitherto considered.
C1 [Sultana, J.] Univ Malta, Fac Sci, Dept Math, Msida 2080, Malta.
[Kazanas, D.; Fukumura, K.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sultana, J (reprint author), Univ Malta, Fac Sci, Dept Math, Msida 2080, Malta.
EM joseph.sultana@um.edu.mt
FU University of Malta
FX We acknowledge useful discussions with Takanori Sakamoto. J.S.
gratefully acknowledges financial support from the University of Malta
during his visit at NASA-GSFC.
NR 45
TC 10
Z9 10
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2012
VL 758
IS 1
AR 32
DI 10.1088/0004-637X/758/1/32
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016LS
UT WOS:000309520500032
ER
PT J
AU Bamber, J
van den Broeke, M
Ettema, J
Lenaerts, J
Rignot, E
AF Bamber, Jonathan
van den Broeke, Michiel
Ettema, Janneke
Lenaerts, Jan
Rignot, Eric
TI Recent large increases in freshwater fluxes from Greenland into the
North Atlantic
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ICE-SHEET; CLIMATE-CHANGE; ARCTIC-OCEAN; 21ST CENTURIES; GLACIERS;
CIRCULATION; DISCHARGE; IMPACTS; RUNOFF; FJORD
AB Freshwater (FW) fluxes from river runoff and precipitation minus evaporation for the pan Arctic seas are relatively well documented and prescribed in ocean GCMs. Fluxes from Greenland on the other hand are generally ignored altogether, despite their potential impacts on ocean circulation and marine biology. Here, we present a reconstruction of the spatially distributedFWflux from Greenland for 1958-2010. We find a modest increase into the Arctic Ocean during this period. Fluxes into the Irminger Basin, however, have increased by fifty percent (6.3 +/- 0.5 km(3) yr(-2)) in less than twenty years. This greatly exceeds previous estimates. For the ice sheet as a whole the rate of increase since 1992 is 16.9 +/- 1.8 km(3) yr(-2). The cumulative FW anomaly since 1995 is 3200 +/- 358 km(3), which is about a third of the magnitude of the Great Salinity Anomaly (GSA) of the 1970s. If this trend continues into the future, the anomaly will exceed that of the GSA by about 2025. Citation: Bamber, J., M. van den Broeke, J. Ettema, J. Lenaerts, and E. Rignot (2012), Recent large increases in freshwater fluxes from Greenland into the North Atlantic, Geophys. Res. Lett., 39, L19501, doi:10.1029/2012GL052552.
C1 [Bamber, Jonathan] Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England.
[van den Broeke, Michiel; Ettema, Janneke; Lenaerts, Jan] Univ Utrecht, Inst Marine & Atmospher Res, Utrecht, Netherlands.
[Ettema, Janneke] Univ Twente, NL-7500 AE Enschede, Netherlands.
[Rignot, Eric] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Rignot, Eric] Univ Calif Irvine, Dept Earth Sci, Irvine, CA USA.
RP Bamber, J (reprint author), Univ Bristol, Sch Geog Sci, Univ Rd, Bristol BS8 1SS, Avon, England.
EM j.bamber@bristol.ac.uk
RI Ettema, Janneke/F-7950-2010; Bamber, Jonathan/C-7608-2011; Rignot,
Eric/A-4560-2014; Van den Broeke, Michiel/F-7867-2011; Lenaerts,
Jan/D-9423-2012
OI Bamber, Jonathan/0000-0002-2280-2819; Rignot, Eric/0000-0002-3366-0481;
Van den Broeke, Michiel/0000-0003-4662-7565; Lenaerts,
Jan/0000-0003-4309-4011
FU NERC Joint RAPID grant [NE/C509474/1]; Colorado University Cooperative
Institute for Research in Environmental Sciences (CIRES) fellowship;
RAPID international programme (Netherlands, UK, Norway); Utrecht
University; Netherlands Polar Programme; NASA Cryosphere Science Program
FX JLB's contribution was made possible through NERC Joint RAPID grant
NE/C509474/1 and Colorado University Cooperative Institute for Research
in Environmental Sciences (CIRES) fellowship. MvDB and JE were supported
by the RAPID international programme (Netherlands, UK, Norway), Utrecht
University, the Netherlands Polar Programme. ER's work was supported by
a grant from the NASA Cryosphere Science Program.
NR 32
TC 86
Z9 87
U1 10
U2 82
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD OCT 9
PY 2012
VL 39
AR L19501
DI 10.1029/2012GL052552
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 020TG
UT WOS:000309836900001
ER
PT J
AU Rupper, S
Schaefer, JM
Burgener, LK
Koenig, LS
Tsering, K
Cook, ER
AF Rupper, Summer
Schaefer, Joerg M.
Burgener, Landon K.
Koenig, Lora S.
Tsering, Karma
Cook, Edward R.
TI Sensitivity and response of Bhutanese glaciers to atmospheric warming
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID HIMALAYAN GLACIERS; CLIMATE-CHANGE; TEMPERATURE; INDEX; AREAS
AB Glacierized change in the Himalayas affects river-discharge, hydro-energy and agricultural production, and Glacial Lake Outburst Flood potential, but its quantification and extent of impacts remains highly uncertain. Here we present conservative, comprehensive and quantitative predictions for glacier area and meltwater flux changes in Bhutan, monsoonal Himalayas. In particular, we quantify the uncertainties associated with the glacier area and meltwater flux changes due to uncertainty in climate data, a critical problem for much of High Asia. Based on a suite of gridded climate data and a robust glacier melt model, our results show that glacier area and melt-water change projections can vary by an order of magnitude for different climate datasets. However, the most conservative results indicate that, even if climate were to remain at the presentday mean values, almost 10% of Bhutan's glacierized area would vanish and the meltwater flux would drop by as much as 30%. Under the conservative scenario of an additional 1 degrees C regional warming, glacier retreat is going to continue until about 25% of Bhutan's glacierized area will have disappeared and the annual meltwater flux, after an initial spike, would drop by as much as 65%. Citation: Rupper, S., J. M. Schaefer, L. K. Burgener, L. S. Koenig, K. Tsering, and E. R. Cook (2012), Sensitivity and response of Bhutanese glaciers to atmospheric warming, Geophys. Res. Lett., 39, L19503, doi:10.1029/2012GL053010.
C1 [Rupper, Summer; Burgener, Landon K.] Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA.
[Schaefer, Joerg M.; Cook, Edward R.] Columbia Univ, Lamont Doherty Earth Observ, Earth Inst, Palisades, NY USA.
[Koenig, Lora S.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA.
[Tsering, Karma] Minist Econ Affairs, Dept Hydromet Serv, Thimphu, Bhutan.
RP Rupper, S (reprint author), Brigham Young Univ, Dept Geol Sci, S389 ESC, Provo, UT 84602 USA.
EM summer_rupper@byu.edu
OI Rupper, Summer/0000-0001-8655-5282
FU Brigham Young University Mentoring Environment Grant
FX Partial funding for this work was provided by a Brigham Young University
Mentoring Environment Grant. R. Forster, R. Harris, A. Gillespie, and an
anonymous reviewer provided feedback and insights that greatly improved
the science and writing.
NR 31
TC 10
Z9 10
U1 5
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 OCT 9
PY 2012
VL 39
AR L19503
DI 10.1029/2012GL053010
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 020TG
UT WOS:000309836900004
ER
PT J
AU Anton, M
Valenzuela, A
Roman, R
Lyamani, H
Krotkov, N
Arola, A
Olmo, FJ
Alados-Arboledas, L
AF Anton, M.
Valenzuela, A.
Roman, R.
Lyamani, H.
Krotkov, N.
Arola, A.
Olmo, F. J.
Alados-Arboledas, L.
TI Influence of desert dust intrusions on ground-based and
satellite-derived ultraviolet irradiance in southeastern Spain
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID AEROSOL OPTICAL-PROPERTIES; MONITORING INSTRUMENT OMI; SURFACE UV
IRRADIANCE; EL ARENOSILLO SPAIN; RADIATIVE PROPERTIES; IBERIAN
PENINSULA; GRANADA SPAIN; BREWER MEASUREMENTS; FORCING EFFICIENCY;
LIGHT-ABSORPTION
AB The desert dust aerosols strongly affect propagation of solar radiation through the atmosphere, reducing surface irradiance available for photochemistry and photosynthesis. This paper evaluates effects of desert dust on surface UV erythemal irradiance (UVER), as measured by a ground-based broadband UV radiometer and retrieved from the satellite Ozone Monitoring Instrument (OMI) at Granada (southern Spain) from January 2006 to December 2010. The dust effects are characterized by the transmittance ratio of the measured UVER to the corresponding modeled clear sky value. The transmittance has an exponential dependency on aerosol optical depth (AOD), with minimum values of similar to 0.6 (attenuation of similar to 40%). The OMI UVER algorithm does not account for UV aerosol absorption, which results in overestimation of the ground-based UVER especially during dust episodes with a mean relative difference up to 40%. The application of aerosol absorption post-correction method reduces OMI bias up to similar to 13%. The results highlight great effect of desert dust on the surface UV irradiance in regions like southern Spain, where dust intrusions from Sahara region are very frequent.
C1 [Anton, M.] Univ Extremadura, Dept Fis, ES-06071 Badajoz, Spain.
[Valenzuela, A.; Lyamani, H.; Olmo, F. J.; Alados-Arboledas, L.] Univ Granada, Dept Fis Aplicada, Granada, Spain.
[Valenzuela, A.; Lyamani, H.; Olmo, F. J.; Alados-Arboledas, L.] Univ Granada, Ctr Andaluz Medio Ambiente, Granada, Spain.
[Roman, R.] Univ Valladolid, Dept Fis Aplicada, Valladolid, Spain.
[Krotkov, N.] NASA, Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD 20771 USA.
[Arola, A.] Finnish Meteorol Inst, Kuopio, Finland.
RP Anton, M (reprint author), Univ Extremadura, Dept Fis, ES-06071 Badajoz, Spain.
EM mananton@unex.es
RI Krotkov, Nickolay/E-1541-2012; Olmo Reyes, Francisco Jose/F-7621-2016;
Anton, Manuel/A-8477-2010; Lyamani, Hassan/J-4380-2013; Roman,
Roberto/K-2104-2014; Alados-Arboledas, Lucas/P-5630-2014;
OI Krotkov, Nickolay/0000-0001-6170-6750; Olmo Reyes, Francisco
Jose/0000-0002-0186-1721; Anton, Manuel/0000-0002-0816-3758; Roman,
Roberto/0000-0003-4889-1781; Alados-Arboledas,
Lucas/0000-0003-3576-7167; Lyamani, Hassan/0000-0002-6386-1102;
Valenzuela, Antonio/0000-0003-0290-4081; Arola,
Antti/0000-0002-9220-0194
FU Fondo Social Europeo; Andalusian Regional Government [P08-RNM-3568,
P10-RNM-6299]; Ministerio de Ciencia e Innovacion
[CGL2008-05939-C03-03/CLI, CGL2010-18782, CGL-2011-2992-1-C02-01,
CSD2007-00067]; European Union through ACTRIS project [EU
INFRA-2010-1.1.16-262254]; NASA Earth Science Division
FX Manuel Anton thanks Ministerio de Ciencia e Innovacion and Fondo Social
Europeo for the award of a postdoctoral grant (Ramon y Cajal). This work
was partially supported by the Andalusian Regional Government through
projects P08-RNM-3568 and P10-RNM-6299, the Ministerio de Ciencia e
Innovacion through projects CGL2008-05939-C03-03/CLI, CGL2010-18782,
CGL-2011-2992-1-C02-01 and CSD2007-00067, and by European Union through
ACTRIS project (EU INFRA-2010-1.1.16-262254). Nickolay Krotkov
acknowledges support from NASA Earth Science Division.
NR 76
TC 6
Z9 6
U1 0
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 9
PY 2012
VL 117
AR D19209
DI 10.1029/2012JD018056
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 020QT
UT WOS:000309829200001
ER
PT J
AU Farrell, WM
Halekas, JS
Killen, RM
Delory, GT
Gross, N
Bleacher, LV
Krauss-Varben, D
Travnicek, P
Hurley, D
Stubbs, TJ
Zimmerman, MI
Jackson, TL
AF Farrell, W. M.
Halekas, J. S.
Killen, R. M.
Delory, G. T.
Gross, N.
Bleacher, L. V.
Krauss-Varben, D.
Travnicek, P.
Hurley, D.
Stubbs, T. J.
Zimmerman, M. I.
Jackson, T. L.
TI Solar-Storm/Lunar Atmosphere Model (SSLAM): An overview of the effort
and description of the driving storm environment
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID ADVANCED COMPOSITION EXPLORER; ENERGETIC PARTICLES; ACE OBSERVATIONS;
MAGNETIC-FIELDS; LUNAR-SURFACE; WIND; SPACECRAFT; ACCELERATION;
ELECTRON; MARS
AB On 29 April 1998, a coronal mass ejection (CME) was emitted from the Sun that had a significant impact at Earth. The terrestrial magnetosphere became more electrically active during the storm passage. Less explored is the effect of such a storm on an exposed rocky body like our Moon. The solar-storm/lunar atmosphere modeling effort (SSLAM) brings together surface interactions, exosphere, plasma, and surface charging models all run with a common driver - the solar storm and CME passage occurring from 1 to 4 May 1998. We present herein an expanded discussion on the solar driver during the 1-4 May 1998 period that included the passage of an intense coronal mass ejection (CME) that had >10 times the solar wind density and had a compositional component of He++ that exceeded 20%. During this time, the plasma mass flux to the exposed lunar surface increased by over 20 times compared to the nominal solar wind, to a value near 10(-13) kg/m(2)-s. Over a two day CME passage by the Moon, this amount approaches 300 tons of added mass to the Moon in the form of individual proton and helium ions. Such an increase in ion flux should have a profound impact on sputtering loss rates from the surface, since this process scales as the mass, energy, and charge state of the incident ion. Associated loss processes were addressed by SSLAM and will be discussed herein.
C1 [Farrell, W. M.; Killen, R. M.; Bleacher, L. V.; Zimmerman, M. I.; Jackson, T. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Farrell, W. M.; Halekas, J. S.; Killen, R. M.; Delory, G. T.; Gross, N.; Bleacher, L. V.; Krauss-Varben, D.; Travnicek, P.; Hurley, D.; Stubbs, T. J.; Zimmerman, M. I.; Jackson, T. L.] NASA, Lunar Sci Inst, Moffett Field, CA USA.
[Halekas, J. S.; Delory, G. T.; Krauss-Varben, D.; Travnicek, P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Gross, N.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
[Hurley, D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Stubbs, T. J.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
[Zimmerman, M. I.] Oak Ridge Associate Univ, Oak Ridge, TN USA.
RP Farrell, WM (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM william.m.farrell@nasa.gov
RI Stubbs, Timothy/I-5139-2013; Farrell, William/I-4865-2013; Hurley,
Dana/F-4488-2015;
OI Stubbs, Timothy/0000-0002-5524-645X; Hurley, Dana/0000-0003-1052-1494;
Halekas, Jasper/0000-0001-5258-6128
FU NASA Lunar Science Institute
FX This work was supported by the NASA Lunar Science Institute. We thank
the ACE EPAM and SIS instrument teams, the Wind EPACT team, the SOHO
COSTEP instrument team, and NASA's CDAWEB for providing energetic
particle data and the Omnidata file.
NR 45
TC 8
Z9 8
U1 1
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD OCT 9
PY 2012
VL 117
AR E00K04
DI 10.1029/2012JE004070
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 020RX
UT WOS:000309832500001
ER
PT J
AU Minazzoli, O
Harko, T
AF Minazzoli, Olivier
Harko, Tiberiu
TI New derivation of the Lagrangian of a perfect fluid with a barotropic
equation of state
SO PHYSICAL REVIEW D
LA English
DT Article
ID REFERENCE SYSTEMS; MOTION
AB In this paper we give a simple proof that when the particle number is conserved, the Lagrangian of a barotropic perfect fluid is L-m = -rho[c(2) + integral P(rho)/rho(2)d rho], where rho is the rest mass density and P(rho) is the pressure. To prove this result, neither additional fields nor Lagrange multipliers are needed. Besides, the result is applicable to a wide range of theories of gravitation. The only assumptions used in the derivation are: 1) the matter part of the Lagrangian does not depend on the derivatives of the metric, and 2) the particle number of the fluid is conserved (del(sigma)(rho u(sigma)) = 0).
C1 [Minazzoli, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Harko, Tiberiu] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China.
[Harko, Tiberiu] Univ Hong Kong, Ctr Theoret & Computat Phys, Hong Kong, Hong Kong, Peoples R China.
RP Minazzoli, O (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
OI Minazzoli, Olivier/0000-0002-3151-7593
FU NASA Postdoctoral Program at the Jet Propulsion Laboratory, California
Institute of Technology; ASA
FX This research 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.
NR 20
TC 14
Z9 14
U1 0
U2 3
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0010
EI 2470-0029
J9 PHYS REV D
JI Phys. Rev. D
PD OCT 9
PY 2012
VL 86
IS 8
AR 087502
DI 10.1103/PhysRevD.86.087502
PG 4
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 017JW
UT WOS:000309587200010
ER
PT J
AU Rocha, J
Palumbo, D
AF Rocha, Joana
Palumbo, Daniel
TI On the sensitivity of sound power radiated by aircraft panels to
turbulent boundary layer parameters
SO JOURNAL OF SOUND AND VIBRATION
LA English
DT Article
ID AIRPLANE FUSELAGE STRUCTURE; WALL-PRESSURE-FLUCTUATIONS; VIBRATION
MEASUREMENTS; FREQUENCY SPECTRUM; INTERIOR NOISE; EXCITED PANELS;
FLAT-PLATE; TRANSMISSION; EXCITATION; FIELD
AB The objective of the present study is to investigate and quantify how sensitive the response of an aircraft panel is to the change of the turbulent flow parameters. Several empirical models currently exist that provide the turbulent boundary layer wall pressure cross spectrum. These wall pressure cross spectrum models are usually dependent on four parameters: the reference power spectrum, the flow convective velocity, and the coherence lengths in streamwise and spanwise directions. All the proposed models provide different predictions for the wall pressure cross spectrum. Also, real flow conditions over aircraft do not conform to the ideal behavior of the turbulent boundary layer pressure predicted by the models. In this context, the questions that this work aims to explore are "What is the impact of different wall pressure estimates in the radiated sound power?" and "What is the effect of the range of possible flow conditions on the radiated sound power?". For that objective, data from flight tests and estimates provided by the empirical models are used to predict radiated sound power, and the results are compared. A sensitivity analysis is performed and the relative contribution of each boundary layer parameter to the radiated sound power is obtained. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Rocha, Joana] Univ Victoria, Dept Mech Engn, Victoria, BC V8W 2Y2, Canada.
[Palumbo, Daniel] NASA, Langley Res Ctr, Struct Acoust Branch, Hampton, VA 23681 USA.
RP Rocha, J (reprint author), Univ Victoria, Dept Mech Engn, 3800 Finnerty Rd, Victoria, BC V8W 2Y2, Canada.
EM jdarocha@uvic.ca; d.l.palumbo@nasa.gov
RI Rocha, Joana/K-2811-2012
FU Foundation for Science and Technology (FCT)
FX The authors are grateful for the financial support of the Foundation for
Science and Technology (FCT).
NR 34
TC 6
Z9 6
U1 1
U2 14
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0022-460X
J9 J SOUND VIB
JI J. Sound Vibr.
PD OCT 8
PY 2012
VL 331
IS 21
BP 4785
EP 4806
DI 10.1016/j.jsv.2012.05.030
PG 22
WC Acoustics; Engineering, Mechanical; Mechanics
SC Acoustics; Engineering; Mechanics
GA 980GM
UT WOS:000306881600014
ER
PT J
AU Zhang, ZB
Ackerman, AS
Feingold, G
Platnick, S
Pincus, R
Xue, HW
AF Zhang, Zhibo
Ackerman, Andrew S.
Feingold, Graham
Platnick, Steven
Pincus, Robert
Xue, Huiwen
TI Effects of cloud horizontal inhomogeneity and drizzle on remote sensing
of cloud droplet effective radius: Case studies based on large-eddy
simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SHALLOW CUMULUS CONVECTION; RADIATIVE-TRANSFER; STRATOCUMULUS CLOUDS;
OPTICAL-THICKNESS; RETRIEVALS; IMPACT; GROWTH; RESOLUTION; ALGORITHM;
ALBEDO
AB This study investigates effects of drizzle and cloud horizontal inhomogeneity on cloud effective radius (r(e)) retrievals from the Moderate Resolution Imaging Spectroradiometer (MODIS). In order to identify the relative importance of various factors, we developed a MODIS cloud property retrieval simulator based on the combination of large-eddy simulations (LES) and radiative transfer computations. The case studies based on synthetic LES cloud fields indicate that at high spatial resolution (similar to 100 m) 3-D radiative transfer effects, such as illumination and shadowing, can induce significant differences between retrievals of r(e) based on reflectance at 2.1 mu m (r(e,2.1)) and 3.7 mu m (r(e,3.7)). It is also found that 3-D effects tend to have stronger impact on r(e,2.1) than r(e,3.7), leading to positive difference between the two (Delta r(e,3.7-2.1)) from illumination and negative Delta r(e,3.7-2.1) from shadowing. The cancellation of opposing 3-D effects leads to overall reasonable agreement between r(e,2.1) and r(e,3.7) at high spatial resolution as far as domain averages are concerned. At resolutions similar to MODIS, however, r(e,2.1) is systematically larger than r(e,3.7) when averaged over the LES domain, with the difference exhibiting a threshold-like dependence on both r(e,2.1) and an index of the sub-pixel variability in reflectance (H-sigma), consistent with MODIS observations. In the LES cases studied, drizzle does not strongly impact r(e) retrievals at either wavelength. It is also found that opposing 3-D radiative transfer effects partly cancel each other when cloud reflectance is aggregated from high spatial resolution to MODIS resolution, resulting in a weaker net impact of 3-D radiative effects on r(e) retrievals. The large difference at MODIS resolution between r(e,3.7) and r(e,2.1) for highly inhomogeneous pixels with H-sigma > 0.4 can be largely attributed to what we refer to as the "plane-parallel r(e) bias," which is attributable to the impact of sub-pixel level horizontal variability of cloud optical thickness on r(e) retrievals and is greater for r(e,2.1) than r(e,3.7). These results suggest that there are substantial uncertainties attributable to 3-D radiative effects and plane-parallel r(e) bias in the MODIS r(e,2.1) retrievals for pixels with strong sub-pixel scale variability, and the Hs index can be used to identify these uncertainties.
C1 [Zhang, Zhibo] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Zhang, Zhibo] Joint Ctr Earth Syst Technol, Baltimore, MD USA.
[Zhang, Zhibo; Platnick, Steven] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Ackerman, Andrew S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Feingold, Graham; Pincus, Robert] NOAA, Earth Syst Res Lab, Boulder, CO USA.
[Pincus, Robert] Univ Colorado, Boulder, CO 80309 USA.
[Xue, Huiwen] Peking Univ, Sch Phys, Dept Atmospher & Ocean Sci, Beijing 100871, Peoples R China.
RP Zhang, ZB (reprint author), Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
EM zhibo.zhang@umbc.edu
RI Ackerman, Andrew/D-4433-2012; Pincus, Robert/B-1723-2013; Feingold,
Graham/B-6152-2009; Zhang, Zhibo/D-1710-2010; Platnick,
Steven/J-9982-2014; Manager, CSD Publications/B-2789-2015
OI Ackerman, Andrew/0000-0003-0254-6253; Pincus,
Robert/0000-0002-0016-3470; Zhang, Zhibo/0000-0001-9491-1654; Platnick,
Steven/0000-0003-3964-3567;
FU NASA [NNX11AI98G, NNX11AF09G]
FX We thank Daniel Grosvenor and the other two anonymous reviewers for
their insightful comments, questions, and suggestions, which have helped
to improve this manuscript. ZZ, AA and SP were supported by NASA under
grant NNX11AI98G, and RP was supported by NASA under grant NNX11AF09G.
Computational support was provided by the NASA Advanced Supercomputing
Division.
NR 44
TC 36
Z9 36
U1 1
U2 33
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 6
PY 2012
VL 117
AR D19208
DI 10.1029/2012JD017655
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 018HE
UT WOS:000309650100001
ER
PT J
AU Musselman, KN
Molotch, NP
Margulis, SA
Lehning, M
Gustafsson, D
AF Musselman, Keith N.
Molotch, Noah P.
Margulis, Steven A.
Lehning, Michael
Gustafsson, David
TI Improved snowmelt simulations with a canopy model forced with
photo-derived direct beam canopy transmissivity
SO WATER RESOURCES RESEARCH
LA English
DT Article
ID LEAF-AREA INDEX; BENEATH FOREST CANOPIES; PHYSICAL SNOATACK MODEL;
MIXED-CONIFER FOREST; WATER EQUIVALENT; SOLAR-RADIATION; SIERRA-NEVADA;
LONGWAVE RADIATION; SURFACE PROCESSES; COMPLEX TERRAIN
AB The predictive capacity of a physically based snow model to simulate point-scale, subcanopy snowmelt dynamics is evaluated in a mixed conifer forest, southern Sierra Nevada, California. Three model scenarios each providing varying levels of canopy structure detail were tested. Simulations of three water years initialized at locations of 24 ultrasonic snow depth sensors were evaluated against observations of snow water equivalent (SWE), snow disappearance date, and volumetric soil water content. When canopy model parameters canopy openness and effective leaf area index were obtained from satellite and literature-based sources, respectively, the model was unable to resolve the variable subcanopy snowmelt dynamics. When canopy parameters were obtained from hemispherical photos, the improvements were not statistically significant. However, when the model was modified to accept photo-derived time-varying direct beam canopy transmissivity, the error in the snow disappearance date was reduced by as much as one week and positive and negative biases in melt-season SWE and snow cover duration were significantly reduced. Errors in the timing of soil meltwater fluxes were reduced by 11 days on average. The optimum aggregated temporal model resolution of direct beam canopy transmissivity was determined to be 30 min; hourly averages performed no better than the bulk canopy scenarios and finer time steps did not increase overall model accuracy. The improvements illustrate the important contribution of direct shortwave radiation to subcanopy snowmelt and confirm the known nonlinear melt behavior of snow cover.
C1 [Musselman, Keith N.; Molotch, Noah P.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
[Musselman, Keith N.; Molotch, Noah P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA.
[Musselman, Keith N.; Margulis, Steven A.] Univ Calif Los Angeles, Dept Civil & Environm Engn, Los Angeles, CA USA.
[Molotch, Noah P.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Lehning, Michael] WSL Inst Snow & Avalanche Res SLF, Davos, Switzerland.
[Lehning, Michael] Ecole Polytech Fed Lausanne, Sch Architecture Civil & Environm Engn, Lausanne, Switzerland.
[Gustafsson, David] Royal Inst Technol KTH, Dept Land & Water Resources Engn, Stockholm, Sweden.
[Gustafsson, David] Swedish Meteorol & Hydrol Inst, S-60176 Norrkoping, Sweden.
RP Musselman, KN (reprint author), Univ Colorado, Inst Arctic & Alpine Res, 1560 30th St,450 UCB, Boulder, CO 80309 USA.
EM musselman1@ucla.edu
RI Gustafsson, David/G-6729-2012; Molotch, Noah/C-8576-2009
FU Sequoia National Park; National Science Foundation [EAR-071160,
EAR-1032295, EAR-1032308, EAR-1141764]; Southern Sierra Critical Zone
Observatory [EAR-0725097]; Major Research Instrumentation grant
[EAR-0619947]; Mountain Research Initiative, NASA grant [NNX11AK35G];
National Aeronautics and Space Administration (NASA) Earth System
Science Fellowship
FX The authors gratefully acknowledge P. Kirchner and R. Bales for their
contribution to field data acquisition. Sequoia National Park supported
field access and research efforts. Financial support was provided by the
National Science Foundation grants EAR-071160, EAR-1032295, EAR-1032308,
EAR-1141764, the Southern Sierra Critical Zone Observatory
(EAR-0725097), a Major Research Instrumentation grant (EAR-0619947), the
Mountain Research Initiative, NASA grant NNX11AK35G and a National
Aeronautics and Space Administration (NASA) Earth System Science
Fellowship. Radiation data from the Tokopah basin were provided by J.
Melack and J. Sickman. Assistance in the field was provided by S.
Roberts, B. Forman, D. Perrot, E. Trujillo, D. Berisford, L. Meromy, M.
Girotto, A. Kahl, and M. Cooper, among many others. The authors thank
three anonymous reviewers for their comments and support of the paper.
NR 75
TC 16
Z9 16
U1 1
U2 14
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 OCT 6
PY 2012
VL 48
AR W10509
DI 10.1029/2012WR012285
PG 21
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 017RS
UT WOS:000309609000006
ER
PT J
AU Tadic, JM
Xu, L
AF Tadic, Jovan M.
Xu, Lai
TI Ab Initio and Density Functional Theory Study of Keto-Enol Equilibria of
Deltic Acid in Gas and Aqueous Solution Phase: A Bimolecular Proton
Transfer Mechanism
SO JOURNAL OF ORGANIC CHEMISTRY
LA English
DT Article
ID CONJUGATED CYCLIC-KETONES; VIBRATIONAL-SPECTRUM; ELECTRONIC-STRUCTURE;
MICROWAVE-SPECTRUM; TROPOLONE; CYCLOPROPENONE; DIHYDROXYCYCLOPROPENONE;
THERMOCHEMISTRY; PHOTOELECTRON; SPECTROSCOPY
AB Keto-enol tautomerism in deltic acid (2,3-dihydroxycycloprop-2-en-1-one) has been studied using ab initio methods and the B3LYP functional of density functional theory, as well as complete basis set (CBS-QB3 and CBS-APNO) and G4 methods. Relative and absolute energies were calculated with each of the methods, whereas computations of geometries and harmonic frequencies for dihydroxycyclopropenone and hydroxycyclopropanedione were computed in the gas phase but were limited to HF, MP2, and the B3LYP functional, in combination with the 6-31++G(3df,3pd) basis set. Using the MP2/6-31++G(3df,3pd) gas phase optimized structure, each species was then optimized fully in aqueous solution by using the polarizable continuum model (PCM) self-consistent reaction field approach, in which HF, MP2, and B3LYP levels of theory were utilized, with the same 6-31++G(3df,3pd) basis set. In both gas and aqueous solution phases, the keto form is higher in energy for all of the model chemistries considered. From the B3LYP/6-31++G(3df,3pd) Gibbs free energy, the keto-enol tautomeric equilibrium constant for 2,3-dihydroxycycloprop-2-en-1-one/3-hydroxy-1,2-cyclopropanedione is computed to be K-T(gas) = 2.768 X 10(-12) and K-T(aq) = 5.469 x 10(-14). It is concluded that the enol form is overwhelmingly predominant in both environments.
C1 [Tadic, Jovan M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Xu, Lai] Texas Tech Univ, Dept Chem & Biochem, Lubbock, TX 79409 USA.
RP Tadic, JM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM jotadic@lycos.com
RI Tadic, Jovan/P-3677-2016
FU NASA; Oak Ridge Associated Universities (ORAU); Serbian Ministry of
Education and Science [ON172035]
FX J.M.T. received support from the NASA Senior Postdoc Program amd Oak
Ridge Associated Universities (ORAU) and participates as a collaborator
in the project ON172035, funded by the Serbian Ministry of Education and
Science.
NR 49
TC 1
Z9 1
U1 1
U2 22
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0022-3263
J9 J ORG CHEM
JI J. Org. Chem.
PD OCT 5
PY 2012
VL 77
IS 19
BP 8621
EP 8626
DI 10.1021/jo301575c
PG 6
WC Chemistry, Organic
SC Chemistry
GA 073UF
UT WOS:000313767800026
PM 22954314
ER
PT J
AU Hurwitz, MM
Newman, PA
Garfinkel, CI
AF Hurwitz, M. M.
Newman, P. A.
Garfinkel, C. I.
TI On the influence of North Pacific sea surface temperature on the Arctic
winter climate
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID STRATOSPHERE; VARIABILITY; CIRCULATION; OSCILLATION; WARMINGS
AB Differences between two ensembles of Goddard Earth Observing System Chemistry-Climate Model simulations isolate the impact of North Pacific sea surface temperatures (SSTs) on the Arctic winter climate. One ensemble of extended winter season forecasts is forced by unusually high SSTs in the North Pacific, while in the second ensemble SSTs in the North Pacific are unusually low. High - Low differences are consistent with a strengthened Western Pacific atmospheric teleconnection pattern, and in particular, a weakening of the Aleutian low. This relative change in tropospheric circulation inhibits planetary wave propagation into the stratosphere, in turn reducing polar stratospheric temperature in mid- and late winter. The number of winters with sudden stratospheric warmings is approximately tripled in the Low ensemble as compared with the High ensemble. Enhanced North Pacific SSTs, and thus a more stable and persistent Arctic vortex, lead to a relative decrease in lower stratospheric ozone in spring, affecting the April clear-sky UV index at Northern Hemisphere midlatitudes.
C1 [Hurwitz, M. M.; Newman, P. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hurwitz, M. M.] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21239 USA.
[Garfinkel, C. I.] Johns Hopkins Univ, Baltimore, MD USA.
RP Hurwitz, MM (reprint author), NASA, Goddard Space Flight Ctr, Code 614, Greenbelt, MD 20771 USA.
EM margaret.m.hurwitz@nasa.gov
RI Newman, Paul/D-6208-2012; garfinkel, chaim/H-6215-2012
OI Newman, Paul/0000-0003-1139-2508; garfinkel, chaim/0000-0001-7258-666X
FU NASA's ACMAP program
FX The authors thank S. Frith for providing the updated TOMS/SBUV data and
processing the model output, M. Rex and P. von der Gathen for supplying
VPSC time series, A. Karpechko and three anonymous reviewers
for helpful comments, and NASA's ACMAP program for funding.
NR 34
TC 21
Z9 21
U1 2
U2 30
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 5
PY 2012
VL 117
AR D19110
DI 10.1029/2012JD017819
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 018HC
UT WOS:000309649900002
ER
PT J
AU Boening, C
Willis, JK
Landerer, FW
Nerem, RS
Fasullo, J
AF Boening, Carmen
Willis, Josh K.
Landerer, Felix W.
Nerem, R. Steven
Fasullo, John
TI The 2011 La Nina: So strong, the oceans fell
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SEA-LEVEL CHANGE; HEAT-CONTENT; EL-NINO; TOPEX/POSEIDON; TEMPERATURE;
VARIABILITY; BUDGET; SCALES; IMPACT; RISE
AB Global mean sea level (GMSL) dropped by 5 mm between the beginning of 2010 and mid 2011. This drop occurred despite the background rate of rise, 3 mm per year, which dominates most of the 18-year record observed by satellite altimeters. Using a combination of satellite and in situ data, we show that the decline in ocean mass, which explains the sea level drop, coincides with an equivalent increase in terrestrial water storage, primarily over Australia, northern South America, and Southeast Asia. This temporary shift of water from the ocean to land is closely related to the transition from El Nino conditions in 2009/10 to a strong 2010/11 La Nina, which affected precipitation patterns world-wide. Citation: Boening, C., J. K. Willis, F. W. Landerer, R. S. Nerem, and J. Fasullo (2012), The 2011 La Nina: So strong, the oceans fell, Geophys. Res. Lett., 39, L19602, doi:10.1029/2012GL053055.
C1 [Boening, Carmen; Willis, Josh K.; Landerer, Felix W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Nerem, R. Steven] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA.
[Fasullo, John] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
RP Boening, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM carmen.boening@jpl.nasa.gov
OI Landerer, Felix/0000-0003-2678-095X
FU NASA [NNX09AH89G-S01, NNG06GB91G]
FX We thank Michael McPhaden and an anonymous reviewer for their detailed
reviews and constructive comments that helped to improve the paper. The
work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA and is partially
sponsored by NASA awards NNX09AH89G-S01 and NNG06GB91G. 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 34
TC 86
Z9 89
U1 1
U2 53
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 OCT 4
PY 2012
VL 39
AR L19602
DI 10.1029/2012GL053055
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 017QT
UT WOS:000309606300001
ER
PT J
AU Garfinkel, CI
Butler, AH
Waugh, DW
Hurwitz, MM
Polvani, LM
AF Garfinkel, C. I.
Butler, A. H.
Waugh, D. W.
Hurwitz, M. M.
Polvani, L. M.
TI Why might stratospheric sudden warmings occur with similar frequency in
El Nino and La Nina winters?
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID MODEL; EVENTS; ATMOSPHERE
AB The effect of El Nino-Southern Oscillation (ENSO) on the frequency and character of Northern Hemisphere major mid-winter stratospheric sudden warmings (SSWs) is evaluated using a meteorological reanalysis data set and comprehensive chemistry-climate models. There is an apparent inconsistency between the impact of opposite phases of ENSO on the seasonal mean vortex and on SSWs: El Nino leads to an anomalously warm, and La Nina leads to an anomalously cool, seasonal mean polar stratospheric state, but both phases of ENSO lead to an increased SSW frequency. A resolution to this apparent paradox is here proposed: the region in the North Pacific most strongly associated with precursors of SSWs is not strongly influenced by El Nino and La Nina teleconnections. In the observational record, both La Nina and El Nino lead to similar anomalies in the region associated with precursors of SSWs and, consistent with this, there is a similar SSW frequency in La Nina and El Nino winters. A similar correspondence between the penetration of ENSO teleconnections into the SSW precursor region and SSW frequency is found in the comprehensive chemistry-climate models. The inability of some of the models to capture the observed relationship between La Nina and SSW frequency appears related to whether the modeled ENSO teleconnections result in extreme anomalies in the region most closely associated with SSWs. Finally, it is confirmed that the seasonal mean polar vortex response to ENSO is only weakly related to the relative frequency of SSWs during El Nino and La Nina.
C1 [Garfinkel, C. I.; Waugh, D. W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21209 USA.
[Butler, A. H.] NOAA, Climate Predict Ctr, NCEP, Camp Springs, MD USA.
[Hurwitz, M. M.] Morgan State Univ, Baltimore, MD 21239 USA.
[Hurwitz, M. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Polvani, L. M.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
[Polvani, L. M.] Columbia Univ, Dept Earth & Environm Sci, New York, NY USA.
[Polvani, L. M.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
RP Garfinkel, CI (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21209 USA.
EM cig4@jhu.edu
RI Butler, Amy/K-6190-2012; garfinkel, chaim/H-6215-2012; Waugh,
Darryn/K-3688-2016
OI Butler, Amy/0000-0002-3632-0925; garfinkel, chaim/0000-0001-7258-666X;
Waugh, Darryn/0000-0001-7692-2798
FU NASA [NNX06AE70G]; NSF [ATM 0905863]; US National Science Foundation
FX This work was supported by NASA grant NNX06AE70G and NSF grant ATM
0905863. The work of L. M. P. is funded, in part, by a grant of the US
National Science Foundation to Columbia University. We thank Andrew
Charlton-Perez for providing the SSW central dates for the CCMVal-2
models.
NR 47
TC 23
Z9 23
U1 1
U2 25
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 4
PY 2012
VL 117
AR D19106
DI 10.1029/2012JD017777
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 018HB
UT WOS:000309649800002
ER
PT J
AU Tierney, JE
Oppo, DW
LeGrande, AN
Huang, Y
Rosenthal, Y
Linsley, BK
AF Tierney, J. E.
Oppo, D. W.
LeGrande, A. N.
Huang, Y.
Rosenthal, Y.
Linsley, B. K.
TI The influence of Indian Ocean atmospheric circulation on Warm Pool
hydroclimate during the Holocene epoch
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID LAST GLACIAL MAXIMUM; SURFACE-TEMPERATURE; OXYGEN ISOTOPES;
PACIFIC-OCEAN; HYDROLOGY; AFRICAN; CLIMATE; MONSOON; MIDHOLOCENE;
PRECIPITATION
AB Existing paleoclimate data suggest a complex evolution of hydroclimate within the Indo-Pacific Warm Pool (IPWP) during the Holocene epoch. Here we introduce a new leaf wax isotope record from Sulawesi, Indonesia and compare proxy water isotope data with ocean-atmosphere general circulation model (OAGCM) simulations to identify mechanisms influencing Holocene IPWP hydroclimate. Modeling simulations suggest that orbital forcing causes heterogenous changes in precipitation across the IPWP on a seasonal basis that may account for the differences in time-evolution of the proxy data at respective sites. Both the proxies and simulations suggest that precipitation variability during the September-November (SON) season is important for hydroclimate in Borneo. The preeminence of the SON season suggests that a seasonally lagged relationship between the Indian monsoon and Indian Ocean Walker circulation influences IPWP hydroclimatic variability during the Holocene.
C1 [Tierney, J. E.; Oppo, D. W.] Woods Hole Oceanog Inst, Dept Geol & Geophys, Woods Hole, MA 02543 USA.
[LeGrande, A. N.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[LeGrande, A. N.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Huang, Y.] Brown Univ, Providence, RI 02912 USA.
[Rosenthal, Y.] Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08903 USA.
[Rosenthal, Y.] Rutgers State Univ, Dept Earth & Planetary Sci, New Brunswick, NJ 08903 USA.
[Linsley, B. K.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
RP Tierney, JE (reprint author), Woods Hole Oceanog Inst, Dept Geol & Geophys, 360 Woods Hole Rd, Woods Hole, MA 02543 USA.
EM tierney@whoi.edu
FU NOAA Climate and Global Change Postdoctoral Fellowship
FX We would like to thank T. Koutavas, E. Schefuss, and two anonymous
reviewers for discussion and comments that have greatly improved the
manuscript. We thank R. Tarozo at Brown University for assistance with
the delta Dwax analyses. We thank the climate modeling groups
participating in PMIP2 for providing their data for this analysis, and
the PMIP2 Data Archive (supported by CEA, CNRS, and PNEDC) for
distributing the data. The analyses were performed using version
02-08-2012 of the PMIP2 database. J. Tierney acknowledges the NOAA
Climate and Global Change Postdoctoral Fellowship for support.
NR 35
TC 13
Z9 14
U1 3
U2 43
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 4
PY 2012
VL 117
AR D19108
DI 10.1029/2012JD018060
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 018HB
UT WOS:000309649800005
ER
PT J
AU Haaser, RA
Earle, GD
Heelis, RA
Klenzing, J
Stoneback, R
Coley, WR
Burrell, AG
AF Haaser, R. A.
Earle, G. D.
Heelis, R. A.
Klenzing, J.
Stoneback, R.
Coley, W. R.
Burrell, A. G.
TI Characteristics of low-latitude ionospheric depletions and enhancements
during solar minimum
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID EQUATORIAL-SPREAD-F; DENSITY IRREGULARITIES; HINOTORI SATELLITE;
IMPEDANCE PROBE; PLASMA BUBBLES; VELOCITY; REGION; RADAR; BOARD
AB Under the waning solar minimum conditions during 2009 and 2010, the Ion Velocity Meter, part of the Coupled Ion Neutral Dynamics Investigation aboard the Communication/Navigation Outage Forecasting System satellite, is used to measure in situ nighttime ion densities and drifts at altitudes between 400 and 550 km during the hours 21:00-03:00 solar local time. A new approach to detecting and classifying well-formed ionospheric plasma depletions and enhancements (bubbles and blobs) with scale sizes between 50 and 500 km is used to develop geophysical statistics for the summer, winter, and equinox seasons during the quiet solar conditions. Some diurnal and seasonal geomagnetic distribution characteristics confirm previous work on equatorial irregularities and scintillations, while other elements reveal new behaviors that will require further investigation before they may be fully understood. Events identified in the study reveal very different and often opposite behaviors of bubbles and blobs during solar minimum. In particular, more bubbles demonstrating deeper density fluctuations and faster perturbation plasma drifts typically occur earlier near the magnetic equator, while blobs of similar magnitude occur more often far away from the geomagnetic equator closer to midnight.
C1 [Haaser, R. A.; Heelis, R. A.; Stoneback, R.; Coley, W. R.; Burrell, A. G.] Univ Texas Dallas, WB Hanson Ctr Space Sci, Richardson, TX 75080 USA.
[Earle, G. D.] Virginia Polytech Inst & State Univ, Ctr Space Sci & Engn, Blacksburg, VA 24061 USA.
[Klenzing, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Haaser, RA (reprint author), Univ Texas Dallas, WB Hanson Ctr Space Sci, 800 W Campbell Rd,WT-15, Richardson, TX 75080 USA.
EM rhaaser@utdallas.edu
RI Klenzing, Jeff/E-2406-2011;
OI Klenzing, Jeff/0000-0001-8321-6074; Burrell,
Angeline/0000-0001-8875-9326; Coley, William Robin/0000-0003-2047-0002;
Stoneback, Russell/0000-0001-7216-4336
FU NASA at the University of Texas at Dallas [NNX10AT02G]
FX This work is supported by NASA grant NNX10AT02G at the University of
Texas at Dallas.
NR 35
TC 6
Z9 6
U1 0
U2 11
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 OCT 4
PY 2012
VL 117
AR A10305
DI 10.1029/2012JA017814
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 017RT
UT WOS:000309609100001
ER
PT J
AU Rousseaux, CS
Gregg, WW
AF Rousseaux, Cecile S.
Gregg, Watson W.
TI Climate variability and phytoplankton composition in the Pacific Ocean
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID PLANKTON COMMUNITY STRUCTURE; EQUATORIAL PACIFIC; PRIMARY PRODUCTIVITY;
EL-NINO; CHLOROPHYLL; PIGMENTS; MODEL
AB The effect of climate variability on the phytoplankton community was assessed for the tropical and sub-tropical Pacific Ocean between 1998 and 2007 using an established biogeochemical assimilation model. The tropical and sub-tropical phytoplankton communities exhibited a wide range of responses to climate variability, from radical shifts in the Equatorial Pacific, to changes of only a couple of phytoplankton groups in the North Central Pacific, to no significant changes in the South Pacific. In the Equatorial Pacific, climate variability represented by ENSO dominated the variability of phytoplankton. Here, nitrate, chlorophyll and all of the 4 phytoplankton types (diatoms, cyanobacteria, chlorophytes and coccolithophores) were strongly correlated (p < 0.05) with the Multivariate El Nino Southern Oscillation Index (MEI). During La Nina events, diatoms increased and expanded westward along the cold tongue (correlation with MEI, r = -0.87, p < 0.05), while cyanobacteria concentrations decreased significantly (r = 0.69, p < 0.05). El Nino produced the reverse pattern, with cyanobacteria populations increasing while diatoms plummeted. In the North Central Pacific, the MEI was significantly correlated with diatoms (r = -0.40) and chlorophytes (r = -0.43). Ocean biology in the South Pacific was not significantly correlated with MEI. The phytoplankton composition from the assimilation model was compared to that from a new empirical algorithm using satellite data. Despite differences in the absolute concentration, the relative abundance from the model and the satellite-derived approach showed a similar shift in phytoplankton community in the Equatorial Pacific. These results highlight the spatially variable nature of the relationship between phytoplankton community structure and climate variability within the Pacific Ocean.
C1 [Rousseaux, Cecile S.; Gregg, Watson W.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Rousseaux, Cecile S.] Univ Space Res Assoc, Columbia, MD USA.
RP Rousseaux, CS (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Bldg 33,G105,Greenbelt Rd, Greenbelt, MD 20771 USA.
EM cecile.s.rousseaux@nasa.gov
RI Rousseaux, Cecile/E-8811-2012
OI Rousseaux, Cecile/0000-0002-3022-2988
FU NASA EOS; MAP Programs
FX We thank the NASA SeaWiFS project for providing the satellite
chlorophyll data and the NASA Center for Climate Simulation for
computational support. This project was funded by the NASA EOS and MAP
Programs.
NR 32
TC 14
Z9 14
U1 0
U2 60
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD OCT 4
PY 2012
VL 117
AR C10006
DI 10.1029/2012JC008083
PG 10
WC Oceanography
SC Oceanography
GA 017TM
UT WOS:000309613900002
ER
PT J
AU Lee, JE
Lintner, BR
Neelin, JD
Jiang, XA
Gentine, P
Boyce, CK
Fisher, JB
Perron, JT
Kubar, TL
Lee, J
Worden, J
AF Lee, Jung-Eun
Lintner, Benjamin R.
Neelin, J. David
Jiang, Xianan
Gentine, Pierre
Boyce, C. Kevin
Fisher, Joshua B.
Perron, J. Taylor
Kubar, Terence L.
Lee, Jeonghoon
Worden, John
TI Reduction of tropical land region precipitation variability via
transpiration
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SOIL-MOISTURE; CLIMATE MODELS; SIMULATIONS; SURFACE; OSCILLATION; STATES
AB Tropical rainforests are known to exhibit low intraseasonal precipitation variability compared with oceanic areas with similar mean precipitation in observations and models. In the present study, the potential role of transpiration for this difference in precipitation variability is investigated using the National Center for Atmospheric Research (NCAR) atmospheric general circulation model. Comparing model results with and without transpiration shows that in the absence of transpiration, mean precipitation decreases as may be expected. However the incidence of both higher daily total column water and more intense precipitation increases without transpiration; consequently the variability of precipitation increases substantially. These results can be understood in terms of the complex interplay of local near-surface and remote moist dynamical processes with both local positive (boundary-layer drying) and large-scale negative (increased large-scale convergence) feedbacks when transpiration is disabled in the model. It is also shown that surface turbulent fluxes over tropical rainforests are highly correlated with incoming solar energy but only weakly correlated with wind speed, possibly decoupling land precipitation from large-scale disturbances like the Madden-Julian Oscillation. Citation: Lee, J.-E., et al. (2012), Reduction of tropical land region precipitation variability via transpiration, Geophys. Res. Lett., 39, L19704, doi:10.1029/2012GL053417.
C1 [Lee, Jung-Eun; Fisher, Joshua B.; Worden, John] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lee, Jung-Eun] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Lintner, Benjamin R.] Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08903 USA.
[Neelin, J. David] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Neelin, J. David] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Gentine, Pierre] Columbia Univ, Dept Earth & Environm Engn, New York, NY USA.
[Boyce, C. Kevin] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
[Perron, J. Taylor] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA.
[Kubar, Terence L.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Lee, Jeonghoon] Polar Res Inst, Inchon, South Korea.
RP Lee, JE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 233-200, Pasadena, CA 91109 USA.
EM jung-eun.lee@jpl.nasa.gov
RI Lee, Jeonghoon/E-8116-2010; Perron, J. Taylor/D-8983-2012; Jiang,
Xianan/A-2283-2012;
OI Lee, Jeonghoon/0000-0002-1256-4431; Perron, J.
Taylor/0000-0002-0404-8701; Fisher, Joshua/0000-0003-4734-9085
FU NASA [NASA 07-NEWS07-20, NNH07ZDA001N-AST07-AST07-006]; NSF [NSF
AGS-1035968, NSF AGS-1102838, NSF AGS-1035843, NSF ATM-0934285]
FX The authors thank I. Held, D. Waliser and R. Pierrehumbert for their
encouragement and A. Sobel, H. -S. Park and anonymous reviewers for
reviewing earlier versions of this paper. The work described here is
performed at the Jet Propulsion Laboratory, California Institute of
Technology under contracts from the National Aeronautics and Space
Administration. The authors acknowledge supports from NASA (JEL: NASA
07-NEWS07-20 and NNH07ZDA001N-AST07-AST07-006) and NSF (BRL: NSF
AGS-1035968; JDN: NSF AGS-1102838; PG: NSF AGS-1035843; XJ: NSF
ATM-0934285).
NR 36
TC 12
Z9 12
U1 2
U2 22
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD OCT 3
PY 2012
VL 39
AR L19704
DI 10.1029/2012GL053417
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 017QP
UT WOS:000309605800005
ER
PT J
AU Weider, SZ
Nittler, LR
Starr, RD
McCoy, TJ
Stockstill-Cahill, KR
Byrne, PK
Denevi, BW
Head, JW
Solomon, SC
AF Weider, Shoshana Z.
Nittler, Larry R.
Starr, Richard D.
McCoy, Timothy J.
Stockstill-Cahill, Karen R.
Byrne, Paul K.
Denevi, Brett W.
Head, James W.
Solomon, Sean C.
TI Chemical heterogeneity on Mercury's surface revealed by the MESSENGER
X-Ray Spectrometer
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID ASTEROID 433 EROS; ENSTATITE CHONDRITES; ELEMENTAL COMPOSITION;
FLUORESCENCE OBSERVATIONS; PHASE-RELATIONS; PARENT BODY; EMISSION;
FLYBY; VOLCANISM; EXOSPHERE
AB We present the analysis of 205 spatially resolved measurements of the surface composition of Mercury from MESSENGER's X-Ray Spectrometer. The surface footprints of these measurements are categorized according to geological terrain. Northern smooth plains deposits and the plains interior to the Caloris basin differ compositionally from older terrain on Mercury. The older terrain generally has higher Mg/Si, S/Si, and Ca/Si ratios, and a lower Al/Si ratio than the smooth plains. Mercury's surface mineralogy is likely dominated by high-Mg mafic minerals (e.g., enstatite), plagioclase feldspar, and lesser amounts of Ca, Mg, and/or Fe sulfides (e.g., oldhamite). The compositional difference between the volcanic smooth plains and the older terrain reflects different abundances of these minerals and points to the crystallization of the smooth plains from a more chemically evolved magma source. High-degree partial melts of enstatite chondrite material provide a generally good compositional and mineralogical match for much of the surface of Mercury. An exception is Fe, for which the low surface abundance on Mercury is still higher than that of melts from enstatite chondrites and may indicate an exogenous contribution from meteoroid impacts.
C1 [Weider, Shoshana Z.; Nittler, Larry R.; Byrne, Paul K.; Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Starr, Richard D.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[McCoy, Timothy J.; Stockstill-Cahill, Karen R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
[Denevi, Brett W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Geol Observ, Palisades, NY 10964 USA.
RP Weider, SZ (reprint author), Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA.
EM sweider@ciw.edu
RI Denevi, Brett/I-6502-2012;
OI Denevi, Brett/0000-0001-7837-6663; Weider, Shoshana/0000-0003-1034-909X
FU NASA Discovery Program [NAS5-97271, NASW-00002]
FX The authors thank Denton Ebel and an anonymous reviewer for constructive
reviews of an earlier version of this paper. We thank the MESSENGER team
for the development, cruise, orbit insertion, and orbital operations of
the MESSENGER spacecraft. This work is supported by the NASA Discovery
Program under contract NAS5-97271 to The Johns Hopkins University
Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of
Washington. S.Z.W. thanks Frances E. Jenner for helpful discussions
during manuscript preparation.
NR 79
TC 76
Z9 76
U1 0
U2 25
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 OCT 3
PY 2012
VL 117
AR E00L05
DI 10.1029/2012JE004153
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 017TK
UT WOS:000309613700002
ER
PT J
AU Schulz, M
Prospero, JM
Baker, AR
Dentener, F
Ickes, L
Liss, PS
Mahowald, NM
Nickovic, S
Garcia-Pando, CP
Rodriguez, S
Sarin, M
Tegen, I
Duce, RA
AF Schulz, Michael
Prospero, Joseph M.
Baker, Alex R.
Dentener, Frank
Ickes, Luisa
Liss, Peter S.
Mahowald, Natalie M.
Nickovic, Slobodan
Garcia-Pando, Carlos Perez
Rodriguez, Sergio
Sarin, Manmohan
Tegen, Ina
Duce, Robert A.
TI Atmospheric Transport and Deposition of Mineral Dust to the Ocean:
Implications for Research Needs
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID DRY AEOLIAN DEPOSITION; IRON SOLUBILITY; DESERT DUST; ATLANTIC-OCEAN;
NORTH-ATLANTIC; AEROSOL INTERACTIONS; PARTICLE DEPOSITION; GLOBAL
DISTRIBUTION; SIZE DISTRIBUTIONS; HARMATTAN DUST
AB This paper reviews our knowledge of the measurement and modeling of mineral dust emissions to the atmosphere, its transport and deposition to the ocean, the release of iron from the dust into seawater, and the possible impact of that nutrient on marine biogeochemistry and climate. Of particular concern is our poor understanding of the mechanisms and quantities of dust deposition as well as the extent of iron solubilization from the dust once it enters the ocean. Model estimates of dust deposition in remote oceanic regions vary by more than a factor of 10. The fraction of the iron in dust that is available for use by marine phytoplankton is still highly uncertain. There is an urgent need for a long-term marine atmospheric surface measurement network, spread across all oceans. Because the southern ocean is characterized by large areas with high nitrate but low chlorophyll surface concentrations, that region is particularly sensitive to the input of dust and iron. Data from this region would be valuable, particularly at sites downwind from known dust source areas in South America, Australia, and South Africa. Coordinated field experiments involving both atmospheric and marine measurements are recommended to address the complex and interlinked processes and role of dust/Fe fertilization on marine biogeochemistry and climate.
C1 [Schulz, Michael] Norwegian Meteorol Inst, Oslo, Norway.
[Prospero, Joseph M.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA.
[Baker, Alex R.; Liss, Peter S.] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England.
[Dentener, Frank] Commiss European Communities, JRC, Inst Environm & Sustainabil, Ispra, Italy.
[Ickes, Luisa; Nickovic, Slobodan] World Meteorol Org, Geneva, Switzerland.
[Mahowald, Natalie M.] Cornell Univ, Ithaca, NY USA.
[Garcia-Pando, Carlos Perez] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Rodriguez, Sergio] Izana Atmospher Res Ctr, Santa Cruz De Tenerife, Spain.
[Sarin, Manmohan] Phys Res Lab, Dept Planetary & Geosci, Ahmadabad 380009, Gujarat, India.
[Tegen, Ina] Leibniz Inst Tropospher Res, Leipzig, Germany.
[Duce, Robert A.] Texas A&M Univ, Dept Oceanog, College Stn, TX 77843 USA.
[Duce, Robert A.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX USA.
RP Schulz, M (reprint author), Norwegian Meteorol Inst, Oslo, Norway.
EM michael.schulz@met.no
RI Baker, Alex/D-1233-2011; LISS, Peter/A-8219-2013; Duce,
Robert/A-9917-2010; Mahowald, Natalie/D-8388-2013; Schulz,
Michael/A-6930-2011; Rodriguez, Sergio/J-5365-2015;
OI Baker, Alex/0000-0002-8365-8953; Mahowald, Natalie/0000-0002-2873-997X;
Schulz, Michael/0000-0003-4493-4158; Rodriguez,
Sergio/0000-0002-1727-3107; Prospero, Joseph/0000-0003-3608-6160; Perez
Garcia-Pando, Carlos/0000-0002-4456-0697
FU World Meteorological Organization (WMO); International Maritime
Organization (IMO); Swedish International Development Agency (SIDA)
FX This paper resulted from the deliberations of GESAMP Working Group 38,
The Atmospheric Input of Chemicals to the ocean with input from members
of the WMO Sand and Dust Storm Warning and Advisory System WMO-SDS. We
thank the Global Atmosphere Watch (GAW) and the World Weather Research
Programme (WWRP) of the World Meteorological Organization (WMO), the
International Maritime Organization (IMO), and the Swedish International
Development Agency (SIDA) for support. The authors are grateful to the
participants of the joint workshop in Malta, 7-9 March 2011 in between
the GESAMP Working Group 38 and the WMO-SDS that has led to the
discussion foundations of the present paper.
NR 168
TC 56
Z9 56
U1 12
U2 156
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
EI 1520-5851
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD OCT 2
PY 2012
VL 46
IS 19
BP 10390
EP 10404
DI 10.1021/es300073u
PG 15
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA 015FG
UT WOS:000309431200003
PM 22994868
ER
PT J
AU Mrowiec, AA
Rio, C
Fridlind, AM
Ackerman, AS
Del Genio, AD
Pauluis, OM
Varble, AC
Fan, JW
AF Mrowiec, Agnieszka A.
Rio, Catherine
Fridlind, Ann M.
Ackerman, Andrew S.
Del Genio, Anthony D.
Pauluis, Olivier M.
Varble, Adam C.
Fan, Jiwen
TI Analysis of cloud-resolving simulations of a tropical mesoscale
convective system observed during TWP-ICE: Vertical fluxes and draft
properties in convective and stratiform regions
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID COMMUNITY CLIMATE MODEL; 1985 SQUALL LINE; TOGA-COARE; CUMULUS
CONVECTION; VELOCITY CHARACTERISTICS; OCEANIC CONVECTION; MOISTURE
BUDGETS; DIURNAL CYCLE; MASS FLUXES; C-POL
AB We analyze three cloud-resolving model simulations of a strong convective event observed during the TWP-ICE campaign, differing in dynamical core, microphysical scheme or both. Based on simulated and observed radar reflectivity, simulations roughly reproduce observed convective and stratiform precipitating areas. To identify the characteristics of convective and stratiform drafts that are difficult to observe but relevant to climate model parameterization, independent vertical wind speed thresholds are calculated to capture 90% of total convective and stratiform updraft and downdraft mass fluxes. Convective updrafts are fairly consistent across simulations (likely owing to fixed large-scale forcings and surface conditions), except that hydrometeor loadings differ substantially. Convective downdraft and stratiform updraft and downdraft mass fluxes vary notably below the melting level, but share similar vertically uniform draft velocities despite differing hydrometeor loadings. All identified convective and stratiform downdrafts contain precipitation below similar to 10 km and nearly all updrafts are cloudy above the melting level. Cold pool properties diverge substantially in a manner that is consistent with convective downdraft mass flux differences below the melting level. Despite differences in hydrometeor loadings and cold pool properties, convective updraft and downdraft mass fluxes are linearly correlated with convective area, the ratio of ice in downdrafts to that in updrafts is similar to 0.5 independent of species, and the ratio of downdraft to updraft mass flux is similar to 0.5-0.6, which may represent a minimum evaporation efficiency under moist conditions. Hydrometeor loading in stratiform regions is found to be a fraction of hydrometeor loading in convective regions that ranges from similar to 10% (graupel) to similar to 90% (cloud ice). These findings may lead to improved convection parameterizations.
C1 [Mrowiec, Agnieszka A.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
[Mrowiec, Agnieszka A.; Fridlind, Ann M.; Ackerman, Andrew S.; Del Genio, Anthony D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Rio, Catherine] CNRS IPSL, Meteorol Dynam Lab, Paris, France.
[Pauluis, Olivier M.] NYU, Courant Inst Math Sci, New York, NY USA.
[Varble, Adam C.] Univ Utah, Dept Atmospher Sci, Salt Lake City, UT USA.
[Fan, Jiwen] Pacific NW Natl Lab, Richland, WA 99352 USA.
RP Mrowiec, AA (reprint author), Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10025 USA.
EM as3845@columbia.edu
RI Ackerman, Andrew/D-4433-2012; Fan, Jiwen/E-9138-2011
OI Ackerman, Andrew/0000-0003-0254-6253;
FU DOE Office of Science, Office of Biological and Environmental Research
[DE-PS02-09ER09-01, DE-AI02-06ER64173, DE-AI02-08ER64547]; DOE
Atmospheric System Research Program; NASA Radiation Sciences Program;
DOE Office of Science, Office of Biological and Environmental Research,
Environmental Science Division
FX This research was supported by the DOE Office of Science, Office of
Biological and Environmental Research, through contracts
DE-PS02-09ER09-01 (Mrowiec), DE-AI02-06ER64173 and DE-AI02-08ER64547
(Rio, Fridlind, Ackerman), by the DOE Atmospheric System Research
Program (Del Genio and Fan), and by the NASA Radiation Sciences Program.
Computational support was provided by the DOE National Energy Research
Scientific Computing Center and the NASA Advanced Supercomputing
Division. TWP-ICE data were obtained from the ARM program archive,
sponsored by the DOE Office of Science, Office of Biological and
Environmental Research, Environmental Science Division. We thank two
anonymous reviewers for helpful comments.
NR 93
TC 12
Z9 13
U1 0
U2 16
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 2
PY 2012
VL 117
AR D19201
DI 10.1029/2012JD017759
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 018GZ
UT WOS:000309649600002
ER
PT J
AU Ackermann, M
Koriabine, M
Hartmann-Fritsch, F
de Jong, PJ
Lewis, TD
Schetle, N
Work, TM
Dagenais, J
Balazs, GH
Leong, JAC
AF Ackermann, Mathias
Koriabine, Maxim
Hartmann-Fritsch, Fabienne
de Jong, Pieter J.
Lewis, Teresa D.
Schetle, Nelli
Work, Thierry M.
Dagenais, Julie
Balazs, George H.
Leong, Jo-Ann C.
TI The Genome of Chelonid Herpesvirus 5 Harbors Atypical Genes
SO PLOS ONE
LA English
DT Article
ID BACTERIAL ARTIFICIAL CHROMOSOME; MARINE TURTLE HERPESVIRUS;
VARICELLA-ZOSTER-VIRUS; COMPLETE DNA-SEQUENCE; GREEN TURTLES; BOVINE
HERPESVIRUS-1; CELL-SURFACE; IN-VITRO; FIBROPAPILLOMATOSIS; MYDAS
AB The Chelonid fibropapilloma-associated herpesvirus (CFPHV; ChHV5) is believed to be the causative agent of fibropapillomatosis (FP), a neoplastic disease of marine turtles. While clinical signs and pathology of FP are well known, research on ChHV5 has been impeded because no cell culture system for its propagation exists. We have cloned a BAC containing ChHV5 in pTARBAC2.1 and determined its nucleotide sequence. Accordingly, ChHV5 has a type D genome and its predominant gene order is typical for the varicellovirus genus within the alphaherpesvirinae. However, at least four genes that are atypical for an alphaherpesvirus genome were also detected, i.e. two members of the C-type lectin-like domain superfamily (F-lec1, F-lec2), an orthologue to the mouse cytomegalovirus M04 (F-M04) and a viral sialyltransferase (F-sial). Four lines of evidence suggest that these atypical genes are truly part of the ChHV5 genome: (1) the pTARBAC insertion interrupted the UL52 ORF, leaving parts of the gene to either side of the insertion and suggesting that an intact molecule had been cloned. (2) Using FP-associated UL52 (F-UL52) as an anchor and the BAC-derived sequences as a means to generate primers, overlapping PCR was performed with tumor-derived DNA as template, which confirmed the presence of the same stretch of "atypical" DNA in independent FP cases. (3) Pyrosequencing of DNA from independent tumors did not reveal previously undetected viral sequences, suggesting that no apparent loss of viral sequence had happened due to the cloning strategy. (4) The simultaneous presence of previously known ChHV5 sequences and F-sial as well as F-M04 sequences was also confirmed in geographically distinct Australian cases of FP. Finally, transcripts of F-sial and F-M04 but not transcripts of lytic viral genes were detected in tumors from Hawaiian FP-cases. Therefore, we suggest that F-sial and F-M04 may play a role in FP pathogenesis.
C1 [Ackermann, Mathias; Hartmann-Fritsch, Fabienne; Schetle, Nelli] Univ Zurich, Inst Virol, Zurich, Switzerland.
[Koriabine, Maxim; de Jong, Pieter J.] Childrens Hosp Oakland, Res Inst, BACPAC Resources Ctr, Oakland, CA 94609 USA.
[Work, Thierry M.; Dagenais, Julie] US Geol Survey, Natl Wildlife Hlth Ctr Honolulu Field Stn, Honolulu, HI USA.
[Balazs, George H.] Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI USA.
[Lewis, Teresa D.; Leong, Jo-Ann C.] Univ Hawaii Manoa, Hawaii Inst Marine Biol, Kaneohe, HI USA.
RP Ackermann, M (reprint author), Univ Zurich, Inst Virol, Zurich, Switzerland.
EM email@vetvir.uzh.ch
RI Work, Thierry/F-1550-2015
OI Work, Thierry/0000-0002-4426-9090
FU Hawaii Institute of Marine Biology; NSF EPSCoR; NOAA [2005-008/682];
Pfizer; UZH Stiftung fur wissenschaftliche Forschung
FX The authors acknowledge support provided by the Hawaii Institute of
Marine Biology Core Sequencing Facility, which is funded by the NSF
EPSCoR program, Investing in Multidisciplinary University Activities,
and the support provided by NOAA funds to the Hawaii Institute of Marine
Biology-Northwestern Hawaiian Islands Coral Reef Ecosystem Reserve
Partnership, MOA #2005-008/682. Financial support for MA's work was
based on MA's Pfizer Award 2000, a grant to MA from the UZH Stiftung fur
wissenschaftliche Forschung
(http://www.researchers.uzh.ch/support/stwf.html), and a donation to MA
from Martha Ackermann Kaiser. This paper is listed as HIMB contribution
#1293. The funders had no role in study design, data collection and
analysis, decision to publish, or preparation of the manuscript.
NR 58
TC 10
Z9 11
U1 1
U2 18
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD OCT 2
PY 2012
VL 7
IS 10
AR e46623
DI 10.1371/journal.pone.0046623
PG 15
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 015NG
UT WOS:000309452600046
PM 23056373
ER
PT J
AU Sultana, J
Kazanas, D
Said, JL
AF Sultana, Joseph
Kazanas, Demosthenes
Said, Jackson Levi
TI Conformal Weyl gravity and perihelion precession
SO PHYSICAL REVIEW D
LA English
DT Article
ID COSMOLOGICAL CONSTANT; LIGHT DEFLECTION
AB We investigate the perihelion shift of planetary motion in conformal Weyl gravity using the metric of the static, spherically symmetric solution discovered by Mannheim and Kazanas [Astrophys. J. 342, 635 (1989)]. To this end we employ a procedure similar to that used by Weinberg for the Schwarzschild solution, which has also been used recently to study the solar system effects of the cosmological constant Lambda. We show that besides the general relativistic terms obtained earlier from the Schwarzschild-de Sitter solution, the expression for the perihelion shift includes a negative contribution which arises from the linear term gamma r in the metric. Using data for perihelion shift observations, we obtain constraints on the value of the constant gamma similar to that obtained earlier using galactic rotational curves.
C1 [Sultana, Joseph] Univ Malta, Dept Math, Msida, Malta.
[Kazanas, Demosthenes] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Said, Jackson Levi] Univ Malta, Dept Phys, Msida, Malta.
RP Sultana, J (reprint author), Univ Malta, Dept Math, Msida, Malta.
EM joseph.sultana@um.edu.mt; demos.kazanas@nasa.gov; jsai0004@um.edu.mt
FU University of Malta
FX J. S. gratefully acknowledges financial support from the University of
Malta during his visit at NASA-GSFC.
NR 28
TC 13
Z9 13
U1 1
U2 5
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD OCT 2
PY 2012
VL 86
IS 8
AR 084008
DI 10.1103/PhysRevD.86.084008
PG 5
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 014PA
UT WOS:000309386800004
ER
PT J
AU Swan, JW
Vasquez, PA
Whitson, PA
Fincke, EM
Wakata, K
Magnus, SH
De Winne, F
Barratt, MR
Agui, JH
Green, RD
Hall, NR
Bohman, DY
Bunnell, CT
Gast, AP
Furst, EM
AF Swan, James W.
Vasquez, Paula A.
Whitson, Peggy A.
Fincke, E. Michael
Wakata, Koichi
Magnus, Sandra H.
De Winne, Frank
Barratt, Michael R.
Agui, Juan H.
Green, Robert D.
Hall, Nancy R.
Bohman, Donna Y.
Bunnell, Charles T.
Gast, Alice P.
Furst, Eric M.
TI Multi-scale kinetics of a field-directed colloidal phase transition
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE magneto-rheological fluid; microgravity science; complex fluids
ID ELECTRORHEOLOGICAL FLUIDS; MAGNETORHEOLOGICAL FLUID; MAGNETIC-FIELD;
SUSPENSIONS; DYNAMICS; GELATION
AB Polarizable colloids are expected to form crystalline equilibrium phases when exposed to a steady, uniform field. However, when colloids become localized this field-induced phase transition arrests and the suspension persists indefinitely as a kinetically trapped, percolated structure. We anneal such gels formed from magneto-rheological fluids by toggling the field strength at varied frequencies. This processing allows the arrested structure to relax periodically to equilibrium-colloid-rich, cylindrical columns. Two distinct growth regimes are observed: one in which particle domains ripen through diffusive relaxation of the gel, and the other where the system-spanning structure collapses and columnar domains coalesce apparently through field-driven interactions. There is a stark boundary as a function of magnetic field strength and toggle frequency distinguishing the two regimes. These results demonstrate how kinetic barriers to a colloidal phase transition are subverted through measured, periodic variation of driving forces. Such directed assembly may be harnessed to create unique materials from dispersions of colloids.
C1 [Swan, James W.; Vasquez, Paula A.; Furst, Eric M.] Univ Delaware, Dept Chem & Biomol Engn, Newark, DE 19716 USA.
[Swan, James W.; Vasquez, Paula A.; Furst, Eric M.] Univ Delaware, Ctr Mol & Engn Thermodynam, Allan P Colburn Lab, Newark, DE 19716 USA.
[Whitson, Peggy A.; Fincke, E. Michael; Wakata, Koichi; Magnus, Sandra H.; Barratt, Michael R.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[De Winne, Frank] European Space Agcy, D-51147 Cologne, Germany.
[Agui, Juan H.; Green, Robert D.; Hall, Nancy R.; Bohman, Donna Y.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Bunnell, Charles T.] Zin Technol Inc, Cleveland, OH 44130 USA.
[Gast, Alice P.] Lehigh Univ, Off President, Bethlehem, PA 18015 USA.
[Gast, Alice P.] Lehigh Univ, Dept Chem Engn, Bethlehem, PA 18015 USA.
RP Furst, EM (reprint author), Univ Delaware, Dept Chem & Biomol Engn, 150 Acad St, Newark, DE 19716 USA.
EM furst@udel.edu
FU NASA [NAG3-1887, NAG3-2398, NAG3-2832, NNX07AD02G]
FX Support from NASA (grant nos. NAG3-1887, NAG3-2398, NAG3-2832 and
NNX07AD02G) is gratefully acknowledged.
NR 30
TC 19
Z9 19
U1 2
U2 52
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 OCT 2
PY 2012
VL 109
IS 40
BP 16023
EP 16028
DI 10.1073/pnas.1206915109
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 017SN
UT WOS:000309611400023
PM 22988079
ER
PT J
AU Bringsjord, S
Clark, MH
AF Bringsjord, Selmer
Clark, Micah H.
TI Red-Pill Robots Only, Please
SO IEEE TRANSACTIONS ON AFFECTIVE COMPUTING
LA English
DT Article
DE Robots; red pill; blue pill; deception; pleasure; truth
AB Blue-pill robots are engineered to deceive (perhaps in an attempt to secure desirable ends). Red-pill robots, on the other hand, are built to do no violence to truth. While "taking the blue pill" is an option some select, this path, in the context of present and future robotics, is an exceedingly bad one by our lights, and we herein defend this position by attempting to show that the production of blue-pill robots via engineering as we know it should be avoided.
C1 [Bringsjord, Selmer] Rensselaer Polytech Inst, Dept Comp Sci, Dept Cognit Sci, Troy, NY 12180 USA.
[Bringsjord, Selmer] Rensselaer Polytech Inst, Lally Sch Management & Technol, Troy, NY 12180 USA.
[Clark, Micah H.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
[Clark, Micah H.] Rensselaer Polytech Inst, Rensselar AI & Reasoning Lab, Troy, NY 12180 USA.
RP Bringsjord, S (reprint author), Rensselaer Polytech Inst, Dept Comp Sci, Dept Cognit Sci, Troy, NY 12180 USA.
EM selmer@rpi.edu; micah.h.clark@jpl.nasa.gov
NR 22
TC 0
Z9 0
U1 2
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1949-3045
J9 IEEE T AFFECT COMPUT
JI IEEE Trans. Affect. Comput.
PD OCT-DEC
PY 2012
VL 3
IS 4
BP 394
EP 397
DI 10.1109/T-AFFC.2011.35
PG 4
WC Computer Science, Artificial Intelligence; Computer Science, Cybernetics
SC Computer Science
GA 207YX
UT WOS:000323642000003
ER
PT J
AU Metzger, BD
Giannios, D
Spiegel, DS
AF Metzger, B. D.
Giannios, D.
Spiegel, D. S.
TI Optical and X-ray transients from planet-star mergers
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; novae, cataclysmic variables; planetary
systems; X-rays: stars
ID SPIN-ORBIT MISALIGNMENT; COMPACT-OBJECT MERGERS; GAS GIANT PLANETS;
EXTRASOLAR PLANETS; BROWN DWARFS; HOT JUPITERS; BLACK-HOLES; V838
MONOCEROTIS; TIDAL DISRUPTION; STELLAR MERGER
AB We evaluate the prompt electromagnetic signatures of the merger between a massive close-in planet (a 'hot Jupiter') and its host star, events with an estimated Galactic rate of similar to 0.1-1 yr-(1.) Depending on the ratio of the mean density of the planet (rho) over bar (p) to that of the star (rho) over bar (star), a planet-star merger results in three possible outcomes. If (rho) over bar (p)/(rho) over bar (star) greater than or similar to 5, then the planet directly plunges below the stellar atmosphere before being disrupted by tidal forces. The dissipation of orbital energy creates a hot wake behind the planet, producing a extreme ultraviolet (EUV)/soft X-ray transient that increases in brightness and temperature as the planet sinks below the stellar surface. The peak luminosity L-EUV/X less than or similar to 10(36) erg s(-1) is achieved weeks to months prior to merger, after which the stellar surface is enshrouded by an outflow driven by the merger. The final stages of the inspiral are accompanied by an optical transient powered by the recombination of hydrogen in the outflow, which peaks at a luminosity of similar to 10(37)-10(38) erg s(-1) on a time-scale similar to days.
If the star is instead significantly denser ((rho) over bar (p)/(rho) over bar (star) less than or similar to 5), then the planet overflows its Roche lobe above the stellar surface. For (rho) over bar (p)/(rho) over bar (star) less than or similar to 1 mass transfer is stable, resulting in the planet being accreted on the relatively slow time-scale set by tidal dissipation. However, for an intermediate-density range 1 less than or similar to (rho) over bar (p)/(rho) over bar (star) less than or similar to 5 mass transfer may instead be unstable, resulting in the dynamical disruption of the planet into an accretion disc around the star. Outflows from the super-Eddington accretion disc power an optical transient with a peak luminosity of similar to 10(37)-10(38) erg s(-1) and characteristic duration similar to week-months. Emission from the disc itself becomes visible once the accretion rate decreases below the Eddington rate, resulting in a bolometric brightening and shift of the spectral peak to ultraviolet (UV) wavelengths. Optical transients from both direct-impact merger and tidal-disruption events in some ways resemble classical novae, but can be distinguished by their higher ejecta mass and lower velocity around hundreds of km s(-1), and by hard pre- and post-cursor emission, respectively. The most promising search strategy is with combined surveys of nearby massive galaxies (e.g. M31) at optical, UV and X-ray wavelengths with cadences from days to months.
C1 [Metzger, B. D.; Giannios, D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Spiegel, D. S.] Inst Adv Study, Princeton, NJ 08540 USA.
RP Metzger, BD (reprint author), NASA, Washington, DC 20546 USA.
EM bmetzger@astro.princeton.edu; giannios@astro.princeton.edu; dave@ias.edu
FU NASA [PF9-00065, NAS8-03060]; Chandra X-ray Center; Fermi 4 Cycle grant
[041305]; NSF [AST-0807444]; Keck Fellowship
FX BDM is supported by NASA through Einstein Postdoctoral Fellowship grant
number PF9-00065 awarded by the Chandra X-ray Center, which is operated
by the Smithsonian Astrophysical Observatory for NASA under contract
NAS8-03060. DG acknowledges support from the Fermi 4 Cycle grant number
041305. DSS gratefully acknowledges support from NSF grant AST-0807444
and the Keck Fellowship.
NR 97
TC 17
Z9 17
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2012
VL 425
IS 4
BP 2778
EP 2798
DI 10.1111/j.1365-2966.2012.21444.x
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 135EN
UT WOS:000318270500014
ER
PT J
AU Minnis, P
Hong, G
Ayers, JK
Smith, WL
Yost, CR
Heymsfield, AJ
Heymsfield, GM
Hlavka, DL
King, MD
Korn, E
McGill, MJ
Selkirk, HB
Thompson, AM
Tian, L
Yang, P
AF Minnis, Patrick
Hong, Gang
Ayers, J. Kirk
Smith, William L., Jr.
Yost, Christopher R.
Heymsfield, Andrew J.
Heymsfield, Gerald M.
Hlavka, Dennis L.
King, Michael D.
Korn, Errol
McGill, Matthew J.
Selkirk, Henry B.
Thompson, Anne M.
Tian, Lin
Yang, Ping
TI Simulations of Infrared Radiances over a Deep Convective Cloud System
Observed during TC4: Potential for Enhancing Nocturnal Ice Cloud
Retrievals
SO REMOTE SENSING
LA English
DT Article
DE clouds; optical depth; particle size; satellite; TC4; multispectral
thermal infrared
ID CIRRUS CLOUD; WINDOW REGION; WATER-CONTENT; PART I; TEMPERATURE; RADAR;
SCATTERING; MODIS; ABSORPTION; RADIOMETER
AB Retrievals of ice cloud properties using infrared measurements at 3.7, 6.7, 7.3, 8.5, 10.8, and 12.0 mu m can provide consistent results regardless of solar illumination, but are limited to cloud optical thicknesses tau < similar to 6. This paper investigates the variations in radiances at these wavelengths over a deep convective cloud system for their potential to extend retrievals of tau and ice particle size D-e to optically thick clouds. Measurements from an imager, an interferometer, the Cloud Physics Lidar (CPL), and the Cloud Radar System (CRS) aboard the NASA ER-2 aircraft during the NASA TC4 (Tropical Composition, Cloud and Climate Coupling) experiment flight during 5 August 2007, are used to examine the retrieval potential of infrared radiances over optically thick ice clouds. Simulations based on coincident in situ measurements and combined cloud tau from CRS and CPL measurements are comparable to the observations. They reveal that brightness temperatures at these bands and their differences (BTD) are sensitive to tau up to similar to 20 and that for ice clouds having tau > 20, the 3.7-10.8 mu m and 3.7-6.7 mu m BTDs are the most sensitive to D-e. Satellite imagery appears to be consistent with these results suggesting that t and D-e could be retrieved for greater optical thicknesses than previously assumed. But, because of sensitivity of the BTDs to uncertainties in the atmospheric profiles of temperature, humidity, and ice water content, and sensor noise, exploiting the small BTD signals in retrieval algorithms will be very challenging.
C1 [Minnis, Patrick; Smith, William L., Jr.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Hong, Gang; Ayers, J. Kirk; Yost, Christopher R.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Heymsfield, Andrew J.; Korn, Errol] Natl Ctr Atmospher Res, Earth Syst Lab, Boulder, CO 80301 USA.
[Heymsfield, Gerald M.; McGill, Matthew J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hlavka, Dennis L.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[King, Michael D.] Univ Colorado, LASP, Boulder, CO 80309 USA.
[Selkirk, Henry B.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Thompson, Anne M.] Penn State Univ, Dept Meteorol, State Coll, PA 16802 USA.
[Tian, Lin] Morgan State Univ, GESTAR, Baltimore, MD 21251 USA.
[Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
RP Minnis, P (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM p.minnis@nasa.gov; gang.hong@nasa.gov; j.k.ayers@nasa.gov;
william.l.smith@nasa.gov; christopher.r.yost@nasa.gov; heyms1@ucar.edu;
gerald.m.heymsfield@nasa.gov; dennis.l.hlavka@nasa.gov;
Michael.king@lasp.colorado.edu; korn@ucar.edu;
matthew.j.mcgill@nasa.gov; henry.b.selkirk@nasa.gov;
amt16@meteo.psu.edu; lin.tian-1@nasa.gov; pyang@ariel.met.tamu.edu
RI King, Michael/C-7153-2011; Yang, Ping/B-4590-2011; Heymsfield,
Andrew/E-7340-2011; Minnis, Patrick/G-1902-2010; Thompson, Anne
/C-3649-2014
OI King, Michael/0000-0003-2645-7298; Minnis, Patrick/0000-0002-4733-6148;
Thompson, Anne /0000-0002-7829-0920
FU NASA Modeling, Analysis, and Prediction Program; NASA CERES;
TC4; NOAA GOES-R Program
FX We thank Hank Revercomb and the S-HIS research team and Sarah T. Bedka
for providing the S-HIS data, June Wang and Kathryn Young for processing
the dropsonde data, and L. Li for help on the CRS data. The MASTER data
are archived at http://masterweb.jpl.nasa.gov/data/, and the CRS
measurements and Alajuela sounding were obtained at
http://espoarchive.nasa.gov/archive/arcs/tc4/. This research was
supported by the NASA Modeling, Analysis, and Prediction Program; the
NASA CERES, TC4, and High Ice Water Content projects; and the
NOAA GOES-R Program. Thanks also to the three anonymous reviewers who
helped improve this manuscript.
NR 70
TC 8
Z9 8
U1 0
U2 14
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD OCT
PY 2012
VL 4
IS 10
BP 3022
EP 3054
DI 10.3390/rs4103022
PG 33
WC Remote Sensing
SC Remote Sensing
GA 075VC
UT WOS:000313914100008
ER
PT J
AU Raj, R
Kim, J
McQuillen, J
AF Raj, Rishi
Kim, Jungho
McQuillen, John
TI Pool Boiling Heat Transfer on the International Space Station:
Experimental Results and Model Verification
SO JOURNAL OF HEAT TRANSFER-TRANSACTIONS OF THE ASME
LA English
DT Article
DE Pool boiling; microgravity; gravity scaling
ID MICROGRAVITY; CYLINDERS; FLUX
AB The relatively poor understanding of gravity effects on pool boiling heat transfer can be attributed to the lack of long duration high-quality microgravity data, g-jitter associated with ground-based low gravity facilities, little data at intermediate gravity levels, and a poor understanding of the effect of important parameters even at earth gravity conditions. The results of over 200 pool boiling experiments with n-perfluorohexane as the test fluid performed aboard the International Space Station (ISS) are presented in this paper. A flat, transparent, constant temperature microheater array was used to perform experiments over a wide range of temperatures (55 degrees C < T-w < 107.5 degrees C), pressures (0.58 atm < P < 1.86 atm), subcoolings (1 degrees C <= Delta T-sub <= 26 degrees C), and heater sizes (4.2 mm <= L-h <= 7.0 mm). The boiling process was visualized from the side and bottom. Based on this high quality microgravity data (a/g < 10(-6)), the recently reported gravity scaling parameter for heat flux, which was primarily based on parabolic flight experiments, was modified to account for these new results. The updated model accurately predicts the experimental microgravity data to within +/- 20%. The robustness of this framework in predicting low gravity heat transfer is further demonstrated by predicting many of the trends in the pool boiling literature that cannot be explained by any single model. [DOI: 10.1115/1.4006846]
C1 [Raj, Rishi; Kim, Jungho] Univ Maryland, Dept Mech Engn, College Pk, MD 20742 USA.
[McQuillen, John] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Kim, J (reprint author), Univ Maryland, Dept Mech Engn, College Pk, MD 20742 USA.
EM kimjh@umd.edu
FU NASA through the Advanced Capabilities Division in the Exploration
Systems Mission Directorate at NASA Headquarters [NNX08AI60A]
FX This work was supported by NASA Grant No. NNX08AI60A through the
Advanced Capabilities Division in the Exploration Systems Mission
Directorate at NASA Headquarters. The authors would also like to thank
ZIN Technologies and the ISS and Human Health Office at NASA Glenn
Research Center in Cleveland, Ohio for fabricating the test apparatus
and providing support during microgravity operations.
NR 30
TC 5
Z9 6
U1 2
U2 19
PU ASME
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0022-1481
J9 J HEAT TRANS-T ASME
JI J. Heat Transf.-Trans. ASME
PD OCT
PY 2012
VL 134
IS 10
AR 101504
DI 10.1115/1.4006846
PG 14
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA 076MC
UT WOS:000313959600005
ER
PT J
AU Lim, YK
Ham, YG
Jeong, JH
Kug, JS
AF Lim, Young-Kwon
Ham, Yoo-Geun
Jeong, Jee-Hoon
Kug, Jong-Seong
TI Improvement in simulation of Eurasian winter climate variability with a
realistic Arctic sea ice condition in an atmospheric GCM
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE sea-ice; mid-latitude winter climate; atmospheric GCM
ID IMPACT; COVER; CIRCULATION; ANOMALIES
AB The present study investigates how much a realistic Arctic sea ice condition can contribute to improve simulation of the winter climate variation over the Eurasia region. Model experiments are set up using different sea ice boundary conditions over the past 24 years (i.e., 1988-2011). One is an atmospheric model inter-comparison (AMIP) type of run forced with observed sea-surface temperature (SST), sea ice, and greenhouse gases (referred to as Exp RSI), and the other is the same as Exp RSI except for the sea ice forcing, which is a repeating climatological annual cycle (referred to as Exp CSI).
Results show that Exp RSI produces the observed dominant pattern of Eurasian winter temperatures and their interannual variation better than Exp CSI (correlation difference up to similar to 0.3). Exp RSI captures the observed strong relationship between the sea ice concentration near the Barents and Kara seas and the temperature anomaly across Eurasia, including northeastern Asia, which is not well captured in Exp CSI. Lagged atmospheric responses to sea ice retreat are examined using observations to understand atmospheric processes for the Eurasian cooling response including the Arctic temperature increase, sea-level pressure increase, upper-level jet weakening and cold air outbreak toward the mid-latitude. The reproducibility of these lagged responses by Exp RSI is also evaluated.
C1 [Lim, Young-Kwon; Ham, Yoo-Geun] NASA, Global Modeling & Assimilat Off, GSFC, Greenbelt, MD 20771 USA.
[Jeong, Jee-Hoon] Chonnam Natl Univ, Fac Earth Syst & Environm Sci, Kwangju, South Korea.
[Kug, Jong-Seong] Korea Inst Ocean Sci & Technol, Ansan, South Korea.
RP Lim, YK (reprint author), NASA, Global Modeling & Assimilat Off, GSFC, Greenbelt, MD 20771 USA.
EM yoo-geun.ham@nasa.gov
RI KUG, JONG-SEONG/A-8053-2013; Jeong, Jee-Hoon/A-4286-2010
OI Jeong, Jee-Hoon/0000-0002-3358-3949
FU National Research Foundation of Korea; Korean Government (MEST)
[NRF-2009-C1AAA001-2009-0093042]; Korea Meteorological Administration
Research and Development Program [CATER 2012-3061(PN12010)]
FX JSK is supported by the National Research Foundation of Korea Grant
funded by the Korean Government (MEST) (NRF-2009-C1AAA001-2009-0093042).
JHJ is supported by the Korea Meteorological Administration Research and
Development Program under grant CATER 2012-3061(PN12010).
NR 21
TC 9
Z9 9
U1 0
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD OCT-DEC
PY 2012
VL 7
IS 4
AR 044041
DI 10.1088/1748-9326/7/4/044041
PG 6
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 059IA
UT WOS:000312696400045
ER
PT J
AU Rhodes, J
Dobke, B
Booth, J
Massey, R
Liewer, K
Smith, R
Amara, A
Aldrich, J
Berge, J
Bezawada, N
Brugarolas, P
Clark, P
Dubbeldam, CM
Ellis, R
Frenk, C
Gallie, A
Heavens, A
Henry, D
Jullo, E
Kitching, T
Lanzi, J
Lilly, S
Lunney, D
Miyazaki, S
Morris, D
Paine, C
Peacock, J
Pellegrino, S
Pittock, R
Pool, P
Refregier, A
Seiffert, M
Sharples, R
Smith, A
Stuchlik, D
Taylor, A
Teplitz, H
Vanderveld, RA
Wu, J
AF Rhodes, Jason
Dobke, Benjamin
Booth, Jeffrey
Massey, Richard
Liewer, Kurt
Smith, Roger
Amara, Adam
Aldrich, Jack
Berge, Joel
Bezawada, Naidu
Brugarolas, Paul
Clark, Paul
Dubbeldam, Cornelis M.
Ellis, Richard
Frenk, Carlos
Gallie, Angus
Heavens, Alan
Henry, David
Jullo, Eric
Kitching, Thomas
Lanzi, James
Lilly, Simon
Lunney, David
Miyazaki, Satoshi
Morris, David
Paine, Christopher
Peacock, John
Pellegrino, Sergio
Pittock, Roger
Pool, Peter
Refregier, Alexandre
Seiffert, Michael
Sharples, Ray
Smith, Alexandra
Stuchlik, David
Taylor, Andy
Teplitz, Harry
Vanderveld, R. Ali
Wu, James
TI Space-quality data from balloon-borne telescopes: The High Altitude
Lensing Observatory (HALO)
SO ASTROPARTICLE PHYSICS
LA English
DT Article
DE Weak lensing; Cosmology; Surveys; Balloons
ID COSMIC SHEAR; ENERGY
AB We present a method for attaining sub-arcsecond pointing stability during sub-orbital balloon flights, as designed for in the High Altitude Lensing Observatory (HALO) concept. The pointing method presented here has the potential to perform near-space quality optical astronomical imaging at similar to 1-2% of the cost of space-based missions. We also discuss an architecture that can achieve sufficient thermo-mechanical stability to match the pointing stability. This concept is motivated by advances in the development and testing of Ultra Long Duration Balloon (ULDB) flights which promise to allow observation campaigns lasting more than three months. The design incorporates a multi-stage pointing architecture comprising: a gondola coarse azimuth control system, a multi-axis nested gimbal frame structure with arcsecond stability, a telescope de-rotator to eliminate field rotation, and a fine guidance stage consisting of both a telescope mounted angular rate sensor and guide CCDs in the focal plane to drive a Fast-Steering Mirror. We discuss the results of pointing tests together with a preliminary thermo-mechanical analysis required for sub-arcsecond pointing at high altitude. Possible future applications in the areas of wide-field surveys and exoplanet searches are also discussed. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Rhodes, Jason; Dobke, Benjamin; Booth, Jeffrey; Liewer, Kurt; Aldrich, Jack; Brugarolas, Paul; Paine, Christopher; Seiffert, Michael; Wu, James] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Massey, Richard; Heavens, Alan; Kitching, Thomas; Peacock, John] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Massey, Richard; Sharples, Ray; Taylor, Andy] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Amara, Adam; Berge, Joel; Lilly, Simon; Refregier, Alexandre] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland.
[Bezawada, Naidu; Gallie, Angus; Henry, David; Lunney, David] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Clark, Paul; Dubbeldam, Cornelis M.; Sharples, Ray] Univ Durham, Ctr Adv Instrumentat, Netpark TS21 3FB, Sedgefield, England.
[Frenk, Carlos] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England.
[Jullo, Eric] Univ Provence, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France.
[Lanzi, James; Stuchlik, David] NASA, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
[Miyazaki, Satoshi] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Morris, David; Pittock, Roger; Pool, Peter] E2v, Chelmsford CM1 2QU, Essex, England.
[Teplitz, Harry] CALTECH, IPAC, Pasadena, CA 91125 USA.
[Vanderveld, R. Ali] Univ Chicago, Enrico Fermi Inst, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
RP Rhodes, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jason.d.rhodes@jpl.nasa.gov
RI Sharples, Ray/N-7309-2013
OI Sharples, Ray/0000-0003-3449-8583
FU STFC Advanced Fellowship [PP/E006450/1]; National Aeronautics and Space
Administration (NASA); ORAU under NASA
FX The authors thank to Joan Ervin, Roger Lee, Tanaz Mozafari, Barth
Netterfield, Wes Traub, Chris Stoughton and David Pierce for work and
discussions relating to the HALO concept. RJM acknowledges financial
support through STFC Advanced Fellowship PP/E006450/1. The work of JR,
BMD, JB, KL, PB, EJ, JA and CP was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration (NASA). EJ acknowledges
the support of ORAU under contract with NASA.
NR 38
TC 9
Z9 9
U1 0
U2 9
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-6505
J9 ASTROPART PHYS
JI Astropart Phys.
PD OCT
PY 2012
VL 38
BP 31
EP 40
DI 10.1016/j.astropartphys.2012.05.015
PG 10
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 052DK
UT WOS:000312177700006
ER
PT J
AU Pohorille, A
Pratt, LR
AF Pohorille, A.
Pratt, L. R.
TI Is Water the Universal Solvent for Life?
SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES
LA English
DT Editorial Material
DE Water; Self-organization; Hydrophobic effect; Non-covalent interactions;
Hydrophilic interactions
ID DENATURATION; PRESSURE
C1 [Pohorille, A.] NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Pratt, L. R.] Tulane Univ, Dept Chem & Biomol Engn, New Orleans, LA 70118 USA.
RP Pohorille, A (reprint author), NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Andrew.Pohorille@nasa.gov; lpratt@tulane.edu
NR 12
TC 11
Z9 11
U1 1
U2 31
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0169-6149
J9 ORIGINS LIFE EVOL B
JI Orig. Life Evol. Biosph.
PD OCT
PY 2012
VL 42
IS 5
BP 405
EP 409
DI 10.1007/s11084-012-9301-6
PG 5
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 052GS
UT WOS:000312186300007
PM 23065397
ER
PT J
AU Pohorille, A
AF Pohorille, Andrew
TI Processes that Drove the Transition from Chemistry to Biology: Concepts
and Evidence
SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES
LA English
DT Editorial Material
DE Ancestral proteins; Origin of protein function; Early evolution of
proteins; Ion channels; Origin of metabolism; Protocells
ID EVOLUTION; REPLICATION; EMERGENCE; PROTEINS; ORIGIN; LIFE
C1 NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Pohorille, A (reprint author), NASA, Exobiol Branch, Ames Res Ctr, MS 239-4, Moffett Field, CA 94035 USA.
EM Andrew.Pohorille@nasa.gov
NR 22
TC 0
Z9 0
U1 0
U2 16
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0169-6149
J9 ORIGINS LIFE EVOL B
JI Orig. Life Evol. Biosph.
PD OCT
PY 2012
VL 42
IS 5
BP 429
EP 432
DI 10.1007/s11084-012-9304-3
PG 4
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 052GS
UT WOS:000312186300011
PM 23080008
ER
PT J
AU Pohorille, A
AF Pohorille, Andrew
TI Comments on Dynamic Kinetic Stability
SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES
LA English
DT Editorial Material
C1 NASA, Exobiol Branch, Ames Res Ctr, Washington, DC 20546 USA.
RP Pohorille, A (reprint author), NASA, Exobiol Branch, Ames Res Ctr, Washington, DC 20546 USA.
NR 4
TC 0
Z9 0
U1 0
U2 6
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0169-6149
J9 ORIGINS LIFE EVOL B
JI Orig. Life Evol. Biosph.
PD OCT
PY 2012
VL 42
IS 5
BP 439
EP 444
PG 6
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 052GS
UT WOS:000312186300014
ER
PT J
AU Beiersdorfer, P
Brown, GV
Graf, AT
Bitter, M
Hill, KW
Kelley, RL
Kilbourne, CA
Leutenegger, MA
Porter, FS
AF Beiersdorfer, P.
Brown, G. V.
Graf, A. T.
Bitter, M.
Hill, K. W.
Kelley, R. L.
Kilbourne, C. A.
Leutenegger, M. A.
Porter, F. S.
TI Rest-wavelength fiducials for the ITER core imaging x-ray spectrometer
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article; Proceedings Paper
CT 19th Topical Conference on High-Temperature Plasma Diagnostics
CY MAY 06-10, 2012
CL Monterey, CA
ID PLASMA ROTATION VELOCITY; BEAM ION-TRAP; CRYSTAL SPECTROMETER;
TEMPERATURE; PROFILES
AB Absolute wavelength references are needed to derive the plasma velocities from the Doppler shift of a given line emitted by a moving plasma. We show that such reference standards exist for the strongest x-ray line in neonlike W64+, which has become the line of choice for the ITER (Latin "the way") core imaging x-ray spectrometer. Close-by standards are the Hf L beta(3) line and the Ir L alpha(2) line, which bracket the W64+ line by +/- 30 eV; other standards are given by the Ir L alpha(1) and L alpha(2) lines and the Hf L beta(1) and L beta(2) lines, which bracket the W64+ line by +/- 40 and +/- 160 eV, respectively. The reference standards can be produced by an x-ray tube built into the ITER spectrometer. We present spectra of the reference lines obtained with an x-ray microcalorimeter and compare them to spectra of the W64+ line obtained both with an x-ray microcalorimeter and a crystal spectrometer. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4733318]
C1 [Beiersdorfer, P.; Brown, G. V.; Graf, A. T.] Lawrence Livermore Natl Lab, Div Phys, Livermore, CA 94550 USA.
[Beiersdorfer, P.] Univ Puerto Rico, Dept Chem, San Juan, PR 00931 USA.
[Beiersdorfer, P.] Univ Puerto Rico, Chem Phys Program, San Juan, PR 00931 USA.
[Bitter, M.; Hill, K. W.] Princeton Plasma Phys Lab, Princeton, NJ 08543 USA.
[Kelley, R. L.; Kilbourne, C. A.; Leutenegger, M. A.; Porter, F. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Beiersdorfer, P (reprint author), Lawrence Livermore Natl Lab, Div Phys, Livermore, CA 94550 USA.
EM beiersdor-fer@llnl.gov
RI Porter, Frederick/D-3501-2012
OI Porter, Frederick/0000-0002-6374-1119
NR 19
TC 4
Z9 4
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 OCT
PY 2012
VL 83
IS 10
AR 10E111
DI 10.1063/1.4733318
PN 2
PG 3
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA 043RB
UT WOS:000311562900119
PM 23126933
ER
PT J
AU Anderson, MS
Katz, I
Petkov, M
Blakkolb, B
Mennella, J
D'Agostino, S
Crisp, J
Evans, J
Feldman, J
Limonadi, D
AF Anderson, M. S.
Katz, I.
Petkov, M.
Blakkolb, B.
Mennella, J.
D'Agostino, S.
Crisp, J.
Evans, J.
Feldman, J.
Limonadi, D.
TI In situ cleaning of instruments for the sensitive detection of organics
on Mars
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
AB A method is presented for in situ cleaning of spacecraft instruments that analyze planetary soil and rock. We have found that vibrating hardware, used to facilitate powder transport, was also effective at removing contamination. Surfaces can be cleaned below monolayer levels using vibrating surfaces in the presence of mineral powder. Both organic and particulate contamination is efficiently removed. Fine grained regolith from the planetary surface or an organic free reference material may serve as the powder used for cleaning. We present both analytical and experimental results for the contamination transfer fraction and the conditions required to clean the hardware prior to sensitive chemical analysis. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4757861]
C1 [Anderson, M. S.; Katz, I.; Petkov, M.; Blakkolb, B.; Mennella, J.; D'Agostino, S.; Crisp, J.; Evans, J.; Feldman, J.; Limonadi, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Anderson, MS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Mark.S.Anderson@jpl.nasa.gov
RI Crisp, Joy/H-8287-2016
OI Crisp, Joy/0000-0002-3202-4416
FU Jet Propulsion Laboratory, California Institute of Technology, under a
with the National Aeronautics and Space Administration
FX The research described in this work was carried out by the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 10
TC 5
Z9 5
U1 0
U2 5
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0034-6748
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD OCT
PY 2012
VL 83
IS 10
AR 105109
DI 10.1063/1.4757861
PN 1
PG 5
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA 043QZ
UT WOS:000311562500064
PM 23126806
ER
PT J
AU Dauphas, N
Roskosz, M
Alp, EE
Golden, DC
Sio, CK
Tissot, FLH
Hu, MY
Zhao, J
Gao, L
Morris, RV
AF Dauphas, N.
Roskosz, M.
Alp, E. E.
Golden, D. C.
Sio, C. K.
Tissot, F. L. H.
Hu, M. Y.
Zhao, J.
Gao, L.
Morris, R. V.
TI A general moment NRIXS approach to the determination of equilibrium Fe
isotopic fractionation factors: Application to goethite and jarosite
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID NUCLEAR RESONANT SCATTERING; DENSITY-OF-STATES; X-RAY-SCATTERING;
DISSIMILATORY FE(III) REDUCTION; AQUO-CHLORO COMPLEXES; AQUEOUS FERROUS
IRON; MOSSBAUER SUM-RULES; MERIDIANI-PLANUM; SYNCHROTRON-RADIATION;
VIBRATIONAL SPECTROSCOPY
AB The equilibrium Fe isotopic fractionation factors of goethite and jarosite have considerable importance for interpreting Fe isotope variations in low temperature aqueous systems on Earth and possibly Mars in the context of future sample return missions. We measured the beta-factors of goethite FeO(OH), potassium-jarosite KFe3(SO4)(2)(OH)(6), and hydronium-jarosite (H3O)Fe-3(SO4)(2)(OH)(6), by Nuclear Resonant Inelastic X-ray Scattering (NRIXS, also known as Nuclear Resonance Vibrational Spectroscopy - NRVS or Nuclear Inelastic Scattering - NIS) at the Advanced Photon Source. These measurements were made on synthetic minerals enriched in Fe-57. A new method (i.e., the general moment approach) is presented to calculate beta-factors from the moments of the NRIXS spectrum S(E). The first term in the moment expansion controls iron isotopic fractionation at high temperature and corresponds to the mean force constant of the iron bonds, a quantity that is readily measured and often reported in NRIXS studies. The mean force constants of goethite, potassium-jarosite, and hydronium-jarosite are 314 +/- 14, 264 +/- 12, and 310 +/- 14 N/m, respectively (uncertainties include statistical and systematic errors). The general moment approach gives Fe-56/Fe-54 beta-factors of 9.7, 8.3, and 9.5& at 22 degrees C for these minerals. The beta-factor of goethite measured by NRIXS is larger than that estimated by combining results from laboratory exchange experiments and calculations based on electronic structure theory. Similar issues have been identified previously for other pairs of mineral-aqueous species, which could reflect inadequacies of approaches based on electronic structure theory to calculate absolute beta-factors (differences in beta-factors between aqueous species may be more accurate) or failure of laboratory experiments to measure mineral-fluid equilibrium isotopic fractionation at low temperature. We apply the force constant approach to published NRIXS data and report 1000 x ln beta for important Fe-bearing phases of geological and biochemical relevance such as myoglobin, cytochrome f, pyroxene, metal, troilite, chalcopyrite, hematite, and magnetite. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Dauphas, N.; Sio, C. K.; Tissot, F. L. H.] Univ Chicago, Dept Geophys Sci, Origins Lab, Chicago, IL 60637 USA.
[Dauphas, N.; Sio, C. K.; Tissot, F. L. H.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Roskosz, M.] Univ Lille 1, Unite Mat & Transformat, CNRS UMR 8207, F-69655 Villeneuve Dascq, France.
[Alp, E. E.; Hu, M. Y.; Zhao, J.; Gao, L.] Argonne Natl Lab, Adv Photon Source, Argonne, IL 60439 USA.
[Golden, D. C.] Engn & Sci Contract Grp Hamilton Sundstrand, Houston, TX 77058 USA.
[Morris, R. V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Dauphas, N (reprint author), Univ Chicago, Dept Geophys Sci, Origins Lab, 5734 S Ellis Ave, Chicago, IL 60637 USA.
EM dauphas@uchicago.edu
FU NASA [NNX09AG59G]; NSF EAR Petrology and Geochemistry [EAR-1144429];
Packard Fellowship; COMPRES under NSF [EAR 10-43050]; US DOE
[DE-AC02-06CH11367]
FX We thank C. Achilles for determination of particle sizes using XRD data.
Discussions with W. Sturhahn, R.N. Clayton, R. Caracas, and T. Fujii
regarding data reduction, background subtraction, and stable isotope
fractionation were greatly appreciated. M. Meheut, V. Polyakov, A.
Shahar, and Associate editor E. Schauble are thanked for their
thoughtful reviews of the manuscript. This work was supported by NASA
(NNX09AG59G), by NSF EAR Petrology and Geochemistry (EAR-1144429), and
by a Packard Fellowship to N. Dauphas. L. Gao acknowledges the financial
support from COMPRES under NSF Cooperative Agreement EAR 10-43050. Use
of the Advanced Photon Source, an Office of Science User Facility
operated for the U. S. Department of Energy (DOE) Office of Science by
Argonne National Laboratory, was supported by the US DOE under contract
No DE-AC02-06CH11367.
NR 104
TC 33
Z9 33
U1 5
U2 51
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD OCT 1
PY 2012
VL 94
BP 254
EP 275
DI 10.1016/j.gca.2012.06.013
PG 22
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 016HV
UT WOS:000309509400016
ER
PT J
AU Agoulmine, N
Kim, K
Kim, S
Rim, T
Lee, JS
Meyyappan, M
AF Agoulmine, Nazim
Kim, Kihyun
Kim, Sungho
Rim, Taiuk
Lee, Jeong-Soo
Meyyappan, M.
TI ENABLING COMMUNICATION AND COOPERATION IN BIO-NANOSENSOR NETWORKS:
TOWARD INNOVATIVE HEALTHCARE SOLUTIONS
SO IEEE WIRELESS COMMUNICATIONS
LA English
DT Article
ID BACTERIA
AB Bio-nanosensors and communication at the nanoscale are a promising paradigm and technology for the development of a new class of ehealth solutions. While recent communication technologies such as mobile and wireless combined with medical sensors have allowed new successful eHealth applications, another level of innovation is required to deliver scalable and cost-effective solutions via developing devices that operate and communicate directly inside the body. This work presents the application of nano technology for the development of miniaturized bio-nanosensors that are able to communicate and exchange information about sensed molecules or chemical compound concentration and therefore draw a global response in the case of health anomalies. Two communication techniques are reviewed: electromagnetic wireless communication in the terahertz band and molecular communication. The characteristics of these two modes of communication are highlighted, and a general architecture for bio-nanosensors is proposed along with examples of cooperation schemes. An implementation of the bio-nanosensor part of the nanomachine is presented along with some experimental results of sensing biomolecules. Finally, a general example of coordination among bio-nanomachines using both communication technologies is presented, and challenges in terms of communication protocols, data transmission, and coordination among nanomachines are discussed.
C1 [Agoulmine, Nazim] Univ Evry Val dEssonne, Evry, France.
Pohang Univ Sci & Technol, Pohang, South Korea.
[Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Agoulmine, N (reprint author), Univ Evry Val dEssonne, Evry, France.
EM nazim.agoulmine@iup.univ-evry.fr; ljs6951@postech.ac.kr
FU World Class University program; Ministry of Education, Science and
Technology through the National Research Foundation of Korea [R31-10100]
FX This research was supported by the World Class University program funded
by the Ministry of Education, Science and Technology through the
National Research Foundation of Korea (R31-10100).
NR 15
TC 11
Z9 11
U1 2
U2 29
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1536-1284
J9 IEEE WIREL COMMUN
JI IEEE Wirel. Commun.
PD OCT
PY 2012
VL 19
IS 5
BP 42
EP 51
PG 10
WC Computer Science, Hardware & Architecture; Computer Science, Information
Systems; Engineering, Electrical & Electronic; Telecommunications
SC Computer Science; Engineering; Telecommunications
GA 035XU
UT WOS:000310987600008
ER
PT J
AU Hartley, TT
Lorenzo, CF
AF Hartley, Tom T.
Lorenzo, Carl F.
TI CHAOTIC BEHAVIOR IN A FRACTIONAL-ORDER SYSTEM CONTAINING A CONTINUOUS
ORDER-DISTRIBUTION
SO INTERNATIONAL JOURNAL OF BIFURCATION AND CHAOS
LA English
DT Article
DE Fractional-order systems; order-distributions; chaos; approximation
ID CALCULUS; POWER
AB This paper discusses the fractional dynamics, and the bifurcation behavior, of a specific nonlinear system that contains a continuous order-distribution. The dynamics of the system are predicted using the describing-function method. General approximation methods are then derived for the continuous order-distribution component. The system is simulated using these approximations, and the results compared with the describing-function predictions. This is believed to be the first observation of chaos in a system with continuous order-distribution.
C1 [Hartley, Tom T.] Univ Akron, Dept Elect & Comp Engn, Akron, OH 44325 USA.
[Lorenzo, Carl F.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Hartley, TT (reprint author), Univ Akron, Dept Elect & Comp Engn, Akron, OH 44325 USA.
EM TomHartley@aol.com; Carl.F.Lorenzo@nasa.gov
NR 30
TC 0
Z9 0
U1 0
U2 12
PU WORLD SCIENTIFIC PUBL CO PTE LTD
PI SINGAPORE
PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE
SN 0218-1274
J9 INT J BIFURCAT CHAOS
JI Int. J. Bifurcation Chaos
PD OCT
PY 2012
VL 22
IS 10
AR 1250253
DI 10.1142/S0218127412502537
PG 12
WC Mathematics, Interdisciplinary Applications; Multidisciplinary Sciences
SC Mathematics; Science & Technology - Other Topics
GA 034NX
UT WOS:000310881300025
ER
PT J
AU Bertacca, D
Maartens, R
Raccanelli, A
Clarkson, C
AF Bertacca, Daniele
Maartens, Roy
Raccanelli, Alvise
Clarkson, Chris
TI Beyond the plane-parallel and Newtonian approach: wide-angle redshift
distortions and convergence in general relativity
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE gravity; cosmological parameters from LSS
ID SPACE
AB We extend previous analyses of wide-angle correlations in the galaxy power spectrum in redshift space to include all general relativistic effects. These general relativistic corrections to the standard approach become important on large scales and at high redshifts, and they lead to new terms in the wide-angle correlations. We show that in principle the new terms can produce corrections of nearly 10% on Gpc scales over the usual Newtonian approximation. General relativistic corrections will be important for future large-volume surveys such as SKA and Euclid, although the problem of cosmic variance will present a challenge in observing this.
C1 [Bertacca, Daniele; Maartens, Roy] Univ Western Cape, Dept Phys, ZA-7535 Cape Town, South Africa.
[Maartens, Roy] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Raccanelli, Alvise] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Raccanelli, Alvise] CALTECH, Pasadena, CA 91125 USA.
[Clarkson, Chris] Univ Cape Town, Ctr Astrophys Cosmol & Gravitat, ZA-7701 Cape Town, South Africa.
[Clarkson, Chris] Univ Cape Town, Dept Math & Appl Math, ZA-7701 Cape Town, South Africa.
RP Bertacca, D (reprint author), Univ Western Cape, Dept Phys, ZA-7535 Cape Town, South Africa.
EM daniele.bertacca@pd.infn.it; Roy.Maartens@port.ac.uk;
Alvise@caltech.edu; Clarkson@maths.uct.ac.za
OI Raccanelli, Alvise/0000-0001-6726-0438; Maartens,
Roy/0000-0001-9050-5894
FU South African Square Kilometre Array Project; STFC (U.K.)
[ST/H002774/1]; National Research Foundation (NRF, South Africa); Royal
Society (U.K.)/NRF (S.A.); National Aeronautics and Space Administration
FX DB and RM are supported by the South African Square Kilometre Array
Project. RM is supported by the STFC (U.K.) (grant no. ST/H002774/1). RM
and CC are supported by the National Research Foundation (NRF, South
Africa). DB, RM and CC are supported by a Royal Society (U.K.)/NRF
(S.A.) exchange grant. 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.
NR 25
TC 30
Z9 30
U1 0
U2 0
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 OCT
PY 2012
IS 10
AR 025
DI 10.1088/1475-7516/2012/10/025
PG 18
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 033KD
UT WOS:000310793700026
ER
PT J
AU Stephens, GL
Li, JL
Wild, M
Clayson, CA
Loeb, N
Kato, S
L'Ecuyer, T
Stackhouse, PW
Lebsock, M
Andrews, T
AF Stephens, Graeme L.
Li, Juilin
Wild, Martin
Clayson, Carol Anne
Loeb, Norman
Kato, Seiji
L'Ecuyer, Tristan
Stackhouse, Paul W., Jr.
Lebsock, Matthew
Andrews, Timothy
TI An update on Earth's energy balance in light of the latest global
observations
SO NATURE GEOSCIENCE
LA English
DT Article
ID RADIATION BUDGET; ATMOSPHERE RADIATION; OBSERVING SYSTEM;
CLIMATE-CHANGE; UPPER-OCEAN; SURFACE; PRECIPITATION; VARIABILITY; CYCLE;
MODEL
AB Climate change is governed by changes to the global energy balance. At the top of the atmosphere, this balance is monitored globally by satellite sensors that provide measurements of energy flowing to and from Earth. By contrast, observations at the surface are limited mostly to land areas. As a result, the global balance of energy fluxes within the atmosphere or at Earth's surface cannot be derived directly from measured fluxes, and is therefore uncertain. This lack of precise knowledge of surface energy fluxes profoundly affects our ability to understand how Earth's climate responds to increasing concentrations of greenhouse gases. In light of compilations of up-to-date surface and satellite data, the surface energy balance needs to be revised. Specifically, the longwave radiation received at the surface is estimated to be significantly larger, by between 10 and 17 Wm(-2), than earlier model-based estimates. Moreover, the latest satellite observations of global precipitation indicate that more precipitation is generated than previously thought. This additional precipitation is sustained by more energy leaving the surface by evaporation - that is, in the form of latent heat flux - and thereby offsets much of the increase in longwave flux to the surface.
C1 [Stephens, Graeme L.; Li, Juilin; Lebsock, Matthew] CALTECH, Jet Prop Lab, Ctr Climate Sci, Pasadena, CA 91109 USA.
[Wild, Martin] ETH, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland.
[Clayson, Carol Anne] Woods Hole Oceanog Inst, Dept Phys Oceanog, Woods Hole, MA 02543 USA.
[Loeb, Norman; Kato, Seiji; Stackhouse, Paul W., Jr.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[L'Ecuyer, Tristan] Univ Wisconsin, Dept Atmospher Sci, Madison, WI USA.
[Andrews, Timothy] UK Met Off, Exeter EX1 3PB, Devon, England.
RP Stephens, GL (reprint author), CALTECH, Jet Prop Lab, Ctr Climate Sci, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM graeme.stephens@jpl.nasa.gov
RI L'Ecuyer, Tristan/C-7040-2013; Andrews, Timothy/C-5912-2014; L'Ecuyer,
Tristan/E-5607-2012; Wild, Martin/J-8977-2012
OI Andrews, Timothy/0000-0002-8248-8753; L'Ecuyer,
Tristan/0000-0002-7584-4836;
NR 57
TC 158
Z9 162
U1 16
U2 180
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
EI 1752-0908
J9 NAT GEOSCI
JI Nat. Geosci.
PD OCT
PY 2012
VL 5
IS 10
BP 691
EP 696
DI 10.1038/NGEO1580
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 016JW
UT WOS:000309515100013
ER
PT J
AU Trujillo, E
Molotch, NP
Goulden, ML
Kelly, AE
Bales, RC
AF Trujillo, Ernesto
Molotch, Noah P.
Goulden, Michael L.
Kelly, Anne E.
Bales, Roger C.
TI Elevation-dependent influence of snow accumulation on forest greening
SO NATURE GEOSCIENCE
LA English
DT Article
ID WESTERN UNITED-STATES; SUB-ALPINE FOREST; SPECIES-RICHNESS PATTERNS;
SPOT-VEGETATION; CLIMATE-CHANGE; AVHRR; MODIS; ECOSYSTEM; EXCHANGE;
INCREASE
AB Rising temperatures and declining water availability have influenced the ecological function of mountain forests over the past half-century. For instance, warming in spring and summer and shifts towards earlier snowmelt are associated with an increase in wildfire activity and tree mortality in mountain forests in the western United States(1,2). Temperature increases are expected to continue during the twenty-first century in mountain ecosystems across the globe(3,4), with uncertain consequences. Here, we examine the influence of interannual variations in snowpack accumulation on forest greenness in the Sierra Nevada Mountains, California, between 1982 and 2006. Using observational records of snow accumulation and satellite data on vegetation greenness we show that vegetation greenness increases with snow accumulation. Indeed, we show that variations in maximum snow accumulation explain over 50% of the interannual variability in peak forest greenness across the Sierra Nevada region. The extent to which snow accumulation can explain variations in greenness varies with elevation, reaching a maximum in the water-limited mid-elevations, between 2,000 and 2,600 m. In situ measurements of carbon uptake and snow accumulation along an elevational transect in the region confirm the elevation dependence of this relationship. We suggest that mid-elevation mountain forest ecosystems could prove particularly sensitive to future increases in temperature and concurrent changes in snow accumulation and melt.
C1 [Trujillo, Ernesto; Molotch, Noah P.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
[Trujillo, Ernesto] Ecole Polytech Fed Lausanne, Sch Architecture Civil & Environm Engn, EPFL ENAC IIE CRYOS Stn 2, CH-1015 Lausanne, Switzerland.
[Molotch, Noah P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA.
[Molotch, Noah P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Goulden, Michael L.; Kelly, Anne E.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Bales, Roger C.] Univ Calif Merced, Sierra Nevada Res Inst, Merced, CA 95343 USA.
RP Trujillo, E (reprint author), Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
EM Ernesto.Trujillo-Gomez@Colorado.edu
RI Trujillo, Ernesto/A-6890-2013; Molotch, Noah/C-8576-2009
OI Trujillo, Ernesto/0000-0001-9731-7482;
FU NSF [EAR-1032295, EAR-1032308, EAR-0619947]; Southern Sierra Critical
Zone Observatory [NSF EAR-0725097]; Jet Propulsion Laboratory Research
and Technology Development Fund; NASA; [NASA-NNX08AH18G]
FX This research was supported by NSF EAR-1032295, NSF EAR-1032308, NSF
EAR-0619947, the Southern Sierra Critical Zone Observatory (NSF
EAR-0725097), NASA-NNX08AH18G and the Jet Propulsion Laboratory Research
and Technology Development Fund. Part of this work was performed at the
Jet Propulsion Laboratory, California Institute of Technology under
contract with NASA. We thank F. Gehrke for facilitating access to the
California Department of Water Resources snow sensor data, M. Meadows
and G. Winston for assistance in the field, and T. Veblen and M.
Williams for comments on the manuscript and useful discussions.
NR 30
TC 55
Z9 56
U1 5
U2 65
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
EI 1752-0908
J9 NAT GEOSCI
JI Nat. Geosci.
PD OCT
PY 2012
VL 5
IS 10
BP 705
EP 709
DI 10.1038/NGEO1571
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 016JW
UT WOS:000309515100016
ER
PT J
AU Meunier, A
Petit, S
Ehlmann, BL
Dudoignon, P
Westall, F
Mas, A
El Albani, A
Ferrage, E
AF Meunier, Alain
Petit, Sabine
Ehlmann, Bethany L.
Dudoignon, Patrick
Westall, Frances
Mas, Antoine
El Albani, Abderrazak
Ferrage, Eric
TI Magmatic precipitation as a possible origin of Noachian clays on Mars
SO NATURE GEOSCIENCE
LA English
DT Article
ID LIGHT LITHOPHILE ELEMENTS; MARTIAN MAGMAS; AQUEOUS ALTERATION; SILICATE
MINERALS; WATER; PHYLLOSILICATES; METEORITES; SPECTROSCOPY; REFLECTANCE;
PYROXENES
AB Hydrous clay minerals detected on the surface of Mars have been interpreted as indicators of the hydrologic and climatic evolution of the planet. The iron-and magnesium-rich clays described in thick, extensive outcrops of Noachian crust have been proposed to originate from aqueous weathering. This would imply that liquid water was stable at the surface of early Mars, presumably when the climate was warmer and wetter. Here we show that iron-and magnesium-rich clays can alternatively form by direct precipitation from residual, water-rich magma-derived fluids. Infrared reflectance spectra from terrestrial lavas from the Mururoa Atoll (French Polynesia) that underwent this precipitation process are similar to those measured for the Noachian crust. Such an origin is also consistent with the D/H ratio of iron-and magnesium-rich clays in some martian meteorites and the widespread presence of these clays in massive basaltic lavas, breccias and regolith. We propose that the progressive degassing of the martian interior over time and the resultant increasingly water-poor magmatic fluids-and not a cooling climate-may explain the absence of clays in Hesperian-aged and more recent formations.
C1 [Meunier, Alain; Petit, Sabine; Dudoignon, Patrick; Mas, Antoine; El Albani, Abderrazak; Ferrage, Eric] Univ Poitiers, CNRS, IC2MP, UMR 7285, F-86022 Poitiers, France.
[Ehlmann, Bethany L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Ehlmann, Bethany L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Westall, Frances] CNRS, Ctr Biophys Mol, F-45071 Orleans 2, France.
RP Meunier, A (reprint author), Univ Poitiers, CNRS, IC2MP, UMR 7285, HydrASA Bat 35,40 Ave Recteur Pineau, F-86022 Poitiers, France.
EM alain.meunier@univ-poitiers.fr
RI FERRAGE, Eric/P-7466-2015
OI FERRAGE, Eric/0000-0001-9257-5976
FU University of Poitiers; French CNRS-INSU; French ANR 'Jeunes Chercheurs'
programme [ANR-09-JCJC-0,106-PorousClay]
FX This study was supported by the University of Poitiers, the French
CNRS-INSU and by a French ANR 'Jeunes Chercheurs' programme (contract
no. ANR-09-JCJC-0,106-PorousClay). We are grateful to V. F. Chevrier and
B. Hynek for their comments and suggestions that have improved our
manuscript. We thank S. Riffault for her contribution to the drawing of
Fig. 3.
NR 38
TC 23
Z9 23
U1 1
U2 32
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
EI 1752-0908
J9 NAT GEOSCI
JI Nat. Geosci.
PD OCT
PY 2012
VL 5
IS 10
BP 739
EP 743
DI 10.1038/NGEO1572
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 016JW
UT WOS:000309515100024
ER
PT J
AU Kellogg, JR
Schlippert, D
Kohel, JM
Thompson, RJ
Aveline, DC
Yu, N
AF Kellogg, James R.
Schlippert, Dennis
Kohel, James M.
Thompson, Robert J.
Aveline, David C.
Yu, Nan
TI A compact high-efficiency cold atom beam source
SO APPLIED PHYSICS B-LASERS AND OPTICS
LA English
DT Article
ID 2-DIMENSIONAL MAGNETOOPTICAL TRAP; SLOW
AB We report on a compact high-efficiency Cs slow atom beam source based on a retro-reflected two-dimensional magneto-optical trap (2D MOT). Employing two laser beams in an angled retro-reflected setup, we achieve 3D MOT loading rates greater than 8 x 10(9) atoms/s using only 20 mW of total laser power for the source.
C1 [Kellogg, James R.; Kohel, James M.; Thompson, Robert J.; Aveline, David C.; Yu, Nan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Schlippert, Dennis] Leibniz Univ Hannover, Inst Quantenopt, D-30167 Hannover, Germany.
RP Yu, N (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM nan.yu@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX We thank P. Hamilton and H. Muller for helpful discussions. This
research was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. (C)2011 California Institute of Technology.
Government sponsorship acknowledged
NR 14
TC 3
Z9 3
U1 3
U2 16
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0946-2171
EI 1432-0649
J9 APPL PHYS B-LASERS O
JI Appl. Phys. B-Lasers Opt.
PD OCT
PY 2012
VL 109
IS 1
BP 61
EP 64
DI 10.1007/s00340-012-5220-5
PG 4
WC Optics; Physics, Applied
SC Optics; Physics
GA 032UD
UT WOS:000310743700010
ER
PT J
AU Kane, SR
Gelino, DM
AF Kane, Stephen R.
Gelino, Dawn M.
TI The Habitable Zone and Extreme Planetary Orbits
SO ASTROBIOLOGY
LA English
DT Article
DE Extrasolar planets; Habitable zone; Astrobiology
ID MAIN-SEQUENCE STARS; EXTRASOLAR PLANET; HD 189733B; EXOMOONS; EVOLUTION;
CLIMATES; DETECTABILITY; GREENHOUSE; ATMOSPHERE; EXOPLANET
AB The habitable zone for a given star describes the range of circumstellar distances from the star within which a planet could have liquid water on its surface, which depends upon the stellar properties. Here we describe the development of the habitable zone concept, its application to our own solar system, and its subsequent application to exoplanetary systems. We further apply this to planets in extreme eccentric orbits and show how they may still retain life-bearing properties depending upon the percentage of the total orbit which is spent within the habitable zone.
C1 [Kane, Stephen R.; Gelino, Dawn M.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RP Kane, SR (reprint author), CALTECH, NASA, Exoplanet Sci Inst, MS 100-22,770 S Wilson Ave, Pasadena, CA 91125 USA.
EM skane@ipac.caltech.edu
RI Kane, Stephen/B-4798-2013
NR 48
TC 16
Z9 16
U1 2
U2 26
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD OCT
PY 2012
VL 12
IS 10
BP 940
EP 945
DI 10.1089/ast.2011.0798
PG 6
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 025TQ
UT WOS:000310217900004
PM 23035897
ER
PT J
AU Race, M
Denning, K
Bertka, CM
Dick, SJ
Harrison, AA
Impey, C
Mancinelli, R
AF Race, Margaret
Denning, Kathryn
Bertka, Constance M.
Dick, Steven J.
Harrison, Albert A.
Impey, Christopher
Mancinelli, Rocco
CA Workshop Participants
TI Astrobiology and Society: Building an Interdisciplinary Research
Community
SO ASTROBIOLOGY
LA English
DT Article
DE Astrobiology; Extraterrestrial life; Life detection
AB This paper reports recent efforts to gather experts from the humanities and social sciences along with astrobiologists to consider the cultural, societal, and psychological implications of astrobiology research and exploration. We began by convening a workshop to draft a research roadmap on astrobiology's societal implications and later formed a Focus Group on Astrobiology and Society under the auspices of the NASA Astrobiology Institute (NAI). Just as the Astrobiology Science Roadmap and various astrobiology science focus groups have helped researchers orient and understand their work across disciplinary contexts, our intent was to apply the same approach to examine areas beyond the physical and life sciences and expand interdisciplinary interaction and scholarly understanding. These efforts continue as an experiment in progress, with an open invitation to interested researchers-astrobiologists as well as scholars in the humanities and social sciences-to become involved in research, analysis, and proactive discussions concerning the potential impacts of astrobiology on society as well as the possible impacts of society on progress in astrobiology.
C1 [Race, Margaret] SETI Inst CSC, Mountain View, CA 94043 USA.
[Denning, Kathryn] York Univ, Dept Anthropol, Toronto, ON M3J 2R7, Canada.
[Bertka, Constance M.] Sci & Soc Resources, Potomac, MD USA.
[Dick, Steven J.] Smithsonian NASA, Washington, DC USA.
[Harrison, Albert A.] Univ Calif Davis, Dept Psychol, Davis, CA 95616 USA.
[Impey, Christopher] Univ Arizona, Steward Observ, Dept Astron, Tucson, AZ USA.
[Mancinelli, Rocco] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
RP Race, M (reprint author), SETI Inst CSC, 189 Bernardo Ave, Mountain View, CA 94043 USA.
EM mrace@seti.org
FU NAI DDF
FX The development of ideas and plans reported in this paper was supported
in several ways: by a grant from the NAI DDF to M. Race and R.
Mancinelli for the 2009 Workshop on Astrobiology Societal Issues; by the
SETI Institute for workshop location and logistical support; and by the
contributions of assorted experts who participated in the 2009 workshop.
Additional support for database development was supplied by a separate
grant from the NAI DDF to K. Denning and L. Moreno.
NR 16
TC 2
Z9 2
U1 1
U2 6
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD OCT
PY 2012
VL 12
IS 10
BP 958
EP 965
DI 10.1089/ast.2011.0723
PG 8
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 025TQ
UT WOS:000310217900007
PM 23046203
ER
PT J
AU Weitkamp, LA
Bentley, PJ
Litz, MNC
AF Weitkamp, Laurie A.
Bentley, Paul J.
Litz, Marisa N. C.
TI Seasonal and interannual variation in juvenile salmonids and associated
fish assemblage in open waters of the lower Columbia River estuary
SO FISHERY BULLETIN
LA English
DT Article
ID DOUBLE-CRESTED CORMORANTS; CHINOOK SALMON; COMMUNITY STRUCTURE; PACIFIC
SALMON; AMERICAN SHAD; ONCORHYNCHUS-KISUTCH; SPECIES COMPOSITION;
FORAGING PATTERNS; WILLAMETTE RIVER; CASPIAN TERNS
AB The transition between freshwater and marine environments is associated with high mortality for juvenile anadromous salmonids, yet little is known about this critical period in many large rivers. To address this deficiency, we investigated the estuarine ecology of juvenile salmonids and their associated fish assemblage in open-water habitats of the lower Columbia River estuary during spring of 2007-10. For coho (Oncorhynchus kisutch), sockeye (O. nerka), chum (O. keta), and yearling (age 1.0) Chinook (O. tshawytscha) salmon, and steelhead (O. mykiss), we observed a consistent seasonal pattern characterized by extremely low abundances in mid-April, maximum abundances in May, and near absence by late June. Subyearling (age 0.0) Chinook salmon were most abundant in late June. Although we observed interannual variation in the presence, abundance, and size of juvenile salmonids, no single year was exceptional across all species-and-age classes. We estimated that >90% of juvenile Chinook and coho salmon and steelhead were of hatchery origin, a rate higher than previously reported. In contrast to juvenile salmonids, the abundance and composition of the greater estuarine fish assemblage, of which juvenile salmon were minor members, were extremely variable and likely responding to dynamic physical conditions in the estuary. Comparisons with studies conducted 3 decades earlier suggest striking changes in the estuarine fish assemblage changes that have unknown but potentially important consequences for juvenile salmon in the Columbia River estuary.
C1 [Weitkamp, Laurie A.] NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Conservat Biol Div, Newport Res Stn, Newport, OR 97365 USA.
[Bentley, Paul J.] NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Point Adams Res Stn, Fish Ecol Div, Hammond, OR 97121 USA.
[Litz, Marisa N. C.] Oregon State Univ, Hatfield Marine Sci Ctr, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA.
RP Weitkamp, LA (reprint author), NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Conservat Biol Div, Newport Res Stn, 2032 SE Marine Sci Dr, Newport, OR 97365 USA.
EM laurie.weitkamp@noaa.gov
FU Northwest Fisheries Science Center; Bonneville Power Administration
FX This research was conducted under Oregon Scientific Research Permits
OR2007-3920, OR2008-3265, 14480, and 15374, and NOAA Fisheries Service
ESA Permit 1290-6M. This work was only possible with an exceptional
field crew, including C. Johnson, T. Sandel, P. Peterson, A. Claiborne,
and A. Claxton, and boat operators C. Taylor, B. Kelly, and R. Nelson.
B. Emmett, S. Hinton, and G. McCabe developed the original idea for this
study and provided considerable insight and guidance. This study was
funded by the Northwest Fisheries Science Center and Bonneville Power
Administration. The manuscript was greatly improved by constructive
comments provided by R. Gustafson, D. Bottom, M. Ford, and J. Kocik.
NR 82
TC 28
Z9 28
U1 1
U2 34
PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE
PI SEATTLE
PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA
SN 0090-0656
J9 FISH B-NOAA
JI Fish. Bull.
PD OCT
PY 2012
VL 110
IS 4
BP 426
EP 450
PG 25
WC Fisheries
SC Fisheries
GA 030HM
UT WOS:000310561700004
ER
PT J
AU Loughner, CP
Allen, DJ
Zhang, DL
Pickering, KE
Dickerson, RR
Landry, L
AF Loughner, Christopher P.
Allen, Dale J.
Zhang, Da-Lin
Pickering, Kenneth E.
Dickerson, Russell R.
Landry, Laura
TI Roles of Urban Tree Canopy and Buildings in Urban Heat Island Effects:
Parameterization and Preliminary Results
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID AIR-QUALITY; CLIMATE-CHANGE; SHADE TREES; PART I; MODEL; ENERGY; OZONE;
HOUSTON; WEATHER; IMPACT
AB Urban heat island (UHI) effects can strengthen heat waves and air pollution episodes. In this study, the dampening impact of urban trees on the UHI during an extreme heat wave in the Washington, D. C., and Baltimore, Maryland, metropolitan area is examined by incorporating trees, soil, and grass into the coupled Weather Research and Forecasting model and an urban canopy model (WRF-UCM). By parameterizing the effects of these natural surfaces alongside roadways and buildings, the modified WRF-UCM is used to investigate how urban trees, soil, and grass dampen the UHI. The modified model was run with 50% tree cover over urban roads and a 10% decrease in the width of urban streets to make space for soil and grass alongside the roads and buildings. Results show that, averaged over all urban areas, the added vegetation decreases surface air temperature in urban street canyons by 4.1 K and road-surface and building-wall temperatures by 15.4 and 8.9 K, respectively, as a result of tree shading and evapotranspiration. These temperature changes propagate downwind and alter the temperature gradient associated with the Chesapeake Bay breeze and, therefore, alter the strength of the bay breeze. The impact of building height on the UHI shows that decreasing commercial building heights by 8 m and residential building heights by 2.5 m results in up to 0.4-K higher daytime surface and near-surface air temperatures because of less building shading and up to 1.2-K lower nighttime temperatures because of less longwave radiative trapping in urban street canyons.
C1 [Loughner, Christopher P.; Pickering, Kenneth E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Loughner, Christopher P.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Allen, Dale J.; Zhang, Da-Lin; Dickerson, Russell R.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Landry, Laura] Maryland Dept Environm, Baltimore, MD 21224 USA.
RP Loughner, CP (reprint author), NASA, Goddard Space Flight Ctr, Code 614, Greenbelt, MD 20771 USA.
EM christopher.p.loughner@nasa.gov
RI Zhang, Da-Lin/F-2634-2010; Pickering, Kenneth/E-6274-2012; Dickerson,
Russell/F-2857-2010; Allen, Dale/F-7168-2010;
OI Zhang, Da-Lin/0000-0003-1725-283X; Dickerson,
Russell/0000-0003-0206-3083; Allen, Dale/0000-0003-3305-9669; Loughner,
Christopher/0000-0002-3833-2014
FU NASA [NNX06AF57H, NNX08AR426]; Maryland Department of the Environment
FX This work was funded by NASA Grant NNX06AF57H ("How do changes to the
urban environment affect precipitation and air quality?") and NASA Grant
NNX08AR426 ("Tropospheric transport processes for trace gases and
aerosols."). We also acknowledge the Maryland Department of the
Environment for their support and for allowing use of their observed
surface temperature and wind data.
NR 47
TC 24
Z9 27
U1 5
U2 93
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD OCT
PY 2012
VL 51
IS 10
BP 1775
EP 1793
DI 10.1175/JAMC-D-11-0228.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 027NK
UT WOS:000310359200005
ER
PT J
AU Smith, WL
Minnis, P
Fleeger, C
Spangenberg, D
Palikonda, R
Nguyen, L
AF Smith, William L., Jr.
Minnis, Patrick
Fleeger, Cecilia
Spangenberg, Douglas
Palikonda, Rabindra
Louis Nguyen
TI Determining the Flight Icing Threat to Aircraft with Single-Layer Cloud
Parameters Derived from Operational Satellite Data
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID PART I; WATER
AB An algorithm is developed to determine the flight icing threat to aircraft utilizing quantitative information on clouds derived from meteorological satellite data as input. Algorithm inputs include the satellite-derived cloud-top temperature, thermodynamic phase, water path, and effective droplet size. The icing-top and -base altitude boundaries are estimated from the satellite-derived cloud-top and -base altitudes using the freezing level obtained from numerical weather analyses or a lapse-rate approach. The product is available at the nominal resolution of the satellite pixel. Aircraft pilot reports (PIREPs) over the United States and southern Canada provide direct observations of icing and are used extensively in the algorithm development and validation on the basis of correlations with Geostationary Operational Environmental Satellite imager data. Verification studies using PIREPs, Tropospheric Airborne Meteorological Data Reporting, and NASA Icing Remote Sensing System data indicate that the satellite algorithm performs reasonably well, particularly during the daytime. The algorithm is currently being run routinely using data taken from a variety of satellites across the globe and is providing useful information on icing conditions at high spatial and temporal resolutions that are unavailable from any other source.
C1 [Smith, William L., Jr.; Minnis, Patrick; Louis Nguyen] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Fleeger, Cecilia; Spangenberg, Douglas; Palikonda, Rabindra] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Smith, WL (reprint author), NASA, Langley Res Ctr, MS 420, Hampton, VA 23681 USA.
EM william.l.smith@nasa.gov
RI Minnis, Patrick/G-1902-2010
OI Minnis, Patrick/0000-0002-4733-6148
FU NASA Applied Sciences Program; NOAA GOES-R program
FX This research was supported by the NASA Applied Sciences Program and by
the NOAA GOES-R program. We thank David Serke of NCAR-RAL and Andrew
Reehorst of NASA Glenn Research Center for providing the NIRSS data and
for useful discussions regarding its use. We also thank the three
anonymous reviewers for their valuable comments and suggestions. The
views, opinions, and findings contained in this report are those of the
author(s) and should not be construed as an official NASA or U.S.
government position, policy, or decision.
NR 35
TC 2
Z9 2
U1 1
U2 11
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD OCT
PY 2012
VL 51
IS 10
BP 1794
EP 1810
DI 10.1175/JAMC-D-12-057.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 027NK
UT WOS:000310359200006
ER
PT J
AU Pearson, JC
Yu, SS
Drouin, BJ
AF Pearson, John C.
Yu, Shanshan
Drouin, Brian J.
TI The ground state torsion rotation spectrum of CH2DOH
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Internal rotation; Torsion; Rotational spectroscopy
ID FAR-INFRARED LASER; DEUTERATED METHANOL; INTERNAL-ROTATION;
ASYMMETRIC-TOP; FREQUENCY MEASUREMENTS; MICROWAVE-SPECTRUM; SOLID
METHANOL; FIR LASER; LINES; TRANSITIONS
AB The ground state torsion rotation spectrum of CH2DOH has been completely characterized through J = 30 and K-a = 10, 9, 9 in the three torsional sub-states of the ground state; e(0), e(1), and o(1). respectively. Additional a-type assignments are presented to K-a = 11 in each of the torsional sub-states. The data has been analyzed with an empirical power series model as well as an empirical internal axis model. Over 8000 transitions have been assigned and fit with near experimental accuracy over the range of 4-1628 GHz. The characterization of the spectrum allows for a complete set of ground state term values enabling a better understanding of the infrared spectrum. Comparison of the torsional contributions of the Hamiltonian with normal methanol provides great insight into the nature of the asymmetric-top asymmetric-frame internal rotation problem. The comparison with normal methanol also provides a relatively straightforward transformation from the well understood C-3v internal rotation problem to the completely asymmetric internal rotation problem. The data and analysis provide some practical wisdom on the impacts of breaking the symmetry and the choice of models for addressing the nearly three fold completely asymmetric internal rotation problem. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Pearson, John C.; Yu, Shanshan; Drouin, Brian J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Pearson, JC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM John.C.Pearson@jpl.nasa.gov
RI Yu, Shanshan/D-8733-2016
FU NASA Herschel Science Center; Astrophysics Research and Analysis Program
FX This research was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration. The present study benefitted greatly from a
laboratory astrophysics grant from the NASA Herschel Science Center and
support from the Astrophysics Research and Analysis Program. We would
like to thank Frank De Lucia and Rebecca Buttler for collecting the
FASSST spectrum and answering numerous questions regarding individual
spectral features and the spectral calibration. We would also like to
thank Rick Suenram for his unassigned Stark data and Steve Kukolich for
the use of his Fourier Transform microwave spectrometer. Most
importantly this work would not have been possible without the insight
and curiosity into this class of problems provided by Herbert Pickett.
NR 69
TC 16
Z9 16
U1 1
U2 15
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
EI 1096-083X
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD OCT
PY 2012
VL 280
SI SI
BP 119
EP 133
DI 10.1016/j.jms.2012.06.012
PG 15
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 031OW
UT WOS:000310652800018
ER
PT J
AU Kisiel, Z
Pszczolkowski, L
Drouin, BJ
Brauer, CS
Yu, SS
Pearson, JC
Medvedev, IR
Fortman, S
Neese, C
AF Kisiel, Zbigniew
Pszczolkowski, Lech
Drouin, Brian J.
Brauer, Carolyn S.
Yu, Shanshan
Pearson, John C.
Medvedev, Ivan R.
Fortman, Sarah
Neese, Christopher
TI Broadband rotational spectroscopy of acrylonitrile: Vibrational energies
from perturbations
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Broadband spectroscopy; Rotational spectrum; THz-spectrum; Interstate
perturbations; Techniques of analysis; Vibrational energies
ID CHLORINE NITRATE CLONO2; SUBMILLIMETER-WAVE SPECTRUM; ELECTRIC-DIPOLE
MOMENTS; MILLIMETER-WAVE; VINYL CYANIDE; MOLECULAR-STRUCTURE;
HYPERFINE-STRUCTURE; MICROWAVE-SPECTRUM; DIETHYL-ETHER; STATES
AB The coverage of the room-temperature rotational spectrum of acrylonitrile has been expanded to a total of 1170 GHz, by recording broadband spectral segments at frequencies ranging 90-1900 GHz. This corresponds, in total, to 61.6% coverage of the rotational spectrum up to 1.9 THz and facilitated an in depth study of rotational transitions in the lowest vibrational states of acrylonitrile and up to large values of rotational quantum numbers. Multiple perturbations between the four lowest vibrational states of the molecule have been identified and successfully fitted within the framework of a coupled four state Hamiltonian. The fit encompasses over 12 500 measured transition frequencies, and delivers precise wave-numbers for the three lowest excited vibrational states entirely on the basis of perturbations in the rotational spectrum: nu(11) = 228.29986(2), nu(15) = 332.67811(2), and 2 nu(11) = 457.17496(2) cm(-1). The new results are compared with ab initio anharmonic force field calculations and the techniques used to deal in an efficient manner with a broadband, high-resolution spectrum of this type are also described in some detail. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Kisiel, Zbigniew; Pszczolkowski, Lech] Polish Acad Sci, Inst Phys, PL-02668 Warsaw, Poland.
[Drouin, Brian J.; Brauer, Carolyn S.; Yu, Shanshan; Pearson, John C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Medvedev, Ivan R.] Wright State Univ, Dept Phys, Dayton, OH 45435 USA.
[Fortman, Sarah; Neese, Christopher] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
RP Kisiel, Z (reprint author), Polish Acad Sci, Inst Phys, Al Lotnikow 32-46, PL-02668 Warsaw, Poland.
EM kisiel@ifpan.edu.pl
RI Medvedev, Ivan/E-8486-2014; Yu, Shanshan/D-8733-2016; Kisiel,
Zbigniew/K-8798-2016; Pszczolkowski, Lech/S-3018-2016
OI Kisiel, Zbigniew/0000-0002-2570-3154;
FU Army Research Office (OSU); Institute of Physics of the Polish Academy
of Sciences (Warsaw)
FX The authors thank Benjamin Moran for assistance with collecting data at
Wright State University and Adam Kragnicki for the ab initio
calculations. Financial support from the Army Research Office (OSU) and
from the Institute of Physics of the Polish Academy of Sciences (Warsaw)
is gratefully acknowledged. This paper presents research carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration.
NR 46
TC 22
Z9 22
U1 3
U2 21
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD OCT
PY 2012
VL 280
SI SI
BP 134
EP 144
DI 10.1016/j.jms.2012.06.013
PG 11
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 031OW
UT WOS:000310652800019
ER
PT J
AU Friedmann, PP
Johnson, W
Scully, MP
AF Friedmann, Peretz P.
Johnson, Wayne
Scully, Michael P.
TI A Tribute to Professor Rene H. Miller: A Pioneer in Aeromechanics and
Rotary Wing Flight Transportation
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Biographical-Item
AB Rene H. Miller (May 19, 1916 January 28, 2003), Emeritus H. N. Slater Professor of Flight Transportation at the Massachusetts Institute of Technology, was one of the most influential pioneers in rotary wing aeromechanics as well as a visionary whose dream was the development of a tilt-wing/tilt-rotor-based, short-haul air transportation system. This paper pays a long overdue tribute to his memory and to his extraordinary contributions.
C1 [Friedmann, Peretz P.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Johnson, Wayne; Scully, Michael P.] NASA, Ames Res Ctr, USA RDECOM, Aeroflightdynam Directorate AMRDEC, Moffett Field, CA 94035 USA.
RP Friedmann, PP (reprint author), Univ Michigan, Ann Arbor, MI 48109 USA.
EM peretzf@umich.edu
NR 1
TC 0
Z9 0
U1 0
U2 1
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD OCT
PY 2012
VL 57
IS 4
AR 042004
DI 10.4050/JAHS.57.042004
PG 8
WC Engineering, Aerospace
SC Engineering
GA 031WD
UT WOS:000310672400004
ER
PT J
AU van Acken, D
Brandon, AD
Lapen, TJ
AF van Acken, David
Brandon, Alan D.
Lapen, Thomas J.
TI Highly siderophile element and osmium isotope evidence for postcore
formation magmatic and impact processes on the aubrite parent body
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID COUNTY ENSTATITE ACHONDRITE; FALLS CHONDRITIC INCLUSIONS; EARLY
SOLAR-SYSTEM; CUMBERLAND FALLS; IRON-METEORITES; CORE FORMATION;
LIQUID-METAL; HIGH-TEMPERATURES; TRACE-ELEMENTS; MARTIAN MANTLE
AB Aubrites exhibit a wide range of highly siderophile element (HSERe, Os, Ir, Ru, Rh, Pt, Pd, Au) concentrations and 187Os/188Os compositions. Their HSE concentrations are one to three orders of magnitude less than chondrites, with the exception of the Shallowater and Mt. Egerton samples. While most aubrites show chondritic HSE abundance ratios, significant enrichments of Pd and Re relative to Os, Ir, and Ru are observed in 12 of 16 samples. Present-day 187Os/188Os ratios range from subchondritic values of 0.1174 to superchondritic values of up to 0.2263. Half of the samples have 187Os/188Os ratios of 0.127 to 0.130, which is in the range of enstatite chondrites. Along with the brecciated nature of aubrites, the HSE and Re-Os isotope systematics support a history of extensive postaccretion processing, including core formation, late addition of chondritic material and/or core material and potential breakup and reassembly. Highly siderophile element signatures for some aubrites are consistent with a mixing of HSE-rich chondritic fragments with a HSE-free aubrite matrix. The enrichments in incompatible HSE such as Pd and Re observed in some aubrites, reminiscent of terrestrial basalts, suggest an extensive magmatic and impact history, which is supported by both the 187Re-187Os isotope system and silicate-hosted isotope systems (Rb-Sr, K-Ar) yielding young formation ages of 1.33.9 Ga for a subset of samples. Compared with other differentiated achondrites derived from small planetary bodies, aubrites show a wide range in HSE concentrations and 187Os/188Os, most similar to angrites. While similarities exist between the diverse groups of achondrites formed early in solar system history, the aubrite parent body(ies) clearly underwent a distinct evolution, different from angrites, brachinites, ureilites, howardites, eucrites, and diogenites.
C1 [van Acken, David; Brandon, Alan D.; Lapen, Thomas J.] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA.
[van Acken, David] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[van Acken, David] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada.
RP van Acken, D (reprint author), Univ Houston, Dept Earth & Atmospher Sci, 312 Sci & Res 1, Houston, TX 77204 USA.
EM vanacken@ualberta.ca
FU ORAU postdoctoral fellowship; NASA Cosmochemistry program [NNX10AB37G,
NNX12AD06G, NNX09AC06G]
FX Samples for this study were kindly provided by the Meteorite Working
Group, Johnson Space Center, Arizona State University, University of New
Mexico, the Monnig Collection, Texas Christian University, Smithsonian
National Museum of Natural History, Natural History Museum London, and
Western Australian Museum. D. v. A. was supported by an ORAU
postdoctoral fellowship. We appreciate discussions with T. McCoy, A.
Riches, J. M. D. Day, and M. Humayun. We thank M. Righter, J. T. Shafer,
Y. Gao, and J. I. Simon for technical support; J. M. D. Day, M. Horan,
and C. Dale for their constructive reviews; and N. Chabot for editorial
handling. This work was supported by the NASA Cosmochemistry program
through grants NNX10AB37G and NNX12AD06G to A. D. Brandon and NNX09AC06G
to T. J. Lapen.
NR 99
TC 8
Z9 8
U1 2
U2 23
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 OCT
PY 2012
VL 47
IS 10
BP 1606
EP 1623
DI 10.1111/j.1945-5100.2012.01425.x
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 034JV
UT WOS:000310869800005
ER
PT J
AU Smets, R
Belmont, G
Aunai, N
AF Smets, R.
Belmont, G.
Aunai, N.
TI Electric and magnetic contributions to spatial diffusion in
collisionless plasmas
SO PHYSICS OF PLASMAS
LA English
DT Article
ID PERPENDICULAR DIFFUSION; CHARGED-PARTICLES; SOLAR-WIND; TURBULENCE;
FIELD
AB We investigate the role played by the different self-consistent fluctuations for particle diffusion in a magnetized plasma. We focus especially on the contribution of the electric fluctuations and how it combines with the (already investigated) magnetic fluctuations and with the velocity fluctuations. For that issue, we compute with a hybrid code the value of the diffusion coefficient perpendicular to the mean magnetic field and its dependence on the particle velocity. This study is restricted to small to intermediate level of electromagnetic fluctuations and focuses on particle velocities on the order of few times the Alfven speed. We briefly discuss the consequences for cosmic ray modulation and for the penetration of thermal solar wind particles in the Earth magnetosphere. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4762845]
C1 [Smets, R.; Belmont, G.] UPMC, Ecole Polytech, CNRS, Lab Phys Plasmas, Paris, France.
[Aunai, N.] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Smets, R (reprint author), UPMC, Ecole Polytech, CNRS, Lab Phys Plasmas, Paris, France.
EM roch.smets@lpp.polytechnique.fr
NR 23
TC 0
Z9 0
U1 0
U2 2
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1070-664X
EI 1089-7674
J9 PHYS PLASMAS
JI Phys. Plasmas
PD OCT
PY 2012
VL 19
IS 10
AR 102309
DI 10.1063/1.4762845
PG 8
WC Physics, Fluids & Plasmas
SC Physics
GA 030VE
UT WOS:000310597400023
ER
PT J
AU Poldrack, RA
Mumford, JA
Schonberg, T
Kalar, D
Barman, B
Yarkoni, T
AF Poldrack, Russell A.
Mumford, Jeanette A.
Schonberg, Tom
Kalar, Donald
Barman, Bishal
Yarkoni, Tal
TI Discovering Relations Between Mind, Brain, and Mental Disorders Using
Topic Mapping
SO PLOS COMPUTATIONAL BIOLOGY
LA English
DT Article
ID NEUROIMAGING TELL; NEUROSCIENCE; SCIENCE
AB Neuroimaging research has largely focused on the identification of associations between brain activation and specific mental functions. Here we show that data mining techniques applied to a large database of neuroimaging results can be used to identify the conceptual structure of mental functions and their mapping to brain systems. This analysis confirms many current ideas regarding the neural organization of cognition, but also provides some new insights into the roles of particular brain systems in mental function. We further show that the same methods can be used to identify the relations between mental disorders. Finally, we show that these two approaches can be combined to empirically identify novel relations between mental disorders and mental functions via their common involvement of particular brain networks. This approach has the potential to discover novel endophenotypes for neuropsychiatric disorders and to better characterize the structure of these disorders and the relations between them.
C1 [Poldrack, Russell A.; Mumford, Jeanette A.; Schonberg, Tom] Univ Texas Austin, Imaging Res Ctr, Austin, TX 78712 USA.
[Poldrack, Russell A.; Mumford, Jeanette A.; Schonberg, Tom] Univ Texas Austin, Dept Psychol, Austin, TX 78712 USA.
[Poldrack, Russell A.; Mumford, Jeanette A.; Schonberg, Tom] Univ Texas Austin, Dept Neurobiol, Austin, TX 78712 USA.
[Kalar, Donald] NASA Ames Res Ctr, Mountain View, CA USA.
[Barman, Bishal] Univ Texas Austin, Dept Elect & Comp Engn, Austin, TX 78712 USA.
[Yarkoni, Tal] Univ Colorado, Dept Psychol, Boulder, CO 80309 USA.
RP Poldrack, RA (reprint author), Univ Texas Austin, Imaging Res Ctr, Austin, TX 78712 USA.
EM poldrack@mail.utexas.edu
OI Schonberg, Tom/0000-0002-4485-816X
FU NIH [RO1MH082795, F32NR012081]; Texas Emerging Technology Fund
FX This work was supported by NIH grant RO1MH082795 (to RAP) and
F32NR012081 (to TY) and by the Texas Emerging Technology Fund. The
funders had no role in study design, data collection and analysis,
decision to publish, or preparation of the manuscript
NR 26
TC 23
Z9 23
U1 0
U2 17
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1553-7358
J9 PLOS COMPUT BIOL
JI PLoS Comput. Biol.
PD OCT
PY 2012
VL 8
IS 10
AR e1002707
DI 10.1371/journal.pcbi.1002707
PG 14
WC Biochemical Research Methods; Mathematical & Computational Biology
SC Biochemistry & Molecular Biology; Mathematical & Computational Biology
GA 030KE
UT WOS:000310568800008
PM 23071428
ER
PT J
AU Hicks, BC
Paravastu-Dalal, N
Stewart, KP
Erickson, WC
Ray, PS
Kassim, NE
Burns, S
Clarke, T
Schmitt, H
Craig, J
Hartman, J
Weiler, KW
AF Hicks, Brian C.
Paravastu-Dalal, Nagini
Stewart, Kenneth P.
Erickson, William C.
Ray, Paul S.
Kassim, Namir E.
Burns, Steve
Clarke, Tracy
Schmitt, Henrique
Craig, Joe
Hartman, Jake
Weiler, Kurt W.
TI A Wide-Band, Active Antenna System for Long Wavelength Radio Astronomy
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID LARGE ARRAY; 6C SURVEY; 74 MHZ; TELESCOPE; LOFAR; SKY
AB We describe an "active" antenna system for HF/VHF (long wavelength) radio astronomy that has been successfully deployed 256-fold as the first station (LWA1) of the planned Long Wavelength Array. The antenna system, consisting of crossed dipoles, an active balun/preamp, a support structure, and a ground screen has been shown to successfully operate over at least the band from 20 MHz (15 m wavelength) to 80 MHz (3.75 m wavelength) with a noise figure that is at least 6 dB better than the Galactic background emission-noise temperature over that band. Thus, we met the goal to design and construct a compact, inexpensive, rugged, and easily assembled antenna system that can be deployed many-fold to form numerous large individual "stations" for the purpose of building a large, long wavelength synthesis array telescope for radio astronomical and ionospheric observations.
C1 [Hicks, Brian C.; Stewart, Kenneth P.; Ray, Paul S.; Kassim, Namir E.; Clarke, Tracy; Schmitt, Henrique] USN, Res Lab, Washington, DC 20375 USA.
[Paravastu-Dalal, Nagini] Northrop Grumman Aerosp Syst, Redondo Beach, CA 90278 USA.
[Erickson, William C.] Univ Tasmania, Sandy Bay, Tas 7005, Australia.
[Craig, Joe] Univ New Mexico, Albuquerque, NM 87131 USA.
[Hartman, Jake] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Weiler, Kurt W.] Computat Phys Inc, Springfield, VA 22151 USA.
RP Hicks, BC (reprint author), USN, Res Lab, Code 7213, Washington, DC 20375 USA.
EM Nagini.Dalal@ngc.com; Kenneth.Stewart@nrl.navy.mil;
bill.erickson@utas.edu; Paul.Ray@nrl.navy.mil;
info@burnsindustriesinc.com; Henrique.Schmitt@nrl.navy.mil;
joecraig@unm.edu; Jacob.M.Hartman@jpl.nasa.gov;
Kurt.Weiler@weilerhome.org
OI Ray, Paul/0000-0002-5297-5278
NR 66
TC 10
Z9 10
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD OCT
PY 2012
VL 124
IS 920
BP 1090
EP 1104
DI 10.1086/668121
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030MJ
UT WOS:000310574500007
ER
PT J
AU Howell, SB
Horch, EP
Everett, ME
Ciardi, DR
AF Howell, Steve B.
Horch, Elliott P.
Everett, Mark E.
Ciardi, David R.
TI Speckle Camera Imaging of the Planet Pluto
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID BINARY STARS; STELLAR OCCULTATION; MOON CHARON; INTERFEROMETRY;
SATELLITES; ATMOSPHERE; PHOTOMETRY; SURFACE; RADIUS; JUNE
AB We have obtained optical wavelength (692 nm and 880 nm) speckle imaging of the planet Pluto and its largest moon Charon. Using our DSSI speckle camera attached to the Gemini North 8 m telescope, we collected high resolution imaging with an angular resolution of similar to 20 mas, a value at the Gemini-N telescope diffraction limit. We have produced for this binary system the first speckle reconstructed images, from which we can measure not only the orbital separation and position angle for Charon, but also the diameters of the two bodies. Our measurements of these parameters agree, within the uncertainties, with the current best values for Pluto and Charon. The Gemini-N speckle observations of Pluto are presented to illustrate the capabilities of our instrument and the robust production of high accuracy, high spatial resolution reconstructed images. We hope our results will suggest additional applications of high resolution speckle imaging for other objects within our solar system and beyond.
C1 [Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Horch, Elliott P.] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA.
[Horch, Elliott P.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RP Howell, SB (reprint author), Gemini N Telescope, 670 N Aohoku Pl, Hilo, HI USA.
OI Ciardi, David/0000-0002-5741-3047
FU Gemini Science Program [GN-2012A-DD-8]; NASA Kepler discovery mission
FX The ground-based observations reported on herein were obtained at the
Gemini-N observatory as part of Gemini Science Program GN-2012A-DD-8.
The authors wish to thank Andy Adamson, Inger Jorgensen, Steve Hardash,
Andrew Stephens, Katherine Roth, Jennifer Holt, Jonathan Kemp, Jesse
Ball, Tony Matulonis, Harlan Uehara, Cooper Nakayama, Rody Kawaihae,
James Franco, Chris Yamasaki, Cy Bagano, Simon Chan, Mike Becher, Tim
Minick, Joseph D'Amato, John White, Arturo Nunez, Fred Chaffee, and
Nancy Levenson of Gemini-N without whom our visit and results could not
have been possible. Bill Merline kindly provided us with the calculated
parameters for Pluto and Charon during the time of our observations. We
want to extend a special thank you to the anonymous referee whose
expertise in Pluto and Charon, as well as their complete review, helped
make this a better paper. This research work was partially funded by the
NASA Kepler discovery mission.
NR 23
TC 4
Z9 4
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD OCT
PY 2012
VL 124
IS 920
BP 1124
EP 1131
DI 10.1086/668405
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 030MJ
UT WOS:000310574500010
ER
PT J
AU Guo, HQ
Meador, MAB
McCorkle, L
Quade, DJ
Guo, J
Hamilton, B
Cakmak, M
AF Guo, Haiquan
Meador, Mary Ann B.
McCorkle, Linda
Quade, Derek J.
Guo, Jiao
Hamilton, Bart
Cakmak, Miko
TI Tailoring Properties of Cross-Linked Polyimide Aerogels for Better
Moisture Resistance, Flexibility, and Strength
SO ACS APPLIED MATERIALS & INTERFACES
LA English
DT Article
DE polyimide; aerogel; mesoporous materials; cross-linking; insulation;
polyoligomeric silsesquioxane
AB Combinations of rigid and flexible aromatic diamines were used to tailor the properties of octa(aminophenyl)-silsesquioxane (OAPS) cross-linked polyimide aerogels. 2,2'-Dimethylbenzidine (DMBZ) or p-phenylenediamine (PPDA) was used in combination with the more-flexible diamine, 4,4'-oxydianiline (ODA). The amount of rigid diamine was varied from 0% to 100% of the total diamines in the backbone. The resulting aerogels vary in density, shrinkage, porosity, surface area, mechanical and thermal properties (depending on the type of diamine and the proportions of rigid diamine to flexible diamine used). Replacing ODA with PPDA increases shrinkage that occurs during gelation and processing, while increasing the DMBZ fraction decreases shrinkage. Replacing ODA with 50 mol % of DMBZ maintains the flexibility of thin films, while the moisture resistance of the aerogels is greatly improved.
C1 [Guo, Haiquan; McCorkle, Linda] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Meador, Mary Ann B.; Quade, Derek J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Guo, Jiao; Hamilton, Bart; Cakmak, Miko] Univ Akron, Natl Polymer Innovat Ctr, Akron, OH 44325 USA.
RP Guo, HQ (reprint author), Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA.
EM haiquan.n.guo@nasa.gov; maryann.meador@nasa.gov
OI Meador, Mary Ann/0000-0003-2513-7372
FU Fundamental Aeronautics Program (Hypersonics); Third Frontier Program of
the State of Ohio
FX We gratefully acknowledge support from the Fundamental Aeronautics
Program (Hypersonics). We also thank Daniel A. Scheiman, Zin
Technologies, Inc., for carrying out porosimetry and thermal analysis;
Baochau N. Nguyen, Ohio Aerospace Institute, for NMR spectra; and Anna
Palczer, for nitrogen sorption experiments. We also thank the Third
Frontier Program of the State of Ohio for funding the construction of
the roll-to-roll film manufacturing line.
NR 19
TC 40
Z9 47
U1 12
U2 121
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 OCT
PY 2012
VL 4
IS 10
BP 5422
EP 5429
DI 10.1021/am301347a
PG 8
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary
SC Science & Technology - Other Topics; Materials Science
GA 024KV
UT WOS:000310109000051
PM 22956659
ER
PT J
AU Adamczak, J
Werner, K
Rauch, T
Schuh, S
Drake, JJ
Kruk, JW
AF Adamczak, J.
Werner, K.
Rauch, T.
Schuh, S.
Drake, J. J.
Kruk, J. W.
TI Chandra grating spectroscopy of three hot white dwarfs
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE white dwarfs; stars: abundances; stars: atmospheres; stars: individual:
LB1919; stars: individual: GD246; stars: individual: PG1520+525
ID PG 1159 STARS; MASS-DISTRIBUTION; EQUILIBRIUM ABUNDANCES; RADIATIVE
LEVITATION; FUSE OBSERVATIONS; INTERSTELLAR; STELLAR; DIFFUSION; HELIUM;
LINES
AB Context. High-resolution soft X-ray spectroscopic observations of single hot white dwarfs are scarce. With the Chandra Low-Energy Transmission Grating, we have observed two white dwarfs, one is of spectral type DA (LB 1919) and the other is a non-DA of spectral type PG1159 (PG1520+525). The spectra of both stars are analyzed, together with an archival Chandra spectrum of another DA white dwarf (GD246).
Aims. The soft X-ray spectra of the two DA white dwarfs are investigated in order to study the effect of gravitational settling and radiative levitation of metals in their photospheres. LB1919 is of interest because it has a significantly lower metallicity than DAs with otherwise similar atmospheric parameters. GD246 is the only white dwarf known that shows identifiable individual iron lines in the soft X-ray range. For the PG1159 star, a precise effective temperature determination is performed in order to confine the position of the blue edge of the GW Vir instability region in the HRD.
Methods. The Chandra spectra are analyzed with chemically homogeneous as well as stratified NLTE model atmospheres that assume equilibrium between gravitational settling and radiative acceleration of chemical elements. Archival EUV and UV spectra obtained with EUVE, FUSE, and HST are utilized to support the analysis.
Results. No metals could be identified in LB1919. All observations are compatible with a pure hydrogen atmosphere. This is in stark contrast to the vast majority of hot DA white dwarfs that exhibit light and heavy metals and to the stratified models that predict significant metal abundances in the atmosphere. For GD246 we find that neither stratified nor homogeneous models can fit the Chandra spectrum. The Chandra spectrum of PG1520+525 constrains the effective temperature to T-eff = 150 000 +/- 10 000 K. Therefore, this nonpulsating star together with the pulsating prototype of the GWVir class (PG 1159-035) defines the location of the blue edge of the GWVir instability region. The result is in accordance with predictions from nonadiabatic stellar pulsation models. Such models are therefore reliable tools to investigate the interior structure of GW Vir variables.
Conclusions. Our soft X-ray study reveals that the understanding of metal abundances in hot DA white dwarf atmospheres is still incomplete. On the other hand, model atmospheres of hydrogen-deficient PG 1159-type stars are reliable and reproduce well the observed spectra from soft X-ray to optical wavelengths.
C1 [Adamczak, J.; Werner, K.; Rauch, T.] Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Adamczak, J.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Schuh, S.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kruk, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Adamczak, J (reprint author), Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany.
EM adamczak@astro.as.utexas.edu
FU German Research Foundation (DFG) [WE 1312/39-1]; German Aerospace Center
(DLR) [05 OR 0806]; NASA [NAS8-39073, NAS5-26555]; NASA Office of Space
Science [NNX09AF08G]
FX We thank the referee for a thorough and constructive report. J.A. and T.
R. were supported by the German Research Foundation (DFG) under grant WE
1312/39-1 and the German Aerospace Center (DLR) under grant 05 OR 0806,
respectively. J.J.D. was supported by NASA contract NAS8-39073 to the
Chandra X-ray Center during the course of this work. This research has
made use of the SIMBAD database, operated at CDS, Strasbourg, France.
Some of the data presented in this paper were obtained from the Mikulski
Archive for Space Telescopes (MAST). STScI is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS5-26555. Support for MAST for non-HST data is provided by
the NASA Office of Space Science via grant NNX09AF08G and by other
grants and contracts.
NR 59
TC 1
Z9 1
U1 0
U2 2
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2012
VL 546
AR A1
DI 10.1051/0004-6361/201219718
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 027JT
UT WOS:000310349100001
ER
PT J
AU Camero-Arranz, A
Pottschmidt, K
Finger, MH
Ikhsanov, NR
Wilson-Hodge, CA
Marcu, DM
AF Camero-Arranz, A.
Pottschmidt, K.
Finger, M. H.
Ikhsanov, N. R.
Wilson-Hodge, C. A.
Marcu, D. M.
TI 4U 1626-67 as seen by Suzaku before and after the 2008 torque reversal
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE accretion, accretion disks; binaries: close; stars: neutron; pulsars:
individual: 4U 1626-67; X-rays: binaries
ID X-RAY PULSAR; QUASI-PERIODIC OSCILLATIONS; NEUTRON-STARS; MAGNETIZED
STARS; ACCRETION DISCS; SPIN-DOWN; 4U-1626-67; BINARY; DISCOVERY;
SPECTRUM
AB Aims. The accretion-powered pulsar 4U1626-67 experienced a new torque reversal at the beginning of 2008, after about 18 years of steadily spinning down. The main goal of the present work is to study this recent torque reversal that occurred in February 2008.
Methods. We present a spectral analysis of this source using two pointed observations performed by Suzaku in March 2006 and in September 2010.
Results. We confirm with Suzaku the presence of a strong emission-line complex centered on 1 keV, with the strongest line being the hydrogen-like Ne Ly alpha at 1.025(3) keV. We were able to resolve this complex with up to seven emission lines. A dramatic increase in the intensity of the Ne Lya line after the 2008 torque reversal occurred, with the equivalent width of this line reaching almost the same value measured by ASCA in 1993. We also report on the detection of a cyclotron line feature centered at similar to 37 keV. In spite of the increase in the X-ray luminosity (0.5-100 keV) of a factor of similar to 2.8 that occurred between these two observations, no significant change in the energy of the cyclotron line feature was observed. However, the intensity of the similar to 1 keV line complex increased by an overall factor of similar to 8.
Conclusions. Our results favor a scenario in which the neutron star in 4U1626-67 accretes material from a geometrically thin disk during both the spin-up and spin-down phases.
C1 [Camero-Arranz, A.; Finger, M. H.] Univ Space Res Assoc, Huntsville, AL 35806 USA.
[Pottschmidt, K.; Marcu, D. M.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Pottschmidt, K.; Marcu, D. M.] CRESST, Baltimore, MD 21250 USA.
[Pottschmidt, K.; Marcu, D. M.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Finger, M. H.; Wilson-Hodge, C. A.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
[Ikhsanov, N. R.] Pulkovo Observ, St Petersburg 196140, Russia.
RP Camero-Arranz, A (reprint author), Univ Space Res Assoc, 6767 Old Madison Pike,Suite 450, Huntsville, AL 35806 USA.
EM camero@ice.csic.es
RI Ikhsanov, Nazar/M-9304-2015; XRAY, SUZAKU/A-1808-2009
OI Ikhsanov, Nazar/0000-0002-3326-5588;
FU NASA [NNX08AW06G, NNX11AE24G, NNX10AJ48G, NNX11AD41G]; Program N21 of
the Prezidium of RAS, Federal program "Scientific and pedagogical
brain-power of Russia" [XXXVII-1.2.1, NSH-1625.2012.2]
FX A.C.A. and M. H. F. acknowledge support from NASA grants NNX08AW06G and
NNX11AE24G. D. M. M. and K. P. acknowledge support from NASA grants
NNX10AJ48G and NNX11AD41G. N.R.I. acknowledges support from the Program
N21 of the Prezidium of RAS, Federal program "Scientific and pedagogical
brain-power of Russia" under the grant XXXVII-1.2.1 and NSH-1625.2012.2.
NR 48
TC 5
Z9 5
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2012
VL 546
AR A40
DI 10.1051/0004-6361/201219656
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 027JT
UT WOS:000310349100040
ER
PT J
AU Defrere, D
Lebreton, J
Le Bouquin, JB
Lagrange, AM
Absil, O
Augereau, JC
Berger, JP
di Folco, E
Ertel, S
Kluska, J
Montagnier, G
Millan-Gabet, R
Traub, W
Zins, G
AF Defrere, D.
Lebreton, J.
Le Bouquin, J. -B.
Lagrange, A. -M.
Absil, O.
Augereau, J. -C.
Berger, J. -P.
di Folco, E.
Ertel, S.
Kluska, J.
Montagnier, G.
Millan-Gabet, R.
Traub, W.
Zins, G.
TI Hot circumstellar material resolved around beta Pic with VLTI/PIONIER
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE instrumentation: high angular resolution; techniques: interferometric;
infrared: planetary systems
ID PICTORIS DISK; STARS; INTERFEROMETRY; CHARA/FLUOR; COMPANIONS; PLANETS;
DUST; VLTI; GAS
AB Aims. We aim at resolving the circumstellar environment around beta Pic in the near-infrared in order to study the inner planetary system (<200 mas, i.e., similar to 4 AU).
Methods. Precise interferometric fringe visibility measurements were obtained over seven spectral channels dispersed across the H band with the four-telescope VLTI/PIONIER interferometer. Thorough analysis of interferometric data was performed to measure the stellar angular diameter and to search for circumstellar material.
Results. We detected near-infrared circumstellar emission around beta Pic that accounts for 1.37% +/- 0.16% of the near-infrared stellar flux and that is located within the field-of-view of PIONIER (i.e., similar to 200 mas in radius). The flux ratio between this excess and the photosphere emission is shown to be stable over a period of 1 year and to vary only weakly across the H band, suggesting that the source is either very hot (greater than or similar to 1500 K) or dominated by the scattering of the stellar flux. In addition, we derive the limb-darkened angular diameter of beta Pic with an unprecedented accuracy (theta(LD)=0.736 +/- 0.019 mas).
Conclusions. The presence of a small H-band excess originating in the vicinity of beta Pic is revealed for the first time thanks to the high-precision visibilities enabled by VLTI/PIONIER. This excess emission is likely due to the scattering of stellar light by circumstellar dust and/or the thermal emission from a yet unknown population of hot dust, although hot gas emitting in the continuum cannot be firmly excluded.
C1 [Defrere, D.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Lebreton, J.; Le Bouquin, J. -B.; Lagrange, A. -M.; Augereau, J. -C.; Ertel, S.; Kluska, J.; Zins, G.] IPAG, CNRS INSU, UJF Grenoble 1, UMR 5274, Grenoble, France.
[Absil, O.] Univ Liege, B-4000 Liege, Belgium.
[Berger, J. -P.; Montagnier, G.] European So Observ, Vitacura 3107, Chile.
[di Folco, E.] Univ Bordeaux, Observe Aquitain Sci Univers, UMR 5804, Florac, France.
[Millan-Gabet, R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Traub, W.] NASA JPL, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Defrere, D (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM ddefrere@mpifr-bonn.mpg.de
FU French National Research Agency (ANR) [ANR-2010 BLAN-0505-01]; EII
(Fizeau programme); F.R.S.-FNRS; Poles TUNES and SMING of Universite
Joseph Fourier (Grenoble); INSU-PNP; INSU-PNPS
FX D.D., J.B. L. B., J.L., O.A., J.C.A., and S. E. thank the French
National Research Agency (ANR) for financial support through contract
ANR-2010 BLAN-0505-01 (EXOZODI). D. D. acknowledges the support of EII
(Fizeau programme). O.A. acknowledges the support from an F.R.S.-FNRS
Postdoctoral Fellowship. PIONIER was originally funded by the Poles
TUNES and SMING of Universite Joseph Fourier (Grenoble) and subsequently
supported by INSU-PNP and INSU-PNPS. The integrated optics beam combiner
is the result of collaboration between IPAG and CEA-LETI based on CNES
R&T funding. The authors thank all the people involved in the VLTI
project. We used the Smithsonian/NASA Astrophysics Data System (ADS) and
the "Centre de Donnees astronomiques de Strasbourg" (CDS).
NR 31
TC 14
Z9 14
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2012
VL 546
AR L9
DI 10.1051/0004-6361/201220287
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 027JT
UT WOS:000310349100136
ER
PT J
AU Mookerjea, B
Hassel, GE
Gerin, M
Giesen, T
Stutzki, J
Herbst, E
Black, JH
Goldsmith, PF
Menten, KM
Krelowski, J
De Luca, M
Csengeri, T
Joblin, C
Kazmierczak, M
Schmidt, M
Goicoechea, JR
Cernicharo, J
AF Mookerjea, B.
Hassel, G. E.
Gerin, M.
Giesen, T.
Stutzki, J.
Herbst, E.
Black, J. H.
Goldsmith, P. F.
Menten, K. M.
Krelowski, J.
De Luca, M.
Csengeri, T.
Joblin, C.
Kazmierczak, M.
Schmidt, M.
Goicoechea, J. R.
Cernicharo, J.
TI Chemistry of C-3 and carbon chain molecules in DR21(OH)
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: molecules; ISM: lines and bands; ISM: individual objects: DR21(OH);
astrochemistry; radiative transfer; molecular data
ID TRANSLUCENT SIGHT LINES; INTERSTELLAR C-3; STAR-FORMATION; HOT-CORE;
SPECTROSCOPY; CLUSTER; MASERS; CLOUDS; METHANOL; REGIONS
AB Context. C-3 is the smallest pure carbon chain detected in the dense environment of star-forming regions, although diatomic C-2 is detected in diffuse clouds. Measurement of the abundance of C-3 and the chemistry of its formation in dense star-forming regions has remained relatively unexplored.
Aims. We aim to identify the primary C-3 formation routes in dense star-forming regions following a chemical network producing species like CCH and c-C3H2 in the star-forming cores associated with DR21(OH), a high-mass star-forming region.
Methods. We observed velocity resolved spectra of four ro-vibrational far-infrared transitions of C-3 between the vibrational ground state and the low-energy nu(2) bending mode at frequencies between 1654-1897 GHz using HIFI on board Herschel, in DR21(OH). Several transitions of CCH and c-C3H2 were also observed with HIFI and the IRAM 30 m telescope. Rotational temperatures and column densities for all chemical species were estimated. A gas and grain warm-up model was used to obtain estimates of densities and temperatures of the envelope. The chemical network in the model was used to identify the primary C-3 forming reactions in DR21(OH).
Results. We detected C-3 in absorption in four far-infrared transitions, P(4), P(10), Q(2), and Q(4). The continuum sources MM1 and MM2 in DR21(OH), though spatially unresolved, are sufficiently separated in velocity to be identified in the C-3 spectra. All C-3 transitions are detected from the embedded source MM2 and the surrounding envelope, whereas only Q(4) and P(4) are detected toward the hot core MM1. The abundance of C-3 in the envelope and MM2 is similar to 6 x 10(-10) and similar to 3 x 10(-9), respectively. For CCH and c-C3H2, we only detect emission from the envelope and MM1. The observed CCH, C-3 and c-C3H2 abundances are most consistent with a chemical model with n(H2) similar to 5 x 10(6) cm(-3), a post-warm-up dust temperature T-max = 30 K, and a time of similar to 0.7-3 Myr.
Conclusions. Post-warm-up gas phase chemistry of CH4 released from the grain at t similar to 0.2 Myr and lasting for 1 Myr can explain the observed C-3 abundance in the envelope of DR21(OH), and no mechanism involving photodestruction of PAH molecules is required. The chemistry in the envelope is similar to the warm carbon chain chemistry found in lukewarm corinos. We interpret the observed lower C-3 abundance in MM1 as compared to MM2 and the envelope to be due to the destruction of C-3 in the more evolved MM1. The timescale for the chemistry derived for the envelope is consistent with the dynamical timescale of 2 Myr derived for DR21(OH) in other studies.
C1 [Mookerjea, B.] Tata Inst Fundamental Res, Mumbai 400005, Maharashtra, India.
[Hassel, G. E.] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA.
[Gerin, M.] CNRS, LERMA, Observ Paris, Paris, France.
[Giesen, T.; Stutzki, J.] Univ Cologne, I Physikal Inst, Cologne, Germany.
[Herbst, E.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA.
[Black, J. H.] Chalmers, Onsala Space Observ, Onsala 43992, Sweden.
[Goldsmith, P. F.] CALTECH, JPL, Pasadena, CA 91125 USA.
[Menten, K. M.; Csengeri, T.] MPI Radioastron, Bonn, Germany.
[Krelowski, J.] Nicholas Copernicus Univ, Torun, Poland.
[Joblin, C.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Joblin, C.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Kazmierczak, M.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands.
[Schmidt, M.] Nicolaus Copernicus Astron Ctr CMAK, Torun, Poland.
[Goicoechea, J. R.; Cernicharo, J.] CSIC INTA, Ctr Astrobiol, Madrid 28850, Spain.
RP Mookerjea, B (reprint author), Tata Inst Fundamental Res, Homi Bhabha Rd, Mumbai 400005, Maharashtra, India.
EM bhaswati@tifr.res.in
RI Giesen, Thomas /B-9476-2015; Goldsmith, Paul/H-3159-2016
OI Giesen, Thomas /0000-0002-2401-0049;
FU Alexander von Humboldt Foundation; CNES; Spanish MICINN [AYA2009-07304,
CSD2009-00038]; Ramon y Cajal; Polish MNiSW [203 393334]; NASA; ERC
[247078]
FX HIFI has been designed and built by a consortium of institutes and
university departments from across Europe, Canada and the United States
under the leadership of SRON Netherlands Institute for Space Research,
Groningen, The Netherlands and with major contributions from Germany,
France and the US. 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 Astrobiologa
(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. B. M. acknowledges the support from the Alexander
von Humboldt Foundation. M. G. acknowledges the support received from
CNES. J.R.G. and J.C. thank the Spanish MICINN for funding support
through grants, AYA2009-07304 and CSD2009-00038. J.R.G. is supported by
a Ramon y Cajal research contract M. S. acknowledges support from grant
No. 203 393334 from Polish MNiSW. E. H. thanks NASA for partial support
of this work through the Herschel program, administered by the Jet
Propulsion Laboratory. This work was carried out in part at the Jet
Propulsion Laboratory, California Institute of Technology, which is
supported by NASA. T.C.'s contribution was funded by ERC Advanced
Investigator Grant GLOSTAR (247078). This paper has made extensive use
of the SIMBAD database, operated at CDS, Strasbourg, France. This
research made use of the myXCLASS program
(https://www.astro.uni-koeln.de/projects/schilke/XCLASS), which accesses
the CDMS (http://www.cdms.de) and JPL (http://spec.jpl.nasa.gov)
molecular data bases.
NR 57
TC 11
Z9 11
U1 0
U2 7
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2012
VL 546
AR A75
DI 10.1051/0004-6361/201219287
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 027JT
UT WOS:000310349100075
ER
PT J
AU Muller, S
Kuhnel, M
Caballero, I
Pottschmidt, K
Furst, F
Kreykenbohm, I
Sagredo, M
Obst, M
Wilms, J
Ferrigno, C
Rothschild, RE
Staubert, R
AF Mueller, S.
Kuehnel, M.
Caballero, I.
Pottschmidt, K.
Fuerst, F.
Kreykenbohm, I.
Sagredo, M.
Obst, M.
Wilms, J.
Ferrigno, C.
Rothschild, R. E.
Staubert, R.
TI The reawakening of the sleeping X-ray pulsar XTE J1946+274
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays: binaries; accretion, accretion disks
ID TIMING-EXPLORER; GALACTIC RIDGE; VELA X-1; MISSION; DISCOVERY; BINARIES;
ENERGY; SUZAKU; STARS; LINES
AB We report on a series of outbursts of the high-mass X-ray binary XTE J1946+274 in 2010/2011 observed with INTEGRAL, RXTE, and Swift. We discuss possible mechanisms resulting in the extraordinary outburst behavior of this source. The X-ray spectra can be described by standard phenomenological models, enhanced by an absorption feature of unknown origin at about 10 keV and a narrow iron K alpha fluorescence line at 6.4 keV, which are variable in flux and pulse phase. We find possible evidence for a cyclotron resonance scattering feature at about 25 keV at the 93% level. The presence of a strong cyclotron line at 35 keV seen in data from the source's 1998 outburst that was confirmed by a reanalysis of these data can be excluded. This result indicates that the cyclotron line feature in XTE J1946+274 is variable between individual outbursts.
C1 [Mueller, S.; Kuehnel, M.; Fuerst, F.; Kreykenbohm, I.; Sagredo, M.; Obst, M.; Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Observ, D-96049 Bamberg, Germany.
[Mueller, S.; Kuehnel, M.; Fuerst, F.; Kreykenbohm, I.; Sagredo, M.; Obst, M.; Wilms, J.] Univ Erlangen Nurnberg, ECAP, D-96049 Bamberg, Germany.
[Caballero, I.] Univ Paris 07, CEA Saclay, DSM, IRFU,SAp UMR AIM 7158,CNRS,CEA, F-91191 Gif Sur Yvette, France.
[Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pottschmidt, K.] CRESST, Greenbelt, MD 20771 USA.
[Pottschmidt, K.] UMBC, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Sagredo, M.] Florida Int Univ, Dept Phys, Miami, FL 33199 USA.
[Ferrigno, C.] Univ Geneva, ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland.
[Rothschild, R. E.] Univ Calif San Diego, Ctr Astron & Space Sci, San Diego, CA 92093 USA.
[Staubert, R.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
RP Muller, S (reprint author), Univ Erlangen Nurnberg, Dr Karl Remeis Observ, Sternwartstr 7, D-96049 Bamberg, Germany.
EM Sebastian.Mueller@sternwarte.uni-erlangen.de
RI Wilms, Joern/C-8116-2013; Kreykenbohm, Ingo/H-9659-2013
OI Wilms, Joern/0000-0003-2065-5410; Kreykenbohm, Ingo/0000-0001-7335-1803
FU Bundesministerium fur Wirtschaft und Technologie under Deutsches Zentrum
fur Luft- und Raumfahrt [50 OR 0808, 50 OR 0905, 50 OR 1113]; French
Space Agency CNES through CNRS; ESA (Denmark); ESA (France); ESA
(Germany); ESA (Italy); ESA (Switzerland); ESA (Spain); Czech Republic,
and Poland
FX The authors thank Jerome Rodriguez for his help with the INTEGRAL
observations, and the schedulers of RXTE and Swift for their role in
making this campaign possible. We thank the anonymous referee for
his/her thorough review of this paper and his/her constructive comments.
We thank John E. Davis for the development of the SLxfig module, which
was used to create all figures in the paper. We acknowledge funding by
the Bundesministerium fur Wirtschaft und Technologie under Deutsches
Zentrum fur Luft- und Raumfahrt grants 50 OR 0808, 50 OR 0905, and 50 OR
1113. I. C. acknowledges financial support from the French Space Agency
CNES through CNRS. This research is also 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.
NR 41
TC 14
Z9 14
U1 0
U2 4
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2012
VL 546
AR A125
DI 10.1051/0004-6361/201219580
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 027JT
UT WOS:000310349100125
ER
PT J
AU Rauch, T
Werner, K
Biemont, E
Quinet, P
Kruk, JW
AF Rauch, T.
Werner, K.
Biemont, E.
Quinet, P.
Kruk, J. W.
TI Stellar laboratories: new GeV and Ge VI oscillator strengths and their
validation in the hot white dwarf RE0503-289
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE atomic data; line: identification; stars: abundances; stars: individual:
RE0503-289; white dwarfs; virtual observatory tools
ID NICKEL-LIKE IONS; IONIZED GERMANIUM; ENERGY-LEVELS; TRANSITION;
WAVELENGTHS; RATES; M1; E2; E1
AB Context. State-of-the-art spectral analysis of hot stars by means of non-LTE model-atmosphere techniques has arrived at a high level of sophistication. The analysis of high-resolution and high-S/N spectra, however, is strongly restricted by the lack of reliable atomic data for highly ionized species from intermediate-mass metals to trans-iron elements. Especially data for the latter has only been sparsely calculated. Many of their lines are identified in spectra of extremely hot, hydrogen-deficient post-AGB stars. A reliable determination of their abundances establishes crucial constraints for AGB nucleosynthesis simulations and, thus, for stellar evolutionary theory.
Aims. In a previous analysis of the UV spectrum of RE 0503-289, spectral lines of highly ionized Ga, Ge, As, Se, Kr, Mo, Sn, Te, I, and Xe were identified. Individual abundance determinations are hampered by the lack of reliable oscillator strengths. Most of these identified lines stem from Ge V. In addition, we identified Ge VI lines for the first time. We calculated Ge V and Ge VI oscillator strengths in order to reproduce the observed spectrum.
Methods. We newly calculated Ge V and Ge VI oscillator strengths to consider their radiative and collisional bound-bound transitions in detail in our non-LTE stellar- atmosphere models for the analysis of the Ge IV-VI spectrum exhibited in high-resolution and high-S/N FUV (FUSE) and UV (ORFEUS/BEFS, IUE) observations of RE 0503-289.
Results. In the UV spectrum of RE 0503-289, we identify four Ge IV, 37 GeV, and seven GeVI lines. Most of these lines are identified for the first time in any star. We can reproduce almost all Ge IV, GeV, and GeVI lines in the observed spectrum of RE 0503-289 (T-eff = 70 kK, log g = 7.5) at log Ge = -3.8 +/- 0.3 (mass fraction, about 650 times solar). The Ge IV/V/VI ionization equilibrium, that is a very sensitive Teff indicator, is reproduced well.
Conclusions. Reliable measurements and calculations of atomic data are a prerequisite for stellar- atmosphere modeling. Our oscillator-strength calculations have allowed, for the first time, Ge V and Ge VI lines to be successfully reproduced in a white dwarf's (RE 0503-289) spectrum and to determine its photospheric Ge abundance.
C1 [Rauch, T.; Werner, K.] Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Biemont, E.; Quinet, P.] Univ Mons UMONS, B-7000 Mons, Belgium.
[Biemont, E.; Quinet, P.] Univ Liege, IPNAS, B-4000 Liege, Belgium.
[Kruk, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Rauch, T (reprint author), Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany.
EM rauch@astro.uni-tuebingen.de
FU German Aerospace Center (DLR) [05 OR 0806]; Belgian FRS-FNRS; NASA
Office of Space Science [NNX09AF08G]
FX T.R. is supported by the German Aerospace Center (DLR, grant 05 OR
0806). Financial support from the Belgian FRS-FNRS is also acknowledged.
E.B. and P.Q. are Research Director and Senior Research Associate,
respectively, of this organization. This research has made use of the
SIMBAD database, operated at the CDS, Strasbourg, France. We thank Ralf
Napiwotzki for providing us the SPY spectrum of RE 0503-289. Some of the
data presented in this paper were obtained from the Mikulski Archive for
Space Telescopes (MAST). STScI is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract
NAS5-26555. Support for MAST for non-HST data is provided by the NASA
Office of Space Science via grant NNX09AF08G and by other grants and
contracts.
NR 25
TC 15
Z9 15
U1 1
U2 4
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2012
VL 546
AR A55
DI 10.1051/0004-6361/201220014
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 027JT
UT WOS:000310349100055
ER
PT J
AU Riviere-Marichalar, P
Barrado, D
Augereau, JC
Thi, WF
Roberge, A
Eiroa, C
Montesinos, B
Meeus, G
Howard, C
Sandell, G
Duchene, G
Dent, WRF
Lebreton, J
Mendigutia, I
Huelamo, N
Menard, F
Pinte, C
AF Riviere-Marichalar, P.
Barrado, D.
Augereau, J. -C.
Thi, W. F.
Roberge, A.
Eiroa, C.
Montesinos, B.
Meeus, G.
Howard, C.
Sandell, G.
Duchene, G.
Dent, W. R. F.
Lebreton, J.
Mendigutia, I.
Huelamo, N.
Menard, F.
Pinte, C.
TI HD 172555: detection of 63 mu m [OI] emission in a debris disc
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE line: formation; Kuiper belt: general; stars: pre-main sequence;
circumstellar matter; stars: individual: HD 172555
ID ALL-SKY SURVEY; BETA-PICTORIS; CIRCUMSTELLAR DISKS; STARS; GAS; DUST;
SPECTROSCOPY; COLLISION; CATALOG; SYSTEM
AB Context. HD 172555 is a young A7 star belonging to the beta Pictoris moving group that harbours a debris disc. The Spitzer/IRS spectrum of the source showed mid-IR features such as silicates and glassy silica species, indicating the presence of a warm dust component with small grains, which places HD 172555 among the small group of debris discs with such properties. The IRS spectrum also shows a possible emission of SiO gas.
Aims. We aim to study the dust distribution in the circumstellar disc of HD 172555 and to asses the presence of gas in the debris disc.
Methods. As part of the GASPS open time key programme, we obtained Herschel/PACS photometric and spectroscopic observations of the source. We analysed PACS observations of HD 172555 and modelled the spectral energy distribution with a modified blackbody and the gas emission with a two-level population model with no collisional de-excitation.
Results. We report for the first time the detection of [OI] atomic gas emission at 63.18 mu m in the HD 172555 circumstellar disc. We detect excesses due to circumstellar dust toward HD 172555 in the three photometric bands of PACS (70, 100, and 160 mu m). We derive a large dust particle mass of (4.8 +/- 0.6) x 10(-4) M-circle plus and an atomic oxygen mass of 2.5 x 10(-2)R(2) M-circle plus, where R in AU is the separation between the star and the inner disc. Thus, most of the detected mass of the disc is in the gaseous phase.
C1 [Riviere-Marichalar, P.; Barrado, D.; Montesinos, B.; Mendigutia, I.; Huelamo, N.] CSIC INTA, Dept Astrofis, Ctr Astrobiol, Villanueva De La Canada 28691, Spain.
[Barrado, D.] Ctr Astron Hispano Aleman, Calar Alto Observ, Almeria 04004, Spain.
[Augereau, J. -C.; Thi, W. F.; Duchene, G.; Lebreton, J.; Menard, F.; Pinte, C.] UJF Grenoble 1, CNRS INSU, Inst Planetol & Astrophys IPAG, UMR 5274, F-38041 Grenoble, France.
[Roberge, A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Eiroa, C.; Meeus, G.; Mendigutia, I.] Fac Ciencias, Dep Fis Teor, Madrid 28049, Spain.
[Howard, C.; Sandell, G.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA.
[Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Dent, W. R. F.] ALMA, Santiago, Chile.
[Menard, F.] U Chile PUC U Conception, UMI CNRS 3386, Lab Franco Chileno Astron, Santiago, Chile.
RP Riviere-Marichalar, P (reprint author), CSIC INTA, Dept Astrofis, Ctr Astrobiol, ESAC Campus,POB 78, Villanueva De La Canada 28691, Spain.
EM riviere@cab.inta-csic.es
RI Roberge, Aki/D-2782-2012; Barrado Navascues, David/C-1439-2017; Huelamo,
Nuria/C-3042-2017; Montesinos, Benjamin/C-3493-2017
OI Roberge, Aki/0000-0002-2989-3725; Barrado Navascues,
David/0000-0002-5971-9242; Huelamo, Nuria/0000-0002-2711-8143;
Montesinos, Benjamin/0000-0002-7982-2095
FU ANR [ANR-2010 BLAN-0505-01]; CNES-PNP; EU [284405]; Millennium Science
Initiative (Chilean Ministry of Economy) [ONucleus P10-022-FO]; [AYA
2010-21161-C02-02]; [CDS2006-00070]; [PRICIT-S2009/ESP-1496];
[RYC-2011-07920]; [AYA-2011-26202]
FX This research has been funded by Spanish grants AYA 2010-21161-C02-02,
CDS2006-00070 and PRICIT-S2009/ESP-1496. J.-C. Augereau and J. Lebreton
thank the ANR (contract ANR-2010 BLAN-0505-01, EXOZODI) and the CNES-PNP
for financial support. C. Pinte, F. Menard and W.-F. Thi acknowledges
funding from the EU FP7-2011 under Grant Agreement nr. 284405. G. Meeus
is supported by RYC-2011-07920. G. Meeus, C. Eiroa, I. Mendigutia and B.
Montesinos are partly supported by AYA-2011-26202. F. M. acknowledges
support from the Millennium Science Initiative (Chilean Ministry of
Economy), through grant ONucleus P10-022-FO.
NR 37
TC 17
Z9 17
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2012
VL 546
AR L8
DI 10.1051/0004-6361/201219745
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 027JT
UT WOS:000310349100135
ER
PT J
AU Makinen, CP
Moisan, TAH
AF Makinen, Carla P.
Moisan, Tiffany A. H.
TI Phytoplankton assemblage patterns in the southern Mid-Atlantic Bight
SO BOTANICA MARINA
LA English
DT Article
DE coastal; diversity; Mid-Atlantic Bight; phytoplankton; time series
ID CHESAPEAKE BAY; EASTERN COAST; COMMUNITY STRUCTURE; CONTINENTAL-SHELF;
DELAWARE; PLANKTON; USA; PRODUCTIVITY; TEMPERATURE; VARIABILITY
AB As part of the Wallops Coastal Oceans Observing Laboratory (Wa-COOL) Project, we sampled a time-series transect in the southern Mid-Atlantic Bight (MAB) biweekly. Our 2-year time-series data included physical parameters, nutrient concentrations, and chlorophyll a concentrations. A detailed phytoplankton assemblage structure was examined in the second year. During the 2-year study, chlorophyll a concentration (and ocean color satellite imagery) indicated that phytoplankton blooms occurred in January/February during mixing conditions and in early autumn under stratified conditions. The chlorophyll a concentrations ranged from 0.25 mu g l(-1) to 15.49 mu g l(-1) during the 2-year period. We were able to discriminate approximately 116 different species under phase contrast microscopy. Dominant phytoplankton included Skeletonema costatum, Rhizosolenia spp., and Pseudo-nitzschia pungens. In an attempt to determine phytoplankton species competition/succession within the assemblage, we calculated a Shannon Weaver diversity index for our diatom microscopy data. Diatom diversity was greatest during the winter and minimal during the spring. Diatom diversity was also greater at nearshore stations than at offshore stations. Individual genera appeared patchy, with surface and subsurface patches appearing abruptly and persisting for only 1-2 months at a time. The distribution of individual species differed significantly from bulk variables of the assemblage (chlorophyll a) and total phytoplankton assemblage (cells), which indicates that phytoplankton species may be limited in growth in ways that differ from those of the total assemblage. Our study demonstrated a highly diverse phytoplankton assemblage throughout the year, with opportunistic species dominating during spring and fall in response to seasonal changes in temperature and nutrients in the southern MAB.
C1 [Moisan, Tiffany A. H.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Field Support Off, Wallops Isl, VA 23337 USA.
[Makinen, Carla P.] NASA, Goddard Space Flight Ctr, URS Corp, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
RP Moisan, TAH (reprint author), NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Field Support Off, Code 610 W,Atomspher Sci Room E-217,Bldg N-159, Wallops Isl, VA 23337 USA.
EM tiffany.a.moisan@nasa.gov
FU NOAA; NASA; NOAA, U.S. Department of Commerce [NA03NOS4730220]
FX This project was supported by NOAA and NASA and was managed by the
Center for Innovative Technology. The paper was prepared under award
#NA03NOS4730220 from NOAA, U.S. Department of Commerce. The statements,
findings, and conclusions are those of the authors and do not
necessarily reflect the views of NOAA or the U.S. Department of
Commerce. Thanks also to M. A. Linkswiler for graphics. In addition, we
appreciate the hard work of the captain and crew of the R/V Philip N.
Parker during cruises. We especially thank Robert N. Swift for his
constructive comments, which always improve our manuscripts. We thank
the reviewers for their excellent suggestions and detailed comments that
greatly improved the manuscript.
NR 34
TC 1
Z9 1
U1 1
U2 21
PU WALTER DE GRUYTER & CO
PI BERLIN
PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY
SN 0006-8055
J9 BOT MAR
JI Bot. Marina
PD OCT
PY 2012
VL 55
IS 5
BP 445
EP 457
DI 10.1515/bot-2012-0110
PG 13
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA 028PR
UT WOS:000310435100001
ER
PT J
AU Fishman, J
Iraci, LT
Al-Saadi, J
Chance, K
Chavez, F
Chin, M
Coble, P
Davis, C
DiGiacomo, PM
Edwards, D
Eldering, A
Goes, J
Herman, J
Hu, C
Jacob, DJ
Jordan, C
Kawa, SR
Key, R
Liu, X
Lohrenz, S
Mannino, A
Natraj, V
Neil, D
Neu, J
Newchurch, M
Pickering, K
Salisbury, J
Sosik, H
Subramaniam, A
Tzortziou, M
Wang, J
Wang, M
AF Fishman, J.
Iraci, L. T.
Al-Saadi, J.
Chance, K.
Chavez, F.
Chin, M.
Coble, P.
Davis, C.
DiGiacomo, P. M.
Edwards, D.
Eldering, A.
Goes, J.
Herman, J.
Hu, C.
Jacob, D. J.
Jordan, C.
Kawa, S. R.
Key, R.
Liu, X.
Lohrenz, S.
Mannino, A.
Natraj, V.
Neil, D.
Neu, J.
Newchurch, M.
Pickering, K.
Salisbury, J.
Sosik, H.
Subramaniam, A.
Tzortziou, M.
Wang, J.
Wang, M.
TI THE UNITED STATES' NEXT GENERATION OF ATMOSPHERIC COMPOSITION AND
COASTAL ECOSYSTEM MEASUREMENTS NASA's Geostationary Coastal and Air
Pollution Events (GEO-CAPE) Mission
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID GULF-OF-MEXICO; OZONE MONITORING INSTRUMENT; SATELLITE MEASUREMENTS;
MARINE-PHYTOPLANKTON; TROPOSPHERIC OZONE; CLIMATE-CHANGE; URBAN OZONE;
OCEAN; AEROSOL; SPACE
AB THE UNITED STATES' NEXT GENERATION OF ATMOSPHERIC COMPOSITION AND COASTAL ECOSYSTEM MEASUREMENTS: NASA'S GEOSTATIONARY COASTAL AND AIR POLLUTION EVENTS (GEO-CAPE) MISSION
The Geostationary Coastal and Air Pollution Events (GEO-CAPE) mission was recommended by the National Research Council's (NRC's) Earth Science Decadal Survey to measure tropospheric trace gases and aerosols' and coastal ocean phytoplankton, water quality, and biogeochemistry from geostationary orbit, providing continuous observations within the field of view. To fulfill the mandate and address the challenge put forth by the NRC, two GEO-CAPE Science Working Groups (SWGs), representing the atmospheric composition and ocean color disciplines, have developed realistic science objectives using input drawn from several community workshops. The GEO-CAPE mission will take advantage of this revolutionary advance in temporal frequency for both of these disciplines. Multiple observations per day are required to explore the physical, chemical, and dynamical processes that determine tropospheric composition and air quality over spatial scales ranging from urban to continental, and over temporal scales ranging from diurnal to seasonal. Likewise, high-frequency satellite Observations are critical to studying and quantifying biological, chemical, and physical processes within the coastal ocean. These observations are to be achieved from a vantage point near 95 degrees-100 degrees W, providing a complete view of North America as well as the adjacent oceans. The SWGs have also endorsed the concept of phased implementation using commercial satellites to reduce mission risk and cost. GEO-CAPE will join the global constellation. of geostationary atmospheric chemistry and coastal ocean color sensors planned to be in orbit in the 2020 time frame.
C1 [Fishman, J.] St Louis Univ, Dept Earth & Atmospher Sci, St Louis, MO 63108 USA.
[Iraci, L. T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Al-Saadi, J.] NASA, Washington, DC 20546 USA.
[Al-Saadi, J.; Neil, D.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Chance, K.; Liu, X.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chavez, F.] Monterey Bay Aquarium Res Inst, Moss Landing, CA USA.
[Chin, M.; Herman, J.; Kawa, S. R.; Mannino, A.; Pickering, K.; Tzortziou, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tzortziou, M.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Coble, P.; Hu, C.] Univ S Florida, Tampa, FL USA.
[Davis, C.] Oregon State Univ, Corvallis, OR 97331 USA.
[DiGiacomo, P. M.; Wang, M.] NOAA, NESDIS Ctr Satellite Applicat & Res, Camp Springs, MD USA.
[DiGiacomo, P. M.; Wang, M.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Eldering, A.; Key, R.; Natraj, V.; Neu, J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Goes, J.; Subramaniam, A.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Jacob, D. J.] Harvard Univ, Cambridge, MA 02138 USA.
[Jordan, C.; Salisbury, J.] Univ New Hampshire, Durham, NH 03824 USA.
[Lohrenz, S.] Univ So Mississippi, Dept Marine Sci, Stennis Space Ctr, MS USA.
[Newchurch, M.] Univ Alabama, Huntsville, AL 35899 USA.
[Sosik, H.] Woods Hole Oceanog Inst, Woods Hole, MA USA.
[Wang, J.] Univ Nebraska, Lincoln, NE USA.
RP Fishman, J (reprint author), St Louis Univ, Dept Earth & Atmospher Sci, 300-F ONeil Hall,3642 Lindell Blvd, St Louis, MO 63108 USA.
EM jfishma2@slu.edu
RI Wang, Menghua/F-5631-2010; Chin, Mian/J-8354-2012; DiGiacomo,
Paul/F-5584-2010; Pickering, Kenneth/E-6274-2012; Kawa,
Stephan/E-9040-2012; Mannino, Antonio/I-3633-2014; Liu,
Xiong/P-7186-2014; Wang, Jun/A-2977-2008;
OI Sosik, Heidi/0000-0002-4591-2842; Lohrenz, Steven/0000-0003-3811-2975;
Wang, Menghua/0000-0001-7019-3125; DiGiacomo, Paul/0000-0003-4550-1899;
Liu, Xiong/0000-0003-2939-574X; Wang, Jun/0000-0002-7334-0490; Herman,
Jay/0000-0002-9146-1632; Chance, Kelly/0000-0002-7339-7577; Subramaniam,
Ajit/0000-0003-1316-5827
FU Earth Science Division of the National Aeronautics and Space
Administration
FX Funding for GEO-CAPE definition activities is provided by the Earth
Science Division of the National Aeronautics and Space Administration.
Portions of this work were carried out at the jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. Contributions to this work were
made by the GEO-CAPE Atmospheric Science Working Group: J. Al-Saadi, K.
Bowman, K. Chance, R. Chatfield, M. Chin, R. Cohen, J. Crawford D.
Edwards, A. Eldering, J. Fishman, D. Henze, L. Iraci, D.J. Jacob, K.
Jucks, S. R. Kawa, S. Kondragunta, N. Krotkov, X. Liu, C. McLinden, V.
Natraj, D. Neil, J. Neu, M. Newchurch, K. Pickering, R. Pierce, R.
Pinder, J. Rodriguez, S. Sander, R. Scheffe, R. Spurr, J. Szykman, O.
Torres, J. Wang, J. Worden and the GEO-CAPE Ocean Science Working Group:
J. Al-Saadi, B. Arnone, W. Balch, P. Bontempi, J. Campbell, J. Chaves,
F. Chavez, P. Coble, C. Davis, C. del Castillo, P.M. DiGiacomo, J. Goes,
J. Herman, S. Hooker, C. Hu, L. Iraci, C. Jordan, Z. P. Lee, S. Lohrenz,
A. Mannino, P. Matrai, C. McClain, R. Morrison, C. Mouw, F.
Muller-Karger, A. Neeley, J. Salisbury, B. Schaeffer, H. Sosik, R.
Stumpf, A. Subramaniam, G. Toro-Farmer, O. Torres, M. Tzortziou, M.
Wang, J. Werdell, C. Wilson.
NR 80
TC 65
Z9 65
U1 2
U2 48
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD OCT
PY 2012
VL 93
IS 10
BP 1547
EP 1566
DI 10.1175/BAMS-D-11-00201.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 024HU
UT WOS:000310101100013
ER
PT J
AU Buchanan, ED
Benford, DJ
Forgione, JB
Moseley, SH
Wollack, EJ
AF Buchanan, Ernest D.
Benford, Dominic J.
Forgione, Joshua B.
Moseley, S. Harvey
Wollack, Edward J.
TI Cryogenic applications of commercial electronic components
SO CRYOGENICS
LA English
DT Article
DE Electronics; Liquid helium; Multiplexer; GISMO; TTL; Analog
AB We have developed a range of techniques useful for constructing analog and digital circuits for operation in a liquid Helium environment (4.2 K), using commercially available low power components. The challenges encountered in designing cryogenic electronics include finding components that can function usefully in the cold and possess low enough power dissipation so as not to heat the systems they are designed to measure. From design, test, and integration perspectives it is useful for components to operate similarly at room and cryogenic temperatures; however this is not a necessity. Some of the circuits presented here have been used successfully in the MUSTANG [1] and in the GISMO [2] camera to build a complete digital to analog multiplexer (which will be referred to as the Cryogenic Address Driver board). Many of the circuit elements described are of a more general nature rather than specific to the Cryogenic Address Driver board, and were studied as a part of a more comprehensive approach to addressing a larger set of cryogenic electronic needs. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Buchanan, Ernest D.] ADNET Syst Inc, Rockville, MD 20852 USA.
[Benford, Dominic J.; Moseley, S. Harvey; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Forgione, Joshua B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Buchanan, ED (reprint author), ADNET Syst Inc, 164 Rollins Ave,Suite 303, Rockville, MD 20852 USA.
EM Ernest.D.Buchanan@NASA.gov
RI Wollack, Edward/D-4467-2012
OI Wollack, Edward/0000-0002-7567-4451
NR 7
TC 5
Z9 5
U1 0
U2 6
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0011-2275
J9 CRYOGENICS
JI Cryogenics
PD OCT
PY 2012
VL 52
IS 10
BP 550
EP 556
DI 10.1016/j.cryogenics.2012.06.017
PG 7
WC Thermodynamics; Physics, Applied
SC Thermodynamics; Physics
GA 028EZ
UT WOS:000310406900018
ER
PT J
AU Schuh, H
Behrend, D
AF Schuh, H.
Behrend, D.
TI VLBI: A fascinating technique for geodesy and astrometry
SO JOURNAL OF GEODYNAMICS
LA English
DT Review
DE Very Long Baseline Interferometry (VLBI); IVS; VLBI2010; CRF; TRF; Earth
orientation; Global Geodetic Observing System (GGOS)
ID BASE-LINE INTERFEROMETRY
AB Since the 1970s Very Long Baseline Interferometry (VLBI) has proven to be a primary space-geodetic technique by determining precise coordinates on the Earth, by monitoring the variable Earth rotation and orientation with highest precision, and by deriving many other parameters of the Earth system. VLBI provides an important linkage to astronomy through, for instance, the determination of very precise coordinates of extragalactic radio sources. Additionally, it contributes to determining parameters of relativistic and cosmological models. After a short review of the history of geodetic VLBI and a summary of recent results, this paper describes future perspectives of this fascinating technique. The International VLBI Service for Geodesy and Astrometry (IVS), as a service of the International Association of Geodesy (IAG) and the International Astronomical Union (IAU), is well on its way to fully defining a next generation VLBI system, called VLBI2010. The goals of the new system are to achieve on scales up to the size of the Earth an accuracy of 1 mm in position and of 0.1 mm/year in velocity. Continuous observations shall be carried out 24 h per day 7 days per week in the future with initial results to be delivered within 24 h after taking the data. Special sessions, e.g. for monitoring the Earth rotation parameters, will provide the results in near real-time. These goals require a completely new technical and conceptual design of VLBI measurements. Based on extensive simulation studies, strategies have been developed by the IVS to significantly improve its product accuracy through the use of a network of small (similar to 12 m) fast-slewing antennas. A new method for generating high precision delay measurements as well as improved methods for handling biases related to radio source structure, system electronics, and deformations of the antenna structures has been developed. Furthermore, as of January 2012, the construction of ten new VLBI2010 sites has been funded, with good prospects for one dozen more antennas, which will improve the geographical distribution of geodetic VLBI sites on Earth and provide an important step toward a global VLBI2010 network. Within this paper, the Global Geodetic Observing System (GGOS) of the IAG will also be introduced and the contribution of VLBI to GGOS will be described. (C) 2012 Published by Elsevier Ltd.
C1 [Schuh, H.] Univ Technol, Inst Geodesy & Geophys, Vienna, Austria.
[Behrend, D.] NASA, NVI Inc, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Schuh, H (reprint author), Univ Technol, Inst Geodesy & Geophys, Vienna, Austria.
FU IVS
FX The continued success of VLBI as a space-geodetic technique would be
impossible without the great support and enthusiasm from many
institutions and individuals. This holds true in equal measure for the
early years and for the last decade, during which VLBI has been done
under the auspices of the IVS. The authors gratefully acknowledge the
commitment made and resources provided by all IVS components. The
authors would like to thank John Gipson and an anonymous reviewer for
their useful comments to improve the manuscript. This paper is an
outgrowth of the 2011 Vening Meinesz Medal speech of the first author at
the European Geosciences Union (EGU) General Assembly in Vienna,
Austria. The first author is grateful to the EGU and its Geodesy Section
for awarding this medal and for recognizing the high significance that
geodetic/astrometric VLBI has reached within the science community.
NR 36
TC 72
Z9 72
U1 4
U2 30
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0264-3707
J9 J GEODYN
JI J. Geodyn.
PD OCT
PY 2012
VL 61
BP 68
EP 80
DI 10.1016/j.jog.2012.07.007
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 024KM
UT WOS:000310108100006
ER
PT J
AU Gaier, JR
Ellis, S
Hanks, N
AF Gaier, James R.
Ellis, Shaneise
Hanks, Nicole
TI Thermal Optical Properties of Lunar Dust Simulants
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article; Proceedings Paper
CT 3rd AIAA Atmospheric and Space Environments Conference
CY JUN 27-30, 2011
CL Honolulu, HI
SP AIAA
AB The total reflectance spectra of lunar simulant dusts (<20 mu m particles) were measured to determine their integrated solar absorptance a and their thermal emittance epsilon for the purpose of analyzing the effect of dust on the performance of thermal control surfaces. All of the simulants except Minnesota Lunar Simulant 1 had a wavelength-dependant reflectivity rho(lambda) near 0.10 over the wavelength range of 8-25 mu m, and so are highly emitting at room temperature and lower. The anomalous behavior of Minnesota Lunar Simulant 1 was attributed to its very low glass content. The 300 K emittance e of all the lunar simulants, except Minnesota Lunar Simulant 1, ranged from 0.78 to 0.92. In all cases, the e was lower for the <20 mu m particles than for larger particles reported earlier. There was considerably more variation in the lunar simulant reflectance in the solar spectral range (250-2500 nm) than in the thermal infrared. As expected, the lunar highlands simulants were more reflective in this wavelength range than the lunar mare simulants. The epsilon(lambda) maxima at the Christiansen frequency were consistent with simulants being largely plagioclase and confirmed that, with the exception of Minnesota Lunar Simulant 1P, addition of agglutinates did not change the mineralogical character of the simulants. The alpha of the simulants ranged from 0.39 to 0.75. This is lower than values reported earlier for larger particles of the same simulants (0.41-0.82) and for representative mare and highlands lunar soils (0.74-0.91). Because the alpha of some mare simulants more closely matched that of highlands lunar soils, it is recommended that alpha and epsilon values be the criteria for choosing a simulant for assessing the effects of dust on thermal control surfaces, rather than whether a simulant has been formulated as a highlands or a mare simulant.
C1 [Gaier, James R.] NASA, John H Glenn Res Ctr Lewis Field, Space Environm & Expt Branch, Cleveland, OH 44135 USA.
[Ellis, Shaneise] NASA, John H Glenn Res Ctr Lewis Field, United Negro Coll Fund Special Programs Corp, Sci & Technol Inst Minor Inst, Cleveland, OH 44135 USA.
[Hanks, Nicole] NASA, John H Glenn Res Ctr Lewis Field, Lewis Educ Res Collaborat Internship Program, Cleveland, OH 44135 USA.
RP Gaier, JR (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Space Environm & Expt Branch, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
NR 18
TC 2
Z9 2
U1 1
U2 8
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0887-8722
J9 J THERMOPHYS HEAT TR
JI J. Thermophys. Heat Transf.
PD OCT-DEC
PY 2012
VL 26
IS 4
BP 573
EP 580
DI 10.2514/1.T3838
PG 8
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA 025HN
UT WOS:000310179400003
ER
PT J
AU Nguyen, TV
Divsalar, D
AF Thuy Van Nguyen
Divsalar, Dariush
TI The Design of Rate-Compatible Protograph LDPC Codes
SO IEEE TRANSACTIONS ON COMMUNICATIONS
LA English
DT Article
DE LPDC codes; protograph codes; rate-compatible; iterative decoding
threshold; EXIT chart
ID PARITY-CHECK CODES
AB This paper presents a simple yet effective method for designing nested families of LDPC codes. Rate compatible codes are essential for many communication applications, e. g. hybrid automatic repeat request (HARQ) systems, and their design is nontrivial due to the difficulty of simultaneously guaranteeing the quality of several related codes. Puncturing can be used to generate rate-compatible LDPC codes, but it produces a gap to capacity that, in practice, often significantly exceeds the gap of the mother code. We propose an alternative method based on successively extending a high-rate protograph. The resulting codes not only inherit the advantages of protograph codes, namely low encoding complexity and efficient decoding algorithms, but also cover a wide range of rates and have very good performance with iterative decoding thresholds that are within 0.2 dB of their capacity limits.
C1 [Thuy Van Nguyen; Divsalar, Dariush] Univ Texas Dallas, Dept Elect Engn, Richardson, TX 75083 USA.
[Divsalar, Dariush] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Nguyen, TV (reprint author), Univ Texas Dallas, Dept Elect Engn, Richardson, TX 75083 USA.
EM nvanthuy@utdallas.edu; aria@utdallas.edu
OI Nosratinia, Aria/0000-0002-3751-0165
FU VOSP program from the Ministry of Education and Training, Vietnam; THECB
[009741-0084-2007]
FX This research was supported in part by the VOSP program from the
Ministry of Education and Training, Vietnam, by the grant
009741-0084-2007 from THECB. This research was in part carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with NASA.
NR 30
TC 21
Z9 21
U1 1
U2 10
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0090-6778
J9 IEEE T COMMUN
JI IEEE Trans. Commun.
PD OCT
PY 2012
VL 60
IS 10
BP 2841
EP 2850
DI 10.1109/TCOMM.2012.081012.110010
PG 10
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA 025NG
UT WOS:000310195700010
ER
PT J
AU Andreadis, KM
Lettenmaier, DP
AF Andreadis, Konstantinos M.
Lettenmaier, Dennis P.
TI Implications of Representing Snowpack Stratigraphy for the Assimilation
of Passive Microwave Satellite Observations
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID QUASI-CRYSTALLINE APPROXIMATION; ARCTIC COASTAL-PLAIN; WATER EQUIVALENT;
SPATIAL VARIABILITY; DEPTH ALGORITHM; WESTERN CANADA; EMISSION MODEL;
SEASONAL SNOW; SMMR DATA; COVER
AB Under certain conditions, passive microwave satellite observations can be used to estimate snow water equivalent (SWE) across large areas, either through direct retrieval or data assimilation. However, the layered character of snowpacks increases the complexities of estimation algorithms. A multilayer model of snowpack stratigraphy that can serve as the forward model of a snow data assimilation system is described and evaluated. The model's ability to replicate large-scale snowpack layer features is evaluated using observations from the Cold Land Processes Experiment (Colorado, 2002 and 2003) and a 2002 Nome-Barrow snowpit transect [Snow Science Traverse-Alaska Region (SnowSTAR2002)]. The multilayer model linked with a radiative transfer scheme improved the estimation of brightness temperatures both in terms of absolute values and frequency/polarization differences (error reductions ranging from 47% to 72%) relative to a one-layer model with similar, but depth-averaged, physics at the Colorado sites. The two models were also employed along the SnowSTAR2002 transect of snowpit measurements. The general unavailability of meteorological forcings along the transect made the use of coarse-scale reanalysis data necessary to simulate snow properties and microwave radiances. Errors in the precipitation forcings led to overestimation of SWE, and the simulated brightness temperatures from the two models showed large differences, due mostly to the inability of the single-layer model to simulate the observed larger grain sizes. These differences had implications for the estimation of snow depth; assimilation of Special Sensor Microwave Imager (SSM/I) observations into the multilayer model resulted in improved snow depth estimates (RMSEs of 18.1 cm versus 34.1 cm without assimilation), while the single-layer assimilation slightly decreased the estimation skill (RMSEs of 34.1 versus 33.6 cm).
C1 [Andreadis, Konstantinos M.] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA.
[Lettenmaier, Dennis P.] Univ Washington, Seattle, WA 98195 USA.
RP Andreadis, KM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM konstantinos.m.andreadis@jpl.nasa.gov
RI lettenmaier, dennis/F-8780-2011
OI lettenmaier, dennis/0000-0003-3317-1327
FU NASA [NNG06GD79G]
FX The authors thank Leung Tsang, Ding Liang, and Xiaolan Xu for providing
the DMRT code, as well as Matthew Sturm and Glen Liston for making the
SnowSTAR2002 data available. This work was suppored in part by NASA
Grant NNG06GD79G to the University of Washington.
NR 69
TC 7
Z9 7
U1 0
U2 8
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD OCT
PY 2012
VL 13
IS 5
BP 1493
EP 1506
DI 10.1175/JHM-D-11-056.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 023NT
UT WOS:000310042400006
ER
PT J
AU Kirschbaum, D
Adler, R
Adler, D
Peters-Lidard, C
Huffman, G
AF Kirschbaum, Dalia
Adler, Robert
Adler, David
Peters-Lidard, Christa
Huffman, George
TI Global Distribution of Extreme Precipitation and High-Impact Landslides
in 2010 Relative to Previous Years
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID EL-NINO; RAINFALL THRESHOLDS; SHALLOW LANDSLIDES; DURATION CONTROL;
CENTRAL-AMERICA; DEBRIS FLOWS; MONSOON; INTENSITY; NEPAL; ENSO
AB It is well known that extreme or prolonged rainfall is the dominant trigger of landslides worldwide. While research has evaluated the spatiotemporal distribution of extreme rainfall and landslides at local or regional scales using in situ data, few studies have mapped rainfall-triggered landslide distribution globally because of the dearth of landslide data and consistent precipitation information. This study uses a newly developed global landslide catalog (GLC) and a 13-yr satellite-based precipitation record from Tropical Rainfall Measuring Mission (TRMM) data. For the first time, these two unique products provide the foundation to quantitatively evaluate the co-occurrence of precipitation and rainfall-triggered landslides globally. Evaluation of the GLC indicates that 2010 had a large number of high-impact landslide events relative to previous years. This study considers how variations in extreme and prolonged satellite-based rainfall are related to the distribution of landslides over the same time scales for three active landslide areas: Central America, the Himalayan arc, and central eastern China. Several test statistics confirm that TRMM rainfall generally scales with the observed increase in landslide reports and fatal events for 2010 and previous years over each region. These findings suggest that the co-occurrence of satellite precipitation and landslide reports may serve as a valuable indicator for characterizing the spatiotemporal distribution of landslide-prone areas in order to establish a global rainfall-triggered landslide climatology. This study characterizes the variability of satellite precipitation data and reported landslide activity at the global scale in order to improve landslide cataloging and attempt to quantify landslide triggering at daily, monthly, and yearly time scales.
C1 [Kirschbaum, Dalia] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
[Adler, Robert; Adler, David] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Huffman, George] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Kirschbaum, D (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
EM dalia.b.kirschbaum@nasa.gov
RI Kirschbaum, Dalia/F-9596-2012; Huffman, George/F-4494-2014;
Peters-Lidard, Christa/E-1429-2012
OI Huffman, George/0000-0003-3858-8308; Peters-Lidard,
Christa/0000-0003-1255-2876
FU Global Precipitation Measurement (GPM) mission; NASA's Applied Sciences
Program
FX The authors acknowledge the individuals who helped to develop the GLC,
including Stephanie Hill, Lynne Shupp, Teddy Allen, Pradeep Adhikari,
Lauren Redmond, David Adler, and Kimberly Rodgers. This work was
supported by the Global Precipitation Measurement (GPM) mission and
NASA's Applied Sciences Program. Thank you also to Yudong Tian, who
helped to provide TMPA data for this analysis. The authors are grateful
for the detailed comments from two anonymous reviews.
NR 55
TC 16
Z9 17
U1 2
U2 30
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD OCT
PY 2012
VL 13
IS 5
BP 1536
EP 1551
DI 10.1175/JHM-D-12-02.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 023NT
UT WOS:000310042400009
ER
PT J
AU Amitai, E
Unkrich, CL
Goodrich, DC
Habib, E
Thill, B
AF Amitai, Eyal
Unkrich, Carl L.
Goodrich, David C.
Habib, Emad
Thill, Bryson
TI Assessing Satellite-Based Rainfall Estimates in Semiarid Watersheds
Using the USDA-ARS Walnut Gulch Gauge Network and TRMM PR
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID PRECIPITATION RADAR; PROFILING ALGORITHM
AB The rain gauge network associated with the Walnut Gulch Experimental Watershed (WGEW) in southeastern Arizona provides a unique opportunity for direct comparisons of in situ measurements and satellite-based instantaneous rain rate estimates like those from the Tropical Rainfall Measuring Mission (TRMM) precipitation radar (PR). The WGEW network is the densest rain gauge network in the PR coverage area for watersheds greater than 10 km(2). It consists of 88 weighing rain gauges within a 149-km(2) area. On average, approximately 10 gauges can be found in each PR field of view (similar to 5-km diameter). All gauges are very well synchronized with 1-min reporting intervals. This allows generating very-high-temporal-resolution rain rate fields and obtaining accurate estimates of the area-average rain rate for the entire watershed and for a single PR field of view. In this study, instantaneous rain rate fields from the PR and the spatially interpolated gauge measurements (on a 100 m 100 m grid, updated every 1 min) are compared for all TRMM overpasses in which the PR recorded rain within the WGEW boundaries (25 overpasses during 1999-2010). The results indicate very good agreement between the fields with low bias values (<10%) and high correlation coefficients, especially for the near-nadir cases (>0.9). The correlation is high at overpass time but the peak occurs several minutes after the overpass, which can be explained by the fact that it takes several minutes for the raindrops to reach the gauge from the time they are observed by the PR. The correlation improves with the new version of the TRMM algorithm (V7). The study includes assessment of the accuracy of the reference products.
C1 [Amitai, Eyal] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Amitai, Eyal; Thill, Bryson] Chapman Univ, Orange, CA USA.
[Unkrich, Carl L.; Goodrich, David C.] USDA ARS, SW Watershed Res Ctr, Tucson, AZ USA.
[Habib, Emad] Univ Louisiana Lafayette, Lafayette, LA 70504 USA.
RP Amitai, E (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM eyal.amitai@nasa.gov
RI Goodrich, David/B-1763-2009
OI Goodrich, David/0000-0001-7735-1448
FU NASA [NNX10AK46G]; NASA GSFC Summer Institute in Earth Sciences
Internship Program
FX Funding for Eyal Amitai and Bryson Thill is from NASA Grant NNX10AK46G
(2010/11) for Verifying Satellite Precipitation Estimates and Supporting
Satellite Algorithm Development. Additional support for Bryson comes
from the NASA GSFC 2011 Summer Institute in Earth Sciences Internship
Program. We wish to thank Robert Meneghini of the NASA GSFC for his
helpful suggestions. The staff of the USDA-ARS Southwest Watershed
Research Center is also commended for their diligent collection of
long-term, high-quality hydrometeorological observations. The anonymous
reviewers are also acknowledged for their valuable comments and careful
reviews.
NR 17
TC 9
Z9 10
U1 1
U2 9
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD OCT
PY 2012
VL 13
IS 5
BP 1579
EP 1588
DI 10.1175/JHM-D-12-016.1
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 023NT
UT WOS:000310042400012
ER
PT J
AU Koster, RD
Mahanama, SPP
AF Koster, Randal D.
Mahanama, Sarith P. P.
TI Land Surface Controls on Hydroclimatic Means and Variability
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID CATCHMENT-BASED APPROACH; PARAMETERIZATION SCHEMES; CLIMATE-CHANGE;
SOIL-MOISTURE; UNITED-STATES; CIRCULATION; PROJECT; EVAPOTRANSPIRATION;
INTERCOMPARISONS; BASIN
AB Hydroclimatic means and variability are determined in large part by the control of soil moisture on surface moisture fluxes, particularly evapotranspiration and runoff. This control is examined here using a simple water balance model and multidecadal observations covering the conterminous United States. Under the assumption that the relevant soil moisture-evapotranspiration and soil moisture-runoff relationships are, to first order, universal, the simple model illustrates the degree to which they interact to determine spatial distributions of hydroclimatic means and variability. In the process, the simple model provides estimates for the underlying relationships that operate in nature. The hydroclimatic sensitivities established with the simple water balance model can be used to evaluate more complex land surface models and to guide their further development, as demonstrated herein with an example.
C1 [Koster, Randal D.; Mahanama, Sarith P. P.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Mahanama, Sarith P. P.] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Koster, RD (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA.
EM randal.d.koster@nasa.gov
RI Koster, Randal/F-5881-2012
OI Koster, Randal/0000-0001-6418-6383
FU Earth System Science Program of the NOAA/Climate Program Office; NASA
FX This work was supported by the Earth System Science Program of the
NOAA/Climate Program Office and by the NASA Terrestrial Hydrology
Program. Greg Walker helped with some of the data analyses, and Matt
Rodell provided advice on the use of the GRACE data. Radiation data were
obtained from the NASA Langley Research Center Atmospheric Sciences Data
Center NASA/GEWEX SRB Project. Providers of basin streamflow data
include the U.S. Army Corps of Engineers (Omaha and Tulsa offices), the
Columbia River Basin Climate Change Scenarios Database, the California
Data Exchange Commission, and the U.S. Bureau of Reclamation; Edwin
Maurer of Santa Clara University helped obtain additional streamflow
data. GRACE land data were processed by Sean Swenson, supported by the
NASA MEASURES Program, and are available at http://grace.jpl.nasa.gov.
NR 31
TC 24
Z9 24
U1 0
U2 21
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD OCT
PY 2012
VL 13
IS 5
BP 1604
EP 1620
DI 10.1175/JHM-D-12-050.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 023NT
UT WOS:000310042400014
ER
PT J
AU Bae, SY
Korniski, RJ
Choi, JM
Shearn, M
Bahrami, P
Manohara, H
Shahinian, HK
AF Bae, Sam Y.
Korniski, Ron J.
Choi, John M.
Shearn, Michael
Bahrami, Poyan
Manohara, Harish
Shahinian, Hrayr K.
TI Development of a miniature single lens dual-aperture stereo imaging
system towards stereo endoscopic imaging application
SO OPTICAL ENGINEERING
LA English
DT Article
DE dual aperture; dual lens; stereo endoscope; disparity; stereoscopic
depth effect; depth perception
ID PERFORMANCE; VISION; NOVICE
AB Studies have shown that stereo images improve surgeons' visuomotor tasks and therefore constructively affect the outcome of a minimally invasive surgery. Stereo images are captured by a stereo endoscope, which consists commonly of duplicate lens systems. However, stereo images can also be captured by a single lens system following a dual aperture scheme (DAS). DAS creates two spatially separated optical channels by placing a dual aperture plate in the limiting aperture of a single lens system. This paper describes efforts to miniaturize the DAS-based imaging system for use in minimally invasive surgery. To demonstrate feasibility, a prototype was fabricated using lens elements 3 mm in diameter and was tested for its stereo depth effect (SDE). The SDE of the prototype was then compared to a duplicate lens system that was constructed theoretically in the same diameter as the 3-mm prototype. The results show that the prototype yields 4/7 of the SDE of the theoretical model. However, the SDE of the prototype provides sufficient SDE, in a viewing range of 1 to 2.5 cm from the lens, for minimally invasive surgery. (C) 2012 Society of PhotoOptical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.OE.51.10.103202]
C1 [Bae, Sam Y.; Korniski, Ron J.; Choi, John M.; Shearn, Michael; Bahrami, Poyan; Manohara, Harish] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Bae, Sam Y.; Bahrami, Poyan] Univ Calif Los Angeles, Los Angeles, CA 90024 USA.
[Shahinian, Hrayr K.] Skull Base Inst, Los Angeles, CA 90048 USA.
RP Bae, SY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM ybae@jpl.nasa.gov
FU Skull Base Institute of Los Angeles, California
FX This work was carried out under funding from the Skull Base Institute of
Los Angeles, California. Mr. Sam Bae wants to give special thanks to
Professor Harold Monbouquette of UCLA for his support and guidance of
the project for his PhD work at UCLA. This research was carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with the National Aeronautics and Space Administration. (C)
2012 California Institute of Technology. Government sponsorship is
acknowledged.
NR 19
TC 2
Z9 3
U1 0
U2 4
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 0091-3286
EI 1560-2303
J9 OPT ENG
JI Opt. Eng.
PD OCT
PY 2012
VL 51
IS 10
AR 103202
DI 10.1117/1.OE.51.10.103202
PG 6
WC Optics
SC Optics
GA 021WF
UT WOS:000309915400017
ER
PT J
AU Gao, J
Vissers, MR
Sandberg, MO
da Silva, FCS
Nam, SW
Pappas, DP
Wisbey, DS
Langman, EC
Meeker, SR
Mazin, BA
Leduc, HG
Zmuidzinas, J
Irwin, KD
AF Gao, J.
Vissers, M. R.
Sandberg, M. O.
da Silva, F. C. S.
Nam, S. W.
Pappas, D. P.
Wisbey, D. S.
Langman, E. C.
Meeker, S. R.
Mazin, B. A.
Leduc, H. G.
Zmuidzinas, J.
Irwin, K. D.
TI A titanium-nitride near-infrared kinetic inductance photon-counting
detector and its anomalous electrodynamics
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID ARRAYS; NOISE; BAND
AB We demonstrate single-photon counting at 1550 nm with titanium-nitride (TiN) microwave kinetic inductance detectors. Full-width-at-half-maximum energy resolution of 0.4 eV is achieved. 0-, 1-, 2-photon events are resolved and shown to follow Poisson statistics. We find that the temperature-dependent frequency shift deviates from the Mattis-Bardeen theory, and the dissipation response shows a shorter decay time than the frequency response at low temperatures. We suggest that the observed anomalous electrodynamics may be related to quasiparticle traps or subgap states in the disordered TiN films. Finally, the electron density-of-states is derived from the pulse response. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4756916]
C1 [Gao, J.; Vissers, M. R.; Sandberg, M. O.; da Silva, F. C. S.; Nam, S. W.; Pappas, D. P.; Irwin, K. D.] NIST, Boulder, CO 80305 USA.
[Wisbey, D. S.] St Louis Univ, Dept Phys, St Louis, MO 63103 USA.
[Langman, E. C.; Meeker, S. R.; Mazin, B. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Leduc, H. G.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gao, J (reprint author), NIST, Boulder, CO 80305 USA.
RI Mazin, Ben/B-8704-2011
OI Mazin, Ben/0000-0003-0526-1114
FU NASA [NNH11AR83I]; Keck Institute for Space Studies
FX We thank T. Klapwijk, T. Norguchi, J. Martinis, G. O'Nell, and A. Lita
for useful discussions. We acknowledge support for this work from the
Keck Institute for Space Studies and NASA under Contract No. NNH11AR83I.
The TiN film was deposited in the JPL Microdevices Lab (MDL), and the
device was fabricated in the NIST cleanroom.
NR 26
TC 27
Z9 27
U1 0
U2 28
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0003-6951
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD OCT 1
PY 2012
VL 101
IS 14
AR 142602
DI 10.1063/1.4756916
PG 4
WC Physics, Applied
SC Physics
GA 017PS
UT WOS:000309603300069
ER
PT J
AU Han, JW
Kim, B
Kobayashi, NP
Li, J
Meyyappan, M
AF Han, Jin-Woo
Kim, Beomseok
Kobayashi, Nobuhiko P.
Li, Jing
Meyyappan, M.
TI A simple method for the determination of doping type in nanomaterials
based on electrical response to humidity
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID CARBON NANOTUBES; GLASS SUBSTRATE; NANOWIRE; SENSORS; BREATH;
SENSITIVITY; TRANSISTORS; SURFACE
AB A simple method to determine the doping type of inorganic nanomaterials is presented. The surface reaction with moisture results in distinctive electrical responses depending on the doping type of the material. The moisture acts as an electron donor, releasing electrons to the semiconductor materials. Thus, the resistance of p-type materials increases due to the withdrawal of holes, while that of n-type decreases due to electron donation. Compared to spectroscopy and Hall measurement techniques, the present method is a simple and fast approach for determining the doping types, enabling fast feedback in material research as well as in device prototyping. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4757609]
C1 [Han, Jin-Woo; Kim, Beomseok; Li, Jing; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
[Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95064 USA.
RP Han, JW (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
EM jin-woo.han@nasa.gov
RI Kobayashi, Nobuhiko/E-3834-2012
NR 21
TC 9
Z9 9
U1 0
U2 14
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0003-6951
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD OCT 1
PY 2012
VL 101
IS 14
AR 142110
DI 10.1063/1.4757609
PG 3
WC Physics, Applied
SC Physics
GA 017PS
UT WOS:000309603300057
ER
PT J
AU Li, D
Jiang, Y
Ding, YJJ
Zotova, IB
Prasad, NS
AF Li, Da
Jiang, Yi
Ding, Yujie J.
Zotova, Ioulia B.
Prasad, Narasimha S.
TI Approaching single-photon detection in near-infrared region
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID FREQUENCY UP-CONVERSION; LINBO3 WAVE-GUIDES; QUANTUM ENTANGLEMENT;
EFFICIENT
AB We have implemented a single-photon detection system in the 1.55-mu m region, based on frequency up-conversion in MgO-doped periodically poled LiNbO3 waveguide. We have subsequently reached a record-low dark count rate of 45 counts per second. The detectable signal photon rate, i.e., the rate for counting the up-converted photons corrected by the dark counts, noises, and losses, reaches a record-low value of 81 photons per second. Through free-space coupling, we have eliminated the dark counts induced by parametric fluorescence. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4757885]
C1 [Li, Da; Jiang, Yi; Ding, Yujie J.] Lehigh Univ, Dept Elect & Comp Engn, Bethlehem, PA 18015 USA.
[Zotova, Ioulia B.] ArkLight, Center Valley, PA 18034 USA.
[Prasad, Narasimha S.] NASA, Laser Remote Sensing Branch, Langley Res Ctr, Hampton, VA 23681 USA.
RP Li, D (reprint author), Lehigh Univ, Dept Elect & Comp Engn, Bethlehem, PA 18015 USA.
EM yud2@lehigh.edu
FU U.S. NASA
FX This work has been supported by U.S. NASA.
NR 9
TC 8
Z9 9
U1 0
U2 7
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0003-6951
EI 1077-3118
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD OCT 1
PY 2012
VL 101
IS 14
AR 141126
DI 10.1063/1.4757885
PG 3
WC Physics, Applied
SC Physics
GA 017PS
UT WOS:000309603300026
ER
PT J
AU Zahorian, SA
Zuckerwar, AJ
Karnjanadecha, M
AF Zahorian, Stephen A.
Zuckerwar, Allan J.
Karnjanadecha, Montri
TI Dual transmission model and related spectral content of the fetal heart
sounds
SO COMPUTER METHODS AND PROGRAMS IN BIOMEDICINE
LA English
DT Article
DE Fetal phonocardiography; Fetal heart monitoring; Heart sound modeling;
Dual transmission model; Digital signal processing
ID PHONOCARDIOGRAPHY; SENSOR; TIME
AB A dual transmission model of the fetal heart sounds is presented in which the properties of the signals received on a sensor, installed on the maternal abdominal surface, depend upon the position of the fetus. For a fetus in the occiput anterior position, the predominant spectral content lies in the frequency band 16-50 Hz ("impact" mode), but for a fetus in the occiput posterior position, it lies in the frequency band 80-110 Hz ("acoustic" mode). Signal processing comprises digital bandpass filtering, matched filtering, Teager energy operator, autocorrelation, and figure of merit algorithms. The digital filter permits the user to select the frequency band that best conforms to the prevailing signal mode. Clinical tests on twelve patients, with some in the occiput anterior and some in the occiput posterior fetal positions, support the validity of the dual transmission model. (c) 2011 Elsevier Ireland Ltd. All rights reserved.
C1 [Zahorian, Stephen A.] SUNY Binghamton, Dept Elect & Comp Engn, Binghamton, NY 13902 USA.
[Zuckerwar, Allan J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Karnjanadecha, Montri] Prince Songkla Univ, Fac Engn, Dept Comp Engn, Hat Yai 90112, Songkhla, Thailand.
RP Zahorian, SA (reprint author), SUNY Binghamton, Dept Elect & Comp Engn, Binghamton, NY 13902 USA.
EM zahorian@binghamton.edu; ajzuckerwar@yahoo.com; montri@coe.psu.ac.th
FU Technology Utilization Office of NASA Langley Research Center
FX The authors gratefully acknowledge the work of Timothy Bryant, Nancy
Holloway, and Dennis Mowrey, NASA Langley Research Center, for
fabricating the fetal heart rate monitor used in this study. The authors
further thank the following persons for assistance in conducting the
fetal heart monitoring tests: Dr. Margarita De Veciana, MD, and Linda
Bennington, RN, of the Fetal Diagnostic Unit, Eastern Virginia Medical
School, Norfolk, VA, and Dr. Micki L. Cabaniss, MD, Western Carolina
Maternal-Fetal Medicine, Asheville, NC. The test protocol was approved
by the institutional review boards of NASA Langley Research Center, Old
Dominion University, Eastern Virginia Medical School, and Western
Carolina Maternal-Fetal Medicine. Financial support was provided by the
Technology Utilization Office of NASA Langley Research Center.
NR 13
TC 2
Z9 3
U1 0
U2 15
PU ELSEVIER IRELAND LTD
PI CLARE
PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000,
IRELAND
SN 0169-2607
J9 COMPUT METH PROG BIO
JI Comput. Meth. Programs Biomed.
PD OCT
PY 2012
VL 108
IS 1
BP 20
EP 27
DI 10.1016/j.cmpb.2011.12.006
PG 8
WC Computer Science, Interdisciplinary Applications; Computer Science,
Theory & Methods; Engineering, Biomedical; Medical Informatics
SC Computer Science; Engineering; Medical Informatics
GA 015JU
UT WOS:000309443000003
PM 22285458
ER
PT J
AU Hacker, J
Urteaga, M
Lin, R
Skalare, A
Mehdi, I
Rieh, JS
Kim, M
AF Hacker, J.
Urteaga, M.
Lin, R.
Skalare, A.
Mehdi, I.
Rieh, J. -S.
Kim, M.
TI 400 GHz HBT Differential Amplifier Using Unbalanced Feed Networks
SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS
LA English
DT Article
DE Differential feed; InP HBT; terahertz amplifier
AB A terahertz differential eight-stage amplifier fabricated using state-of-the-art 125 nm double-heterojunction bipolar transistors (DHBT) is presented. The four-port unit-cell chain is designed for optimum forward differential gain with no even and odd-mode reverse gains. Unbalanced single-ended feed networks are added to preserve the amplifier gain without inducing oscillations. The proposed feed scheme is validated by a stable amplifier operation in 325-to-450 GHz range with the peak gain of 22 dB at 375 GHz.
C1 [Hacker, J.; Urteaga, M.] Teledyne Sci Co, Thousand Oaks, CA 91360 USA.
[Lin, R.; Skalare, A.; Mehdi, I.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Rieh, J. -S.; Kim, M.] Korea Univ, Sch Elect Engn, Seoul 136701, South Korea.
RP Hacker, J (reprint author), Teledyne Sci Co, Thousand Oaks, CA 91360 USA.
EM mkim@korea.ac.kr
FU KCC (Korea Communications Commission) [KCA-2012-12-911-01-101]
FX This work was supported by the KCC (Korea Communications Commission)
under the R&D program supervised by the KCA (Korea Communications
Agency) [KCA-2012-12-911-01-101].
NR 5
TC 6
Z9 6
U1 0
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1531-1309
J9 IEEE MICROW WIREL CO
JI IEEE Microw. Wirel. Compon. Lett.
PD OCT
PY 2012
VL 22
IS 10
BP 536
EP 538
DI 10.1109/LMWC.2012.2214767
PG 3
WC Engineering, Electrical & Electronic
SC Engineering
GA 019IT
UT WOS:000309732600014
ER
PT J
AU Pogorzelski, RJ
AF Pogorzelski, Ronald J.
TI On the Design of Coupling Networks for Coupled Oscillator Arrays (vol
51, pg 794, 2003)
SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION
LA English
DT Correction
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Pogorzelski, RJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM pogo@ieee.org
NR 1
TC 0
Z9 0
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-926X
J9 IEEE T ANTENN PROPAG
JI IEEE Trans. Antennas Propag.
PD OCT
PY 2012
VL 60
IS 10
BP 4980
EP 4980
DI 10.1109/TAP.2012.2207365
PG 1
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA 019LY
UT WOS:000309742400065
ER
PT J
AU Galofaro, JT
Vayner, BV
Hillard, GB
AF Galofaro, Joel T.
Vayner, Boris V.
Hillard, G. Barry
TI Dependence of String Electron Current on Array Plasma Aspect Angle and
Temperature
SO IEEE TRANSACTIONS ON PLASMA SCIENCE
LA English
DT Article
DE Aerospace simulations; current measurements; laboratories; low Earth
orbital (LEO) satellites
AB In most cases, the incident aspect angle of a photovoltaic array to the local plasma continuously changes for a spacecraft in low Earth orbit. It is possible to simulate the combined effects of changing array ram aspect angle with respect to the plasma flow inside a vacuum chamber. On-orbit solar array collected current will significantly vary as a function of the angle between the spacecraft velocity vector and the solar array front surface normal vector. The purpose of this paper is to extract this angular dependence of electron current collection of UltraFlex solar array coupons, as well as to measure the dependence of string electron collection current on array temperature. It is found that collected current can be approximated by a cosine function with a 70% drop when the array coupon front surface normal vector is rotated to an angle from 15 degrees to 90 degrees. It was also determined in subsequent tests with two electron number densities of N-e = 0.5 . 10(6) cm(-3) and 1.0 . 10(6) cm(-3) that electron current collection does not depend on the sample temperature.
C1 [Galofaro, Joel T.; Hillard, G. Barry] NASA, Photovolta & Power Technol Branch, John H Glenn Res Ctr, Cleveland, OH 44135 USA.
[Vayner, Boris V.] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
RP Galofaro, JT (reprint author), NASA, Photovolta & Power Technol Branch, John H Glenn Res Ctr, Cleveland, OH 44135 USA.
EM joel.t.galofaro@nasa.gov
NR 10
TC 0
Z9 0
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0093-3813
J9 IEEE T PLASMA SCI
JI IEEE Trans. Plasma Sci.
PD OCT
PY 2012
VL 40
IS 10
BP 2745
EP 2750
DI 10.1109/TPS.2012.2211897
PN 2
PG 6
WC Physics, Fluids & Plasmas
SC Physics
GA 021EO
UT WOS:000309868300013
ER
PT J
AU Himberg, H
Motai, Y
Bradley, A
AF Himberg, Henry
Motai, Yuichi
Bradley, Arthur
TI Interpolation Volume Calibration: A Multisensor Calibration Technique
for Electromagnetic Trackers
SO IEEE TRANSACTIONS ON ROBOTICS
LA English
DT Article
DE AC magnetic tracking; magnetic tracker calibration; position and
orientation measurements
ID TRACKING-SYSTEMS; MAGNETIC POSITION; RAPID METHOD; TELEOPERATION;
ACCURACY; REALITY; DEVICE
AB AC electromagnetic trackers are well suited for head tracking but are adversely affected by conductive and ferromagnetic materials. Tracking performance can be improved by mapping the tracking volume to produce coefficients that correct position and orientation (PnO) measurements caused by stationary distorting materials. The mapping process is expensive and time consuming, requiring complicated high-precision equipment to provide registration of the measurements to the source reference frame. In this study, we develop a new approach to mapping that provides registration of mapping measurements without precision equipment. Our method, i.e., the interpolation volume calibration system, uses two simple fixtures, each with multiple sensors in a rigid geometry, to determine sensor PnO in a distorted environment without mechanical measurements or other tracking technologies. We test our method in a distorted tracking environment, constructing a lookup table of the magnetic field that is used as the basis for distortion compensation. The new method compares favorably with the traditional approach providing a significant reduction in cost and effort.
C1 [Himberg, Henry] Polhemus Inc, Colchester, VT 05446 USA.
[Motai, Yuichi] Virginia Commonwealth Univ, Dept Elect & Comp Engn, Richmond, VA 23284 USA.
[Bradley, Arthur] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Himberg, H (reprint author), Polhemus Inc, Colchester, VT 05446 USA.
EM hhimberg@polhemus.com; ymotai@vcu.edu; arthur.t.bradley@nasa.gov
FU National Science Foundation under Grant ECCS [1054333]; School of
Engineering, Virginia Commonwealth University, Richmond, VA; Polhemus,
Inc., Colchester, VA
FX This work was supported in part by the National Science Foundation under
Grant ECCS #1054333 and by the School of Engineering, Virginia
Commonwealth University, Richmond, VA.; The authors would like to thank
Polhemus, Inc., Colchester, VA, for support, time, and equipment used in
this study. They would also like to thank H. Jones, J. Farr, and B.
Himberg for their assistance.
NR 35
TC 4
Z9 4
U1 1
U2 8
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1552-3098
J9 IEEE T ROBOT
JI IEEE Trans. Robot.
PD OCT
PY 2012
VL 28
IS 5
BP 1120
EP 1130
DI 10.1109/TRO.2012.2198929
PG 11
WC Robotics
SC Robotics
GA 019HL
UT WOS:000309728700011
ER
PT J
AU Rodrigues, F
Galante, D
Paulino-Lima, IG
Duarte, RTD
Friaca, ACS
Lage, C
Janot-Pacheco, E
Teixeira, R
Horvath, JE
AF Rodrigues, Fabio
Galante, Douglas
Paulino-Lima, Ivan G.
Duarte, Rubens T. D.
Friaca, Amancio C. S.
Lage, Claudia
Janot-Pacheco, Eduardo
Teixeira, Ramachrisna
Horvath, Jorge E.
TI Astrobiology in Brazil: early history and perspectives
SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY
LA English
DT Article
DE SPASA 2011; astrobiology; Brazil; history; astrobiologia
ID STAR-FORMING REGIONS; EFFECTIVE SOLAR-RADIATION; TRANSFER-RNA
SYNTHETASES; MEAN-MOTION RESONANCE; SOUTH-CENTRAL BRAZIL; SOFT X-RAYS;
AMINO-ACIDS; ORGANIC-MOLECULES; SPORE DOSIMETRY; DEINOCOCCUS-RADIODURANS
AB This review reports the Brazilian history in astrobiology, as well as the first delineation of a vision of the future development of the field in the country, exploring its abundant biodiversity, highly capable human resources and state-of-the-art facilities, reflecting the last few years of stable governmental investments in science, technology and education, all conditions providing good perspectives on continued and steadily growing funding for astrobiology-related research. Brazil is growing steadily and fast in terms of its worldwide economic power, an effect being reflected in different areas of the Brazilian society, including industry, technology, education, social care and scientific production. In the field of astrobiology, the country has had some important landmarks, more intensely after the First Brazilian Workshop on Astrobiology in 2006. The history of astrobiology in Brazil, however, is not so recent and had its first occurrence in 1958. Since then, researchers carried out many individual initiatives across the country in astrobiology-related fields, resulting in an ever growing and expressive scientific production. The number of publications, including articles and theses, has particularly increased in the last decade, but still counting with the effort of researchers working individually. That scenario started to change in 2009, when a formal group of Brazilian researchers working with astrobiology was organized, aiming at congregating the scientific community interested in the subject and to promote the necessary interactions to achieve a multidisciplinary work, receiving facilities and funding from the University de Sao Paulo and other funding agencies. Received 29 February 2012, accepted 17 May 2012, first published online 18 July 2012
C1 [Rodrigues, Fabio] Univ Sao Paulo, Inst Quim, BR-05508 Sao Paulo, Brazil.
[Galante, Douglas; Friaca, Amancio C. S.; Janot-Pacheco, Eduardo; Teixeira, Ramachrisna; Horvath, Jorge E.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508 Sao Paulo, Brazil.
[Paulino-Lima, Ivan G.] NASA, Ames Res Ctr, Washington, DC USA.
[Duarte, Rubens T. D.] Univ Sao Paulo, Inst Oceanog, BR-05508 Sao Paulo, Brazil.
[Lage, Claudia] Univ Fed Rio de Janeiro, Inst Biofis Carlos Chagas Filho, BR-21941 Rio De Janeiro, Brazil.
RP Rodrigues, F (reprint author), Univ Sao Paulo, Inst Quim, BR-05508 Sao Paulo, Brazil.
EM farod@iq.usp.br
RI Galante, Douglas/G-8752-2011; Lage, Claudia/K-6563-2012; Horvath, Jorge
/C-3075-2012; Tecnologias espaciai, Inct/I-2415-2013; Duarte,
Rubens/E-3129-2012; Institute of Chemistry - USP, Dept. of
Chemistry/B-8988-2012; Paulino Lima, Ivan Glaucio/K-8908-2012
OI Galante, Douglas/0000-0002-3265-2527; Lage, Claudia/0000-0001-9870-9955;
Paulino Lima, Ivan Glaucio/0000-0003-1580-8435
FU FAPESP (Sao Paulo Research Foundation); National Institute of Space
Research (INEspaco - MCT/CNPq); Brazilian Antarctic Program (PROANTAR -
CNPq); Universidade de Sao Paulo; Brazilian Astrobiology Research Center
(NAP-Astrobio)
FX The authors would like to thank FAPESP (Sao Paulo Research Foundation),
the National Institute of Space Research (INEspaco - MCT/CNPq), the
Brazilian Antarctic Program (PROANTAR - CNPq) and Universidade de Sao
Paulo for the financial support of the Brazilian Astrobiology Research
Center (NAP-Astrobio). The authors also would like to thank the
Brazilian Synchrotron Light Source (LNLS - Campinas) for the use of its
facilities (TGM beamline) and to Professor Dimas A. M. Zaia and
Professor Jorge A. Quillfeldt for the information given about
astrobiology in their institutions.
NR 139
TC 3
Z9 3
U1 0
U2 12
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 1473-5504
J9 INT J ASTROBIOL
JI Int. J. Astrobiol.
PD OCT
PY 2012
VL 11
IS 4
SI SI
BP 189
EP 202
DI 10.1017/S1473550412000250
PG 14
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 019GF
UT WOS:000309724800002
ER
PT J
AU Lage, CAS
Dalmaso, GZL
Teixeira, LCRS
Bendia, AG
Paulino-Lima, IG
Galante, D
Janot-Pacheco, E
Abrevaya, XC
Azua-Bustos, A
Pelizzari, VH
Rosado, AS
AF Lage, Claudia A. S.
Dalmaso, Gabriel Z. L.
Teixeira, Lia C. R. S.
Bendia, Amanda G.
Paulino-Lima, Ivan G.
Galante, Douglas
Janot-Pacheco, Eduardo
Abrevaya, Ximena C.
Azua-Bustos, Armando
Pelizzari, Vivian H.
Rosado, Alexandre S.
TI Mini-Review: Probing the limits of extremophilic life in
extraterrestrial environment-simulated experiments
SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY
LA English
DT Review
DE astrobiology; cosmic dust; extremophiles; panspermia; ultraviolet
ID BACTERIUM DEINOCOCCUS RADIODURANS; MIXED WASTE ENVIRONMENTS;
RADIATION-RESISTANCE; ATACAMA DESERT; SURVIVAL; MARS; SPACE; TITAN;
DEGRADATION; PERSPECTIVE
AB Astrobiology is a relatively recent scientific field that seeks to understand the origin and dynamics of life in the Universe. Several hypotheses have been proposed to explain life in the cosmic context throughout human history, but only now, technology has allowed many of them to be tested. Laboratory experiments have been able to show how chemical elements essential to life, such as carbon, nitrogen, oxygen and hydrogen combine in biologically important compounds. Interestingly, these compounds are ubiquitous. How these compounds were combined to the point of originating cells and complex organisms is still to be unveiled by science. However, our 4.5 billion years old Solar system appeared in a 10 billion years old Universe. Thus, simple cells such as micro-organisms may have had time to form in planets older than ours or in other suitable places in the Universe. One hypothesis related to the appearance of life on Earth is called panspermia, which predicts that microbial life could have been formed in the Universe billions of years ago, travelling between planets, and inseminating units of life that could have become more complex in habitable planets such as Earth. A project designed to test the viability of extremophile micro-organisms exposed to simulated extraterrestrial environments is in progress at the Carlos Chagas Filho Institute of Biophysics (UFRJ, Brazil) to test whether microbial life could withstand inhospitable environments. Radiation-resistant (known or novel ones) micro-organisms collected from extreme terrestrial environments have been exposed (at synchrotron accelerators) to intense radiation sources simulating Solar radiation, capable of emitting radiation in a few hours equivalent to many years of accumulated doses. The results obtained in these experiments reveal an interesting possibility of the existence of microbial life beyond Earth. Received 29 February 2012, accepted 6 July 2012, first published online 16 August 2012
C1 [Lage, Claudia A. S.; Dalmaso, Gabriel Z. L.; Teixeira, Lia C. R. S.; Bendia, Amanda G.] Univ Fed Rio de Janeiro, Lab Radiacoes Biol, Inst Biofis Carlos Chagas Filho, BR-21941 Rio De Janeiro, Brazil.
[Paulino-Lima, Ivan G.] NASA, Ames Res Ctr, Washington, DC USA.
[Galante, Douglas; Janot-Pacheco, Eduardo] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508 Sao Paulo, Brazil.
[Abrevaya, Ximena C.] Univ Buenos Aires, Inst Astron & Fis Espacio, CONICET, RA-1053 Buenos Aires, DF, Argentina.
[Azua-Bustos, Armando] Pontificia Univ Catolica Chile, Santiago, Chile.
[Pelizzari, Vivian H.] Univ Sao Paulo, Inst Oceanog, BR-05508 Sao Paulo, Brazil.
[Rosado, Alexandre S.] Univ Fed Rio de Janeiro, Inst Microbiol Prof Paulo Goes, BR-21941 Rio De Janeiro, Brazil.
RP Lage, CAS (reprint author), Univ Fed Rio de Janeiro, Lab Radiacoes Biol, Inst Biofis Carlos Chagas Filho, BR-21941 Rio De Janeiro, Brazil.
EM lage@biof.ufrj.br
RI Galante, Douglas/G-8752-2011; Lage, Claudia/K-6563-2012; Tecnologias
espaciai, Inct/I-2415-2013; Dalmaso, Gabriel/P-3966-2014; Paulino Lima,
Ivan Glaucio/K-8908-2012;
OI Galante, Douglas/0000-0002-3265-2527; Lage, Claudia/0000-0001-9870-9955;
Paulino Lima, Ivan Glaucio/0000-0003-1580-8435; Rosado,
Alexandre/0000-0001-5135-1394
FU Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES);
Conselho Nacional de Pesquisas e Desenvolvimento Tecnologico (CNPq);
Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de
Janeiro (FAPERJ); Laboratorio Nacional de Luz Sincrotron (LNLS-CNPEM);
Ministry of Science, Technology Innovation; CNPq joint program of
National Institutes of Science and Technology (INCT), INEspaco
FX Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES),
Conselho Nacional de Pesquisas e Desenvolvimento Tecnologico (CNPq),
Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de
Janeiro (FAPERJ) and Laboratorio Nacional de Luz Sincrotron (LNLS-CNPEM)
for research Grants and fellowships. This project was also funded by the
Ministry of Science, Technology & Innovation and CNPq joint program of
National Institutes of Science and Technology (INCT), INEspaco.
NR 47
TC 2
Z9 2
U1 13
U2 144
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 1473-5504
J9 INT J ASTROBIOL
JI Int. J. Astrobiol.
PD OCT
PY 2012
VL 11
IS 4
SI SI
BP 251
EP 256
DI 10.1017/S1473550412000316
PG 6
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 019GF
UT WOS:000309724800008
ER
PT J
AU Arens, E
AF Arens, Ellen
TI TANK test Thermal Imaging for Inspection of Large Cryogenic Tanks
SO MATERIALS EVALUATION
LA English
DT Article
C1 NASA, Appl Phys Lab, Kennedy Space Ctr, FL 32935 USA.
RP Arens, E (reprint author), NASA, Appl Phys Lab, NE L5, Kennedy Space Ctr, FL 32935 USA.
FU Fluids and Propulsion groups at Kennedy Space Center
FX This work was performed with support from members of the Applied Physics
Laboratory, as well as Fluids and Propulsion groups at Kennedy Space
Center. Thanks are given for their valuable inputs.
NR 3
TC 1
Z9 1
U1 0
U2 0
PU AMER SOC NONDESTRUCTIVE TEST
PI COLUMBUS
PA 1711 ARLINGATE LANE PO BOX 28518, COLUMBUS, OH 43228-0518 USA
SN 0025-5327
J9 MATER EVAL
JI Mater. Eval.
PD OCT
PY 2012
VL 70
IS 10
BP 1147
EP 1152
PG 6
WC Materials Science, Characterization & Testing
SC Materials Science
GA 019JV
UT WOS:000309736700003
ER
PT J
AU Vassen, R
Kagawa, Y
Subramanian, R
Zombo, P
Zhu, DM
AF Vassen, Robert
Kagawa, Yutaka
Subramanian, Ramesh
Zombo, Paul
Zhu, Dongming
TI Testing and evaluation of thermal-barrier coatings
SO MRS BULLETIN
LA English
DT Article
ID YTTRIA-STABILIZED ZIRCONIA; ACOUSTIC THERMOGRAPHY; MECHANICAL FATIGUE;
CREEP-BEHAVIOR; TEMPERATURE; SPECTROSCOPY; GENERATION; GRADIENT; TBC;
CONDUCTIVITY
AB Thermal-barrier coatings are complex systems with properties that largely depend on their specific microstructure. Their properties change during operation, typically leading to degradation. A further difficulty arises from the fact that this degradation also depends on specific loading conditions that can be rather complex. Different laboratory setups are described that simulate, at least partially, the actual loading conditions. In addition, sensing and nondestructive methods are described that are targeted toward reliable operation of a gas-turbine engine with thermal-barrier coated components.
C1 [Vassen, Robert] Forschungszentrum Julich GmbH, Inst Energy & Climate Res, Julich, Germany.
[Kagawa, Yutaka] Univ Tokyo, Res Ctr Adv Sci & Technol, Tokyo 1138654, Japan.
[Zombo, Paul] Siemens Energy Inc, Engine & Component Diagnost, Orlando, FL USA.
[Zhu, Dongming] NASA Glenn Res Ctr, Durabil & Protect Coatings Branch, Struct & Mat Div, Cleveland, OH USA.
RP Vassen, R (reprint author), Forschungszentrum Julich GmbH, Inst Energy & Climate Res, Julich, Germany.
EM r.vassen@fz-juelich.de; kagawa@rcast.u-tokyo.ac.jp;
Ramesh.Subramanian@siemens.com; Paul.Zombo@siemens.com;
dongming.zhu@nasa.gov
NR 37
TC 9
Z9 9
U1 6
U2 36
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0883-7694
J9 MRS BULL
JI MRS Bull.
PD OCT
PY 2012
VL 37
IS 10
BP 911
EP 916
DI 10.1557/mrs.2012.235
PG 6
WC Materials Science, Multidisciplinary; Physics, Applied
SC Materials Science; Physics
GA 019IX
UT WOS:000309733100015
ER
PT J
AU Zang, TA
AF Zang, Thomas A.
TI On the expression of uncertainty intervals in engineering
SO THEORETICAL AND COMPUTATIONAL FLUID DYNAMICS
LA English
DT Article
DE Uncertainty quantification; Intervals; Engineering; Statistics
ID STATISTICAL COVERAGE INTERVALS; SYSTEMS
AB The paper summarizes the terminology of the statistics and probability disciplines as they pertain to uncertainty quantification in engineering.
C1 NASA Langley Res Ctr, Hampton, VA 23681 USA.
RP Zang, TA (reprint author), NASA Langley Res Ctr, Hampton, VA 23681 USA.
EM tzangmands@wildblue.net
NR 43
TC 0
Z9 0
U1 0
U2 1
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0935-4964
EI 1432-2250
J9 THEOR COMP FLUID DYN
JI Theor. Comput. Fluid Dyn.
PD OCT
PY 2012
VL 26
IS 5
SI SI
BP 403
EP 414
DI 10.1007/s00162-012-0273-y
PG 12
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA 021JX
UT WOS:000309882200002
ER
PT J
AU Barth, T
AF Barth, Timothy
TI On the propagation of statistical model parameter uncertainty in CFD
calculations
SO THEORETICAL AND COMPUTATIONAL FLUID DYNAMICS
LA English
DT Article
DE Uncertainty quantification; Computational fluid dynamics; Finite-volume
methods
ID PARTIAL-DIFFERENTIAL-EQUATIONS; GENERALIZED POLYNOMIAL CHAOS; FLOW
SIMULATIONS; QUANTIFICATION; EXPANSIONS; SCHEMES
AB This work considers a new class of finite-volume approximations for scalar and system nonlinear conservation laws with multiple sources of stochastic model parameter uncertainty. The deterministic propagation of model parameter uncertainty is achieved through the introduction of additional stochastic coordinates. Particular attention is given to the construction of specialized piecewise polynomial approximation spaces well suited to the high-order accurate approximation of solution discontinuities in both physical and stochastic dimensions without exhibiting Gibbs-like oscillations characteristic of polynomial approximation. The proposed discretization easily retrofits existing finite-volume CFD codes in use today. Numerical results are presented for inviscid Burgers equation with uncertain initial data as well as the compressible Reynolds-averaged Navier-Stokes equations with uncertain boundary data and turbulence model parameters.
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Barth, T (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Timothy.J.Barth@nasa.gov
NR 37
TC 4
Z9 4
U1 0
U2 13
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0935-4964
EI 1432-2250
J9 THEOR COMP FLUID DYN
JI Theor. Comput. Fluid Dyn.
PD OCT
PY 2012
VL 26
IS 5
SI SI
BP 435
EP 457
DI 10.1007/s00162-011-0221-2
PG 23
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA 021JX
UT WOS:000309882200004
ER
PT J
AU Chuss, DT
Wollack, EJ
Pisano, G
Ackiss, S
U-Yen, K
Ng, MW
AF Chuss, David T.
Wollack, Edward J.
Pisano, Giampaolo
Ackiss, Sheridan
U-Yen, Kongpop
Ming Wah Ng
TI A translational polarization rotator
SO APPLIED OPTICS
LA English
DT Article
ID HALF-WAVE PLATE; POLARIMETRY
AB We explore a free-space polarization modulator in which a variable phase is introduced between the right-and left-handed circular polarization components and used to rotate the linear polarization of the outgoing beam relative to that of the incoming beam. In this device, the polarization states are separated by a circular polarizer that consists of a quarter-wave plate in combination with a wire grid. A movable mirror is positioned behind and parallel to the circular polarizer. As the polarizer-mirror distance is changed, an incident linear polarization will be rotated through an angle that is proportional to the introduced phase delay. We demonstrate a prototype device that modulates Stokes Q and U over a 20% bandwidth, from 77 to 94 GHz.
C1 [Chuss, David T.; Wollack, Edward J.; U-Yen, Kongpop] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pisano, Giampaolo; Ming Wah Ng] Univ Manchester, Sch Phys Astron, Manchester M13 9PL, Lancs, England.
[Ackiss, Sheridan] Georgia Tech, Atlanta, GA 30332 USA.
RP Chuss, DT (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM David.T.Chuss@nasa.gov
RI Wollack, Edward/D-4467-2012
OI Wollack, Edward/0000-0002-7567-4451
FU Goddard Space Flight Center; Georgia Tech Undergraduate Student
Researchers' Program; NASA Georgia Space Act Consortium
FX This work was funded by an internal research award at the Goddard Space
Flight Center. Funding for S. Ackiss was provided in part through the
Georgia Tech Undergraduate Student Researchers' Program and the NASA
Georgia Space Act Consortium.
NR 19
TC 7
Z9 7
U1 1
U2 10
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD OCT 1
PY 2012
VL 51
IS 28
BP 6824
EP 6830
DI 10.1364/AO.51.006824
PG 7
WC Optics
SC Optics
GA 016UI
UT WOS:000309544600016
PM 23033098
ER
PT J
AU Ryan, DF
Milligan, RO
Gallagher, PT
Dennis, BR
Tolbert, AK
Schwartz, RA
Young, CA
AF Ryan, Daniel F.
Milligan, Ryan O.
Gallagher, Peter T.
Dennis, Brian R.
Tolbert, A. Kim
Schwartz, Richard A.
Young, C. Alex
TI THE THERMAL PROPERTIES OF SOLAR FLARES OVER THREE SOLAR CYCLES USING
GOES X-RAY OBSERVATIONS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; methods: statistical; Sun: atmosphere; Sun: corona; Sun:
flares; Sun: X-rays, gamma rays
ID RHESSI MICROFLARE STATISTICS; EMISSION MEASURE; ATOMIC DATABASE;
ELECTRON-TEMPERATURE; ELEMENTS HYDROGEN; RATE COEFFICIENTS; EVOLUTION;
CHIANTI; PLASMA; LINES
AB Solar flare X-ray emission results from rapidly increasing temperatures and emission measures in flaring active region loops. To date, observations from the X-Ray Sensor (XRS) on board the Geostationary Operational Environmental Satellite (GOES) have been used to derive these properties, but have been limited by a number of factors, including the lack of a consistent background subtraction method capable of being automatically applied to large numbers of flares. In this paper, we describe an automated Temperature and Emission measure-Based Background Subtraction method (TEBBS), that builds on the methods of Bornmann. Our algorithm ensures that the derived temperature is always greater than the instrumental limit and the pre-flare background temperature, and that the temperature and emission measure are increasing during the flare rise phase. Additionally, TEBBS utilizes the improved estimates of GOES temperatures and emission measures from White et al. TEBBS was successfully applied to over 50,000 solar flares occurring over nearly three solar cycles (1980-2007), and used to create an extensive catalog of the solar flare thermal properties. We confirm that the peak emission measure and total radiative losses scale with background subtracted GOES X-ray flux as power laws, while the peak temperature scales logarithmically. As expected, the peak emission measure shows an increasing trend with peak temperature, although the total radiative losses do not. While these results are comparable to previous studies, we find that flares of a given GOES class have lower peak temperatures and higher peak emission measures than previously reported. The TEBBS database of flare thermal plasma properties is publicly available at http://www.SolarMonitor.org/TEBBS/.
C1 [Ryan, Daniel F.; Gallagher, Peter T.] Univ Dublin Trinity Coll, Sch Phys, Dublin 2, Ireland.
[Milligan, Ryan O.; Dennis, Brian R.; Tolbert, A. Kim; Schwartz, Richard A.; Young, C. Alex] NASA, Solar Phys Lab Code 671, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Milligan, Ryan O.; Schwartz, Richard A.] Catholic Univ Amer, Washington, DC 20064 USA.
RP Ryan, DF (reprint author), Univ Dublin Trinity Coll, Sch Phys, Dublin 2, Ireland.
RI Gallagher, Peter/C-7717-2011
OI Gallagher, Peter/0000-0001-9745-0400
FU Irish Research Council for Science, Engineering, and Technology
(IRCSET); Queen's University Belfast
FX D.F.R. thanks the Irish Research Council for Science, Engineering, and
Technology (IRCSET) for funding this research. R.O.M. thanks Queen's
University Belfast for the award of a Leverhulme Trust Research
Fellowship. In addition, thanks are given to Drs. Stephen White, Jack
Ireland, D. Shaun Bloomfield, and Claire L. Raftery for their insightful
discussions which contributed to this work. Finally, thanks is due to
David Perez-Suarez for his invaluable contribution in designing the
TEBBS Website (http://www.SolarMonitor.org/TEBBS/).
NR 40
TC 22
Z9 23
U1 1
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 OCT
PY 2012
VL 202
IS 2
AR 11
DI 10.1088/0067-0049/202/2/11
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 016ZM
UT WOS:000309558400001
ER
PT J
AU Martin, DS
Caine, TL
Matz, T
Lee, SMC
Stenger, MB
Sargsyan, AE
Platts, SH
AF Martin, David S.
Caine, Timothy L.
Matz, Timothy
Lee, Stuart M. C.
Stenger, Michael B.
Sargsyan, Ashot E.
Platts, Steven H.
TI Virtual Guidance as a Tool to Obtain Diagnostic Ultrasound for
Spaceflight and Remote Environments
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Article
DE just-in-time training; exploration missions; International Space Station
ID INTERNATIONAL-SPACE-STATION; SONOGRAPHY; ABOARD
AB MARTIN DS, CAINE TL, MATZ T, LEE SMC, STENGER MB, SARGSYAN AE, PLATTS SH. Virtual guidance as a tool to obtain diagnostic ultrasound for spaceflight and remote environments. Aviat Space Environ Med 2012; 83:995-1000.
Introduction: With missions planned to travel greater distances trom Earth at ranges that make real-time two-way communication impractical, astronauts will be required to perform autonomous medical diagnostic procedures during future exploration missions. Virtual guidance is a form of just-in-time training developed to allow novice ultrasound operators to acquire diagnostically-adequate images of clinically relevant anatomical structures using a prerecorded audio/visual tutorial viewed in real-time. Methods: Individuals without previous experience in ultrasound were recruited to perform carotid artery (N = 10) and ophthalmic (N = 9) ultrasound examinations using virtual guidance as their only training tool. In the carotid group, each untrained operator acquired two-dimensional, pulsed and color Doppler of the carotid artery. In the ophthalmic group, operators acquired representative images of the anterior chamber of the eye, retina, optic nerve, and nerve sheath. Ultrasound image quality was evaluated by independent imaging experts. Results: Of the studies, 8 of the 10 carotid and 17 of 18 of the ophthalmic images (2 images collected per study) were judged to be diagnostically adequate. The quality of all but one of the ophthalmic images ranged from adequate to excellent. Discussion: Diagnostically-adequate carotid and ophthalmic ultrasound examinations can be obtained by previously untrained operators with assistance from only an audio/video tutorial viewed in real time while scanning. This form of just-in-time training, which can be applied to other examinations, represents an opportunity to acquire important information for NASA flight surgeons and researchers when trained medical
C1 [Martin, David S.; Caine, Timothy L.; Lee, Stuart M. C.; Stenger, Michael B.; Sargsyan, Ashot E.] Wyle Sci, Technol & Engn Grp, Houston, TX USA.
[Platts, Steven H.] NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA.
RP Martin, DS (reprint author), Wyle Integrated Sci & Engn, 1290 Hercules Blvd, Houston, TX USA.
EM david.s.martin@nasa.gov
FU NASA Innovative Charge Account
FX The authors thank the subjects for their participation in this study and
the support of the Johnson Space Center's Cardiovascular Laboratory
personnel. This study was funded by the NASA Innovative Charge Account.
NR 13
TC 4
Z9 4
U1 0
U2 9
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD OCT
PY 2012
VL 83
IS 10
BP 995
EP 1000
DI 10.3357/ASEM.3279.2012
PG 6
WC Public, Environmental & Occupational Health; Medicine, General &
Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
Medicine; Sport Sciences
GA 013TO
UT WOS:000309329000011
PM 23066623
ER
PT J
AU Minchew, B
Jones, CE
Holt, B
AF Minchew, Brent
Jones, Cathleen E.
Holt, Benjamin
TI Polarimetric Analysis of Backscatter From the Deepwater Horizon Oil
Spill Using L-Band Synthetic Aperture Radar
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Oil spill; radar polarimetry; synthetic aperture radar
ID TARGET DECOMPOSITION-THEOREMS; WIND-GENERATED WAVES; SURFACE-FILMS;
OCEAN SURFACE; SAR IMAGES; SEA CLUTTER; CRUDE OILS; SCATTERING; SLICKS;
CLASSIFICATION
AB We analyze the fully-polarimetric Uninhabited Aerial Vehicle Synthetic Aperture Radar (UAVSAR) data acquired on June 23, 2010, from two adjacent, overlapping flight tracks that imaged the main oil slick near the Deepwater Horizon (DWH) rig site in the Gulf of Mexico. Our results show that radar backscatter from both clean water and oil in the slick is predominantly from a single surface scatterer, consistent with the tilted Bragg scattering mechanism, across the range of incidence angles from 26 degrees to 60 degrees. We show that the change of backscatter over the main slick is due both to a damping of the ocean wave spectral components by the oil and an effective reduction of the dielectric constant resulting from a mixture of 65-90% oil with water in the surface layer. This shows that synthetic aperture radar can be used to measure the oil volumetric concentration in a thick slick. Using the H/A/alpha parameters, we show that surface scattering is dominant for oil and water whenever the data are above the noise floor and that the entropy (H) and a parameters for the DWH slick are comparable to those from the clean water. The anisotropy, A, parameter shows substantial variation across the oil slick and a significant range-dependent signal whenever the backscatter in all channels is above the instrument noise floor. For slick detection, we find the most reliable indicator to be the major eigenvalue of the coherency matrix, which is approximately equal to the total backscatter power for both oil in the slick and clean sea water.
C1 [Minchew, Brent] CALTECH, Seismol Lab, Pasadena, CA 91125 USA.
[Jones, Cathleen E.; Holt, Benjamin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Minchew, B (reprint author), CALTECH, Seismol Lab, Pasadena, CA 91125 USA.
EM bminchew@caltech.edu; cathleen.e.jones@jpl.nasa.gov;
benjamin.m.holt@jpl.nasa.gov
FU National Aeronautics and Space Administration; DESDynl Pre-mission Task
FX The research described in this paper was carried out at the Jet
Propulsion Laboratory (JPL), California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. The
UAVSAR data are processed by the UAVSAR team at JPL and archived for
open distribution at the Alaska Satellite Facility. The authors would
like to acknowledge C. Dobson, NASA Headquarters, for endorsing the
UAVSAR flights; and S. Hensley, JPL, I. Leifer, University of Santa
Barbara, and I. MacDonald and O. Garcia-Pineda, Florida State
University, for valuable discussions. Thanks are also extended to B.
Hawkins, Y. Zheng, and B. Chapman, JPL. The third author would also like
to acknowledge the DESDynl Pre-mission Task for support. This paper is
Caltech Seismo Lab contribution 10055.
NR 55
TC 49
Z9 51
U1 3
U2 36
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD OCT
PY 2012
VL 50
IS 10
BP 3812
EP 3830
DI 10.1109/TGRS.2012.2185804
PN 1
PG 19
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 014FV
UT WOS:000309361500016
ER
PT J
AU Gu, GJ
Adler, RF
AF Gu, Guojun
Adler, Robert F.
TI Large-scale, inter-annual relations among surface temperature, water
vapour and precipitation with and without ENSO and volcano forcings
SO INTERNATIONAL JOURNAL OF CLIMATOLOGY
LA English
DT Article
DE precipitation variability; water vapour variability; surface temperature
variations
ID EL-NINO; ATMOSPHERIC CIRCULATION; TROPICAL CONVECTION; HYDROLOGICAL
CYCLE; CLIMATE; VARIABILITY; FEEDBACK; SENSITIVITY; EVOLUTION; TOGA
AB How the global hydrological cycle, generally denoted by precipitation, responds to surface temperature change has been debated for decades. This debate is crucial to correctly assess the global warming-related climate variability/change in the water cycle, but reflects our limited understanding of the relationships that exist among key components of the water cycle on various spatial and temporal scales. Primarily using satellite-based measurements, we find that correlations between precipitation and surface temperature anomalies averaged over large domains (i.e. tropical and global ocean/land areas) during 19882008 are very weak once the effects from two large-scale forcings, ENSO and volcanic eruptions, are removed, whereas tropospheric water vapour content varies with surface temperature no matter whether the ENSO and volcanic effects are included or not. We thus conclude that precipitation variability on the inter-annual time scale, once the net large-scale dynamic effects particularly associated with ENSO become weak or limited, does not follow surface temperature and related water vapour variations, even though inter-decadal signals may still exist. This is consistent with the fact that ENSO precipitation signals are usually weak over combined land plus ocean areas for both tropical and global regimes, though ENSO can greatly modulate global precipitation patterns through shifting large-scale circulation systems. These findings are also similar to the weak global-mean precipitation responses under the recent global warming that have been evident in both observations and models, compared to large associated tropospheric water vapour changes, roughly following the Clausius-Clapeyron (CC) relation. Copyright (c) 2011 Royal Meteorological Society
C1 [Gu, Guojun; Adler, Robert F.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Gu, Guojun; Adler, Robert F.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Gu, GJ (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613-1, Greenbelt, MD 20771 USA.
EM Guojun.Gu-1@nasa.gov
FU NASA Energy and Water-cycle Study (NEWS) program
FX The global surface temperature anomaly data and the tropical mean
stratospheric aerosol optical thickness were provided by the NASA-GISS
from its Web Site at http://data.giss.nasa.gov. The RSS-SSM/I columnar
water vapour data were downloaded from http://www.remss.com. This
research is supported under the NASA Energy and Water-cycle Study (NEWS)
program.
NR 37
TC 3
Z9 3
U1 3
U2 21
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0899-8418
EI 1097-0088
J9 INT J CLIMATOL
JI Int. J. Climatol.
PD OCT
PY 2012
VL 32
IS 12
BP 1782
EP 1791
DI 10.1002/joc.2393
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 015OB
UT WOS:000309454700002
ER
PT J
AU Sibeck, DG
Omidi, N
AF Sibeck, D. G.
Omidi, N.
TI Flux transfer events: Motion and signatures
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Flux transfer events; Magnetopause; Reconnection
ID DAYSIDE RECONNECTION; MAGNETIC-FIELD; MAGNETOPAUSE; FLOW; MAGNETOSPHERE;
LOCATION; INTERVAL; PLASMA; IMF
AB We present results from a 2.5 dimensional hybrid code simulation for the evolution of flux transfer events (FTEs) during intervals of due southward interplanetary magnetic field (IMF) orientation. The structures invariably form between pairs of reconnection lines, often remaining nearly stationary on the subsolar magnetopause before their motion begins. Although a few structures move sunward, ultimately coalescing with others, most eventually accelerate antisunward, reaching velocities many times greater than the sound speed in the magnetosheath but only about one Alfven speed greater than the ambient magnetosheath flow. At these velocities, slow mode wakes (but not shocks) marked by density enhancements and magnetic field strength decreases extend outward from the structures into the magnetosheath. Upon encountering the cusps, the structures decelerate, undergo reconnection, and are destroyed. Published by Elsevier Ltd.
C1 [Sibeck, D. G.] NASA GSFC, Greenbelt, MD 20723 USA.
[Omidi, N.] Solana Sci, Solana Beach, CA 92075 USA.
RP Sibeck, DG (reprint author), NASA GSFC, Code 674,Greenbelt Rd, Greenbelt, MD 20723 USA.
EM david.g.sibeck@nasa.gov; omidi@roadrunner.com
FU NASA's Heliophysics Guest Investigator Program; NSF [ATM-0502992,
AGS-1007449]
FX Research at GSFC was funding by NASA's Heliophysics Guest Investigator
Program. Research at Solana Scientific was funded by NSF grants
ATM-0502992 and AGS-1007449.
NR 27
TC 1
Z9 1
U1 1
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD OCT
PY 2012
VL 87-88
SI SI
BP 20
EP 24
DI 10.1016/j.jastp.2011.07.010
PG 5
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 017EN
UT WOS:000309573000004
ER
PT J
AU Jiang, XA
Zhao, M
Waliser, DE
AF Jiang, Xianan
Zhao, Ming
Waliser, Duane E.
TI Modulation of Tropical Cyclones over the Eastern Pacific by the
Intraseasonal Variability Simulated in an AGCM
SO JOURNAL OF CLIMATE
LA English
DT Article
ID MADDEN-JULIAN OSCILLATION; NORTH-AMERICAN-MONSOON; GULF-OF-MEXICO;
BOREAL SUMMER; SOUTHERN-HEMISPHERE; HURRICANE ACTIVITY; MIDSUMMER
DROUGHT; WESTERN PACIFIC; FORECAST SYSTEM; PRINCIPAL MODES
AB This study illustrates that observed modulations of tropical cyclone (TC) genesis over the eastern Pacific (EPAC) by large-scale intraseasonal variability (ISV) are well represented in a recently developed high-resolution atmospheric model (HiRAM) at the NOAA/Geophysical Fluid Dynamics Laboratory (GFDL) with a horizontal resolution of about 50 km. Considering the intrinsic predictability of the ISV of 2-4 weeks, this analysis thus has significant implications for dynamically based TC predictions on intraseasonal time scales. Analysis indicates that the genesis potential index (GPI) anomalies associated with the ISV can generally well depict ISV modulations of EPAC TC genesis in both observations and HiRAM simulations. Further investigation is conducted to explore the key factors associated with ISV modulation of TC activity based on an analysis of budget terms of the observed GPI during the ISV life cycle. It is found that, while relative roles of GPI factors are dependent on ISV phase and location, lower-level cyclonic vorticity, enhanced midlevel relative humidity, and reduced vertical wind shear can all contribute to the observed active TC genesis over the EPAC during particular ISV phases. In general, the observed anomalous ISV patterns of these large-scale GPI factors are well represented in HiRAM. Model deficiencies are also noted particularly in the anomalous midlevel relative humidity patterns and amplitude of vertical wind shear associated with the EPAC ISV.
C1 [Jiang, Xianan; Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Jiang, Xianan] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Zhao, Ming] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
RP Jiang, XA (reprint author), CALTECH, Jet Prop Lab, MS 233-300,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM xianan@jifresse.ucla.edu
RI Jiang, Xianan/A-2283-2012; Zhao, Ming/C-6928-2014
FU NOAAMAPP Program [NA09OAR4310191, NA11OAR4310086]; NSF Climate and
Large-Scale Dynamics Program [ATM-0934285]; U.S. Office of Naval
Research through UCSD [N00014-10-1-0541]; NOAA CTB Program through the
University of Hawaii at Manoa; National Aeronautics and Space
Administration
FX XJ acknowledges support by the NOAAMAPP Program under Awards
NA09OAR4310191 and NA11OAR4310086, and NSF Climate and Large-Scale
Dynamics Program under Award ATM-0934285. DW acknowledges support by the
U.S. Office of Naval Research under Grant N00014-10-1-0541 through UCSD,
and by the NOAA CTB Program through the University of Hawaii at Manoa.
We thank the editor, Dr. K. Walsh, and anonymous reviewers for their
constructive comments on an earlier version of this manuscript, and B.
Kahn and I.-S. Kang for insightful discussions. Thanks also to T. Kubar
for his comments and editorial assistance. The Fortran code for GPI
calculation was obtained from K. Emanuel's website. Part of this
research was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration.
NR 69
TC 24
Z9 24
U1 0
U2 9
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
J9 J CLIMATE
JI J. Clim.
PD OCT
PY 2012
VL 25
IS 19
BP 6524
EP 6538
DI 10.1175/JCLI-D-11-00531.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 018IO
UT WOS:000309653800005
ER
PT J
AU Aumann, HH
Ruzmaikin, A
Behrangi, A
AF Aumann, Hartmut H.
Ruzmaikin, Alexander
Behrangi, Ali
TI On the Surface Temperature Sensitivity of the Reflected Shortwave,
Outgoing Longwave, and Net Incident Radiation
SO JOURNAL OF CLIMATE
LA English
DT Article
ID FEEDBACK PROCESSES; CLIMATE FEEDBACKS; CLOUD FEEDBACK; AIRS/AMSU/HSB;
SYSTEMS; MODELS; EARTH; IRIS
AB The global-mean top-of-atmosphere incident solar radiation (ISR) minus the outgoing longwave radiation (OLR) and the reflected shortwave radiation (RSW) is the net incident radiation ( NET). This study analyzes the global-mean NET sensitivity to a change in the global-mean surface temperature by applying the interannual anomaly correlation technique to 9 yr of Atmospheric Infrared Sounder (AIRS) global measurements of RSW and OLR under cloudy and clear conditions. The study finds the observed sensitivity of NET that includes the effects of clouds to be -1.5 +/- 0.25 (1 sigma) W m(-2) K-1 and the clear NET sensitivity to be -2.0 +/- 0.2 (1 sigma) W m(-2) K-1, consistent with previous work using Earth Radiation Budget Experiment and Clouds and the Earth's Radiant Energy System data. The cloud effect, +0.5 +/- 0.2 (1 sigma) W m(-2) K-1, is a positive component of the NET sensitivity. The similarity of the NET sensitivities derived from forced and unforced models invites a comparison between the observed sensitivities and the effective sensitivities calculated for the Fourth Assessment Report models, although this requires some caution: The effective model sensitivities with clouds range from -0.88 to -1.64 W m(-2) K-1, the clear NET sensitivity in the models ranges from -2.32 to -1.73 W m(-2) K-1, and the cloud forcing sensitivities range from +0.14 to +1.18 W m(-2) K-1. The effective NET and clear NET sensitivities derived from the models are statistically consistent with those derived from the AIRS data, considering the observational and model derivation uncertainties.
C1 [Aumann, Hartmut H.; Ruzmaikin, Alexander; Behrangi, Ali] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Aumann, HH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM hhaumann@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The research described in this paper was carried out at the Jet
Propulsion Laboratory at the California Institute of Technology under a
contract with the National Aeronautics and Space Administration. We are
grateful for the long-term support of Dr. Ramesh Kakar, Aqua Program
Scientist at NASA HQ. We acknowledge the discussions with Dr. Joao
Teixeira at JPL and the helpful comments by two anonymous reviewers.
NR 33
TC 1
Z9 2
U1 1
U2 16
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD OCT
PY 2012
VL 25
IS 19
BP 6585
EP 6593
DI 10.1175/JCLI-D-11-00607.1
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 018IO
UT WOS:000309653800009
ER
PT J
AU Masud, MM
Woolam, C
Gao, J
Khan, L
Han, JW
Hamlen, KW
Oza, NC
AF Masud, Mohammad M.
Woolam, Clay
Gao, Jing
Khan, Latifur
Han, Jiawei
Hamlen, Kevin W.
Oza, Nikunj C.
TI Facing the reality of data stream classification: coping with scarcity
of labeled data
SO KNOWLEDGE AND INFORMATION SYSTEMS
LA English
DT Article
DE Data stream classification; Semi-supervised clustering; Ensemble
classification; Concept drift
ID EVOLVING DATA STREAMS; CLASSIFIERS
AB Recent approaches for classifying data streams are mostly based on supervised learning algorithms, which can only be trained with labeled data. Manual labeling of data is both costly and time consuming. Therefore, in a real streaming environment where large volumes of data appear at a high speed, only a small fraction of the data can be labeled. Thus, only a limited number of instances will be available for training and updating the classification models, leading to poorly trained classifiers. We apply a novel technique to overcome this problem by utilizing both unlabeled and labeled instances to train and update the classification model. Each classification model is built as a collection of micro-clusters using semi-supervised clustering, and an ensemble of these models is used to classify unlabeled data. Empirical evaluation of both synthetic and real data reveals that our approach outperforms state-of-the-art stream classification algorithms that use ten times more labeled data than our approach.
C1 [Masud, Mohammad M.; Woolam, Clay; Khan, Latifur; Hamlen, Kevin W.] Univ Texas Dallas, Dept Comp Sci, Richardson, TX 75080 USA.
[Gao, Jing; Han, Jiawei] Univ Illinois, Dept Comp Sci, Urbana, IL 61801 USA.
[Oza, Nikunj C.] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
RP Masud, MM (reprint author), Univ Texas Dallas, Dept Comp Sci, Richardson, TX 75080 USA.
EM mehedy@utdallas.edu
OI Masud, Mohammad/0000-0002-5274-5982
FU NASA [NNX08AC35A]; Air Force of Scientific Research (AFOSR)
[FA9550-08-1-0260]
FX This material is based upon work supported by NASA under Award No.
NNX08AC35A and the Air Force of Scientific Research (AFOSR) under Award
No. FA9550-08-1-0260.
NR 45
TC 22
Z9 22
U1 2
U2 11
PU SPRINGER LONDON LTD
PI LONDON
PA 236 GRAYS INN RD, 6TH FLOOR, LONDON WC1X 8HL, ENGLAND
SN 0219-1377
EI 0219-3116
J9 KNOWL INF SYST
JI Knowl. Inf. Syst.
PD OCT
PY 2012
VL 33
IS 1
BP 213
EP 244
DI 10.1007/s10115-011-0447-8
PG 32
WC Computer Science, Artificial Intelligence; Computer Science, Information
Systems
SC Computer Science
GA 017KC
UT WOS:000309587800009
ER
PT J
AU Page, MJ
Brindle, C
Talavera, A
Still, M
Rosen, SR
Yershov, VN
Ziaeepour, H
Mason, KO
Cropper, MS
Breeveld, AA
Loiseau, N
Mignani, R
Smith, A
Murdin, P
AF Page, M. J.
Brindle, C.
Talavera, A.
Still, M.
Rosen, S. R.
Yershov, V. N.
Ziaeepour, H.
Mason, K. O.
Cropper, M. S.
Breeveld, A. A.
Loiseau, N.
Mignani, R.
Smith, A.
Murdin, P.
TI The XMM-Newton serendipitous ultraviolet source survey catalogue
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE catalogues; astrometry; stars: general; galaxies: photometry;
ultraviolet: general
ID PHOTOMETRIC STANDARD STARS; PHOTON-COUNTING DETECTORS; IN-FLIGHT
PERFORMANCE; ON-ORBIT PERFORMANCE; DIGITAL SKY SURVEY; TD-1A SATELLITE;
IMAGING CAMERA; MILKY-WAY; TELESCOPE; SPECTRA
AB The XMMNewton Serendipitous Ultraviolet Source Survey (XMM-SUSS) is a catalogue of ultraviolet (UV) sources detected serendipitously by the Optical Monitor (XMM-OM) on board the XMMNewton observatory. The catalogue contains UV-detected sources collected from 2417 XMM-OM observations in one to six broad-band UV and optical filters, made between 2000 February 24 and 2007 March 29. The primary contents of the catalogue are source positions, magnitudes and fluxes in one to six passbands, and these are accompanied by profile diagnostics and variability statistics. XMM-SUSS is populated by 753?578 UV source detections above a 3s signal-to-noise ratio threshold limit which relate to 624?049 unique objects. Taking account of substantial overlaps between observations, the net sky area covered is 2954?deg2, depending on UV filter. The magnitude distributions peak at mAB = 20.2, 20.9 and 21.2 in UVW2 (?eff = 2120 angstrom), UVM2 (?eff = 2310 angstrom) and UVW1 (?eff = 2910 angstrom), respectively. More than 10 per cent of the sources have been visited more than once using the same filter during XMMNewton operation, and >20 per cent of sources are observed more than once per filter during an individual visit. Consequently, the scope for science based on temporal source variability on time-scales of hours to years is broad. By comparison with other astrophysical catalogues we test the accuracy of the source measurements and define the nature of the serendipitous UV XMM-OM source sample. The distributions of source colours in the UV and optical filters are shown together with the expected loci of stars and galaxies, and indicate that sources which are detected in multiple UV bands are predominantly star-forming galaxies and stars of type G or earlier.
C1 [Page, M. J.; Brindle, C.; Still, M.; Rosen, S. R.; Yershov, V. N.; Ziaeepour, H.; Mason, K. O.; Cropper, M. S.; Breeveld, A. A.; Mignani, R.; Smith, A.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Talavera, A.; Loiseau, N.] ESA, XMM Newton Sci Operat Ctr, Villafranca Del Castillo 28691, Villanueva De L, Spain.
[Still, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rosen, S. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Ziaeepour, H.] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany.
[Mason, K. O.] Sci & Technol Facil Council, Swindon SN2 1SZ, Wilts, England.
[Mignani, R.] Univ Zielona Gora, Kepler Inst Astron, PL-65265 Zielona Gora, Poland.
[Murdin, P.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
RP Page, MJ (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
EM mjp@mssl.ucl.ac.uk
FU National Aeronautics and Space Administration; National Science
Foundation
FX This research has made use of the following archives: the USNOFS Image
and Catalogue Archive operated by the United States Naval Observatory,
Flagstaff Station; the Two Micron All Sky Survey, which is a joint
project of the University of Massachusetts and the Infrared Processing
and Analysis Center/California Institute of Technology, funded by the
National Aeronautics and Space Administration and the National Science
Foundation. We thank Tom Dwelly for supplying the Subaru B-band image
and source list for the 13h deep field.
NR 59
TC 11
Z9 11
U1 0
U2 4
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2012
VL 426
IS 2
BP 903
EP 926
DI 10.1111/j.1365-2966.2012.21706.x
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 015OQ
UT WOS:000309456200008
ER
PT J
AU Zdziarski, AA
Maitra, C
Frankowski, A
Skinner, GK
Misra, R
AF Zdziarski, Andrzej A.
Maitra, Chandreyee
Frankowski, Adam
Skinner, Gerald K.
Misra, Ranjeev
TI Energy-dependent orbital modulation of X-rays and constraints on
emission of the jet in Cyg X-3
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiation mechanisms: non-thermal; binaries: general; stars: individual:
Cyg X-3; stars: winds; outflows; gamma rays: stars; X-rays: binaries
ID SCATTERING HALO; TIMING EXPLORER; RADIO-EMISSION; LIGHT-CURVE;
CYGNUS-X-3; PERIOD; VARIABILITY; MISSION; EPHEMERIS; DISTANCE
AB We study the orbital modulation of X-rays from Cyg X-3, using data from Swift, INTEGRAL and RXTE. Using the wealth of data presently available and an improved averaging method, we obtain energy-dependent folded and averaged light curves with unprecedented accuracy. We find that above similar to 5?keV the modulation depth decreases with increasing energy, which is consistent with the modulation being caused by both boundfree absorption and Compton scattering in the stellar wind of the donor, with minima corresponding to the highest optical depth, which occurs around the superior conjunction. We find a decrease of the depth below similar to 3?keV, which appears to be due to re-emission of the absorbed continuum by the wind in soft X-ray lines. Based on the shape of the folded light curves, any X-ray contribution from the jet in Cyg X-3, which emits ?-rays detected at energies >0.1?GeV in the soft spectral states, is found to be minor up to similar to 100?keV. This implies the presence of a rather sharp low-energy break in the jet MeV-range spectrum. We also calculate phase-resolved RXTE X-ray spectra and show that the difference between the spectra corresponding to phases around superior and inferior conjunctions can indeed be accounted for by the combined effect of boundfree absorption in an ionized medium and Compton scattering.
C1 [Zdziarski, Andrzej A.; Frankowski, Adam] Ctr Astron M Kopernika, PL-00716 Warsaw, Poland.
[Maitra, Chandreyee] Raman Res Inst, Bangalore 560080, Karnataka, India.
[Maitra, Chandreyee] Indian Inst Sci, Joint Astron Programme, Bangalore 560012, Karnataka, India.
[Frankowski, Adam] Univ Geneva, ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland.
[Skinner, Gerald K.] CRESST, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Skinner, Gerald K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Skinner, Gerald K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Misra, Ranjeev] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
RP Zdziarski, AA (reprint author), Ctr Astron M Kopernika, Bartycka 18, PL-00716 Warsaw, Poland.
EM aaz@camk.edu.pl
RI M, Manjunath/N-4000-2014
OI M, Manjunath/0000-0001-8710-0730
FU Polish NCN [N N203 581240, 362/1/N-INTEGRAL/2008/09/0]
FX This research has been supported in part by the Polish NCN grants N N203
581240 and 362/1/N-INTEGRAL/2008/09/0. We thank P. Lubinski for help
with the analysis of the BAT data, S. Kitamoto for providing us with his
updated ephemeris and G. Dubus, the referee, for valuable suggestions
and comments. We acknowledge the use of quick-look results provided by
the RXTE ASM team and of data obtained through the HEASARC online
service provided by NASA/GSFC.
NR 58
TC 10
Z9 10
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 OCT
PY 2012
VL 426
IS 2
BP 1031
EP 1042
DI 10.1111/j.1365-2966.2012.21635.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 015OQ
UT WOS:000309456200018
ER
PT J
AU Hillier, DJ
Bouret, JC
Lanz, T
Busche, JR
AF Hillier, D. John
Bouret, Jean-Claude
Lanz, Thierry
Busche, Joseph R.
TI The influence of rotation on optical emission profiles of O stars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE line: formation; line: profiles; radiative transfer; stars: atmospheres;
stars: early-type; stars: individual: ? Puppis
ID LINE FORMATION; MASS-LOSS; H-ALPHA; WINDS; CLASSIFICATION
AB We study the formation of photospheric emission lines in O stars and show that the rectangular profiles, sometimes double peaked, that are observed for some stars are a direct consequence of rotation, and it is unnecessary to invoke an enhanced density structure in the equatorial regions. Emission lines, such as N?iv ?4058 and the N?iii ??463446404642 multiplet, exhibit non-standard limb-darkening laws. The lines can be in absorption for rays striking the centre of the star and in emission for rays near the limb. Weak features in the flux spectrum do not necessarily indicate an intrinsically weak feature instead the feature can be weak because of cancellation between absorption in core rays and emission from rays near the limb. Rotation also modifies line profiles of wind diagnostics such as He?ii ?4686 and Ha and should not be neglected when inferring the actual stratification, level and nature of wind structures.
C1 [Hillier, D. John] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Hillier, D. John] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr P, Pittsburgh, PA 15260 USA.
[Bouret, Jean-Claude] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France.
[Bouret, Jean-Claude] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lanz, Thierry] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab JL Lagrange, F-06304 Nice 4, France.
[Busche, Joseph R.] Wheeling Jesuit Univ, Wheeling, WV 26003 USA.
RP Hillier, DJ (reprint author), Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
EM hillier@pitt.edu
FU NASA ADP Grant [NNG04GC81G]; NASA STScI theory grant [HST-AR-11756.01.A,
HST-AR-12640.01]; NASA [NAS5-26555]; French Agence Nationale de la
Recherche (ANR)
FX DJH acknowledges support from NASA ADP Grant: NNG04GC81G, STScI theory
grant HST-AR-11756.01.A and HST-AR-12640.01. STScI is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS5-26555. JCB thanks the French Agence Nationale de la
Recherche (ANR) for financial support. The authors thank the referee,
Joachim Puls, for his suggestions and his careful reading of the paper.
The authors would also like to thank Francisco Najarro for comments on a
draft of the paper.
NR 22
TC 10
Z9 10
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2012
VL 426
IS 2
BP 1043
EP 1049
DI 10.1111/j.1365-2966.2012.21646.x
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 015OQ
UT WOS:000309456200019
ER
PT J
AU Du, AM
Tsurutani, BT
Sun, W
AF Du, A. M.
Tsurutani, B. T.
Sun, W.
TI Comments on "Interplanetary and geomagnetic parameters during January
16-26, 2005" by RP Kane
SO PLANETARY AND SPACE SCIENCE
LA English
DT Editorial Material
DE Geomagnetic storms; Northward interplanetary magnetic field; Solar wind
ID MAGNETIC STORMS; SOLAR; MAGNETOSPHERE; DST
AB We write this note of clarification to show that Kane (2012) has incorrectly interpreted the interplanetary magnetic field during the event by using low time-resolution data, and has thus misinterpreted the concluding comments of Du et al. (2008). Our recent paper (Du et al., 2011b) has shown that the solar wind energy input during northward IMF events is very low. Thus the interpretation of the Du et al. (2008) article given by the authors stand as was stated. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Du, A. M.] Chinese Acad Sci, Inst Geol & Geophys, Beijing 100029, Peoples R China.
[Tsurutani, B. T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Sun, W.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA.
RP Du, AM (reprint author), Chinese Acad Sci, Inst Geol & Geophys, Beijing 100029, Peoples R China.
EM amdu@mail.iggcas.ac.cn
NR 16
TC 1
Z9 1
U1 0
U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD OCT
PY 2012
VL 71
IS 1
BP 55
EP 56
DI 10.1016/j.pss.2012.07.002
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 017WF
UT WOS:000309621200006
ER
PT J
AU McKay, CP
Khare, BN
Amin, R
Klasson, M
Kral, TA
AF McKay, C. P.
Khare, B. N.
Amin, R.
Klasson, M.
Kral, T. A.
TI Possible sources for methane and C-2-C-5 organics in the plume of
Enceladus
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Enceladus; Plume; Organics; Methane; Acetylene
ID OUTER SOLAR-SYSTEM; EARLY EARTH; HYDROTHERMAL CONDITIONS; PREBIOTIC
CHEMISTRY; ORIGIN; TITAN; LIFE; HYDROCARBONS; EVOLUTION; SURFACE
AB We consider six possible sources of CH4 and other lowmass (C-2-C-5) organics in the plume of Enceladus: three of these sources represent initial endowments of organics: cometary organics, Titan-like tholin, and the Fisher-Tropsch type reactions in the gases from which Enceladus formed. The other three sources represent processes inside Enceladus: water-rock reactions, microbiology, and thermogenesis. We report on new laboratory results for C-2 hydrocarbons released by thermogenesis of laboratory tholin and the Fisher-Tropsch type synthesis. Thermal processing of Titan-like tholin produced ratios of CH4/C2H4 and CH4/C2H6 of about two for temperatures up to 450 degrees C and about six for a temperature of 650 degrees C. The low pressure (similar to 1 atm) Fisher-Tropsch type experiments produced CH4/C2H4 of similar to 1.5, similar to previous results. C2H2 was not produced by either process. Tests of gas production by four strains of methanogens confirmed the absence of any detectable production of non-methane hydrocarbons. Cometary endowment, the Fisher-Tropsch type synthesis, and Titan-like tholin incorporation could be primary inputs of organics and subsequent thermal processing of any of these all are possible sources of low mass organics in the plume. Biological production and water-rock reactions are an alternative source of CH4. Aqueous reactions with CO and H-2 can produce C-2-C-5 organics even at the low pressures of the interior of Enceladus. If there is a confirmed detection of CO and C2H2 in the plume of Enceladus, this provides an important constraint on sources, as we have identified no process, other than the initial volatile component of cometary organics, which can supply these gases. Precise determination of the relative concentrations of C-1-C-5 hydrocarbons may provide additional constraints on sources, but a detailed isotopic analysis of C and H in these organics and a search for amino acids constitute the next important steps in resolving the sources of the organics in Enceladus' plume. Published by Elsevier Ltd.
C1 [McKay, C. P.; Khare, B. N.; Amin, R.; Klasson, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Amin, R.; Klasson, M.] Lulea Univ Technol, S-95187 Lulea, Sweden.
[Kral, T. A.] Univ Arkansas, Dept Biol Sci, Fayetteville, AR 72701 USA.
RP McKay, CP (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM chris.mckay@nasa.gov
FU Cassini Data Analysis Program grant
FX We thank Hunter Waite and Carolyn Porco for insightful and motivating
discussions. We thank Tomoko Ishihara for assistance in the laboratory.
Funding for this work was provided by a Cassini Data Analysis Program
grant to B.N.K. We appreciate the constructive comments of two
reviewers.
NR 53
TC 3
Z9 5
U1 3
U2 69
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD OCT
PY 2012
VL 71
IS 1
BP 73
EP 79
DI 10.1016/j.pss.2012.07.011
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 017WF
UT WOS:000309621200009
ER
PT J
AU Barger, LK
Sullivan, JP
Vincent, AS
Fiedler, ER
McKenna, LM
Flynn-Evans, EE
Gilliland, K
Sipes, WE
Smith, PH
Brainard, GC
Lockley, SW
AF Barger, Laura K.
Sullivan, Jason P.
Vincent, Andrea S.
Fiedler, Edna R.
McKenna, Laurence M.
Flynn-Evans, Erin E.
Gilliland, Kirby
Sipes, Walter E.
Smith, Peter H.
Brainard, George C.
Lockley, Steven W.
TI Learning to Live on a Mars Day: Fatigue Countermeasures during the
Phoenix Mars Lander Mission
SO SLEEP
LA English
DT Article
DE Shift work; performance; sleep; circadian; light
ID HUMAN CIRCADIAN PACEMAKER; PSYCHOMOTOR VIGILANCE TASK; SHORT-WAVELENGTH
LIGHT; NIGHT-SHIFT WORK; BRIGHT LIGHT; COGNITIVE PERFORMANCE; INTRINSIC
PERIOD; DOSE-RESPONSE; NEUROBEHAVIORAL PERFORMANCE; SUBJECTIVE ALERTNESS
AB Study Objectives: To interact with the robotic Phoenix Mars Lander (PML) spacecraft, mission personnel were required to work on a Mars day (24.65 h) for 78 days. This alien schedule presents a challenge to Earth-bound circadian physiology and a potential risk to workplace performance and safety. We evaluated the acceptability, feasibility, and effectiveness of a fatigue management program to facilitate synchronization with the Mars day and alleviate circadian misalignment, sleep loss, and fatigue.
Design: Operational field study.
Setting: PML Science Operations Center.
Participants: Scientific and technical personnel supporting PML mission.
Interventions: Sleep and fatigue education was offered to all support personnel. A subset (n = 19) were offered a short-wavelength (blue) light panel to aid alertness and mitigate/reduce circadian desynchrony. They were assessed using a daily sleep/work diary, continuous wrist actigraphy, and regular performance tests. Subjects also completed 48-h urine collections biweekly for assessment of the circadian 6-sulphatoxymelatonin rhythm.
Measurements and Results: Most participants (87%) exhibited a circadian period consistent with adaptation to a Mars day. When synchronized, main sleep duration was 5.98 +/- 0.94 h, but fell to 4.91 +/- 1.22 h when misaligned (P < 0.001). Self-reported levels of fatigue and sleepiness also significantly increased when work was scheduled at an inappropriate circadian phase (P < 0.001). Prolonged wakefulness (>= 21 h) was associated with a decline in performance and alertness (P < 0.03 and P < 0.0001, respectively).
Conclusions: The ability of the participants to adapt successfully to the Mars day suggests that future missions should utilize a similar circadian rhythm and fatigue management program to reduce the risk of sleepiness-related errors that jeopardize personnel safety and health during critical missions.
C1 [Barger, Laura K.; Sullivan, Jason P.; McKenna, Laurence M.; Flynn-Evans, Erin E.; Lockley, Steven W.] Brigham & Womens Hosp, Div Sleep Med, Dept Med, Boston, MA 02115 USA.
[Barger, Laura K.; Flynn-Evans, Erin E.; Lockley, Steven W.] Harvard Univ, Sch Med, Div Sleep Med, Boston, MA USA.
[Vincent, Andrea S.; Gilliland, Kirby] Univ Oklahoma, Cognit Sci Res Ctr, Norman, OK 73019 USA.
[Fiedler, Edna R.] Baylor Coll Med, Menninger Dept Psychiat & Behav Sci, Houston, TX 77030 USA.
[Sipes, Walter E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Smith, Peter H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Brainard, George C.] Thomas Jefferson Univ, Jefferson Med Coll, Dept Neurol, Philadelphia, PA 19107 USA.
RP Barger, LK (reprint author), Brigham & Womens Hosp, Div Sleep Med, Dept Med, 221 Longwood Ave,BLI 438, Boston, MA 02115 USA.
EM lkbarger@hms.harvard.edu
FU National Aeronautics and Space Administration [NNX08AD66A]; National
Space Biomedical Research Institute through NASA [NCC 9-58]; NASA
[NNH04CC16C]
FX The study presented here was primarily supported by a grant from the
National Aeronautics and Space Administration (NNX08AD66A). During the
performance of the study, Drs. Barger, Brainard, and Lockley were
supported in part by the National Space Biomedical Research Institute
through NASA NCC 9-58. The Phoenix Mars Lander mission was supported by
NASA contract NNH04CC16C.
NR 93
TC 11
Z9 11
U1 1
U2 14
PU AMER ACAD SLEEP MEDICINE
PI WESTCHESTER
PA ONE WESTBROOK CORPORATE CTR, STE 920, WESTCHESTER, IL 60154 USA
SN 0161-8105
EI 1550-9109
J9 SLEEP
JI Sleep
PD OCT 1
PY 2012
VL 35
IS 10
BP 1423
EP 1435
DI 10.5665/sleep.2128
PG 13
WC Clinical Neurology; Neurosciences
SC Neurosciences & Neurology
GA 016KJ
UT WOS:000309516600018
PM 23024441
ER
PT J
AU Venter, G
Scotti, SJ
AF Venter, Gerhard
Scotti, Stephen J.
TI Accounting for Proof Test Data in a Reliability-Based Design
Optimization Framework
SO AIAA JOURNAL
LA English
DT Article
ID APPROXIMATION; INTEGRALS
AB This paper investigates the use of proof (or acceptance) test data during the reliability-based design optimization of structural components. It is assumed that every component will be proof tested and that the component will only enter into service if it passes the proof test. The goal is to reduce the component weight while maintaining high reliability by exploiting the proof test results during the design process. The proposed procedure results in the simultaneous design of the structural component as well as the proof test itself, and it provides the designer with direct control over the probability of failing the proof test. The procedure is illustrated using two analytical example problems, and the results indicate that significant weight savings are possible when exploiting the proof test results during the design process.
C1 [Venter, Gerhard] Univ Stellenbosch, Dept Mech & Mechatron Engn, ZA-7602 Stellenbosch, South Africa.
[Scotti, Stephen J.] NASA, Langley Res Ctr, Res Directorate, Hampton, VA 23681 USA.
RP Venter, G (reprint author), Univ Stellenbosch, Dept Mech & Mechatron Engn, ZA-7602 Stellenbosch, South Africa.
EM gventer@sun.ac.za; Stephen.J.Scotti@nasa.gov
OI Venter, Gerhard/0000-0001-9513-9774
NR 25
TC 3
Z9 3
U1 0
U2 0
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 OCT
PY 2012
VL 50
IS 10
BP 2159
EP 2167
DI 10.2514/I.J051495
PG 9
WC Engineering, Aerospace
SC Engineering
GA 013KY
UT WOS:000309305500012
ER
PT J
AU Reda, DC
Wilder, MC
Prabhu, DK
AF Reda, Daniel C.
Wilder, Michael C.
Prabhu, Dinesh K.
TI Transition Experiments on Slightly Blunted Cones with Distributed
Roughness in Hypersonic Flight
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT 41st AIAA Fluid Dynamics Conference and Exhibit
CY JUN 27-30, 2011
CL Honolulu, HI
SP AIAA
ID BOUNDARY-LAYER-TRANSITION; SLENDER CONES; RANGE; NOISE; NUMBERS; TUNNEL;
BODIES; SHARP
AB Slightly blunted cones with smooth tips and roughened frusta were flown in the NASA Ames Research Center hypersonic ballistic range through quiescent air environments at a Mach number of 10. Global surface-temperature distributions were optically measured and analyzed to determine the transition onset location on the roughened surface of each model. A series of tests was conducted over a range of freestream pressures, from which the progression of the transition front over the roughened surface was determined as a function of freestream pressure. Real-gas Navier-Stokes calculations of the laminar boundary layer were conducted at the measured flight Mach number and wall temperature at the transition onset location for each shot, and results used to predict key dimensionless parameters required to correlate transition on such configurations in hypersonic flow. For distributed roughness elements totally immersed within the laminar boundary layer, the critical-roughness-Reynolds-number correlating approach was found to well model transition onset and progression over the roughened conic frusta. The critical value of the roughness Reynolds number for transition was found to be 266 +/- 20%, in agreement with the critical value of 250 +/- 20% determined in earlier experiments for transition on rough blunt bodies in hypersonic free flight.
C1 [Reda, Daniel C.; Wilder, Michael C.] NASA, Ames Res Ctr, Aerothermodynam Branch, Moffett Field, CA 94035 USA.
[Prabhu, Dinesh K.] ERC Inc, Moffett Field, CA 94035 USA.
RP Reda, DC (reprint author), NASA, Ames Res Ctr, Aerothermodynam Branch, MS 230-2, Moffett Field, CA 94035 USA.
NR 34
TC 1
Z9 1
U1 2
U2 10
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
J9 AIAA J
JI AIAA J.
PD OCT
PY 2012
VL 50
IS 10
BP 2248
EP 2254
DI 10.2514/I.J051616
PG 7
WC Engineering, Aerospace
SC Engineering
GA 013KY
UT WOS:000309305500020
ER
PT J
AU Ham, YG
Rienecker, MM
AF Ham, Yoo-Geun
Rienecker, Michele M.
TI Flow-dependent empirical singular vector with an ensemble Kalman filter
data assimilation for El Nino prediction
SO CLIMATE DYNAMICS
LA English
DT Article
DE Singular vector; Seasonal prediction; Ensemble Kalman filter; El Nino;
ENSO
ID GENERAL-CIRCULATION MODEL; OCEAN RECHARGE PARADIGM; SEA-SURFACE
TEMPERATURE; COUPLED MODEL; BRED VECTORS; SOUTHERN OSCILLATION;
ATMOSPHERE MODEL; OPTIMAL-GROWTH; ERROR GROWTH; ANNUAL-CYCLE
AB In this study, a new approach for extracting flow-dependent empirical singular vectors (FESVs) for seasonal prediction using ensemble perturbations obtained from an ensemble Kalman filter (EnKF) assimilation is presented. Due to the short interval between analyses, EnKF perturbations primarily contain instabilities related to fast weather variability. To isolate slower, coupled instabilities that would be more suitable for seasonal prediction, an empirical linear operator for seasonal time-scales (i.e. several months) is formulated using a causality hypothesis; then, the most unstable mode from the linear operator is extracted for seasonal time-scales. It is shown that the flow-dependent operator represents nonlinear integration results better than a conventional empirical linear operator static in time. Through 20 years of retrospective seasonal predictions, it is shown that the skill of forecasting equatorial SST anomalies using the FESV is systematically improved over that using Conventional ESV (CESV). For example, the correlation skill of the NINO3 SST index using FESV is higher, by about 0.1, than that of CESV at 8-month leads. In addition, the forecast skill improvement is significant over the locations where the correlation skill of conventional methods is relatively low, indicating that the FESV is effective where the initial uncertainty is large.
C1 [Ham, Yoo-Geun; Rienecker, Michele M.] NASA, Global Modeling & Assimilat Off, GSFC Code 610 1, Greenbelt, MD USA.
[Ham, Yoo-Geun] Univ Space Res Assoc, Baltimore, MD USA.
RP Ham, YG (reprint author), NASA, Global Modeling & Assimilat Off, GSFC Code 610 1, Greenbelt, MD USA.
EM yoo-geun.ham@nasa.gov
FU NASA Modeling, Analysis and Prediction program under WBS
[802678.02.17.01.25]
FX We appreciate the helpful suggestions and comments from two anonymous
reviewers. This research was supported by the NASA Modeling, Analysis
and Prediction program under WBS 802678.02.17.01.25. Computational
resources for this study were provided by the NASA Center for Climate
Simulation.
NR 63
TC 1
Z9 1
U1 1
U2 5
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
J9 CLIM DYNAM
JI Clim. Dyn.
PD OCT
PY 2012
VL 39
IS 7-8
BP 1727
EP 1738
DI 10.1007/s00382-012-1302-7
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 013ZZ
UT WOS:000309346100012
ER
PT J
AU Verstraete, MM
Hunt, LA
Scholes, RJ
Clerici, M
Pinty, B
Nelson, DL
AF Verstraete, Michel M.
Hunt, Linda A.
Scholes, Robert J.
Clerici, Marco
Pinty, Bernard
Nelson, David L.
TI Generating 275-m Resolution Land Surface Products From the Multi-Angle
Imaging SpectroRadiometer Data
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Africa; Earth observing system; ecosystems; high-resolution imaging;
inverse problems; spectroradiometers; vegetation mapping
ID REMOTELY-SENSED IMAGES; SHARPENED MULTISPECTRAL IMAGERY; MULTIANGULAR
MEASUREMENTS; SPATIAL-RESOLUTION; URBAN AREAS; MISR; MODEL;
SUPERRESOLUTION; FUSION; CLASSIFICATION
AB This paper shows how to reconstruct the original 275-m resolution data of the Multi-angle Imaging SpectroRadiometer (MISR) instrument in the 24 spectrodirectional global mode channels that are spatially averaged to 1.1 km on-board the Terra platform, with negligible loss of information relative to images acquired in native-resolution local mode. Standard approaches to improve the spatial resolution of products rely on one (typically panchromatic) high-resolution (HR) image to sharpen multiple spectral images. In the case of the MISR-HR package described here, three of the 12 available HR channels are combined to regenerate each of the 24 reduced-resolution channel to its native resolution. The accurate and rigorously reconstructed spectral bidirectional reflectance data allow sensitive and physically meaningful land surface attributes to be recovered at a spatial resolution appropriate to document the spatial heterogeneity of the land surface and relevant for climate and environment studies. MISR has been in continuous operation since February 2000 and provides global coverage in at most nine days (depending on latitude). This technique allows the generation of quantitative information to monitor change and model ecosystem function virtually anywhere and at any time during the last decade. The potential is demonstrated for a savanna landscape in South Africa.
C1 [Verstraete, Michel M.; Clerici, Marco; Pinty, Bernard] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, VA, Italy.
[Verstraete, Michel M.] CSIR, NRE, ZA-0001 Pretoria, South Africa.
[Hunt, Linda A.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Pinty, Bernard] ESA ESRIN, I-00044 Frascati, Rm, Italy.
[Nelson, David L.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Verstraete, MM (reprint author), Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, VA, Italy.
EM Michel.Verstraete@jrc.ec.europa.eu
OI Verstraete, Michel/0000-0003-0968-8721; Scholes,
Robert/0000-0001-5537-6935
NR 46
TC 3
Z9 3
U1 0
U2 9
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD OCT
PY 2012
VL 50
IS 10
BP 3980
EP 3990
DI 10.1109/TGRS.2012.2189575
PN 2
PG 11
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 014FX
UT WOS:000309361700006
ER
PT J
AU Driggers, WB
Hannan, KM
Hoffmayer, ER
Jensen, J
AF Driggers, W. B., III
Hannan, K. M.
Hoffmayer, E. R.
Jensen, J.
TI Abnormal blacktip shark, Carcharhinus limbatus, embryo from the northern
Gulf of Mexico
SO JOURNAL OF APPLIED ICHTHYOLOGY
LA English
DT Article
ID CHONDRICHTHYES; TERATOLOGY
C1 [Driggers, W. B., III; Hannan, K. M.; Hoffmayer, E. R.] Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS 39567 USA.
[Jensen, J.] Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Fisheries Stat Field Off, New Orleans, LA USA.
RP Driggers, WB (reprint author), Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Mississippi Labs, PO Drawer 1207, Pascagoula, MS 39567 USA.
EM william.driggers@noaa.gov
NR 14
TC 1
Z9 2
U1 1
U2 6
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0175-8659
J9 J APPL ICHTHYOL
JI J. Appl. Ichthyol.
PD OCT
PY 2012
VL 28
IS 5
BP 827
EP 828
DI 10.1111/j.1439-0426.2011.01924.x
PG 2
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 007GY
UT WOS:000308878000026
ER
PT J
AU Basusta, A
Basusta, N
Sulikowski, JA
Driggers, WB
Demirhan, SA
Cicek, E
AF Basusta, A.
Basusta, N.
Sulikowski, J. A.
Driggers, W. B., III
Demirhan, S. A.
Cicek, E.
TI Length-weight relationships for nine species of batoids from the
Iskenderun Bay, Turkey
SO JOURNAL OF APPLIED ICHTHYOLOGY
LA English
DT Article
ID RHINOBATOS-RHINOBATOS; COMMON GUITARFISH
AB Presented are lengthweight relationships for Rhinobatos rhinobatos, Rhinobatos cemiculus, Gymnura altevela, Dasyatis pastinaca, Rhinoptera marginata, Pteromylaeus bovinus, Torpedo nobiliana, Raja miraletus and Raja clavata captured by gillnet, longline and bottom trawl fishing between May 2010 and July 2011 off the east coast of Iskenderun Bay, Turkey.
C1 [Basusta, A.; Basusta, N.] Firat Univ, Fac Fisheries, TR-23119 Elazig, Turkey.
[Basusta, N.; Sulikowski, J. A.] Univ New England, Dept Marine Sci, Biddeford, ME USA.
[Driggers, W. B., III] Natl Marine Fisheries Serv, Mississippi Labs, SE Fisheries Sci Ctr, Pascagoula, MS USA.
[Demirhan, S. A.] Mustafa Kemal Univ, Fac Fisheries, Iskenderun, Hatay, Turkey.
[Cicek, E.] Nevsehir Univ, Fac Sci & Art, Dept Biol, Nevsehir, Turkey.
RP Basusta, N (reprint author), Firat Univ, Fac Fisheries, TR-23119 Elazig, Turkey.
EM nbasusta@hotmail.com
FU Scientific and Technological Research Council of Turkey (TUBITAK)
[TO-VAG 1 09O 634]
FX The authors thank E. Aslan, N. Beyazit, A. K. Ozcan, and N. Gayir for
their assistance in obtaining the fish samples and E. I. Ozer, O. V.
Duman and H. Girgin for their help in the laboratory. The permit for
experimental fishing was granted to us by the General Directorate of
Protection and Control, Ministry of Agriculture and Rural Affairs of
Turkish Republic to collect elasmobranches in these locations and during
the months of April, May and June when the waters are closed to
commercial fishing. All data were obtained from Project, which was
supported by The Scientific and Technological Research Council of Turkey
(TUBITAK), Project No: TO-VAG 1 09O 634.
NR 7
TC 11
Z9 11
U1 1
U2 19
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0175-8659
J9 J APPL ICHTHYOL
JI J. Appl. Ichthyol.
PD OCT
PY 2012
VL 28
IS 5
BP 850
EP 851
DI 10.1111/j.1439-0426.2012.02013.x
PG 2
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 007GY
UT WOS:000308878000034
ER
PT J
AU Wiersema, K
Curran, PA
Kruhler, T
Melandri, A
Rol, E
Starling, RLC
Tanvir, NR
van der Horst, AJ
Covino, S
Fynbo, JPU
Goldoni, P
Gorosabel, J
Hjorth, J
Klose, S
Mundell, CG
O'Brien, PT
Palazzi, E
Wijers, RAMJ
D'Elia, V
Evans, PA
Filgas, R
Gomboc, A
Greiner, J
Guidorzi, C
Kaper, L
Kobayashi, S
Kouveliotou, C
Levan, AJ
Rossi, A
Rowlinson, A
Steele, IA
Postigo, AD
Vergani, SD
AF Wiersema, K.
Curran, P. A.
Kruehler, T.
Melandri, A.
Rol, E.
Starling, R. L. C.
Tanvir, N. R.
van der Horst, A. J.
Covino, S.
Fynbo, J. P. U.
Goldoni, P.
Gorosabel, J.
Hjorth, J.
Klose, S.
Mundell, C. G.
O'Brien, P. T.
Palazzi, E.
Wijers, R. A. M. J.
D'Elia, V.
Evans, P. A.
Filgas, R.
Gomboc, A.
Greiner, J.
Guidorzi, C.
Kaper, L.
Kobayashi, S.
Kouveliotou, C.
Levan, A. J.
Rossi, A.
Rowlinson, A.
Steele, I. A.
de Ugarte Postigo, A.
Vergani, S. D.
TI Detailed optical and near-infrared polarimetry, spectroscopy and
broad-band photometry of the afterglow of GRB 091018: polarization
evolution
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE acceleration of particles; techniques: polarimetric; gamma-ray burst:
individual: GRB 091018
ID GAMMA-RAY BURST; MAGNETIC-FIELD STRUCTURE; 28 FEBRUARY 1997;
LINEAR-POLARIZATION; LIGHT CURVES; CIRCULAR-POLARIZATION; WAVELENGTH
DEPENDENCE; HOST GALAXIES; JET STRUCTURE; SWIFT ERA
AB Follow-up observations of large numbers of gamma-ray burst (GRB) afterglows, facilitated by the Swift satellite, have produced a large sample of spectral energy distributions and light curves, from which their basic micro- and macro-physical parameters can in principle be derived. However, a number of phenomena have been observed that defy explanation by simple versions of the standard fireball model, leading to a variety of new models. Polarimetry can be a major independent diagnostic of afterglow physics, probing the magnetic field properties and internal structure of the GRB jets. In this paper we present the first high-quality multi-night polarimetric light curve of a Swift GRB afterglow, aimed at providing a well-calibrated data set of a typical afterglow to serve as a benchmark system for modelling afterglow polarization behaviour. In particular, our data set of the afterglow of GRB 091018 (at redshift z = 0.971) comprises optical linear polarimetry (R band, 0.132.3?d after burst); circular polarimetry (R band) and near-infrared linear polarimetry (Ks band). We add to that high-quality optical and near-infrared broad-band light curves and spectral energy distributions as well as afterglow spectroscopy. The linear polarization varies between 0 and 3?per cent, with both long and short time-scale variability visible. We find an achromatic break in the afterglow light curve, which corresponds to features in the polarimetric curve. We find that the data can be reproduced by jet break models only if an additional polarized component of unknown nature is present in the polarimetric curve. We probe the ordered magnetic field component in the afterglow through our deep circular polarimetry, finding Pcirc < 0.15?per cent (2s), the deepest limit yet for a GRB afterglow, suggesting ordered fields are weak, if at all present. Our simultaneous R- and Ks-band polarimetry shows that dust-induced polarization in the host galaxy is likely negligible.
C1 [Wiersema, K.; Starling, R. L. C.; Tanvir, N. R.; O'Brien, P. T.; Evans, P. A.; Rowlinson, A.] Univ Leicester, Leicester LE1 7RH, Leics, England.
[Curran, P. A.] Univ Paris Diderot, Lab AIM, Ctr Saclay, CEA,IRFU,CNRS,INSU,CEA DSM,SAp, F-91191 Gif Sur Yvette, France.
[Kruehler, T.; Fynbo, J. P. U.; Hjorth, J.; de Ugarte Postigo, A.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Melandri, A.; Covino, S.; Vergani, S. D.] Osserv Astron Brera, INAF, I-23807 Merate, Italy.
[Melandri, A.; Mundell, C. G.; Kobayashi, S.; Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Rol, E.; van der Horst, A. J.; Wijers, R. A. M. J.; Rowlinson, A.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Goldoni, P.] Lab Astroparticule & Cosmol, F-75205 Paris 13, France.
[Gorosabel, J.; de Ugarte Postigo, A.] CSIC, IAA, E-18008 Granada, Spain.
[Klose, S.; Rossi, A.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany.
[Palazzi, E.] Ist Astrofis Spaziale & Fis Cosm Bologna, INAF, I-40129 Bologna, Italy.
[D'Elia, V.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[D'Elia, V.] ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Filgas, R.; Greiner, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Gomboc, A.] Univ Ljubljana, Fac Math & Phys, SI-1000 Ljubljana, Slovenia.
[Gomboc, A.] Ctr Excellence SPACE SI, SI-1000 Ljubljana, Slovenia.
[Guidorzi, C.] Univ Ferrara, Dept Phys, I-44122 Ferrara, Italy.
[Kouveliotou, C.] NASA, Space Sci Off, Marshall Space Flight Ctr Huntsville, Huntsville, AL 35812 USA.
[Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
RP Wiersema, K (reprint author), Univ Leicester, Univ Rd, Leicester LE1 7RH, Leics, England.
EM kw113@star.le.ac.uk
RI Curran, Peter/B-5293-2013; Fynbo, Johan/L-8496-2014; Hjorth,
Jens/M-5787-2014; Palazzi, Eliana/N-4746-2015; Rossi,
Andrea/N-4674-2015;
OI de Ugarte Postigo, Antonio/0000-0001-7717-5085; Curran,
Peter/0000-0003-3003-4626; Fynbo, Johan/0000-0002-8149-8298; Hjorth,
Jens/0000-0002-4571-2306; Palazzi, Eliana/0000-0002-8691-7666; Rossi,
Andrea/0000-0002-8860-6538; Wijers, Ralph/0000-0002-3101-1808; D'Elia,
Valerio/0000-0002-7320-5862; Covino, Stefano/0000-0001-9078-5507;
Kruehler, Thomas/0000-0002-8682-2384
FU STFC; European Commission; Danish National Research Foundation; Royal
Society; British Council; Platform Beta Techniek through the Partnership
Programme in Science [PPS WS 005]; DFG [HA 1850/28-1, Kl 766/16-1];
BLANCE-FLOR Boncompagni-Ludovisi, nee Bildt foundation
FX We warmly thank the ESO staff for obtaining the VLT data discussed here.
We thank Justyn Maund, Dave Russell, Daniele Malesani, Piergiorgio
Casella, Elena Rossi, Christina Thone and Alexander Kann for their help
and useful discussions. We thank the anonymous referee for useful
comments and suggestions. Based on observations made with ESO Telescopes
at the Paranal Observatory under programmes 084.D-0949 and 084.A-0260.
KW acknowledges support from STFC. TK acknowledges support by the
European Commission under the Marie Curie Intra-European Fellowship
Programme. The Dark Cosmology Centre is funded by the Danish National
Research Foundation. RLCS is supported by a Royal Society Fellowship.
The financial support of the British Council and Platform Beta Techniek
through the Partnership Programme in Science (PPS WS 005, PI: Wiersema)
is gratefully acknowledged. Part of the funding for GROND (both hardware
as well as personnel) was generously granted from the Leibniz-Prize to
Prof. G. Hasinger (DFG grant HA 1850/28-1). SK and AR acknowledge
support by DFG grant Kl 766/16-1, and AR in addition from the
BLANCE-FLOR Boncompagni-Ludovisi, nee Bildt foundation. This work made
use of data supplied by the UK Swift Science Data Centre at the
University of Leicester. IRAF is distributed by the 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.
NR 93
TC 25
Z9 25
U1 1
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2012
VL 426
IS 1
BP 2
EP 22
DI 10.1111/j.1365-2966.2012.20943.x
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009ZQ
UT WOS:000309064600002
ER
PT J
AU D'Ammando, F
Orienti, M
Finke, J
Raiteri, CM
Angelakis, E
Fuhrmann, L
Giroletti, M
Hovatta, T
Max-Moerbeck, W
Perkins, JS
Readhead, ACS
Richards, JL
Stawarz, L
Donato, D
AF D'Ammando, F.
Orienti, M.
Finke, J.
Raiteri, C. M.
Angelakis, E.
Fuhrmann, L.
Giroletti, M.
Hovatta, T.
Max-Moerbeck, W.
Perkins, J. S.
Readhead, A. C. S.
Richards, J. L.
Stawarz, L.
Donato, D.
TI SBS 0846+513: a new gamma-ray-emitting narrow-line Seyfert 1 galaxy
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; galaxies: individual: SBS 0846+513; galaxies: nuclei;
galaxies: Seyfert; gamma-rays: general
ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; BLACK-HOLE MASS; BL-LAC
OBJECT; SPECTRUM RADIO QUASARS; DIGITAL SKY SURVEY; X-RAY; PMN
J0948+0022; RELATIVISTIC JET; COMPTON ANALYSIS
AB We report Fermi Large Area Telescope (LAT) observations of the radio-loud active galactic nucleus SBS 0846+513 (z = 0.5835), optically classified as a narrow-line Seyfert 1 galaxy, together with new and archival radio-to-X-ray data. The source was not active at ?-ray energies during the first two years of Fermi operation. A significant increase in activity was observed during 2010 October2011 August. In particular, a strong ?-ray flare was observed in 2011 June reaching an isotropic ?-ray luminosity (0.1300?GeV) of 1.0 X 1048?erg?s-1, comparable to that of the brightest flat spectrum radio quasars, and showing spectral evolution in ? rays. An apparent superluminal velocity of (8.2 +/- 1.5)c in the jet was inferred from 2011 to 2012 Very Long Baseline Array (VLBA) images, suggesting the presence of a highly relativistic jet. Both the power released by this object during the flaring activity and the apparent superluminal velocity are strong indications of the presence of a relativistic jet as powerful as those of blazars. In addition, variability and spectral properties in radio and ?-ray bands indicate blazar-like behaviour, suggesting that, except for some distinct optical characteristics, SBS 0846+513 could be considered as a young blazar at the low end of the blazar's black hole mass distribution.
C1 [D'Ammando, F.] Univ Perugia, Dip Fis, I-060123 Perugia, Italy.
[D'Ammando, F.; Orienti, M.; Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[D'Ammando, F.] CIFS, I-10133 Turin, Italy.
[Orienti, M.] Univ Bologna, Dip Astron, I-40127 Bologna, Italy.
[Finke, J.] USN, Res Lab, Washington, DC 20375 USA.
[Raiteri, C. M.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, TO, Italy.
[Angelakis, E.; Fuhrmann, L.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Hovatta, T.; Max-Moerbeck, W.; Readhead, A. C. S.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Perkins, J. S.; Donato, D.] Univ Maryland, Dept Astron, Baltimore, MD 20742 USA.
[Perkins, J. S.; Donato, D.] Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
[Richards, J. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Stawarz, L.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[Perkins, J. S.; Donato, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP D'Ammando, F (reprint author), Univ Perugia, Dip Fis, Via A Pascoli, I-060123 Perugia, Italy.
EM filippo.dammando@fisica.unipg.it
FU NASA [NNX08AW31G, NNX11A043G]; NSF [AST-0808050, AST-1109911];
[ASI-INAF I/009/10/0]
FX We thank the Swift team for making these observations possible, the duty
scientists and science planners. This research has made use of data from
the MOJAVE data base that is maintained by the MOJAVE team (Lister et
al. 2009). The OVRO 40-m monitoring program is supported in part by NASA
grants NNX08AW31G and NNX11A043G, and NSF grants AST-0808050 and
AST-1109911. This paper is partly based on observations with the 100-m
telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at
Effelsberg and the Medicina telescope operated by INAF-Istituto di
Radioastronomia. We acknowledge A. Orlati, S. Righini and the Enhanced
Single-dish Control System (ESCS) Development Team. We acknowledge
financial contribution from agreement ASI-INAF I/009/10/0. 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. 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. We thank the anonymous
referee for useful suggestions. FD would like to thank Gino Tosti and
Marco Ajello for fruitful comments and discussions, and Paola Grandi who
has made the data of her paper available.
NR 84
TC 49
Z9 49
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2012
VL 426
IS 1
BP 317
EP 329
DI 10.1111/j.1365-2966.2012.21707.x
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009ZQ
UT WOS:000309064600023
ER
PT J
AU Faimali, A
Thompson, MA
Hindson, L
Urquhart, JS
Pestalozzi, M
Carey, S
Shenoy, S
Veneziani, M
Molinari, S
Clark, JS
AF Faimali, A.
Thompson, M. A.
Hindson, L.
Urquhart, J. S.
Pestalozzi, M.
Carey, S.
Shenoy, S.
Veneziani, M.
Molinari, S.
Clark, J. S.
TI The G305 star-forming complex: embedded massive star formation
discovered by Herschel Hi-GAL
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: statistical; stars: formation; H II regions; infrared: ISM
ID YOUNG STELLAR OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; FORMATION RATE
INDICATORS; GALACTIC PLANE SURVEY; MSX SOURCE SURVEY; II REGIONS;
MILKY-WAY; LUMINOSITY FUNCTION; MOLECULAR CLOUDS; (CO)-C-13 OBSERVATIONS
AB We present a Herschel far-infrared study towards the rich massive star-forming complex G305, utilizing PACS 70, 160?mu m and SPIRE 250, 350, and 500?mu m observations from the Hi-GAL survey of the Galactic plane. The focus of this study is to identify the embedded massive star-forming population within G305, by combining far-infrared data with radio continuum, H2O maser, methanol maser, MIPS and Red MSX Source survey data available from previous studies. By applying a frequentist technique we are able to identify a sample of the most likely associations within our multiwavelength data set, which can then be identified from the derived properties obtained from fitted spectral energy distributions (SEDs). By SED modelling using both a simple modified blackbody and fitting to a comprehensive grid of model SEDs, some 16 candidate associations are identified as embedded massive star-forming regions. We derive a two-selection colour criterion from this sample of log?(F70/F500)?=?1 and log?(F160/F350)?=?1.6 to identify an additional 31 embedded massive star candidates with no associated star formation tracers. Using this result we can build a picture of the present-day star formation of the complex, and by extrapolating an initial mass function, suggest a current population of approximate to 2?x?104 young stellar objects (YSOs) present, corresponding to a star formation rate (SFR) of 0.010.02?M??yr-1. Comparing this resolved SFR, to extragalactic SFR tracers (based on the KennicuttSchmidt relation), we find that the star formation activity is underestimated by a factor of =2 in comparison to the SFR derived from the YSO population.
C1 [Faimali, A.; Thompson, M. A.; Hindson, L.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Hindson, L.] CSIRO Astron & Space Sci, ATNF, Epping, NSW 1710, Australia.
[Urquhart, J. S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Pestalozzi, M.; Molinari, S.] CNR, Inst Fis Spazio Interplanetario, I-00133 Rome, Italy.
[Carey, S.; Veneziani, M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Shenoy, S.] NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Clark, J. S.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
RP Faimali, A (reprint author), Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
EM a.faimali@herts.ac.uk
RI Molinari, Sergio/O-4095-2016
OI Molinari, Sergio/0000-0002-9826-7525
FU Science and Technology Facilities Council of the UK; Science and
Technology Facilities Council; BMVIT (Austria); ESA-PRODEX (Belgium);
CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain);
CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); CEA, CNES, CNRS
(France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA
(USA)
FX The authors would first like to thank the entire Herschel Hi-GAL team
for their continuing work on the survey. We would also like to thank
Sean Carey and Sachin Shenoy for producing, and making available the
MIPSGAL point source catalogue for inclusion in our analysis. This
research has made possible with the use of the NASA Astrophysics Data
System Bibliographic Services. This paper made use of information from
the Red MSX Source survey data base at www.ast.leeds.ac.uk/RMS, which
was constructed with support from the Science and Technology Facilities
Council of the UK. We made use of positional data on 6.7 GHz methanol
masers provided by the Methanol Multi-Beam (MMB) survey, also supported
by the Science and Technology Facilities Council, and with a maser data
base available at http://astromasers.org.; PACS has been developed by a
consortium of institutes led by MPE (Germany) and including UVIE
(Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA
(Germany); INAFIFSI/OAA/OAP/OAT, LENS, SISSA (Italy); and IAC (Spain).
This development has been supported by the funding agencies BMVIT
(Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany),
ASI/INAF (Italy) and CICYT/MCYT (Spain). SPIRE has been developed by a
consortium of institutes led by Cardiff University (UK) and including
Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ.
Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial
College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech,
JPL, NHSC, Univ. Colorado (USA). This development has been supported by
national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS
(France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA
(USA).
NR 88
TC 15
Z9 15
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2012
VL 426
IS 1
BP 402
EP 415
DI 10.1111/j.1365-2966.2012.21765.x
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 009ZQ
UT WOS:000309064600031
ER
PT J
AU Oates, SR
Page, MJ
De Pasquale, M
Schady, P
Breeveld, AA
Holland, ST
Kuin, NPM
Marshall, FE
AF Oates, S. R.
Page, M. J.
De Pasquale, M.
Schady, P.
Breeveld, A. A.
Holland, S. T.
Kuin, N. P. M.
Marshall, F. E.
TI A correlation between the intrinsic brightness and average decay rate of
Swift/UVOT gamma-ray burst optical/ultraviolet light curves
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gamma-ray burst: general
ID OPTICAL AFTERGLOW; IDENTIFICATION; TELESCOPE
AB We examine a sample of 48 Swift/UVOT long gamma-ray burst light curves and find a correlation between the logarithmic luminosity at 200 s and average decay rate determined from 200 s onwards, with a Spearman rank coefficient of -0.58 at a significance of 99.998 per cent (4.2s). We discuss the causes of the log L200 sa>200 s correlation, finding it to be an intrinsic property of long gamma-ray bursts, and not resulting from the selection criteria. We find two ways to produce the correlation. One possibility is that there is some property of the central engine, outflow or external medium that affects the rate of energy release so that the bright afterglows release their energy more quickly and decay faster than the fainter afterglows. Alternatively, the correlation may be produced by variation of the observers viewing angle, with observers at large viewing angles observing fainter and slower decaying light curves.
C1 [Oates, S. R.; Page, M. J.; Breeveld, A. A.; Kuin, N. P. M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[De Pasquale, M.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA.
[Schady, P.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Holland, S. T.] Space Telescope Sci Ctr, Baltimore, MD 21218 USA.
[Marshall, F. E.] Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Oates, SR (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
EM sro@mssl.ucl.ac.uk
FU UK Space Agency
FX We thank the referee for useful comments and suggestions. This research
has made use of data from the High Energy Astrophysics Science Archive
Research Center (HEASARC) and the Leicester Database and Archive Service
(LEDAS), provided by NASA's Goddard Space Flight Center and the
Department of Physics and Astronomy, Leicester University, UK,
respectively. SRO, AAB, NPMK and MJP acknowledge support from the UK
Space Agency.
NR 23
TC 4
Z9 4
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2012
VL 426
IS 1
BP L86
EP L90
DI 10.1111/j.1745-3933.2012.01331.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 015OM
UT WOS:000309455800018
ER
PT J
AU Sbarrato, T
Ghisellini, G
Nardini, M
Tagliaferri, G
Foschini, L
Ghirlanda, G
Tavecchio, F
Greiner, J
Rau, A
Gehrels, N
AF Sbarrato, T.
Ghisellini, G.
Nardini, M.
Tagliaferri, G.
Foschini, L.
Ghirlanda, G.
Tavecchio, F.
Greiner, J.
Rau, A.
Gehrels, N.
TI SDSS J102623.61+254259.5: the second most distant blazar at z=5.3
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; quasars: general; quasars: individual: B2 1023+25;
X-rays: general
ID DIGITAL SKY SURVEY; LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; DATA
RELEASE; FERMI BLAZARS; BLACK-HOLES; MISSION; CATALOG; Q0906+6930;
EMISSION
AB The radio-loud quasar SDSS J102623.61+254259.5, at a redshift z similar to= 5.3, is one of the most distant radio-loud objects. Since its radio flux exceeds 100 mJy at a few GHz, it is also one of the most powerful radio-loud sources. We propose that this source is a blazar, i.e. we are seeing its jet at a small viewing angle. This claim is based on the spectral energy distribution of this source, and especially on its strong and hard X-ray spectrum, as seen by Swift, very typical of powerful blazars. Observations by the Gamma-Ray Burst Optical/Near-Infrared Detector (GROND) and by the Wide-field Infrared Survey Explorer (WISE) allow us to establish the thermal nature of the emission in the near-IRoptical band. Assuming that this is produced by a standard accretion disc, we derive that it emits a luminosity of Ld? 9 similar to x 1046 erg s-1 and that the black hole has a mass between 2 and 5 billion solar masses. This poses interesting constraints on the mass function of heavy (>109 M?) black holes at high redshifts.
C1 [Sbarrato, T.] Univ Insubria, Dipartimento Fis & Matemat, I-22100 Como, Italy.
[Sbarrato, T.; Ghisellini, G.; Tagliaferri, G.; Foschini, L.; Ghirlanda, G.; Tavecchio, F.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
[Nardini, M.] Univ Milano Bicocca, Dipartimento Fis G Occhialini, I-20126 Milan, Italy.
[Greiner, J.; Rau, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Sbarrato, T (reprint author), Univ Insubria, Dipartimento Fis & Matemat, Via Valleggio 11, I-22100 Como, Italy.
EM tullia.sbarrato@brera.inaf.it
OI Sbarrato, Tullia/0000-0002-3069-9399; Tagliaferri,
Gianpiero/0000-0003-0121-0723; Ghirlanda, Giancarlo/0000-0001-5876-9259;
Ghisellini, Gabriele/0000-0002-0037-1974
FU National Aeronautics and Space Administration; DFG [HA 1850/28-1]
FX We would like to thank the anonymous referee for useful comments. 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. Part of this work is based on archival data, software or
online services provided by the ASI Data Center (ASDC). Part of the
funding for GROND (both hardware as well as personnel) was generously
granted from the Leibniz Prize to Professor G. Hasinger (DFG grant HA
1850/28-1). This work made use of data supplied by the UK Swift Science
Data Centre at the University of Leicester.
NR 37
TC 20
Z9 20
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2012
VL 426
IS 1
BP L91
EP L95
DI 10.1111/j.1745-3933.2012.01332.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 015OM
UT WOS:000309455800019
ER
PT J
AU Alexandrov, MD
Cairns, B
Emde, C
Ackerman, AS
van Diedenhoven, B
AF Alexandrov, Mikhail D.
Cairns, Brian
Emde, Claudia
Ackerman, Andrew S.
van Diedenhoven, Bastiaan
TI Accuracy assessments of cloud droplet size retrievals from polarized
reflectance measurements by the research scanning polarimeter
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Electromagnetic scattering; Polarization; Mie theory; Rainbow; Optical
particle characterization; Remote sensing
ID EFFECTIVE RADIUS; RADIATIVE-TRANSFER; LIGHT-SCATTERING; SOLAR-RADIATION;
WATER CLOUDS; AEROSOL; POLDER; IMPACT; OCEAN; SENSITIVITY
AB We present an algorithm for the retrieval of cloud droplet size distribution parameters (effective radius and variance) from the Research Scanning Polarimeter (RSP) measurements. The RSP is an airborne prototype for the Aerosol Polarimetery Sensor (APS), which was on-board of the NASA Glory satellite. This instrument measures both polarized and total reflectance in 9 spectral channels with central wavelengths ranging from 410 to 2260 nm. The cloud droplet size retrievals use the polarized reflectance in the scattering angle range between 135 degrees and 165 degrees, where they exhibit the sharply defined structure known as the rain- or cloud-bow. The shape of the rainbow is determined mainly by the single scattering properties of cloud particles. This significantly simplifies both forward modeling and inversions, while also substantially reducing uncertainties caused by the aerosol loading and possible presence of undetected clouds nearby. In this study we present the accuracy evaluation of our algorithm based on the results of sensitivity tests performed using realistic simulated cloud radiation fields. (c) 2012 Elsevier Inc. All rights reserved.
C1 [Alexandrov, Mikhail D.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA.
[Alexandrov, Mikhail D.; Cairns, Brian; Ackerman, Andrew S.; van Diedenhoven, Bastiaan] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Emde, Claudia] Univ Munich, Inst Meteorol, D-80333 Munich, Germany.
[van Diedenhoven, Bastiaan] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
RP Alexandrov, MD (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, 2880 Broadway, New York, NY 10025 USA.
EM mda14@columbia.edu
RI Ackerman, Andrew/D-4433-2012; van Diedenhoven, Bastiaan/A-2002-2013;
Emde, Claudia/B-5447-2010;
OI Ackerman, Andrew/0000-0003-0254-6253; Cairns, Brian/0000-0002-1980-1022
FU NASA Radiation Sciences Program; NASA Glory Mission project
FX This research was funded by the NASA Radiation Sciences Program managed
by Hal Maring and by the NASA Glory Mission project.
NR 47
TC 19
Z9 19
U1 2
U2 23
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 OCT
PY 2012
VL 125
BP 92
EP 111
DI 10.1016/j.rse.2012.07.012
PG 20
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 013UJ
UT WOS:000309331100009
ER
PT J
AU Aurin, DA
Dierssen, HM
AF Aurin, Dirk A.
Dierssen, Heidi M.
TI Advantages and limitations of ocean color remote sensing in
CDOM-dominated, mineral-rich coastal and estuarine waters
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Ocean color; Remote sensing; Semi-analytical algorithm development;
Regional optimization
ID INHERENT OPTICAL-PROPERTIES; TOTAL SUSPENDED MATTER; ABSORPTION-SPECTRA;
PHYTOPLANKTON ABSORPTION; DIFFUSE-REFLECTANCE; LEAVING RADIANCE; NATURAL
PHYTOPLANKTON; BACKSCATTERING RATIO; SHALLOW WATERS; COMPLEX WATERS
AB Current operational approaches to ocean color remote sensing tend to be least accurate in coastal regions with waters rich in terrigenous material. Semi-analytical models can be used to retrieve the absorption and backscattering properties of dissolved and suspended materials unique to these environments, and subsequently biogeochemical parameters such as total suspended material (TSM) and chlorophyll (Chl). In this study, optical data collected over several years are used to select and optimize a semi-analytical ocean color algorithm for the dynamic and optically complex Long Island Sound estuary. The most successful algorithm requires a red reflectance channel between 600 and 650 nm, which is not included in many current ocean color sensors, but is essential in highly scattering waters. Regional optimization including the use of a dynamic, spectrally variable f/Q a value related to the bidirectional reflectance distribution function (BRDF), results in an approximately five-fold decrease in retrieval bias in highly backscattering, sediment-laden waters near river outflows. Retrievals of dissolved and particulate spectral absorption, backscattering, dissolved and detrital absorption coefficients and total suspended matter obtained from the optimized algorithm agree well with field observations (r(2) >= 0.90). These parameters are useful for assessing riverine discharge, mixing and residence times of surface waters, as well as assessing the turbidity and light penetration in this estuary. Estimation of Chl remains challenging (r(2) = 0.59) due to the stepwise nature of the algorithm and the relatively high proportion of dissolved and non-algal constituents masking phytoplankton absorption (generally <20% of total absorption at 440 nm). Moreover, diverse phytoplankton assemblages throughout the region create variability between spectral absorption and chlorophyll and highlight the benefits of increased spectral resolution of ocean color satellites going forward. (c) 2012 Elsevier Inc. All rights reserved.
C1 [Aurin, Dirk A.; Dierssen, Heidi M.] Univ Connecticut, Dept Marine Sci, Groton, CT 06340 USA.
RP Aurin, DA (reprint author), NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Mail Code 616,Bldg 22,Rm 248, Greenbelt, MD 20771 USA.
EM dirk.a.aurin@nasa.gov
RI aurin, dirk/E-1597-2013
FU Department of Defense National Defense Science and Engineering Graduate
Fellowship; National Aeronautic and Space Administration Ocean Biology
and Biogeochemistry research program [NNG04GN61G]; University of
Connecticut
FX This work was funded in part by the Department of Defense National
Defense Science and Engineering Graduate Fellowship, National Aeronautic
and Space Administration Ocean Biology and Biogeochemistry research
program (NNG04GN61G to H.M. Dierssen), and the University of
Connecticut. Many thanks to the Long Island Sound Integrated Coastal
Observation System (LISICOS) and the crew on the R/V Connecticut, to
Scott Freeman, Brandon Russell, and Kelley Bostrom for providing optical
field data, and to Emmanuel Boss and Steve Ackleson for equipment and
ship time provided in support of the project.
NR 92
TC 17
Z9 19
U1 4
U2 72
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 OCT
PY 2012
VL 125
BP 181
EP 197
DI 10.1016/j.rse.2012.07.001
PG 17
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 013UJ
UT WOS:000309331100016
ER
PT J
AU Gopalswamy, N
Nitta, NV
AF Gopalswamy, N.
Nitta, N. V.
TI Ground Level Enhancement Events of Solar Cycle 23 Preface
SO SPACE SCIENCE REVIEWS
LA English
DT Editorial Material
C1 [Gopalswamy, N.] NASA, GSFC, Greenbelt, MD 20771 USA.
[Nitta, N. V.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
RP Gopalswamy, N (reprint author), NASA, GSFC, Code 671, Greenbelt, MD 20771 USA.
EM nat.gopalswamy@nasa.gov
NR 0
TC 2
Z9 2
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD OCT
PY 2012
VL 171
IS 1-4
BP 1
EP 2
DI 10.1007/s11214-012-9934-9
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 014CJ
UT WOS:000309352400001
ER
PT J
AU Gopalswamy, N
Xie, H
Yashiro, S
Akiyama, S
Makela, P
Usoskin, IG
AF Gopalswamy, N.
Xie, H.
Yashiro, S.
Akiyama, S.
Maekelae, P.
Usoskin, I. G.
TI Properties of Ground Level Enhancement Events and the Associated Solar
Eruptions During Solar Cycle 23
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE CME; Solar flare; GLE; Shock; Radio bursts; SEP
ID CORONAL MASS EJECTIONS; ENERGETIC PARTICLE EVENTS; RADIO-BURSTS;
MAGNETIC-FIELD; RELEASE TIMES; SHOCK ACCELERATION; PROTON EVENTS;
NEAR-EARTH; III BURSTS; FLARES
AB Solar cycle 23 witnessed the most complete set of observations of coronal mass ejections (CMEs) associated with the Ground Level Enhancement (GLE) events. We present an overview of the observed properties of the GLEs and those of the two associated phenomena, viz., flares and CMEs, both being potential sources of particle acceleration. Although we do not find a striking correlation between the GLE intensity and the parameters of flares and CMEs, the solar eruptions are very intense involving X-class flares and extreme CME speeds (average similar to 2000 km/s). An M7.1 flare and a 1200 km/s CME are the weakest events in the list of 16 GLE events. Most (80 %) of the CMEs are full halos with the three non-halos having widths in the range 167 to 212 degrees. The active regions in which the GLE events originate are generally large: 1290 msh (median 1010 msh) compared to 934 msh (median: 790 msh) for SEP-producing active regions. For accurate estimation of the CME height at the time of metric type II onset and GLE particle release, we estimated the initial acceleration of the CMEs using flare and CME observations. The initial acceleration of GLE-associated CMEs is much larger (by a factor of 2) than that of ordinary CMEs (2.3 km/s(2) vs. 1 km/s(2)). We confirmed the initial acceleration for two events for which CME measurements are available in the inner corona. The GLE particle release is delayed with respect to the onset of all electromagnetic signatures of the eruptions: type II bursts, low frequency type III bursts, soft X-ray flares and CMEs. The presence of metric type II radio bursts some 17 min (median: 16 min; range: 3 to 48 min) before the GLE onset indicates shock formation well before the particle release. The release of GLE particles occurs when the CMEs reach an average height of similar to 3.09 R (s) (median: 3.18 R (s) ; range: 1.71 to 4.01 R (s) ) for well-connected events (source longitude in the range W20-W90). For poorly connected events, the average CME height at GLE particle release is similar to 66 % larger (mean: 5.18 R (s) ; median: 4.61 R (s) ; range: 2.75-8.49 R (s) ). The longitudinal dependence is consistent with shock accelerations because the shocks from poorly connected events need to expand more to cross the field lines connecting to an Earth observer. On the other hand, the CME height at metric type II burst onset has no longitudinal dependence because electromagnetic signals do not require magnetic connectivity to the observer. For several events, the GLE particle release is very close to the time of first appearance of the CME in the coronagraphic field of view, so we independently confirmed the CME height at particle release. The CME height at metric type II burst onset is in the narrow range 1.29 to 1.8 R (s) , with mean and median values of 1.53 and 1.47 R (s) . The CME heights at metric type II burst onset and GLE particle release correspond to the minimum and maximum in the Alfv,n speed profile. The increase in CME speed between these two heights suggests an increase in Alfv,nic Mach number from 2 to 3. The CME heights at GLE particle release are in good agreement with those obtained from the velocity dispersion analysis (Reames in Astrophys. J. 693:812, 2009a; Astrophys. J. 706:844, 2009b) including the source longitude dependence. We also discuss the implications of the delay of GLE particle release with respect to complex type III bursts by similar to 18 min (median: 16 in; range: 2 to 44 min) for the flare acceleration mechanism.
A similar analysis is also performed on the delay of particle release relative to the hard X-ray emission.
C1 [Gopalswamy, N.; Xie, H.; Yashiro, S.; Akiyama, S.; Maekelae, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Xie, H.; Yashiro, S.; Akiyama, S.; Maekelae, P.] Catholic Univ Amer, Washington, DC 20064 USA.
[Usoskin, I. G.] Univ Oulu, Sodankyla Geophys Observ, Oulu Unit, Oulu 90014, Finland.
[Usoskin, I. G.] Univ Oulu, Dept Phys, Oulu 90014, Finland.
RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Nat.Gopalswamy@nasa.gov
RI Usoskin, Ilya/E-5089-2014
OI Usoskin, Ilya/0000-0001-8227-9081
FU NASA [NNX09AT38A, NNX10AL50A]
FX Works done by H.X., S.Y., S.A., and P.M. were supported by NASA
(NNX09AT38A; NNX10AL50A). Part of this work was done during two LWS
CDAWs on Ground Level Enhancement events held in Palo Alto, CA (January
6-9, 2009) and Huntsville, AL (November 16-18, 2009). We acknowledge
downloading neutron monitor data from three GLE databases: Australian
Antarctic Data Centre http://data.aad.gov.au/aadc/gle/; NMDB
http://www.nmdb.eu/nest/search.php and Moscow database
ftp://cr0.izmiran.rssi.ru/COSRAY!/. Oulu NM data are available at
http://cosmicrays.oulu.fi. We also thank the Mauna Loa solar Observatory
for making coronal images available online, which we used for Fig. 15.
We also thank the referee, E.W. Cliver, for critical comments, which
helped improve the presentation of the paper.
NR 86
TC 78
Z9 80
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD OCT
PY 2012
VL 171
IS 1-4
BP 23
EP 60
DI 10.1007/s11214-012-9890-4
PG 38
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 014CJ
UT WOS:000309352400003
ER
PT J
AU Mewaldt, RA
Looper, MD
Cohen, CMS
Haggerty, DK
Labrador, AW
Leske, RA
Mason, GM
Mazur, JE
von Rosenvinge, TT
AF Mewaldt, R. A.
Looper, M. D.
Cohen, C. M. S.
Haggerty, D. K.
Labrador, A. W.
Leske, R. A.
Mason, G. M.
Mazur, J. E.
von Rosenvinge, T. T.
TI Energy Spectra, Composition, and Other Properties of Ground-Level Events
During Solar Cycle 23
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Sun: particle emission; Sun: coronal mass ejections (CMEs); Acceleration
of particles; Solar energetic particle acceleration; Sun: composition;
Ionic charge states
ID IONIC CHARGE STATES; CORONAL MASS EJECTIONS; ADVANCED COMPOSITION
EXPLORER; PARTICLE EVENTS; ISOTOPE SPECTROMETER; SHOCK ACCELERATION;
MAGNETIC-FIELD; DRIVEN SHOCKS; HOT PLASMA; PROTON
AB We report spacecraft measurements of the energy spectra of solar protons and other solar energetic particle properties during the 16 Ground Level Events (GLEs) of Solar Cycle 23. The measurements were made by eight instruments on the ACE, GOES, SAMPEX, and STEREO spacecraft and extend from similar to 0.1 to similar to 500-700 MeV. All of the proton spectra exhibit spectral breaks at energies ranging from similar to 2 to similar to 46 MeV and all are well fit by a double power-law shape. A comparison of GLE events with a larger sample of other solar energetic particle (SEP) events shows that the typical spectral indices are harder in GLE events, with a mean slope of -3.18 at > 40 MeV/nuc. In the energy range 45 to 80 MeV/nucleon about similar to 50 % of GLE events have properties in common with impulsive He-3-rich SEP events, including enrichments in Ne/O, Fe/O, Ne-22/Ne-20, and elevated mean charge states of Fe. These He-3-rich events contribute to the seed population accelerated by CME-driven shocks. An analysis is presented of whether highly-ionized Fe ions observed in five events could be due to electron stripping during shock acceleration in the low corona. Making use of stripping calculations by others and a coronal density model, we can account for events with mean Fe charge states of aOE (c) Q (Fe)> a parts per thousand+20 if the acceleration starts at similar to 1.24-1.6 solar radii, consistent with recent comparisons of CME trajectories and type-II radio bursts. In addition, we suggest that gradual stripping of remnant ions from earlier large SEP events may also contribute a highly-ionized suprathermal seed population. We also discuss how observed SEP spectral slopes relate to the energetics of particle acceleration in GLE and other large SEP events.
C1 [Mewaldt, R. A.; Cohen, C. M. S.; Labrador, A. W.; Leske, R. A.] CALTECH, Pasadena, CA 91125 USA.
[Looper, M. D.] Aerosp Corp, Los Angeles, CA 90009 USA.
[Haggerty, D. K.; Mason, G. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Mazur, J. E.] Aerosp Corp, Chantilly, VA 20151 USA.
[von Rosenvinge, T. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Mewaldt, RA (reprint author), CALTECH, Pasadena, CA 91125 USA.
EM rmewaldt@srl.caltech.edu
FU NASA at Caltech [NNX8AI11G, NNX06AC21G]; UC Berkeley under NASA
[SA2715-26309, NAS5-03131]
FX This work was supported by NASA at Caltech under grants NNX8AI11G and
NNX06AC21G, and under subcontract SA2715-26309 from UC Berkeley under
NASA contract NAS5-03131. We appreciate the availability of GOES data at
the NOAA website, SOHO CME data at the Catholic University website, and
thank Allan Tylka for advice on using HEPAD data. We are grateful for
helpful suggestions from both reviewers. Finally, we thank Nat
Gopalswamy and Nariaki Nitta for helpful discussions, for organizing the
two LWS workshops on GLEs, and for serving as editors for this volume.
NR 91
TC 46
Z9 46
U1 0
U2 4
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD OCT
PY 2012
VL 171
IS 1-4
BP 97
EP 120
DI 10.1007/s11214-012-9884-2
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 014CJ
UT WOS:000309352400006
ER
PT J
AU Li, G
Moore, R
Mewaldt, RA
Zhao, L
Labrador, AW
AF Li, G.
Moore, R.
Mewaldt, R. A.
Zhao, L.
Labrador, A. W.
TI A Twin-CME Scenario for Ground Level Enhancement Events
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Solar energetic particles; Ground level enhancement events; Diffusive
shock acceleration
ID ENERGETIC PARTICLE EVENTS; EJECTION-DRIVEN SHOCKS; CORONAL MASS
EJECTIONS; II RADIO-BURSTS; SOLAR-WIND; INTERPLANETARY SHOCKS;
HEAVY-IONS; CHARGE STATES; 1 AU; ACCELERATION
AB Ground Level Enhancement (GLEs) events are extreme Solar Energetic Particle (SEP) events. Protons in these events often reach similar to GeV/nucleon. Understanding the underlying particle acceleration mechanism in these events is a major goal for Space Weather studies. In Solar Cycle 23, a total of 16 GLEs have been identified. Most of them have preceding CMEs and in-situ energetic particle observations show some of them are enhanced in ICME or flare-like material. Motivated by this observation, we discuss here a scenario in which two CMEs erupt in sequence during a short period of time from the same Active Region (AR) with a pseudo-streamer-like pre-eruption magnetic field configuration. The first CME is narrower and slower and the second CME is wider and faster. We show that the magnetic field configuration in our proposed scenario can lead to magnetic reconnection between the open and closed field lines that drape and enclose the first CME and its driven shock. The combined effect of the presence of the first shock and the existence of the open close reconnection is that when the second CME erupts and drives a second shock, one finds both an excess of seed population and an enhanced turbulence level at the front of the second shock than the case of a single CME-driven shock. Therefore, a more efficient particle acceleration will occur. The implications of our proposed scenario are discussed.
C1 [Li, G.; Zhao, L.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Li, G.; Zhao, L.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Moore, R.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
[Mewaldt, R. A.; Labrador, A. W.] CALTECH, SRL, Pasadena, CA 91125 USA.
RP Li, G (reprint author), Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
EM gang.li@uah.edu
RI Li, Gang/B-4977-2012
OI Li, Gang/0000-0003-4695-8866
FU NSF [ATM-0847719]; NASA [NNX07AL52A, NNX8AI11G, NNX06AC21G]; ORAU
FX This work is supported in part by NSF ATM-0847719 (CAREER), NASA
NNX07AL52A (EpSCoR) and an ORAU Ralph E. Power Junior Faculty
Enhancement Award for GL at UAHuntsville. The work at Caltech was
supported by NASA grants under grants NNX8AI11G and NNX06AC21G. The
authors thank Dr. Nat Gopalswamy and Dr. Nariaki Nitta for organizing
the two GLE workshops where this work was largely completed.
NR 68
TC 37
Z9 41
U1 6
U2 11
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD OCT
PY 2012
VL 171
IS 1-4
BP 141
EP 160
DI 10.1007/s11214-011-9823-7
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 014CJ
UT WOS:000309352400008
ER
PT J
AU Arlen, T
Aune, T
Beilicke, M
Benbow, W
Bouvier, A
Buckley, JH
Bugaev, V
Byrum, K
Cannon, A
Cesarini, A
Ciupik, L
Collins-Hughes, E
Connolly, MP
Cui, W
Dickherber, R
Dumm, J
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
Holder, J
Huan, H
Hughes, G
Humensky, TB
Imran, A
Kaaret, P
Karlsson, N
Kertzman, M
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
Pohl, M
Prokoph, H
Quinn, J
Ragan, K
Reyes, LC
Reynolds, PT
Roache, E
Ruppel, J
Saxon, DB
Schroedter, M
Sembroski, GH
Skole, C
Smith, AW
Telezhinsky, I
Tesic, G
Theiling, M
Thibadeau, S
Tsurusaki, K
Varlotta, A
Vivier, M
Wakely, SP
Ward, JE
Weinstein, A
Welsing, R
Williams, DA
Zitzer, B
Pfrommer, C
Pinzke, A
AF Arlen, T.
Aune, T.
Beilicke, M.
Benbow, W.
Bouvier, A.
Buckley, J. H.
Bugaev, V.
Byrum, K.
Cannon, A.
Cesarini, A.
Ciupik, L.
Collins-Hughes, E.
Connolly, M. P.
Cui, W.
Dickherber, R.
Dumm, J.
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.
Holder, J.
Huan, H.
Hughes, G.
Humensky, T. B.
Imran, A.
Kaaret, P.
Karlsson, N.
Kertzman, M.
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.
Pohl, M.
Prokoph, H.
Quinn, J.
Ragan, K.
Reyes, L. C.
Reynolds, P. T.
Roache, E.
Ruppel, J.
Saxon, D. B.
Schroedter, M.
Sembroski, G. H.
Skole, C.
Smith, A. W.
Telezhinsky, I.
Tesic, G.
Theiling, M.
Thibadeau, S.
Tsurusaki, K.
Varlotta, A.
Vivier, M.
Wakely, S. P.
Ward, J. E.
Weinstein, A.
Welsing, R.
Williams, D. A.
Zitzer, B.
Pfrommer, C.
Pinzke, A.
TI CONSTRAINTS ON COSMIC RAYS, MAGNETIC FIELDS, AND DARK MATTER FROM
GAMMA-RAY OBSERVATIONS OF THE COMA CLUSTER OF GALAXIES WITH VERITAS AND
FERMI
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic rays; dark matter; galaxies: clusters: general; galaxies:
clusters: individual (Coma (ACO 1656)); gamma rays: galaxies: clusters;
magnetic fields
ID LARGE-SCALE STRUCTURE; ATMOSPHERIC CHERENKOV TELESCOPES; DIFFUSE
RADIO-EMISSION; ALL-SKY SURVEY; X-RAY; UPPER LIMITS; SHOCK-WAVES;
NONTHERMAL EMISSION; GALACTIC-CENTER; SOURCE CATALOG
AB Observations of radio halos and relics in galaxy clusters indicate efficient electron acceleration. Protons should likewise be accelerated and, on account of weak energy losses, can accumulate, suggesting that clusters may also be sources of very high energy (VHE; E > 100 GeV) gamma-ray emission. We report here on VHE gamma-ray observations of the Coma galaxy cluster with the VERITAS array of imaging Cerenkov telescopes, with complementing Fermi Large Area Telescope observations at GeV energies. No significant gamma-ray emission from the Coma Cluster was detected. Integral flux upper limits at the 99% confidence level were measured to be on the order of (2-5) x 10(-8) photonsm(-2) s(-1) (VERITAS, >220 GeV) and similar to 2 x 10(-6) photonsm(-2) s(-1) (Fermi, 1-3GeV), respectively. We use the gamma-ray upper limits to constrain cosmic rays (CRs) and magnetic fields in Coma. Using an analytical approach, the CR-to-thermal pressure ratio is constrained to be < 16% from VERITAS data and <1.7% from Fermi data (averaged within the virial radius). These upper limits are starting to constrain the CR physics in self-consistent cosmological cluster simulations and cap the maximum CR acceleration efficiency at structure formation shocks to be <50%. Alternatively, this may argue for non-negligible CR transport processes such as CR streaming and diffusion into the outer cluster regions. Assuming that the radio-emitting electrons of the Coma halo result from hadronic CR interactions, the observations imply a lower limit on the central magnetic field in Coma of similar to(2-5.5) mu G, depending on the radial magnetic field profile and on the gamma-ray spectral index. Since these values are below those inferred by Faraday rotation measurements in Coma (for most of the parameter space), this renders the hadronic model a very plausible explanation of the Coma radio halo. Finally, since galaxy clusters are dark matter (DM) dominated, the VERITAS upper limits have been used to place constraints on the thermally averaged product of the total self-annihilation cross section and the relative velocity of the DM particles, .
C1 [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.; Ward, J. E.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Benbow, W.; Galante, N.; Roache, E.; Schroedter, M.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cannon, A.; Collins-Hughes, E.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[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.
[Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 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.; Ruppel, J.; Skole, C.; Telezhinsky, I.; Welsing, R.] DESY, D-15738 Zeuthen, Germany.
[Federici, S.; Pohl, M.; Ruppel, J.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Finnegan, G.; Godambe, S.; Kieda, D.; 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.
[Griffin, S.; McCann, A.; Ragan, K.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[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.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Imran, A.; Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[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.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Perkins, J. S.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Perkins, J. S.] Univ Maryland, Ctr Space Sci & Technol, 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.
[Pfrommer, C.] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany.
[Pinzke, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
RP Arlen, T (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
EM pohlmadq@gmail.com; christoph.pfrommer@h-its.org
RI Khassen, Yerbol/I-3806-2015;
OI Khassen, Yerbol/0000-0002-7296-3100; Cui, Wei/0000-0002-6324-5772;
Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794
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; National Aeronautics and
Space Administration; Department of Energy in the United States;
Commissariat a l'Energie Atomique; Centre National de la Recherche
Scientifique/Institut National de Physique Nucleaire et de Physique des
Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di
Fisica Nucleare in Italy; Ministry of Education, Culture, Sports,
Science and Technology (MEXT); High Energy Accelerator Research
Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan;
K. A. Wallenberg Foundation; Swedish Research Council; Swedish National
Space Board in Sweden; Istituto Nazionale di Astrofisica in Italy;
Centre National d'Etudes Spatiales in France; Klaus Tschira Foundation;
NSF [AST-0908480]
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 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 operation phase is gratefully acknowledged from the Istituto
Nazionale di Astrofisica in Italy and the Centre National d'Etudes
Spatiales in France.; C. P. gratefully acknowledges financial support of
the Klaus Tschira Foundation. A. P. acknowledges NSF grant AST-0908480
for support.
NR 97
TC 43
Z9 43
U1 0
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2012
VL 757
IS 2
AR 123
DI 10.1088/0004-637X/757/2/123
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 010QF
UT WOS:000309108500016
ER
PT J
AU Corsaro, E
Stello, D
Huber, D
Bedding, TR
Bonanno, A
Brogaard, K
Kallinger, T
Benomar, O
White, TR
Mosser, B
Basu, S
Chaplin, WJ
Christensen-Dalsgaard, J
Elsworth, YP
Garcia, RA
Hekker, S
Kjeldsen, H
Mathur, S
Meibom, S
Hall, JR
Ibrahim, KA
Klaus, TC
AF Corsaro, Enrico
Stello, Dennis
Huber, Daniel
Bedding, Timothy R.
Bonanno, Alfio
Brogaard, Karsten
Kallinger, Thomas
Benomar, Othman
White, Timothy R.
Mosser, Benoit
Basu, Sarbani
Chaplin, William J.
Christensen-Dalsgaard, Jorgen
Elsworth, Yvonne P.
Garcia, Rafael A.
Hekker, Saskia
Kjeldsen, Hans
Mathur, Savita
Meibom, Soren
Hall, Jennifer R.
Ibrahim, Khadeejah A.
Klaus, Todd C.
TI ASTEROSEISMOLOGY OF THE OPEN CLUSTERS NGC 6791, NGC 6811, AND NGC 6819
FROM 19 MONTHS OF KEPLER PHOTOMETRY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE open clusters and associations: individual; stars: evolution; stars:
oscillations; techniques: photometric
ID SOLAR-LIKE OSCILLATIONS; MAIN-SEQUENCE STARS; INFRARED FLUX METHOD;
RED-GIANT STARS; 1ST 4 MONTHS; STELLAR OSCILLATIONS; HELIUM CONTENT;
PARAMETERS; COROT; DIAGRAMS
AB We studied solar-like oscillations in 115 red giants in the three open clusters, NGC 6791, NGC 6811, and NGC 6819, based on photometric data covering more than 19 months with NASA's Kepler space telescope. We present the asteroseismic diagrams of the asymptotic parameters delta nu(02), delta nu(01), and epsilon, which show clear correlation with fundamental stellar parameters such as mass and radius. When the stellar populations from the clusters are compared, we see evidence for a difference in mass of the red giant branch stars and possibly a difference in structure of the red clump stars, from our measurements of the small separations delta nu(02) and delta nu(01). Ensemble echelle diagrams and upper limits to the linewidths of l = 0 modes as a function of Delta nu of the clusters NGC 6791 and NGC 6819 are also shown, together with the correlation between the l = 0 ridge width and the T-eff of the stars. Lastly, we distinguish between red giant branch and red clump stars through the measurement of the period spacing of mixed dipole modes in 53 stars among all the three clusters to verify the stellar classification from the color-magnitude diagram. These seismic results also allow us to identify a number of special cases, including evolved blue stragglers and binaries, as well as stars in late He-core burning phases, which can be potentially interesting targets for detailed theoretical modeling.
C1 [Corsaro, Enrico] Univ Catania, Dept Phys & Astron, Astrophys Sect, I-95123 Catania, Italy.
[Corsaro, Enrico; Bonanno, Alfio] Astrophys Observ Catania, INAF, I-95123 Catania, Italy.
[Stello, Dennis; Huber, Daniel; Bedding, Timothy R.; Benomar, Othman; White, Timothy R.] Univ Sydney, SIfA, Sch Phys, Sydney, NSW 2006, Australia.
[Brogaard, Karsten] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada.
[Kallinger, Thomas] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Mosser, Benoit] Univ Paris 07, Univ Paris 06, LESIA Observ Paris, CNRS, F-92195 Meudon, France.
[Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Chaplin, William J.; Elsworth, Yvonne P.; Mathur, Savita] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Chaplin, William J.; Christensen-Dalsgaard, Jorgen; Garcia, Rafael A.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
[Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans] Aarhus Univ, DASC, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Garcia, Rafael A.] Univ Paris Diderot IRFU SAp, Lab AIM, CEA DSM CNRS, F-91191 Gif Sur Yvette, France.
[Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Mathur, Savita] NCAR, High Altitude Observ, Boulder, CO 80307 USA.
[Meibom, Soren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Hall, Jennifer R.; Ibrahim, Khadeejah A.; Klaus, Todd C.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
RP Corsaro, E (reprint author), Univ Catania, Dept Phys & Astron, Astrophys Sect, Via S Sofia 78, I-95123 Catania, Italy.
RI Bonanno, Alfio/J-1845-2012;
OI Kallinger, Thomas/0000-0003-3627-2561; Bonanno,
Alfio/0000-0003-3175-9776; Brogaard, Karsten/0000-0003-2001-0276;
Bedding, Timothy/0000-0001-5943-1460; Bedding, Tim/0000-0001-5222-4661;
Basu, Sarbani/0000-0002-6163-3472; Garcia, Rafael/0000-0002-8854-3776
FU NASA's Science Mission Directorate; European Community [269194];
Australian Research Council; Carlsberg Foundation; Netherlands
Organisation for Scientific Research (NWO); FWO-Flanders
[O6260-G.0728.11]; National Science Foundation [NSF PHY05-51164]
FX Funding for this Discovery mission is provided by NASA's Science Mission
Directorate. The authors thank the entire Kepler team, without whom this
investigation would not have been possible. The research leading to
these results has received funding from the European Community's Seventh
Framework Programme (FP7/2007-2013) under grant agreement No. 269194. D.
S. acknowledges support from the Australian Research Council. K. B.
acknowledges funding from the Carlsberg Foundation. S. H. acknowledges
financial support from the Netherlands Organisation for Scientific
Research (NWO). T. K. is supported by the FWO-Flanders under project
O6260-G.0728.11. NCAR is partially supported by the National Science
Foundation. This research was supported in part by the National Science
Foundation under grant No. NSF PHY05-51164. Data presented in this paper
are available upon request to the first author.
NR 60
TC 72
Z9 72
U1 2
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2012
VL 757
IS 2
AR 190
DI 10.1088/0004-637X/757/2/190
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 010QF
UT WOS:000309108500083
ER
PT J
AU de Martino, I
Atrio-Barandela, F
da Silva, A
Ebeling, H
Kashlinsky, A
Kocevski, D
Martins, CJAP
AF de Martino, I.
Atrio-Barandela, F.
da Silva, A.
Ebeling, H.
Kashlinsky, A.
Kocevski, D.
Martins, C. J. A. P.
TI MEASURING THE REDSHIFT DEPENDENCE OF THE COSMIC MICROWAVE BACKGROUND
MONOPOLE TEMPERATURE WITH PLANCK DATA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; cosmology: theory
ID BRIGHTEST CLUSTER SAMPLE; X-RAY SEARCH; GALAXY CLUSTERS; HYDRODYNAMICAL
SIMULATIONS; RADIATION TEMPERATURE; RADIO HALOS; MILKY-WAY; ZELDOVICH;
PROBE; COSMOLOGIES
AB We study the capability of Planck data to constrain deviations of the cosmic microwave background (CMB) blackbody temperature from adiabatic evolution using the thermal Sunyaev-Zeldovich anisotropy induced by clusters of galaxies. We consider two types of data sets depending on how the cosmological signal is removed: using a CMB template or using the 217 GHz map. We apply two different statistical estimators, based on the ratio of temperature anisotropies at two different frequencies and on a fit to the spectral variation of the cluster signal with frequency. The ratio method is biased if CMB residuals with amplitude similar to 1 mu K or larger are present in the data, while residuals are not so critical for the fit method. To test for systematics, we construct a template from clusters drawn from a hydro-simulation included in the pre-launch Planck Sky Model. We demonstrate that, using a proprietary catalog of X-ray-selected clusters with measured redshifts, electron densities, and X-ray temperatures, we can constrain deviations of adiabatic evolution, measured by the parameter alpha in the redshift scaling T(z) = T-0(1 + z)(1-alpha), with an accuracy of sigma(alpha) = 0.011 in the most optimal case and with sigma(alpha) = 0.018 for a less optimal case. These results represent a factor of 2-3 improvement over similar measurements carried out using quasar spectral lines and a factor 6-20 with respect to earlier results using smaller cluster samples.
C1 [de Martino, I.; Atrio-Barandela, F.] Univ Salamanca, E-37008 Salamanca, Spain.
[da Silva, A.; Martins, C. J. A. P.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Ebeling, H.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Kashlinsky, A.] NASA, Goddard Space Flight Ctr, SSAI, Greenbelt, MD 20771 USA.
[Kashlinsky, A.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Kocevski, D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
RP de Martino, I (reprint author), Univ Salamanca, E-37008 Salamanca, Spain.
EM ivan.demartino@usal.es; atrio@usal.es; asilva@astro.up.pt;
ebeling@ifa.hawaii.edu; alexander.kashlinsky@nasa.gov;
kocevski@physics.ucdavis.edu; Carlos.Martins@astro.up.pt
RI Da Silva, Antonio/A-2693-2010; de Martino, Ivan/B-4165-2015;
Atrio-Barandela, Fernando/A-7379-2017;
OI Da Silva, Antonio/0000-0002-6385-1609; de Martino,
Ivan/0000-0001-5948-9689; Atrio-Barandela, Fernando/0000-0002-2130-2513;
Martins, Carlos/0000-0002-4886-9261
FU FCT/MICINN [AIC10-D-000443]; FCT, Portugal [PTDC/FIS/111725/2009];
Ministerio de Educacion y Ciencia, Spain [FIS2009-07238, CSD
2007-00050]; Ciencia Research Contract; FCT/MCTES (Portugal); POPH/FSE
(EC)
FX This work was done in the context of the FCT/MICINN cooperation grant
"Cosmology and Fundamental Physics with the Sunyaev-Zeldovich Effect"
AIC10-D-000443, with additional support from project
PTDC/FIS/111725/2009 from FCT, Portugal and FIS2009-07238 and CSD
2007-00050 from the Ministerio de Educacion y Ciencia, Spain. The work
of C.M. is funded by a Ciencia2007 Research Contract, funded by
FCT/MCTES (Portugal) and POPH/FSE (EC).
NR 60
TC 11
Z9 11
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 OCT 1
PY 2012
VL 757
IS 2
AR 144
DI 10.1088/0004-637X/757/2/144
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 010QF
UT WOS:000309108500037
ER
PT J
AU Hartman, JM
Patruno, A
Chakrabarty, D
Markwardt, CB
Morgan, EH
van der Klis, M
Wijnands, R
AF Hartman, Jacob M.
Patruno, Alessandro
Chakrabarty, Deepto
Markwardt, Craig B.
Morgan, Edward H.
van der Klis, Michiel
Wijnands, Rudy
TI A DECADE OF TIMING AN ACCRETION-POWERED MILLISECOND PULSAR: THE
CONTINUING SPIN-DOWN AND ORBITAL EVOLUTION OF SAX J1808.4-3658 (vol 702,
pg 1673, 2009)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Patruno, Alessandro; van der Klis, Michiel; Wijnands, Rudy] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands.
[Chakrabarty, Deepto; Morgan, Edward H.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Chakrabarty, Deepto; Morgan, Edward H.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Markwardt, Craig B.] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA.
[Markwardt, Craig B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Hartman, Jacob M.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
EM jacob.hartman@nrl.navy.mil; a.patruno@uva.nl; deepto@space.mit.edu;
craigm@milkyway.gsfc.nasa.gov; ehm@space.mit.edu;
m.b.m.vanderklis@uva.nl; r.a.d.wijnands@uva.nl
NR 1
TC 0
Z9 0
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2012
VL 757
IS 2
AR 193
DI 10.1088/0004-637X/757/2/193
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 010QF
UT WOS:000309108500086
ER
PT J
AU Hirsch, L
Adams, JD
Herter, TL
Hora, JL
De Buizer, JM
Megeath, ST
Gull, GE
Henderson, CP
Keller, LD
Schoenwald, J
Vacca, W
AF Hirsch, Lea
Adams, Joseph D.
Herter, Terry L.
Hora, Joseph L.
De Buizer, James M.
Megeath, S. Thomas
Gull, George E.
Henderson, Charles P.
Keller, Luke D.
Schoenwald, Justin
Vacca, William
TI SOFIA/FORCAST AND SPITZER/IRAC IMAGING OF THE ULTRACOMPACT HII REGION
W3(OH) AND ASSOCIATED PROTOSTARS IN W3
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; HII regions; infrared: stars; radiative transfer;
stars: formation
ID GIANT MOLECULAR CLOUD; SPECTRAL ENERGY-DISTRIBUTIONS; YOUNG STELLAR
OBJECTS; ARRAY CAMERA IRAC; SPACE-TELESCOPE; STAR-FORMATION; EMISSION;
MASERS; AMMONIA; GRAINS
AB We present infrared observations of the ultracompact HII region W3(OH) made by the FORCAST instrument aboard the Stratospheric Observatory for Infrared Astronomy (SOFIA) and by the Spitzer/Infrared Array Camera. We contribute new wavelength data to the spectral energy distribution (SED), which constrains the optical depth, grain size distribution, and temperature gradient of the dusty shell surrounding the HII region. We model the dust component as a spherical shell containing an inner cavity with radius similar to 600 AU, irradiated by a central star of type O9 and temperature similar to 31,000 K. The total luminosity of this system is 7.1x10(4) L-circle dot. An observed excess of 2.2-x4.5 mu m emission in the SED can be explained by our viewing a cavity opening or clumpiness in the shell structure whereby radiation from the warm interior of the shell can escape. We claim to detect the nearby water maser source W3 (H2O) at 31.4 and 37.1 mu m using beam deconvolution of the FORCAST images. We constrain the flux densities of this object at 19.7-x37.1 mu m. Additionally, we present in situ observations of four young stellar and protostellar objects in the SOFIA field, presumably associated with the W3 molecular cloud. Results from the model SED fitting tool of Robitaille et al. suggest that two objects (2MASS J02270352+6152357 and 2MASS J02270824+6152281) are intermediate-luminosity (similar to 236-x432 L-circle dot) protostars; one object (2MASS J02270887+6152344) is either a high-mass protostar with luminosity 3 x 10(3) L-circle dot or a less massive young star with a substantial circumstellar disk but depleted envelope; and the other (2MASS J02270743+6152281) is an intermediate-luminosity (similar to 768 L-circle dot) protostar nearing the end of its envelope accretion phase or a young star surrounded by a circumstellar disk with no appreciable circumstellar envelope.
C1 [Hirsch, Lea; Adams, Joseph D.; Herter, Terry L.; Gull, George E.; Henderson, Charles P.; Schoenwald, Justin] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Hora, Joseph L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[De Buizer, James M.; Vacca, William] NASA, Ames Res Ctr, SOFIA Univ Space Res Assoc, Moffett Field, CA 94035 USA.
[Megeath, S. Thomas] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
[Keller, Luke D.] Ithaca Coll, Dept Phys, Ctr Nat Sci 264, Ithaca, NY 14850 USA.
RP Hirsch, L (reprint author), Cornell Univ, Dept Astron, 105 Space Sci Bldg, Ithaca, NY 14853 USA.
OI Hora, Joseph/0000-0002-5599-4650
FU NASA [NAS2-97001, 8500-98-014]; Deutsches SOFIA Institut (DSI) under DLR
[50 OK 0901]; USRA; National Science Foundation
FX We thank R. Grashius, S. Adams, H. Jakob, A. Reinacher, and U. Lampeter
for their SOFIA telescope engineering and operations support. We also
thank the SOFIA flight crews and mission operations team (A. Meyer, N.
McKown, C. Kaminski) for their SOFIA flight planning and flight support.
We are grateful to an anonymous referee for his or her comments which
have improved this manuscript. This work is based on observations made
with the NASA/DLR Stratospheric Observatory for Infrared Astronomy
(SOFIA). SOFIA science mission operations are conducted jointly by the
Universities Space Research Association, Inc. (USRA), under NASA
contract NAS2-97001, and the Deutsches SOFIA Institut (DSI) under DLR
contract 50 OK 0901. Financial support for FORCAST was provided to
Cornell by NASA through award 8500-98-014 issued by USRA. 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. 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, 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, which is operated by
the Jet Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. This
research has made use of NASA's Astrophysics Data System Abstract
Service.
NR 40
TC 8
Z9 8
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2012
VL 757
IS 2
AR 113
DI 10.1088/0004-637X/757/2/113
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 010QF
UT WOS:000309108500006
ER
PT J
AU Isensee, K
Olmschenk, G
Rudnick, L
DeLaney, T
Rho, J
Smith, JD
Reach, WT
Kozasa, T
Gomez, H
AF Isensee, Karl
Olmschenk, Greg
Rudnick, Lawrence
DeLaney, Tracey
Rho, Jeonghee
Smith, J. D.
Reach, William T.
Kozasa, Takashi
Gomez, Haley
TI NUCLEOSYNTHETIC LAYERS IN THE SHOCKED EJECTA OF CASSIOPEIA A
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: ISM; ISM: individual objects (Cassiopeia A); ISM: supernova
remnants; supernovae: general; X-rays: ISM
ID A SUPERNOVA REMNANT; CORE-COLLAPSE SUPERNOVAE; X-RAY; 3-DIMENSIONAL
STRUCTURE; INSTABILITIES; CONSTRAINTS; EXPLOSION; ASYMMETRY; STABILITY;
SPECTRA
AB We present a three-dimensional analysis of the supernova remnant Cassiopeia A using high-resolution spectra from the Spitzer Space Telescope. We observe supernova ejecta both immediately before and during the shock-ejecta interaction. We determine that the reverse shock of the remnant is spherical to within 7%, although the center of this sphere is offset from the geometric center of the remnant by 810 km s(-1). We determine that the velocity width of the nucleosynthetic layers is similar to 1000 km s(-1) over 4000 arcsec(2) regions, although the velocity width of a layer along any individual line of sight is <250 km s(-1). Si and O, which come from different nucleosynthetic layers in the progenitor star, are observed to be coincident in velocity space in some directions, but segregated by up to similar to 500 km s(-1) in other directions. We compare these observations of the nucleosynthetic layers to predictions from supernova explosion models in an attempt to constrain such models. Finally, we observe small-scale, corrugated velocity structures that are likely caused during the supernova explosion itself, rather than hundreds of years later by dynamical instabilities at the remnant's reverse shock.
C1 [Isensee, Karl; Olmschenk, Greg; Rudnick, Lawrence] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
[DeLaney, Tracey] W Virginia Wesleyan Coll, Dept Phys & Engn, Buckhannon, WV 26201 USA.
[Rho, Jeonghee] NASA, SOFIA Sci Ctr, Univ Space Res Assoc, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Smith, J. D.] Univ Toledo, Ritter Astrophys Observ, Toledo, OH 43606 USA.
[Reach, William T.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Kozasa, Takashi] Hokkaido Univ, Grad Sch Sci, Dept Cosmosci, Sapporo, Hokkaido 0600810, Japan.
[Gomez, Haley] Univ Wales Coll Cardiff, Sch Phys & Astron, Cardiff CF24 3YB, S Glam, Wales.
RP Isensee, K (reprint author), Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
EM isensee@astro.umn.edu; delaney_t@wvwc.edu; jrho@sofia.usra.edu;
jd.smith@utoledo.edu; reach@ipac.caltech.edu;
kozasa@mail.sci.hokudai.ac.jp; haley.morgan@astro.cf.ac.uk
RI Kozasa, Takashi/A-5213-2012;
OI Reach, William/0000-0001-8362-4094
FU NASA [1407]; NASA/SAO [AR5-6008X]; NASA/JPL [1265552]
FX This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under NASA contract 1407. This work
was supported in part by NASA/SAO Award No. AR5-6008X and NASA/JPL
through award 1265552 to the University of Minnesota.
NR 47
TC 10
Z9 10
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2012
VL 757
IS 2
AR 126
DI 10.1088/0004-637X/757/2/126
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 010QF
UT WOS:000309108500019
ER
PT J
AU Johnson, TV
Mousis, O
Lunine, JI
Madhusudhan, N
AF Johnson, Torrence V.
Mousis, Olivier
Lunine, Jonathan I.
Madhusudhan, Nikku
TI PLANETESIMAL COMPOSITIONS IN EXOPLANET SYSTEMS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: formation; planets and satellites: general;
protoplanetary disks
ID OUTER SOLAR-SYSTEM; HEAVY ELEMENT CONTENT; EXTRASOLAR PLANETS;
REFRACTORY ELEMENTS; KINETIC INHIBITION; INTERSTELLAR ICES; JOVIAN
SUBNEBULA; CARBON-MONOXIDE; HARBORING STARS; N-2 REDUCTION
AB We have used recent surveys of the composition of exoplanet host stars to investigate the expected composition of condensed material in planetesimals formed beyond the snow line in the circumstellar nebulae of these systems. Of the major solid-forming elements, C and O abundances (and particularly the C/O abundance ratio) strongly affect the amounts of volatile ices and refractory phases in icy planetesimals formed in these systems. This results from these elements' effects on the partitioning of O among gas, refractory solid and ice phases in the final condensate. The calculations use a self-consistent model for the condensation sequence of volatile ices from the nebula gas after refractory (silicate and metal) phases have condensed. The resultant mass fractions (compared to the total condensate) of refractory phases and ices were calculated for a range of nebular temperature structures and redox conditions. Planetesimals in systems with sub-solar C/O should be water ice-rich, with lower than solar mass fractions of refractory materials, while in super-solar C/O systems planetesimals should have significantly higher mass fractions of refractories, in some cases having little or no water ice. C-bearing volatile ices and clathrates also become increasingly important with increasing C/O depending on the assumed nebular temperatures. These compositional variations in early condensates in the outer portions of the nebula will be significant for the equivalent of the Kuiper Belt in these systems, icy satellites of giant planets, and the enrichment (over stellar values) of volatiles and heavy elements in giant planet atmospheres.
C1 [Johnson, Torrence V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mousis, Olivier] Univ Franche Comte, Observ THETA, Inst UTINAM, UMR CNRS 6213, F-25010 Besancon, France.
[Mousis, Olivier] Univ Toulouse, UPS OMP, CNRS INSU, IRAP, F-31400 Toulouse, France.
[Lunine, Jonathan I.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Madhusudhan, Nikku] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA.
RP Johnson, TV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM torrence.v.johnson@jpl.nasa.gov
FU NASA HST grant; NASA JPL/Spitzer grant; NASA; CNES
FX T.V.J.'s work was done at the Jet Propulsion Laboratory, California
Institute of Technology under a contract from NASA. Government
sponsorship acknowledged. N.M. acknowledges support from NASA HST and
JPL/Spitzer grants. J.I.L. was supported by the James Webb Space
Telescope Project through NASA. O.M. acknowledges support from CNES. We
also thank an anonymous referee for helpful comments and Dr. Neal Turner
for discussions of the warm nebula models.
NR 49
TC 30
Z9 30
U1 1
U2 15
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2012
VL 757
IS 2
AR 192
DI 10.1088/0004-637X/757/2/192
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 010QF
UT WOS:000309108500085
ER
PT J
AU Kwon, RY
Chae, J
Davila, JM
Zhang, J
Moon, YJ
Poomvises, W
Jones, SI
AF Kwon, Ryun-Young
Chae, Jongchul
Davila, Joseph M.
Zhang, Jie
Moon, Yong-Jae
Poomvises, Watanachak
Jones, Shaela I.
TI THREE-DIMENSIONAL STRUCTURE AND EVOLUTION OF EXTREME-ULTRAVIOLET BRIGHT
POINTS OBSERVED BY STEREO/SECCHI/EUVI
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: transition region; Sun: UV radiation
ID EPHEMERAL ACTIVE REGIONS; MAGNETIC RECONNECTION; TEMPORAL VARIATIONS;
OBSERVED HEIGHTS; TRANSITION ZONE; SOLAR-FLARE; QUIET-SUN; FLUX;
CANCELLATION; FEATURES
AB We unveil the three-dimensional structure of quiet-Sun EUV bright points and their temporal evolution by applying a triangulation method to time series of images taken by SECCHI/EUVI on board the STEREO twin spacecraft. For this study we examine the heights and lengths as the components of the three-dimensional structure of EUV bright points and their temporal evolutions. Among them we present three bright points which show three distinct changes in the height and length: decreasing, increasing, and steady. We show that the three distinct changes are consistent with the motions (converging, diverging, and shearing, respectively) of their photospheric magnetic flux concentrations. Both growth and shrinkage of the magnetic fluxes occur during their lifetimes and they are dominant in the initial and later phases, respectively. They are all multi-temperature loop systems which have hot loops (similar to 10(6.2) K) overlying cooler ones (similar to 10(6.0) K) with cool legs (similar to 10(4.9) K) during their whole evolutionary histories. Our results imply that the multi-thermal loop system is a general character of EUV bright points. We conclude that EUV bright points are flaring loops formed by magnetic reconnection and their geometry may represent the reconnected magnetic field lines rather than the separator field lines.
C1 [Kwon, Ryun-Young; Poomvises, Watanachak] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
[Kwon, Ryun-Young; Davila, Joseph M.; Poomvises, Watanachak; Jones, Shaela I.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Chae, Jongchul] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul, South Korea.
[Zhang, Jie] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA.
[Moon, Yong-Jae] Kyung Hee Univ, Sch Space Res, Yongin 446701, South Korea.
[Jones, Shaela I.] Univ Maryland, Dept Phys, College Pk, MD 20740 USA.
RP Kwon, RY (reprint author), Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, 620 Michigan Ave, Washington, DC 20064 USA.
EM ryunyoung.kwon@nasa.gov
RI Moon, Yong-Jae/E-1711-2013
FU NASA [NNX10AN10G]; Korea Research Foundation; Korean Government
[KRF-2008-220-C00022]
FX We are grateful to the referee for a number of constructive comments.
This work was supported by NASA grant NNX10AN10G and the Korea Research
Foundation Grant funded by the Korean Government (KRF-2008-220-C00022).
NR 32
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 OCT 1
PY 2012
VL 757
IS 2
AR 167
DI 10.1088/0004-637X/757/2/167
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 010QF
UT WOS:000309108500060
ER
PT J
AU Loewenstein, M
Davis, DS
AF Loewenstein, Michael
Davis, David S.
TI AN IN-DEPTH STUDY OF THE ABUNDANCE PATTERN IN THE HOT INTERSTELLAR
MEDIUM IN NGC 4649
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: abundances; galaxies: elliptical and lenticular, cD; galaxies:
individual (NGC 4649); X-rays: galaxies
ID EARLY-TYPE GALAXIES; X-RAY BINARIES; RECENT STAR-FORMATION; STELLAR
POPULATION HISTORIES; OBSERVATORY SUPERNOVA SEARCH; GALACTIC CHEMICAL
EVOLUTION; DELAY-TIME DISTRIBUTION; RED-SEQUENCE GALAXIES; NEARBY
EARLY-TYPE; SIMILAR-TO 2
AB We present our X-ray imaging spectroscopic analysis of data from deep Suzaku and XMM-Newton Observatory exposures of the Virgo Cluster elliptical galaxy NGC 4649 (M60), focusing on the abundance pattern in the hot interstellar medium (ISM). All measured elements show a radial decline in abundance, with the possible exception of O. We construct steady-state solutions to the chemical evolution equations that include infall in addition to stellar mass return and Type Ia supernova (SNIa) enrichment, and consider recently published SNIa yields. By adjusting a single model parameter to obtain a match to the global abundance pattern in NGC 4649, we infer that introduction of subsolar metallicity external gas has reduced the overall ISM metallicity and diluted the effectiveness of SNIa to skew the pattern toward low alpha/Fe ratios, and estimate the combination of SNIa rate and level of dilution. Evidently, newly introduced gas is heated as it is integrated into, and interacts with, the hot gas that is already present. These results indicate a complex flow and enrichment history for NGC 4649, reflecting the continual evolution of elliptical galaxies beyond the formation epoch. The heating and circulation of accreted gas may help reconcile this dynamic history with the mostly passive evolution of elliptical stellar populations. In an Appendix, we examine the effects of the recent updated atomic database AtomDB in spectral fitting of thermal plasmas with hot ISM temperatures in the elliptical galaxy range.
C1 [Loewenstein, Michael] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Davis, David S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Loewenstein, Michael; Davis, David S.] NASA GSFC, CRESST, Greenbelt, MD USA.
[Loewenstein, Michael] NASA GSFC, Astroparticle Phys Lab, Greenbelt, MD USA.
[Davis, David S.] NASA GSFC, Xray Astrophys Lab, Greenbelt, MD USA.
RP Loewenstein, M (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM Michael.Loewenstein.1@nasa.gov; David.S.Davis@nasa.gov
RI XRAY, SUZAKU/A-1808-2009
FU NASA ADAP; Suzaku GO program; XMM-Newton GO program
FX We are grateful to Adam Foster, and Randall Smith for their input
regarding atomic physics issues. This work could not have been completed
without support from NASA ADAP, and Suzaku, and XMM-Newton GO programs,
and was improved by feedback from a constructive referee's report.
NR 131
TC 7
Z9 7
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2012
VL 757
IS 2
AR 121
DI 10.1088/0004-637X/757/2/121
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 010QF
UT WOS:000309108500014
ER
EF